Home

Manual

1. 5 1 2 The data selection widget 51 3 Flageinp 4 ko WR a ng 5 1 4 Logical editing and flag tables on nn nn 5 2 JAstrometry ox wu X R Xed ale uk MRE WE RO oe gis a RUE S 5 85 SpeciroscODy bue dde ae Henke E das Rr A RET RC de Sot ea de 5 4 3Photometky la aat rae e desde Re PL ie oo 4 11 13 13 14 14 15 15 15 16 17 17 17 18 18 18 19 19 21 21 21 22 6 Programmers reference 6 1 Code 8 Introduction 7 1 About AMOEBA 7 2 Data files 7 2 1 Interferometry 7 2 2 7 2 3 Spectroscopy 7 2 4 7 3 7 4 Stellar models 7 4 1 7 4 2 Uniform disks 7 4 3 Limb darkened disks 7 4 4 7 4 5 7 4 6 Rotating stars 7 4 7 7 5 Fit scenarios 7 5 1 7 5 2 7 5 3 7 5 4 7 5 5 7 6 Pass band integrations Basic widget procedures Load data Manipulation of a model 8 1 8 2 8 3 Command line procedures 9 1 Interferometry data buffering 6 1 1 6 1 2 Fit routines ASTROMETRYFIT INTERFEROMETRYFIT CONTROL sii B zede telen a SEEN WW 8 3 1 8 3 2 8 3 3 Script library files ek eA ANNE A 6 1 3 Mixed and FORTRAN libraries Astrometry Photometry 27 lata UR The Hierarchical Stellar Systems Model Format Uncorrelated flux component Miscellaneous stellar disks Images tak en ne Ee Young stellar objects and disks Single lined spectroscopic binary Double lined spe
2. Coherent integration Dispersion Metrology corrections A standard recipe ri vo fab Sad ran YW RE 20 6 Imaging simulations attente A UR 21 HDS procedures 21 1 hds_ 21 2 cmp 21 3 dat_ 22 Programmers reference 221 Widget TOUGINGS er at aant Ik dur re eub coi Aye DOR 22 1 1 22 1 2 22 1 3 22 1 4 22 1 5 22 1 6 22 1 7 22 1 8 22 1 9 FILE feta A A px a ACCESS BROWSE 5 3X atadas E E ii EA ACCESS INTEREEROMETRY AGOESSIPOINTDAPA a E es lea ACCESS WRITES e Dora os o ae Yuri Ca REDUCE anita ard nn a a a t ow Ert s REDUCE POINTDATAP LOD Pa a o EUER GATIBRATE u at a ee We Ri ne a es CATADOR A ee dn era 22 LO WAVE g Lx Pec do do Me gs 97 97 97 98 99 100 100 101 102 102 102 103 104 105 107 107 107 108 108 109 109 109 109 110 110 110 111 113 113 113 114 8 CONTENTS 22 2 Organization of data ss so 22 2 0 a2 an A EI 118 22 3 Array configuration ooa e 119 22 3 1 Optical path lengths s ccor GG uag 119 22 3 2 Basic definitions and sign conventions 119 22 4 Command line procedures 120 22 5 Plotting en RUE A a A Se ee 120 22 5 1 Adding plot variabl
3. Te eit de dei ur em Ry he 95 18 6 Utilities a et erpen do SERERE MU SRG e et OD eh NOG 95 18 6 1 Catalog access 96 CONTENTS 19 Command line procedures 19 1 Accessing data hlesi scs As a Ue esc dde Res BIR ARI s 19 1 1 19 1 2 19 1 3 Loading configuration and logs nn Loading tables tcs ete ed a kg tee ee i AR O Leading data er ip EA Ai s 19 2 PointData manipulation 19 2 1 19 2 2 ASLLOMELEY b E A d RO Jo a es M edd 2 Other ra A ii ET a ge ao A 19 3 Writing HDS objects ne 19 4 Analysis 19 5 List procedures s sons 1 2 0 moon BE Be ea ADR 19 6 Date conversion functions 19 7 Astrometry procedures FF ee 19 8 Data base Toutines 2 2 MGE a ae WY FD rydw iue Ty yW s 20 Discussion of reduction issues 2021 SUb arTays a eg e r dru Ii Rd A UE be AYER YR a ate ds d Dd 20 2 Bias correction of visibilities 22 22 I GG G G9 uu ua Y Y Ya 20 3 Photometry aS 2a Ru Ay nn 20 4 Calibration of visibilities oo nn 20 5 Astrometry data 20 5 1 20 5 2 20 5 3 20 5 4 20 5 5 20 5 6 Introduction a er Y WYD en Ke yl Y RS CONSTRICTOR parameters for astrometric reductions
4. To rename the entire STARID field of STARTABLE use rename_starids for example rename_starids fkv hdn In the last example the command will cause STARBASE to access the crossindex for all entries with an FKV ID and try to produce HDN IDs If an HDN ID is already available in the table this will also cause the STARID field to be renamed Note this behaviour might be changed in an upcoming release Chapter 14 Widget procedures There are currently only two widget routines installed 14 1 Spectrum plotter This widget allows to plot spectra read from a Library of Stellar Spectra by Jacoby Hunter and Christian 1984 and to identify lines of various elements and molecules lotspectrum Invoke spectrum plotter widget 14 2 Startable editor Starts a GUI to edit the contents of a specific entry of the startable update_startable starid Invoke update widget 69 70 CHAPTER 14 WIDGET PROCEDURES Part IV STARWHEEL Chapter 15 Introduction STARWHEEL is a container name for utilities related to observing list preparations including simulations The actual creation of the NPOI observing list is performed by the stand alone Python based obsprep software 15 1 Simulations A set of procedures described in Section 15 2 of this manual is used to create a star table Note that the plotuptime procedure which produces a plot with the rise and set times of the stars does not currently take the delay limit
5. lt long dims long values dat getnr ndim long dims long values dat getni ndim long dims long values dat clen clen dat size size dat prim reply dat_there name lt _char gt reply dat_erase name lt _char gt dat_new0c name lt _char gt len lt _long gt dat_new name lt _char gt type lt _char gt ndim lt _long gt dims lt _long gt HDS PROCEDURES Chapter 22 Programmer s reference 22 1 Widget routines In the following we will list the IDL widget procedures connected to buttons in the main widget The names of all these procedures start with ww 22 1 1 FILE ww file ww fileopen ww filecancel ww filehelp 22 1 2 AccESS BROWSE WW_access ww_look ww lookdestroyed ww find 22 1 3 ACCESS INTERFEROMETRY WW_access get_GenConfig get Date get SystemId get Format get GeoParms get scantable get bgtable 115 cont d 116 CHAPTER 22 get_bgscans get_ObserverLog get_ConstrictorLog 22 1 4 ACCESS POINTDATA WW_access ww_loadstarsel ww_loadstar 22 1 5 ACCEss WRITE ww_write put_Syslog put_ConstrictorLog put_GeoParms put_GenConfig put_ScanData put_mark3data 22 1 6 REDUCE ww_reduce ww_reducept ww_reducebg ww reducedl 22 1 7 REDUCE POINTDATA PLOT ww reducept init plotsel ww plot ww plotdestroyed ww plotoptions ww plothelp ww plotok ww plot ww setxaxis ww setyaxis PROGRAMMER S REFERENCE cont d cont d 22 1 W
6. A o RR URL A X 66 13 7 Danib darkening daat LIBE RUE Wed 66 13 8 Derived parameters 67 13 8 1 Absolute 67 19 02 Dist nces aa RU S E A A 67 138 3 Diameters ura soa ae a dn ard A A Elie er as 67 13 8 4 Orbital inclinations semi major axes and secondary masses 68 13 9 Cross indices nui xu a BA md 68 14 Widget procedures 69 14 1 Spectrum Plotter ROUEN eeu b gebe uM 69 14 2 Startable editor 2 22 8 8 2 er EE ae peers 69 IV STARWHEEL 71 15 Introduction 73 15 1 Simulations ee a 2 els a ad a A 73 15 2 Observing list preparation 73 6 CONTENTS V CHAMELEON 77 16 Introduction 79 16 1 About CHAMELEON 79 16 2 Data and auxiliary files I GG I eee eee 79 16 3 A Eee dy ee M S 80 16 3 1 Introduction and command syntax 80 16 32 Output files emita deet qub Parks la ue s 81 16 28 Flag tables ok and ox ob lea dne how db wet 81 16 94 Bias Correction 3 2 o9 en AD e or deg Edi UR LA BS 81 16 3 5 Phase unwrapping 81 16 3 6 Logging and quality 81 17 Quick Guide 83 Open the data shle Aan ost ees e foe P ae e eos 83 17 2 Read configuration information
7. REDUCE POINT DATA ASTROMETRY PHASEWRAP Unwrap the phases as a function of chan nel REDUCE POINT DATA ASTROMETRY DISPCORR Compute dispersion correction REDUCE POINT DATA ASTROMETRY PLOT Plot VACDELAY i e the dispersion corrected delay relative to the predicted geometric delay and flag Use PLOT AUTO The reference station values are zero by definition hds_open 2001 03 16 inch Open INCHWORM file get_metroconfig get motiongroup 1 hds close pivotfit An optional step which fits siderostat pivot coordinates RMS residuals should be on the order of a couple of microns After this step plotting ParXYZ corr will display the residuals see next step REDUCE INCH DATA PLOT Plot azimuth versus elevation connecting data points with lines Smooth curves should be the result This is a test whether proper siderostat models are loaded Also plot ParX Y Z to look for outliers REDUCE INCH DATA INIT For now we plan on computing and applying the metrology cor rection after averaging so we have to initialize the metrology correction to zero for the calibrated delays not to be flagged during averaging average inchav CALIBRATE ASTROMETRY METROCORR Compute and apply constant term and pivot correc tions CALIBRATE ASTROMETRY SOLVE Compute astrometric solutions 20 6 Imaging simulations To use OYSTER for imaging simulations first create a data set using the fakedata procedure This will create scans for w
8. NumCorr NumPar NumPar 1 2 Corr NumCorr lt _char gt ReducedChi2 NumTime lt _double gt XCorr NumTime NumCorr lt _double gt NumSingVal NumTime lt _integer gt SingValFlag NumTime NumPar lt _integer gt WRatio NumTime NumPar lt _double gt Par NumTime NumPar lt _double gt ParFitErr NumTime NumPar lt _double gt ParThErr NumTime NumPar lt _double gt MotCorrFlags NumFlag lt _char gt OpticalAnchor NumPlate NumPar lt integer NumPar 6 Par NumPar lt _char gt NumCorr lt _integer gt NumCorr NumPar NumPar 1 2 Corr NumCorr lt _char gt ReducedChi2 NumTime lt _double gt XCorr NumTime NumCorr lt _double gt NumSingVal NumTime lt _integer gt SingValFlag NumTime NumPar lt _integer gt WRatio NumTime NumPar lt _double gt Par NumTime NumPar lt _double gt ParFitErr NumTime NumPar lt _double gt ParThErr NumTime NumPar lt _double gt MotCorrFlags NumFlag lt _char gt Pier2Pier NumPar lt _integer gt NumPar 3 NumPlate 1 Par NumPar lt _char gt NumCorr lt _integer gt NumCorr NumPar NumPar 1 2 Corr NumCorr lt _char gt ReducedChi2 NumTime lt _double gt XCorr NumTime NumCorr lt _double gt NumSingVal NumTime lt _integer gt SingValFlag NumTime NumPar lt _integer gt WRatio NumTime NumPar lt _double gt Par NumTime NumPar lt _double gt ParFitErr NumTime NumPar lt _double gt ParThErr NumT
9. e ZEROSPACING float Zerospacing visibility e AO Linear limb darkening fit coefficient absolut e Al Linear limb darkening fit coefficient linear 58 CHAPTER 11 INTRODUCTION e A2 Linear limb darkening fit coefficient quadratic e MASSI float Mass of component 1 Mo e MASS2 float Mass of component 2 Mo e string Binary flag B calibrator C other e HFLAG string Hipparcos status flag e g C component sol e SFLAG string Status flag as a result of computations OK or e MODEL string Model on which diameter is based e g LD e REFERENCE string General diameter reference e g 080 D 0514 11 3 Available primary catalogs e HIC Hipparcos Input Catalogue HIC HDN RA DEC PMRA PMDEC RV PX MV BV SPECTRUM TYPE1 TYPE2 CLASS1 CLASS2 e SAO Smithsonian Astrophysical Observatory Star Catalogue National Space Science Data Center 1990 SAO HDN RA DEC PMRA PMDEC MV SPECTRUM TYPE1 TYPE2 e HDN Sky Catalogue 2000 0 Volume 1 Second Edition Sky Publishing Corp 1991 NAME HDN SAO ADS RA DEC PMRA PMDEC RV PX MV BV SPECTRUM TYPE1 TYPE2 CLASS1 CLASS2 11 3 AVAILABLE PRIMARY CATALOGS 59 e FKV Fundamental Katalog No 5 FKV HDN RA DEC PMRA PMDEC RV PX MV SPECTRUM TYPE1 TYPE2 e BSC Bright Star Catalogue 4th Edition Hoffleit 1982 National Spac
10. limb stars Compute limb darkening fit coefficients for all stars limb_star spectrum lt _char gt filter lt _char gt 13 8 DERIVED PARAMETERS 67 Function Return linear limb darkening coefficient integrated over specified band pass Example print limb star GOl V limb filter teff real log g real filter lt _char gt Function Return linear limb darkening coefficient integrated over specified band pass Example print limbfilter 5500 0 5 R limbband teff real log g real center real width real Function Return linear limb darkening coefficient integrated over band pass with specified center and full width in nm Example print limbband 5000 0 5 700 25 limbfactor coeff real Function Return factor to multiply the uniform disk diameter with in order to get a limb darkened diameter using the specified linear limb darkening coefficient Based on the squared visibility matching at 0 3 and a formula derived by Hanbury Brown 1974 MNRAS 1067 475 13 8 Derived parameters 13 8 1 Absolute magnitudes Absolute magnitudes are derived from the spectral type or trigonometric parallax For dwarfs it can also be computed from the B V color index a stars Derive absolute visual magnitude from apparent magnitude and parallax 13 8 2 Distances d stars Compute distance D from parallax absolute magnitude or both 13 8 3 Diameters Diameters computed with the following
11. ThetaErr NumLaser lt integer Phi NumLaser lt integer PhiErr NumLaser lt integer LaunchInfo NumLaser 162 APPENDIX B CONSTRICTOR OUTPUT FILE STRUCTURE NumGlass lt _integer gt NumAirGap lt _integer gt Loc 3 lt _double gt LocErr 3 lt _double gt GlassThick NumGlass lt _double gt GlassThickErr NumGlass lt _double gt GlassCode NumGlass lt _integer gt ExFrac NumGlass lt _double gt ExFracErr NumGlass lt _double gt AirGapThick NumAirGap lt _double gt AirGapThickErr NumAirGap lt _double gt RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass lt _double gt AirGapThick NumAirGap lt _double gt AirGapThickErr NumAirGap lt _double gt Pier2PierConfig NumLaser lt _integer gt CountsPerWaveln lt _integer gt LaserWavelength lt _double gt SampleInterval lt _integer gt IFBox NumLaser lt _integer gt Channel NumLaser lt _integer gt Theta NumLaser lt _integer gt ThetaErr NumLaser lt _integer gt Phi NumLaser lt _integer gt PhiErr NumLaser lt _integer gt LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt dou
12. addstar FKV0621 FKV0641 Also sorts the stars by ID removestar stars lt _char gt Remove one or more stars from the startable addcal star lt _char gt vlimit lt _real gt Lookup a calibrator for given star The nearest calibrator based on classification in diameter bsc with a visual magnitude brighter than vlimit default 4 5 is added to the startable compileobslist Rename stars in startable to their FKV equivalents if possible read the catalogs get auxilliary information and re order stars 15 2 OBSERVING LIST PREPARATION T5 plotuptime from_data lt _int gt stations stations stars stars Compute visibility for stars in startable and plot If from_data 1 plot actual visi bility for currently loaded scan data A list of stars can be passed to this procedure which is a shurtcut over allocation with get startable If stations are not defined a four station astrometric array is assumed writeobslist from data int time time Compute visibility and write startable with auxilliary information to file The name of the file is derived from the date the extension is obs The RA and declination fields in the observing list now refer to a suitable background i e blank sky location compile_astrometry Compile astrometry observing list 76 CHAPTER 15 INTRODUCTION Part V CHAMELEON Chapter 16 Introduction 16 1 About CHAMELEON The CHAMELEON collection of scripts as part
13. lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double MetPressConf NumPlate NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double MetHumConf NumPlate NumSensor lt integer APPENDIX E INCHWORM FILE STRUCTURE 177 SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 double LabAirTempConf NumSensor integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double LabSolidTmpConf NumSensor lt integer SampleInterval integer Chain NumS
14. y in Str mgren system MI float m1 of Str mgren system C1 float cl of Str mgren system BETA float 8 index of Str mgren system FEH float Fe H PMRA float Centennial proper motion in RA s PMDEC float Centennial proper motion in DEC RV float Radial velocity km s PX float Parallax PXE float Error of parallax D float Distance pc 11 2 THE FORMAT OF STARTABLE 57 e SPECTRUM string Spectrum e float Floating point spectral type of component 1 e TYPE2 float Floating point spectral type of component 2 e CLASSI float Floating point luminosity class of component 1 e CLASS2 float Floating point luminosity class of component 2 e float Effective temperature of component 1 K e TEFF2 float Effective temperature of component 2 K e LOGGI float Surface gravity of component 1 cgs e LOGG2 float Surface gravity of component 2 cgs e P float Orbital period d T double JD epoch of periastron e O float Argument of periastron deg of primary e E float Orbital eccentricity e I float Orbital inclination deg e N float Argument of ascending node deg e A float Semi major axis e Kl float km s e K2 float km s e VO float km s e MF float Mass function for single lined binaries e MISIN3I float km e M2SIN3I float km s e AISINI float km e A2SINI float km e DIAMETER float Stellar diameter mas
15. z are available 5 1 1 The plot selection widget Here you define what is plotted along the axes for which stars and other various options If the choice for an axis required additional selection on what range of data indices to plot another widget the data selection widget will open see below If more than one channel baseline or point is selected multiple plots will appear in the plot widget for those indices not corresponding to the selected slice the SLICE menu is optional in 23 24 CHAPTER 5 PLOTTING AND EDITING classes scan and astrom in class point the default slice is pt In order to have all plots in a single graph select the ALL IN 1 option The PRESET menu implements a short cut to setting the most common selection for plots of the visibility either for slice pt or ch Clicking on PLOT SCREEN will display the plot At this stage you can fit functions to the data FIT the residuals are plotted and can be manually edited enter a new plot range RANGE enter 0 0 for automatic scaling or by defining a window WINDOW click left button to anchor upper left corner click middle button fix size and shift box click left button again to fix position or right button to select automatic scaling and exit identify data points IDENTIFY click left button for repeated identifications right button to exit and edit data manually EDIT PLOT SCREEN Open new plot window and display plot FILE Write PostScript output
16. 1 42200 lt _REAL gt BINCOUNTS 8 32 42200 BYTE INPUTBEAM 3 lt gt FDLDELAY 42200 lt _DOUBLE gt QUAD 4 42200 lt _REAL gt Appendix E INCHWORM file structure The HDS file format of INCHWORM data is described here as of the last recorded revision September 28 1995 Note All the metrology subsystems have not been included under the Motion HDS object yet It will not be necessary to have all the metrology subsystem data under the same cell of the Motion HDS object some cells will have solutions from different subsystems done in different ways that can be combined in the INCHWORM software Session Format lt _char gt Format in the constrictor file FormatInch lt _char gt Format in the inchworm file Date lt _char gt Date in the constrictor file DateInch lt _charx gt Date the inchworm file was created SystemID lt _char gt GenConfig NumLaserP2P integer P2PLaunchPlate NumLaserP2P integer P2PRetroPlate NumLaserP2P integer MasterPlateID lt _char gt NumPlate lt integer Plate NumPlate NumCluster integer PlateEmbedded integer PlateID lt _char gt PlateLoc lt double PlateLocErr 3 lt double SidMetConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser lt integer Theta NumLaser lt integer ThetaErr NumLase
17. ACCESS again ACCESS TREE Print a directory of an HDS file to screen BROWSE Expand different levels in an HDS file 18 2 2 Load configuration tables and logs Before any data the system configuration consisting of the general configuration and the earth and geometric parameters and the background and scan tables must be loaded You do not have to load all these by individually selecting each one just use the ACCEss LOAD INTERFEROMETRY button which will load all items listed above it This button is also used to read cha files as it automatically detects the format to read the relevant data Please note that in addition to this the INTERFEROMETRY button will load the startable for the observed stars and will compute for scan data the derived geometric quantities uv coverage hour and zenith angles etc ACCESS LOAD cont d INTERFEROMETRY All objects in the file get auxilliary data SYSCONFIG GENCONFIG General configuration GEOPARMS Longitude latitude etc TABLES SCANTABLE Table of scan information BG TABLE Table of background scan information Logs Observers log CoNLoG CONSTRICTOR parameters DATA BG SCANS Background scans SCANS Scan data POINTS Point data 18 2 ACCESS A DATA FILE 89 18 2 3 Load point data Loading point data when using the widget is based on stars or groups of stars Note that loading all data at once might lead to excessive memory requirements When loa
18. FORMAT CHAR DATE CHAR SYSTEMID CHAR USERID CHAR OBSERVERLOG CHAR CONSTRICTORLOG CHAR GEOPARMS LATITUDE DOUBLE LONGITUDE DOUBLE ALTITUDE DOUBLE EARTHRADIUS DOUBLE J2 DOUBLE TAI UTC DOUBLE TDT TAI DOUBLE GENCONFIG INSTRCOHINT DOUBLE BEAMCOMBINERID lt INTEGER REFSTATION INTEGER INPUTBEAM NUMSID INTEGER SIDEROSTATID NumSid INTEGER BCINPUTID NumSid INTEGER STARTRACKERID NumSid lt INTEGER STATIONID NumSid CHAR 3 DELAYLINEID NumSid INTEGER STATIONCOORD 4 NumSid lt _DOUBLE gt OUTPUTBEAM NUMOUTBEAM lt _INTEGER gt NUMBASELINE NumDutBeam lt _INTEGER gt NUMSPECCHAN NumDutBeam lt _INTEGER gt SPECTROMETERID NumOutBeam lt _CHAR 7 gt BASELINEID MaxNumBaseline NumOutBeam WAVELENGTH MaxNumSpecChan NumOutBeam WAVELENGTHERR MaxNumSpecChan NumOutBeam CHANWIDTH MaxNumSpecChan NumDutBeam CHANWIDTHERR MaxNumSpecChan NumDutBeam FRINGEMOD MaxNumBaseline NumOutBeam TRIPLE NUMTRIPLE lt INTEGER OUTPUTBEAM 1 11 lt _INTEGER gt BASELINE 3 L 1 INTEGER 169 CONSTRICTOR CHAMELEON INCHWORM YYYY MM DD UT date of first data point NPOI Mark III Login name Parameters used to run CONSTRICTOR degrees N degrees E n n s s Instrumental coherent integration time ms Station to which delays are referenced First 1 Unique ID Which beam combiner input
19. Note that FDL_O C for the reference station is identical to zero by definition To change the reference station use the AstrometrySolution widget The reference station is station 1 by default in the con file Do not solve for star positions When the solution widget is displayed the default settings do not need to be changed for this step Check the O C values again and save the StationTable if you are happy with the fit If for any reason there are outliers try to locate and flag them in the corresponding point data then average again 17 8 Calibration of visibility amplitudes and closure phases CALIBRATE VISIBILITY Select PLOT and flag first the channels 21 32 since their SNR is usually very low if you observed with the 3 way system the 6 way system has only 16 channels To do this plot VisSq vs channel selecting all channels and the All in 1 option Then for calibration look at the data from the calibrator stars select them using the information in the StarForm then select CALIBRATE to display the calibration widget Make sure the star selection in the plot widget is set to the stars to which you want the calibration be applied before solving for a set of calibration coefficients The calibration will be applied to the data automatically Save the calibration table entries if you expect to restart OYSTER and want to redo some of the calibrations For more information on calibration see section 18 5 17 9 Write data AC
20. Rate NumBGScan NumSpecChan beam lt real ScanData Table NumScan lt integer ScanID NumScan lt integer StartTime NumScan lt double StopTime NumScan double Code NumScan integer NumPoint NumScan lt integer StarID NumScan lt char WASA Image NumScan intensity and position s of stars in field 167 NumCoh NumScan lt _integer gt instr coh int s per CONSTRICTOR coh int NumIncoh NumScan lt integer PointData NumScan lt ExtTable gt NumPoint lt integer Time NumPoint lt double time of mid point SoftDelay NumPoint NumSid lt double InputBeam NumSid FDLPos NumPoint lt double FDLPosErr NumPoint double NATJitter NumPoint lt real NATJitterErr NumPoint lt real OutputBeam NumOutBeam lt ExtColumn gt SoftDelay NumPoint NumBaseline beam lt _real gt SoftDelayErr NumPoint NumBaseline beam lt _real gt DelayJitter NumPoint NumBaseline beam lt _real gt VisSq NumPoint NumBaseline beam NumSpecChan beam lt _real gt VisSqErr NumPoint NumBaseline beam NumSpecChan beam lt _real gt ComplexVis NumPoint NumBaseline beam 1 NumSpecChan beam R 1 lt _real gt ComplexVisErr NumPoint NumBaseline beam NumSpecChan beam A B C lt _real gt PhotonRate NumPoint NumSpecChan beam lt _real gt PhotonRateErr NumPoint NumSpecChan beam lt _real gt Triple NumTriple lt ExtColumn gt ComplTripl
21. log and the scan log extension starlog 24 2 Preparation of parameter file The parameter file contains information for CONSTRICTOR on the location of the raw data files start and stop times integration time etc These are parameters used to control the output but not parameters describing system configuration The parameter file YY Y Y MM DD par can now be created using the rawlist procedure of OYSTER If you want to create the parameter file for the previous night just run rawlist from the OYSTER prompt for other dates you should supply the date e g rawlist 2002 12 13 This procedure will look for files YY Y Y MMDD in dataconll if run on the site data reduction computer octans On any other computer the raw data files should be in the current directory Should you want to exclude certain files from being processed compress them since rawlist ignores compressed files The procedure will do some basic file integrity tests and it will also update header time stamps in the packet directories with the first time stamp found in the packet body This is to prevent buffer overflows in CONSTRICTOR when synchronizing the records The rawlist procedure will also write the packet directories dir files and packet listings lst files The latter were previously produced by the pktlist program Check beginning and tail of the listing for each file There should be an END OF DISK packet If not there will be an appropriate entry
22. lt double LocErr NumSensor 3 double DLPressConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double FBPressConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 double LocErr NumSensor 3 lt double WxAirTempConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double 166 APPENDIX B CONSTRICTOR OUTPUT FILE STRUCTURE WxPressConf NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor double ScaleErr NumSen
23. lt _integer gt 1 air temperature Data NumTime lt _ DataErr NumTime ensor lt integer double double or lt integer _double gt lt _double gt lt _integer gt _double gt lt _double gt r lt integer double double r lt integer _double gt lt _double gt sor lt _integer gt double gt lt _double gt r lt integer _double gt lt _double gt lt _integer gt double gt lt _double gt sor lt _integer gt double gt lt _double gt r lt integer _double gt lt _double gt gt roup NumLaserMax double gt lt _double gt te NumLaserMax lt _double gt e NumLaserMax double gt lt _double gt NumClusterMax NumLaserMax lt _double gt er double gt lt _double gt etc etc etc etc etc 181 182 APPENDIX E INCHWORM FILE STRUCTURE NumMotionGroup lt integer MotionGroup NumMotionGroup AveGroup lt integer EnvCorrGroup lt integer ZeroFlag lt integer Mode lt integer PlateList NumPlatelist integer ClusterList NumPlateList NumClusterList integer LaserListSid NumPlateList NumLaserList integer LaserListOA NumPlateList NumClusterList NumLaserList lt _integer gt LaserListP2P NumLaserList lt _integer gt Siderostat NumPlate NumPar integer NumPar 3 Par NumPar lt _char gt NumCorr lt _integer gt
24. permission to this data base file obsstars stars Print to screen or return list of stars contained in data base obsnights nights Print to screen or return list of nights contained in data base obsdates star lt _char gt dates scans Print to screen or return list of dates and number of scans when star was observed 106 CHAPTER 19 COMMAND LINE PROCEDURES Chapter 20 Discussion of reduction issues 20 1 Sub arrays With the advent of the 6 way NPOI configuration in which the observer can switch in and out stations the number of participating stations can change throughout the night This is equiv alent to VLBI where different sub arrays are observing In OYSTER this is so far the only allowed exemption from the required invariability of the system configuration during observa tions It is handled using a field in the scan table scantable station which for every scan indicates which stations were used When reading point data this so called scan configuration is used to flag the data involving unused stations as CONSTRICTOR has processed all data good or bad Some calibration procedures must consider which configuration was used and therefore re quire input as to which scans are to be combined in the analysis In these cases the scan selection directive has the list of different scan configurations attached to the standard directives This acts as a simple scan selection but based on a criterion here the scan c
25. slide slide Plot the groupdelay plot fringephase baseline int beam int scanfilec char For the specified baseline plot the corrected fringe phase If beam is not specified use currently loaded data With the datum parameter all available scan files will be read and analysed 26 7 COMPOUND PLOT PROCEDURES 141 plot_dispsol baseline lt _int gt beam lt _int gt scanfile lt _char gt compute compute classic classic Plot the dispersion corrected delays along with the raw FDL delays for comparison plot_ratehist channels Plot count rate histograms for the specified channels plot_coherence baseline channels Plot coherence analysis for the selected baseline and channel plot_nathist sid Plot NAT count rate histograms 142 CHAPTER 26 INTRODUCTION Chapter 27 NPOI raw packet data files A small number of procedures capable of directly accessing NPOI raw packet files packetdir file Function Return packet directory for specified file This is an array of struc tures each one specifying file day number time type length and offset in bytes from the beginning of the file for a packet Example pdr packetdir 2001 1121 131547 fringeData packettype type Function Return human readable name of packet type specified through type Ex ample print packettype 0x000b0000 readpacket packet dir record Function Read and return packet specified in argument which is an entry in the packet di
26. 2 1 Interferometry The integration time INT_TIME is defined as the length of time over which the data were averaged to yield the given data point For large sources e g wide binaries long integration times can significantly lower the averaged fringe contrasts Taking the system variable lint time to specify an upper limit for the integration time in seconds which will not require integrating the model visibilities OYSTER will compare the actual integration times to this limit and determine the maximum number of computations required to cover the largest integration interval The step size for each observation will be adjusted according to the actual integration time of the particular observation given the number of computations 7 2 2 Astrometry Astrometry data file have to have the extension psn The following gives an example for Algol where the columns give the hierarchical component designation the Julian year of observation separation in mas and position angle in degrees from N over E major and minor axis in mas and position angle of the major axis of the error ellipse in degrees from N over E AB C 1991 7487 10 68 67 30 1 511 0 265 107 8 1991 7545 15 70 83 18 0 589 0 091 86 8 1991 8036 25 52 105 36 0 253 0 086 91 1 35 36 AB C AB C AB C AB C AB C AB C AB C AB C AB C 7 2 3 Spectroscopy 1991 1992 7756 1992 1992 1992 1992 1992 1992 1992 8336 6936 7864 7921
27. 8822 8930 9203 9450 33 AT 19 15 14 25 28 35 43 24 11 04 16 64 27 01 86 11 111 141 160 165 174 292 295 53 305 301 73 94 03 57 39 96 10 27 POOOOOOOoOOo 186 874 283 210 714 692 956 862 106 oooooooo o 061 165 090 093 133 198 208 223 237 92 99 95 150 87 81 92 97 91 Ee 0 o o o O o o CHAPTER 7 INTRODUCTION Spectroscopy data files have the extension vel The following gives an example for Algol where the columns are the component designation the Julian date of observation and value and error of the radial velocity in km s measured Optionally plot symbol and color can be added to each record Available symbols are 0 x 1 2 triangle up 3 triangle down 4 square 5 diamond 6 pentagon 7 star 8 and circle 9 added to the symbol number The available colors are black 0 white 1 red 2 green 3 blue 4 and more gt 2428890 2428918 2443477 2443478 2443497 2443498 2443501 9305 16 6569 54 748 145 743 199 646 179 673 169 689 201 2422984 4 10 5 1 6 2425125 5 ooooo 5 e 5 9 0 6 7 2 4 Photometry These are open symbol unless 10 is Photometry data files have the extension mag The following gives an example for Algol where the columns are th
28. FITS files observing lists or stellar data base tables OYSTER never automatically saves any data for reasons of not destroying existing files or creating files the user doesn t know about 3 7 Using oysterat NPOI At the US Naval Observatory raw data from the interferometer is first reduced with CON STRICTOR which is a stand alone program It computes the visibilities and averages the data into 1 second intervals the so called point data Averaged raw data from CONSTRICTOR can be found in home constrictor on octans at the site It is best to start up OYSTER in a directory owned by the user and then to enter the full path to the data file when opening it The path is stripped off by OYSTER when deriving output file names from the input file name so that all files are written into the local directory Due to the size of the con files it is best not to make copies of them Averaged scan data from OYSTERis output into HDS files with the extension cha If you have a file with unknown history the data might have been calibrated or they might not It is best to assume that they have to be calibrated in which case one should remove any existing calibration before continuing In order to find the right file for observations of a particular star use the obsdates procedure see section 19 8 20 CHAPTER 3 USING OYSTER Chapter 4 oyssrsupport for other interferometers 4 1 Motivation Once interferometric data have been reduced and ave
29. GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass lt double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double PlateExpConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval integer IFBox NumLaser integer Channel NumLaser lt integer Theta NumLaser integer ThetaErr NumLaser lt integer Phi NumLaser lt integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass lt double AirGapThick NumAirGap double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double MetAirTempConf NumPlate NumSensor lt integer 164 APPENDIX B CONSTRICTOR OUTPUT FILE STRUCTURE SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offs
30. Unique ID of quadcell e g AWO EO2 x east y north z up d delay constant all in m Also the number of spectrometers Number of baselines in output for spectrometer Number of spectral channels for each spectrometer Unique ID lt _CHAR 7 gt Made up of StationIDs e g AWO EO2 lt _DOUBLE gt m lt _DOUBLE gt m lt _DOUBLE gt m lt _DOUBLE gt m lt _INTEGER gt For each baseline which output beam is it from For each baseline which baseline in that output beam is 170 APPENDIX C CHAMELEON FILE STRUCTURE SPECCHAN L 32 L 3 L 1 INTEGER For each baseline which channel number of these output 1 NUMSPECCHAN 1 lt _INTEGER gt How many spectral channels in this triple SCANDATA lt TABLE gt NUMSCAN lt _INTEGER gt SCANID NumScan lt _INTEGER gt Unique observed STARID NumScan lt _CHAR 7 gt e g BSC1948 SCANTIME NumScan lt _DOUBLE gt s from OUT of date OUTPUTBEAM NumDutBeam lt EXTCOLUMN gt VISSQ NumSpecChan beam 1 NumBaseline beam NumScan lt _REAL gt VISSQERR NumSpecChan beam 1 NumBaseline beam NumScan lt _REAL gt VISSQC NumSpecChan beam 1 NumBaseline beam NumScan lt _REAL gt VISSQCERR NumSpecChan beam 1 NumBaseline beam NumScan lt _REAL gt DELAYJITTER NumBaseline beam NumScan lt _REAL gt m DELAYJITTERERR NumBaseline beam NumScan lt REAL m PHOTONRATE NumSpecChan beam NumScan lt _REAL gt per coherent integration PHOTONRATEERR NumSpecC
31. are expansions of single date configura tions to multiple day configurations for use in AMOEBA In general any interferometric data from a single night are not buffered Thus the two standard procedures to read data into CHAMELEON get scandata and get_xdr empty the buffer and only initialize the geoinfo and geninfo structures for use in AMOEBA Similarly any procedures creating a CHAMELEON data set from other formats do the same with the exception of get_oifits because these files may contain multiple data sets Finally fakedata which simulates a data set also empties the buffer Finally model and image data are contained in two common blocks 22 3 Array configuration 22 3 1 Optical path lengths The total optical path through the NPOI can be found by adding various contributions listed in the files npoi stations config npoi fdl config and npoi 6way config For the purpose of calculat ing delay constant term and optical path lengths we break up the paths into segments of four types associated with siderostat station delay line beam combiner number ID and beam combiner input number It is best to make the break between station and delay line associated lengths at the intersection of the N and E arms However the west arm never reaches that point We treat the feed pipes associated with delay lines 4 5 and 6 as if they run to the N and E arm intersection If they feed the W arm the path length is reduced by 1 4455m which is
32. are used Responses you are asked to type at the command level appear in these fonts open filename In this example lower case italic font indicates numeric or character parameters you have to supply Procedure names in the text appear like this average whereas widget buttons are typed like this OPEN or DIsPCORR depending on whether or not they bring up a new widget or take immediate action respectively Note that IDL is not case sensitive Messages from the OYSTER software or IDL are denoted in this style Averaging complete Chapter 2 Installing OYSTER The OYSTER installation consists of code catalog and stellar atmosphere data The IDL proce dure code can be downloaded from http www eso org chummel oyster download html The external C and FORTRAN library compiled for Linux 64 bit systems is included but can be recompiled if necessary from the C code which can be obtained from the author Download files oyster tar gz catalogs tar gz and atmospheres tar gz and unpack OYSTER first e g tar zxf oyster tar gz Then unpack the other two inside the newly created oyster home folder Two directories are created atmospheres and catalogs 2 1 Compiling oyster Compilation always includes the procedure code which is then saved in oyster oyster cpr This does not apply to GDL installations where code is compiled on the fly Makefiles exists in the main OYSTER directory which simplify the installation Use make f Makefile
33. by the radial velocity data 7 5 3 Single lined spectroscopic binary with astrometric orbit Add the remaining astrometric orbital elements to the fit parameters and vary the secondary mass only If you have a measurement of the parallax say from the Hipparcos catalogue you can add this measurement using the set parallax procedure In this case you may add also the primary mass to the fit parameters as the system is now constrained just like a double lined spectroscopic binary 7 5 4 Triple with velocity curves of close pair Select all three masses as fit parameters The mass ratio of the close pair will be constrained but as far as the absolute masses this system is identical to a single lined binary 7 5 5 Triple with velocity curves for all components Fit all three masses as well as the inclination of one of the pairs That not any combination of orbital inclinations is allowed can be seen from the fact that the triple consists of two double lined binaries and only one mass solution exists for a given inclination Which inclination to vary depends on whether the adopted value of the other orbital inclination is larger or smaller than the true value 7 6 Pass band integrations As any interferometer even those with spectrometers measure the visibilities integrated over band passes of non negligible widths OYSTER computes model visibilities on a grid of wave lengths The results visibilities fluxes are then integrated over wa
34. can be computed by OYSTER for them using the uv coordinates But OYSTER considers the latter as secondary data and usually computes these from the apparent star positions observation dates and times as well as the station coordinates This is due to one of the original applications of OYSTER to astrometry with NPOI In practical terms use of astrometric routines such as calcastrom should therefore be avoided e Object coordinates are also not strictly necessary for the computation of model data and thus OYSTER will read OIFITS even without the OL TARGET table However inter 21 22 CHAPTER 4 OYSTER SUPPORT FOR OTHER INTERFEROMETERS nally each target must have an ID composed of a three letter catalog name e g HDN or HIP and an index into this catalog e g HDN123306 This is the so called star ID Again this has to do with the use of OYSTERas astrometric software for NPOI The OYSTER installation includes several tables in the starbase folder e g vlti hdn which are used for looking up catalog IDs for a given target name If no entry can be found the default OBJ designation is used OBJ HHMMSSFFDDMMSSF This is usually not a problem except that the STARBASE procedures will not work anymore such as compiling stellar data for the observed targets from installed catalogs e General configuration items stored in the genconfig structure will often be incomplete when reading an OIFITS file 4 3 Programmer s reference Almost all int
35. channels and beams If none are specified do channels 11 and 21 to 32 in all beams If beams are not specified but channels are assume this selection is valid for all beams If channels is a linear array and beams are specified use the same channel selection for the specified beams If channels is a two dimensional array the first index refers to the beam and the second index to the channels to be flagged for the beam specified in the second parameter 19 2 POINTDATA MANIPULATION 101 dispclose Enforce the closure relations Since the fringe delays computed for the coherent integration of the complex visibilities are baseline based they do not necessarily close i e add up to zero This procedure makes sure they do and adds the correction to the phases unwrapphase Unwrap the visibility phase as a function of wavelength dispcorr Compute the dispersion correction Place the results in common block metroinit Initialize zero the metrology delay corrections They can be recomputed using metrocorr or astrocorr metrocorr Compute delay corrections from 2 solutions provided by INCHWORM and stored in variables parz pary and parz Interpolate to the epochs of the point data Results are stored in variable metropos astrocorr Compute delay corrections by interpolation of the INCHWORM solutions already converted to delays and stored in variable metropath to the observed point data times The results are stored in metro
36. compared to the median value derived from all calibrator observations in the same data file If despite this initial step the calibrated visibility measured on a baseline is less then half of what is predicted by a model the baseline is considered to have been tracking noise and all values are flagged 16 8 PIPELINE 81 16 3 2 Output files All output files will be written into a directory called npoipipe so that no files in the current directory will be overwritten However existing files in npoipipe may be overwritten For each processed file in addition to the CHAMELEON file a log file extension tzt a plot file with results from the bias correction ps and a flag table flg will be written 16 3 3 Flag tables If upon inspection of the calibrated data some data points need to be flagged this can be done manually and the flag table saved in the current directory will be read by npoipipe if run again It is thus important to keep only those flag table files in the current directory that shall be used 16 3 4 Bias correction As usual bias correction is based in incoherent scans and is performed separately for each interferometer configuration First bias correction fit coefficients are computed combining all observations for each configuration to make sure that a basic correction is performed Second bias corrections are updated for each star with the measurement obtained for this star only 16 3 5 Phase unwrappi
37. contains variables which control the performance of the Marquardt Levenberg M L non linear least squares fitting FIT OPTIONS 8 3 FIT ROUTINES 4T ONE One iteration only FLOAT Allow V calibration to float OPT Optimize step size for M L LAMBDA Gradient Brute force parameter TOLERANCE Ratio of smallest over largest eigenvalue allowed CONVERGENCE Convergence criterion as ratio of new over previous x Choosing the OPT option will cause a one time delay before starting M L including the loading of the interferometric data a second time as the optimization of the step size overwrites the currently loaded visibilities The step size data is written into a file Z_h_steps xdr 48 CHAPTER 8 BASIC WIDGET PROCEDURES Chapter 9 Command line procedures 9 1 Interferometry data buffering storenight mode lt _int gt Manipulate interferometric scan data buffer mode O Free allocated buffer 10 Store new night 11 Store overwrite existing night in buffer loadnight night lt _char gt Load night from buffer 9 2 Model manipulation readmodel file lt _char gt Read a model file calcmodel Compute the model data for data sets with non zero weight modelchisq Function Return reduced y of currently loaded data wrt model binarypos epoch lt _real gt component lt char gt lambda lambda com com abs abs Function Return 0 relative position for binary model at JD epoch Use today if no epoch is speci
38. coordinate list respectively e pti stations pti e keck stations keck e viti stations ulti e mark3 stations mark3 16 3 Pipeline 16 3 1 Introduction and command syntax The pipeline automatically performs all of the steps described in the interactive session below with the exception of the astrometry The full command is as follows npoipipe confiles calibrators calstars addcal calstar model modelfile confiles is a string file specifier given to IDL s file_search function to return a list of files for processing If confiles is omitted all CONSTRICTOR files in the current directory are processed A list of calibrators to be used can be specified as a string array for the calibrators keyword otherwise npoipipe will determine which stars can be used as calibrators based on information found in the standard NPOI calibrator list diameter bsc Calibrators can be added to the standard list using the addcal keyword It is thus important to keep in mind that npoipipe will normally use all calibrators observed to calibrate the science targets If not enough calibrators were observed a warning message will be displayed and processing will continue with the next data file Finally the model keyword can be used to pass the name of a model file which will be used to flag data on non tracking baselines Non tracking reference baselines are difficult to detect and the method used by npoipipe is based on the delay jitter which is
39. corrected with the incoherent scan immeadiately following it Implementation has been delayed however because of the new possibility to do bias correction with unused fringe frequencies 20 3 Photometry With this we do not mean to talk about using NPOI as an interferometer Instead photometric calibration is an important part of checking the system and calibrating visibility amplitudes of the 6 station array 20 4 Calibration of visibilities In OYSTER the visibility amplitudes and phases of the program stars are calibrated using cal ibrator stars for which those variables are modeled and the resulting model coefficients trans ferred to the program star data In practical terms the software keeps four copies of the amplitudes squared and triple which correspond to the uncalibrated amplitudes the uncalibrated but normalized amplitudes the calibrated amplitudes and the normalized and calibrated amplitudes Normalization is based on a model of the star currently a single disk with a diameter taken from a file compiled with a STARBASE procedure When calibrating the data the user should begin by looking at the calibrated and normalized amplitudes first to see whether the data has already been 20 5 ASTROMETRY DATA REDUCTION 109 calibrated for example when a cha file was read In addition this data type is the only one which should approach unity for the calibrator stars after calibration In the case of visibility phases
40. create tables and load data 83 17 2 Print dorm sheets Eee AR aeos wisi te a Eu d e 84 17 4 Reduce the background data sh 84 175 Reduce point data ua antie ae ene oa 84 17 6 Average aria a o WOW a eee da o Regis 85 17 7 AStrometry se a A A O DWR ROC WB 85 17 8 Calibration of visibility amplitudes and closure phases 85 Write datar tio hu ay EEE med uuu su s 85 18 Basic widget procedures 87 1351 Opera data Mez ae vM a EP A E bsc e 87 18 2 Access data 87 18 2 1 Browse through an HDS 87 18 2 2 Load configuration tables and logs 88 18 23 Load point zr an ar a A ds Bb aer a ee 89 18 24 Load Scan data Ar ic a RII edm Sa Eee eee e 89 18 2 5 Load 89 18 2 0 Write data ik ur 404 02 o WAL een E 89 18 3 Reduce visibility data 90 3 4 Reduce delay data umi a rei N ta sn 91 18 5 Calibraterd tar Hita RUE ned dedo E tu qc eit 92 18 51 Seancdatar cu sa em xeu SIUE ee re ONUS dex Uns 92 18 5 2 Calibrating amplitude errors 94 18 5 8 Unwrapping triple phases 94 18 5 4 Astrometry eas nar met esee Fuge Oo qm e A Red Rs 95 18 0 0 Rupee RED RIMIS Geox e es NUS dew EO a 95 18 59 65 System A ne
41. get genconfigl stations Load GenConfig object from HDS file If file not open or stations are defined close file and create object from inputs get metroconfig Load MetroConfig object from HDS file get sysconfig sysid sysid datum datum stations stations Load GenConfig MetroConfig and GeoParms Input parameters if defined cause creation of objects from inputs rather than reading the from file In this case the file will be closed get observerlog Get ObserverLog from HDS file get_constrictorlog Get ConstrictorLog from HDS file get_format format Get Format of HDS file either CHAMELEON CONSTRICTOR INCHWORM or COBRA 19 1 2 Loading tables get_numscan num_scan Read NumScan object for number of scans in HDS file get_numbgscan num_bg_scan Read NumBGScan object in HDS file for number of background scans get_scantable 19 1 ACCESSING DATA FILES Read data relevant to scansin HDS file in order to fill the scantable The scantable is a somewhat antiquated concept since it could be easily absorbed into the scans structure get_bgtable Read objects in HDS file in order to fill the background table get_stationtable stationfile lt _char gt Read stationfile with station coordinate information If not specified read default files stations config fdl config and Sway config or 6way config depending on GenCon fig BeamCombinerID Remember to run calcastrom if you have scan data loaded in order to upda
42. indices Plot variable IDL name inbeam outbeam triple channel baseline point Time bgscans time Sc ScanNo SC BGRate bgscans rate ob ch SC Table A 3 Plot variables class scan and their indices Plot variable IDL name inbeam outbeam triple channel baseline point Time scans time SC ScanNo SC VisSq scans vissq ob ch bl SC VisSq c scans vissqc ob ch bl SC VisSq e scans vissqe ob ch bl sc VisSq c e scans vissqec ob ch bl SC TripleAmp scans tripleamp tr ch SC TripleAmp c scans tripleampc tr ch SC TripleAmp e scans tripleampe tr ch SC TripleAmp c e scans tripleampec tr ch SC PhotonRate scans photonrate ob ch SC NAT Counts scans natcounts ib SC BeamCounts scans natcounts ob SC SpecCounts scans photonrate ob SC BackgndRate scans backgndrate ob ch sc FDLPath scans fdlpos ib sc DelayJitter scans delayjitter ob bl SC TrackJitter scans natjitter ob bl sc FDLDelay scans fdlpos ib SC GeoDelay scans geodelay ib SC uv radius SCANS UVW ob ch bl sc HourAngle scans ha SC ZenithAngle scans za SC Mirror Angle scans ma sc U scans UVW ob ch bl SC V SCANS UVW ob ch bl SC W SCANS UVW ob ch bl SC FDL_O C ib sc Grp O C ib SC Dry O C ib SC Wet_O C ib sc VisSq m scans vissqm ob ch bl SC TripleAmp m scans tripleampm tr ch sc TriplePhase m scans triplephasem tr ch SC ModelDelay scans modeldelay ib SC MetroDelay scans metrodelay ib sc Plot variable MetroTime Par X Par Y Par Z MetroPath MetroDelay Plot variable Wavelength Channel BL
43. lt _double gt SidMetData NumPlate NumLaserMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt ExtCatEyeData NumPlate NumLaserMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt PlateExpData NumPlate NumLaserMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt MetAirTempData NumPlate NumSensorMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt MetSolidTmpData NumPlate NumSensorMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt MetPressData NumPlate NumSensorMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt MetHumData NumPlate NumSensorMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt OptAnchData NumPlate NumClusterMax NumLaserMax NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt Pier2PierData NumLaser NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt LabAirTempData NumSensor NumData NumTime lt _integer gt Data NumTime lt _double gt DataErr NumTime lt _double gt A LabSolidTmpData NumS NumData NumTime Da
44. routines exclude super giants and binaries If you want to bypass the latter restriction set the BFLAG field to it is set to B for binaries The routine computing the diameter from B V also excludes bright giants and stars later than K diameter ri Compute diameter from R I color index and V magnitude diameter bv Compute diameter from B V color index and V magnitude 68 CHAPTER 13 COMMAND LINE PROCEDURES 13 8 4 Orbital inclinations semi major axes and secondary masses binaries Estimate I from MASS1 2 MF or MASS1 24 MI1 2SINGI a binaries Estimate A from MASS1 2 P D k binaries Estimate K14 K2 m binaries Estimate secondary mass from primary of an SB2 13 9 Cross indices A comprehensive array of crossindices has been installed in catalogs crossindex The files have the extension cri and are read by IDL within the crossindex function cri To obtain for ex ample the BSC number for FKV0193 Capella enter print cri 193 fkv hdn This function can be nested if a particular index does not exist and the reguest needs to be routed around it The function will return 1 if the ID number could not be found If you know the Bayer or Flamsteed names of the star or its proper name you can also use cri to obtain its ID in any catalog Note that in the following example only the destination catalog is specified in the function call print cri capella fkv or print cri alp aur bsc
45. selected stars identified by a primary catalog ID e g jhk hdn contains JHK magnitude for selected HD stars 11 2 The format of STARTABLE Inside IDL STARTABLE is in the table format Thus for example to access the NAME field you access the variable STARTABLE NAME In the following we list all valid fields e STAR string Identifier of form CCCNNNNNN CCCNNNN e NAME string Star name e VAR string Star name in Variable Star Catalogs e TOE string Common name e g Capella RA double Right Ascension h RAE double Error in Right Ascension h 55 56 CHAPTER 11 INTRODUCTION DEC double Declination deg DECE double Error in Declination deg BAT short int Number in Batten s Catalogue FKV short int Number in Fundamental Katalog No 5 BSC short int Number in Bright Star Catalogue FLN short int Number in Finding list for Interacting Stars ADS short int Number in Aitken Double Star Catalogue HDN long int Number in Henry Draper Catalogue HIC long int Number in HIPPARCOS Input Catalogue SAO long int Number in Smithsonian Astrophysical Catalogue WDS long int Number in Washington Double star catalog MV float Johnson V magnitude for combined system if multiple BV float B V color for combined system if multiple UB float U B RI float R I DMV float V magnitude difference for binaries AMV float Absolute V magnitude for combined system if multiple BY float b
46. startable to file in NPOI embedded catalog file format 13 4 Lists Note that data only for those stars in the table is retrieved which have the right ID available If for example there is no BSC number in the table startable bsc for a specific star no diameter will be read for it get diameter get parallax get position get ubvri get ubv get uvbybeta get feh get toe Diameters BSC identifier Parallaxes HDN identifier Coordinates HDN identifier UBVRI photometry HDN identifier UBV photometry HDN identifier Str mgren photometry HDN identifier Fe H metallicity HDN identifier Common names BSC identifier 13 5 PLOT DATA FROM THE WDS 65 13 5 Plot data from the WDS Visual and speckle observations from the Washington Double Star catalog can be plotted if a startable with good epoch 2000 0 positions is loaded The coordinates are used to locate a binary in the WDS The data are placed into a file tmp wdsdat psn which can be read by AMOEBA for orbit fitting plot_wds starid lt _char gt This command will print out the following example here Capella if a star is found RA Dec Disc Comp _DafDal 0PAfPAlSepfSeplMagAMagBSpectrum_pmrapmdeDM No hhmmf ddmm YYYYYY degdeg m m S y 1000 century 05167 4600ANJ 1 91999799 49 01 008 G3III 076 425 45 1077NO 05167 4600BAR 25AB 898898 1 23 23 466 466 21 171 05167 4600BU 1392AC 878878 1318318 782 782 21 151 05167 4600BU 1392AD 878878 11831831262
47. the point data for all stars or a specific selection of them Load all data if you have sufficient memory this may take a few moments If not all data can be loaded select a group of stars by dragging the cursor over the star list in the widget Load the data for the selected stars by clicking the LOAD button Use REDUCE POINTDATA IMAGING PLOT to plot and edit the point data data in much the same way as you did with the background data Start by plotting the DelayJitter versus Index and use the AUTO editor PL E AuTO on it Do the same for NATJitter if data present The first one has an OutputBeam and Baseline index the second one an InputBeam index The jitter data provide a good first check whether the visibility data is going to be useful or not Make sure you look at all spectrometers and baselines If more than one baseline is selected they are plotted along the X axis channels are stacked vertically Use plots vs channel if you have to flag several entire channels Use the PLOT AUTO option to automatically edit outliers in PhotonRate and VisSq select all channels for speed It is recommended to not flag the data in the laser channels since VisSq will not be averaged anyway if the background data for these channels has been removed This prevents the flag table from getting too large Save the PointFlag Table Examine and edit the FDLDelay data on a star by star basis using the Fit utility to detect outliers You should plot FDLDelay
48. to be stored in the buffer storenight for AMOEBA routines to load the new data A general exception has been implemented which does not load data from the buffer if the buffer has only one night stored 51 52 CHAPTER 10 PROGRAMMER S REFERENCE Part III STARBASE Chapter 11 Introduction 11 1 About STARBASE STARBASE is a collection of scripts written in IDL with additional functions written in C callable from within IDL The scripts are run interactively STARBASE provides a table structure which can be filled with astrometric and astrophysical information on a list of stars from catalogs auxilliary data files and by computation The star list can be either an entire catalog or a list compiled by the user The former option can be invoked using a single command for various catalogs e g the Bright Star Catalog get bsc The name of the data base variable is STARTABLE STARBASE distinguishes several types of external data files Primary catalogs have their own unique identifier e g HDN and are accessed using C external functions T hese catalogs are static and never changed Secondary catalogs are either extensions of primary catalogs as in the case of HDN which is based on SkyCat 2000 only complete to V 8 and does not contain many of the MIDI calibrators or implement dynamical catalogs as in the case of MIR for mid infrared targets not contained in the HD primary catalog Finally lists contain specific data for
49. use three element vectors with East North Up as the order of the elements For directions we use two element vectors with the first element 0 being the angle from the zenith and the second element being the angle in the horizontal plane measured from east through north We have not specified the units in the database description For lengths we will use meters Time stamps are offsets from 0 h UT of DataSet Date For time stamps and sample intervals we will use milliseconds We use lt _integer gt which is int 4 with a range of 2e9 or 68 days for time stamps and lt _double gt for times e g start and stop times The format for the descriptions is VariableName IndexLimit source Data type So for instance ComplexVis NumPoint NumBaseline beam NumSpecChan beam 1 R T under ScanData PointData 0utputBeam NumOutBeam is a four dimensional array with the first dimension ranging from 0 to NumPoint 1 the second from 0 to NumBaseline beam 1 where NumBaseline can differ from one beam combiner output beam to another and the 159 160 APPENDIX B CONSTRICTOR OUTPUT FILE STRUCTURE third ranging from O to NumSpecChan beam 1 In the fourth index 0 corresponds to the real part and 1 to the imaginary part In this example NumPoint could have been indicated as NumPoint scan however we suppress listing the source of the parameter if that source is in the same object as the inde
50. 0 98 omega 0 1 0 teff 0 0 gr 0 1 0 albedo 0 1 0 magnitudes 0 2 26 2 36 name 1 B type 1 1 mass 1 0 82 diameter 1 21 2 omega 1 1 0 teff 1 0 gr 1 0 3 albedo 1 0 5 magnitudes 1 5 23 4 26 name 2 gt C type 2 1 mass 2 1 88 diameter 2 0 58 5 1 4 8 magnitudes 2 3 38 CHAPTER 7 INTRODUCTION Binary parameters for each binary component 0 gt A B method 0 1 wdmode 0 5 semimajoraxis 0 2 04 eccentricity 0 0 0 inclination 0 97 69 periastron 0 91 86 of primary apsidalmotion 0 0 0 ascendingnode 0 47 4 period 0 2 8673285 epoch 0 2441773 4894 Fit to AB C astrometry component 1 gt AB C method 1 1 semimajoraxis 1 94 6 eccentricity 1 0 229 inclination 1 84 0 periastron 1 310 5 apsidalmotion 1 0 0 ascendingnode 1 312 3 period 1 epoch 1 679 9966 2453731 4d0 The syntax of the model format is identical to the language e g IDL The individual lines are actually commands which are executed by AMOEBA upon reading the model file Model parameters are defined in the following Please note that Julian Day epochs model parameters and data are stored internally with 2440000 days subtracted e System Starid Star identifier Character string CCCNNNN or CCCNNNNNN RA Right Ascension Needed for precession computation Dec Declination Needed for precession computation Rv Systemic ra
51. 1 1931 DayNumber 89 StartTime 00 00 00 StopTime 24 00 00 LogFile datacon11 2003 0330 log ScnFile datacon11 2003 0330 030621 starLog OutFile 2003 03 30 con Raw Off Lock Off Triple On NumAv 500 RefStation 2 SmartFDLAverage Off Metrology On Nat On 24 4 System configuration As described in Chapter VI the system configuration is not yet automatically produced by the control system Neither is the system config file which is used by CONSTRICTOR for system configuration information control the NPOI configuration Ideally the system configuration file is deposited in the same directory used for the observing list the day before observing A script on sextans automatically transfers this file to the proper system area If this is not done the file system config can always be placed in the directory where CONSTRICTOR is run and will be loaded automatically overriding any system configuration embedded in the raw data stream The system configuration is supposed to be written by the control system into the SYS_CONFIG packet stored in the raw data stream This however is not currently implemented and instead the text packet in KEYIN format is fetched from disk file system config Therefore the stored system configuration can be wrong if the configuration file was out of date In this case placing this file in the current directory for CONSTRICTOR will cause the software to load this file automatica
52. 1262 21 136 05167 4600BU 1392AE 878878 131631614321432 21 121 05167 4600HJ 2256AF 8519221014714416951415 21 111 003 006 Np 05167 4600SHJ 51AG 821895 234834845424846 21 101 05167 4600FRH 1AH 895 1141 7233 21 117 N Component to select Enter the component name you wish to select Aa for example and the available data will be plotted 13 6 Stellar parameters from calibrations of spectral types Files containing stellar parameter data reside in oyster starbase Extensive photometric data is found in files spec_par X where X signifies the luminosity classes for dwarfs giants and supergiants V III lab respectively For subgiants brightgiants and the subclasses of the su pergiants limited data is in files spec_MV IV spec_M V II spec_MV Ia spec_MV lab spec_MV Ib 13 6 1 Absolute visual magnitudes Absolute visual magnitudes for stars are derived from their spectral type and luminosity class Calibrations are stored in files spec_par V spec_MV IV spec_par III spec_MV II spec_ MV la spec_MV Iab spec_MV Ib in oyster starbase amv_stars Compute MV for all stars in startable amv_star spectrum lt _char gt Function Return MV for star with specified spectrum 66 CHAPTER 13 COMMAND LINE PROCEDURES 13 6 2 Masses Masses for single stars are derived from their spectral type and luminosity class In addition for double lined binaries with the secondary component not classified mass binaries will compute the secondary
53. 18 5 CALIBRATE DATA 93 For each selected indicator a list of base function will be displayed and you will select a minimum number of functions necessary to represent the dependence of the visibility on this indicator The final fit will be multi dimensional with all functions fitted to the calibrator data simultaneously Exception the selection of a smoothing function see below The mathe matical procedure used is the Singular Value Decomposition SVD In case of a design matrix singularity SVD will edit the small eigenvalues and proceed to calculate a solution for the calibration The smoothing functions 5 the index gives the width in minutes are available for hour angle and time calibrations Selection of these disable any other selection since they cannot be used in the multi dimensional fit This is brought to the attention of the user by making all other base function widgets insensitive while a smoothing function has been selected Which indicators and functions are to be used in the calibration depends on atmospheric and instrumental circumstances and has not been fully investigated for the NPOI yet Therefore even though a wide array of indicators is available only one or two might typically be used Ideally the visibility amplitude should depend only on the delay jitter but instrumental effects might require an additional time dependent calibration either depending on time itself or on hour angle if the delay line position
54. 9 OutputBeam ChanWidth 17 20 31 3e 9 28 9e 9 26 7e 9 24 7e 9 OutputBeam ChanWidth 21 24 22 9e 9 21 3e 9 19 8e 9 18 5e 9 OutputBeam ChanWidth 25 28 17 2e 9 16 1e 9 15 1e 9 14 2e 9 OutputBeam ChanWidth 29 32 13 4e 9 12 7e 9 12 0e 9 11 3e 9 OutputBeam ChanWidthErr 01 04 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 05 08 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 09 12 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 13 16 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 17 20 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 21 24 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 25 28 0 1e 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidthErr 29 32 0 1e 9 0 1e 9 0 1 9 0 1 9 Note the OutputBeam NumSid and OutputBeam StationID parameters these parameters replace the old OutputBeam FringeMod and OutputBeam InputPair parameters which specified the baselines and their modulations directly Even though CONSTRICTOR still understands the old parameters the new ones are easier to use since CONSTRICTOR will compute the combinations and their modulations amplitudes automatically from the list of stations in each spectrometer and their strokes OutputBeam StationID tells which stations are in a given spec trometer by giving its index in the InputBeam StationID array starting with 1 That means that th values specified should always be smaller or equa
55. CALIBRATE ASTROMETRY PLOT Plot residual delays CALC Compute zenith angles etc MCORR Apply metrology and white light corrections to group dry and wet delays It is not applied to the FDL position data This is a toggle i e if you click on this button a second time the corrections will be removed again and so forth SOLVE Solve for new station coordinates 18 5 5 Stars Plots based on data for individual stars are accessed through this button e g uv coverage visibility amplitude versus projected baseline length etc 18 5 6 System Plots based on data for individual channels are accessed through this button e g the sensitivity of the channels versus the B V color index of the stars or visiblity amplitude biases In addition relative flux contributions from the stations can be calibrated with this widget for 6 way applications The calibration works as follows For the selected type any plots produced store the cor responding calibration and fit results in a field of the general configuration structure These numbers are used in the average procedure to compensate visibility biases based on incoherent photons and fixed pattern noise Remember that BrAs and RELFLUX plots have channel base line and scan indices For the latter is it advised to only use the listed sub array configurations 18 6 Utilities A collection of various tasks supporting the data reduction in CHAMELEON UTILITIES OBSBASE Invoke
56. CESS WRITE HDS will after closing any data file currently in use open the output cha file in order to write the ScanData uncalibrated and calibrated along with the configuration 86 CHAPTER 17 QUICK GUIDE information The file name is derived from the date with an extension cha If you restarted the session by reading the averaged data the input file is closed first since it is identical with the output file and all files opened with the File menu are read only FITS will ask for a star to be written in FITS format You have to run CALIBRATE VISIBILITY SETCOMPLEX before that in order to set the baseline phases Chapter 18 Basic widget procedures This section describes the complete line of data processing within the CHAMELEON widget environment To invoke the main widget type the following command at the IDL prompt OYSTER gt oyster 18 1 Open a data file Data files for CHAMELEON are in the HDS format The FILE OPEN button opens HDS files for read only access Note that when writing files using widget commands any file currently open will be closed and then the output file is opened in UPDATE mode It will be closed after writing has finished The file selection menu will be displayed with an initial filter for files having extension c CONSTRICTOR data files have extension con CHAMELEON output data files extension cha Only one data file can be open at a time to close a data file use the FiLE CLOSE button The CLRST b
57. D 01 04 1 3 4 6 OutputBeam StationID 05 08 1 2 4 5 OutputBeam Wavelength 01 04 849 4e 9 820 9e 9 793 9e 9 768 3e 9 OutputBeam Wavelength 05 08 744 2e 9 722 9e 9 701 5e 9 683 1e 9 OutputBeam Wavelength 09 12 664 6e 9 648 9e 9 617 7e 9 603 5e 9 OutputBeam Wavelength 13 16 590 7e 9 577 9e 9 566 5e 9 556 6e 9 OutputBeam Wavelength 17 20 849 4e 9 820 9e 9 793 9e 9 768 3e 9 OutputBeam Wavelength 21 24 744 2e 9 722 9e 9 701 5e 9 683 1e 9 OutputBeam Wavelength 25 28 664 6e 9 648 9e 9 617 7e 9 603 5e 9 OutputBeam Wavelength 29 32 590 7e 9 577 9e 9 566 5e 9 556 6e 9 OutputBeam WavelengthErr 01 04 0 1e 9 0 1 9 0 1 9 0 1 9 OutputBeam WavelengthErr 05 08 0 1e 9 0 1 9 0 1 9 0 1 9 OutputBeam WavelengthErr 09 12 0 1e 9 0 1e 9 0 1 9 0 1 9 24 4 SYSTEM CONFIGURATION 129 OutputBeam WavelengthErr 13 16 0 1 9 0 1e 9 0 1 9 0 1 9 OutputBeam WavelengthErr 17 20 0 1 9 0 1 9 0 1 9 0 1 9 OutputBeam WavelengthErr 21 24 0 1 9 0 1e 9 0 1 9 0 1 9 OutputBeam WavelengthErr 25 28 0 1 9 0 1e 9 0 1 9 0 1 9 OutputBeam WavelengthErr 29 32 0 1 9 0 1e 9 0 1 9 0 1 9 OutputBeam ChanWidth 01 04 31 3e 9 28 9e 9 26 7e 9 24 7e 9 OutputBeam ChanWidth 05 08 22 9e 9 21 3e 9 19 8e 9 18 5e 9 OutputBeam ChanWidth 09 12 17 2e 9 16 1e 9 15 1e 9 14 2e 9 OutputBeam ChanWidth 13 16 13 4e 9 12 7e 9 12 0e 9 11 3e
58. EDIT AUTO Do automatic editing ZERO Do automatic zero value editing UTIL single plots only EDIT Manual editing WINDOW Set new range by placing a box RANGE Enter new range MEAN Return average data value in a window IDENTIFY Identify data point H LINE Display horizontal line V LINE Display vertical line FIT Fit functions to data As for editing you have three options automatic zero and manual editing The first option will put the data through a median filter point data or edit outliers based on their deviation from a 3 rd order polynomial fit to the data scan data The second option will remove data points with value zero and the last option recommended will let you define boxes to delete data inside or outside of a box Note that the data selection applies to both plotting and editing OPTION ERRORS Display error bars FLAGGED Display flagged data too LINES Connect data points ALL IN 1 Plot all graphs in one plot 3D Open 3D plot widget 5 1 INTERFEROMETRY 25 IMAGE Plot 3rd dim in TV style NoFIR Fits to all data NoSoRT Do not sort x values NOTRACE x will not trace y selection ALL OBs Do all spectrometers uv plots only ALL IBs Do all IBs not implemented MODEL Plot model too AMOEBA only COLOR Select color printer SUBMIT Submit hard copy to printer and delete PAPER Use camera ready plot labels CUSTOM Vis plot for NPOI scale data to model 5 1 2 The data selection widget A data selection widg
59. Function returns Julian date corrresponding to input Besselian year jy2jd year lt _real gt Function returns Julian date for input Julian year jd2jy jd lt _real gt Function returns Julian year for input Julian date jd2by jd lt _real gt Function returns Besselian year for input Julian date 19 7 Astrometry procedures All arguments for these procedures and functions can be arrays All require existence of GeoP arms variable A default can be created by using get_geoparms utc2uti utc real Function Returns UT1 in seconds with UTC input in seconds uti2gst utc real ut1 real Function Returns GST in hours inputs are in seconds hourangle gst real ra real Function Return hourangle in hours with inputs also in hours zenithangle hac real dec real Function Return zenithangle in degrees with inputs ha in hours and dec in degrees mirrorangle ha lt _real gt dec lt _real gt Function Return mirrorangle in degrees with inputs ha in hours and dec in degrees horizon2equatorial coord lt _real gt Function Return equatorial coordinates for input horizontal coordinates X east Y north and Z up equatorial2horizon coord lt _real gt Function Return horizon coordinates for input equatorial coordinates X projection of local meridian on equator Y east and Z north angle2horizon coord lt _real gt 19 8 DATA BASE ROUTINES 105 Function Return horizon coordinates for input azimuth a
60. IDGET ROUTINES ww_setzaxis ww_datasel ww_setslice ww_setstdir ww_setstarsel ww_setwsize ww_datasel ww_setyinbeam ww_setyoutbeam ww_setybldir ww_setytrdir ww_setychdir ww_setyptdir ww_setysel ww_yseldestroyed 22 1 8 CALIBRATE ww_calibrate ww_cal ww_plot ww_astrom ww cal ww caldestroyed ww calindicator ww calfunction ww caloptions ww calstars ww calok ww listcalreasons ww caledit 22 1 9 CATALOG ww_catalog ww_starinfo 117 118 CHAPTER 22 PROGRAMMER S REFERENCE 22 1 10 WAVE ww_wave ww_restore ww_restorecancel ww_restorehelp ww_quit 22 2 Organization of data The data inside CHAMELEON is organized in tables e g ScanTable structures e g Gen Config arrays of structures e g scans and plain arrays e g VisSq Some of the choices made might be different from what one would make today if one were to write CHAMELEON from scratch but obviously can t be changed that easily anymore Common blocks exist for the major data groups i e e RawData unaveraged typically 2 ms integrations flat arrays bin counts laser positions quad cell counts e MetroData unaveraged typically 1 4 to several Hz flat arrays temperature data sidero stat laser metrology etc very incomplete since INCHWORM is mainly used to process these data e InchData 15 s averaged integrations output from INCHWORM flat arrays e PointData 1 s averaged fringe data output from CONSTRICTO
61. IG packets for date and configuration information It then proceeds to process all packets whose time stamps fall in between start and stop times defined in the input parameter file The packets of the high rate data types FRINGE DATA or BG_DATA for 6 way data FDL_POSITION and NAT COUNTS are processed by the fringeav c fdlav c and natav c modules respectively Individual 2ms records of these packets are aligned synchronized and missing matches discarded The integration length is defined by the number of records not by a time interval This is a pecularity which one has to keep in mind especially when reducing data for nights with very bad seeing In earlier versions of CONSTRICTOR it was enabled to do both incoherent and coherent integrations of the visibilities Since the latter has never worked well this capability has been removed and is now part of OVSTER s COBRA procedures The lean version of CONSTRICTOR therefore serves two purposes now provide an output file with incoherently averaged data and optionally reformat the raw data and store individual scans in separate HDS files for COBRA 123 124 CHAPTER 23 INTRODUCTION Chapter 24 How to use CONSTRICTOR 24 1 NPOI raw data files High rate data files are files with the extensions fringeData and alignData Metrology data files have the extension sidData where the index refers to the SIDcon ID not the siderostat ID Other files include the observer log extension
62. ON SESSION DATE lt _CHAR 10 gt SYSTEMID lt _CHAR 4 gt FORMAT lt _CHAR 11 gt GENCONFIG lt gt INSTRCOHINT DOUBLE BEAMCOMBINERID INTEGER REFSTATION INTEGER INPUTBEAM TABLE NUMSID lt INTEGER STATIONID 3 lt _CHAR 16 gt SIDEROSTATID 3 INTEGER DELAYLINEID 3 INTEGER BCINPUTID 3 INTEGER STARTRACKERID 3 INTEGER STATIONCOORD all 3 lt _DOUBLE gt OUTPUTBEAM lt TABLE gt NUMOUTBEAM lt _INTEGER gt SPECTROMETERID 3 16 gt NUMSPECCHAN 3 INTEGER NUMBASELINE 3 INTEGER FRINGEMOD 1 3 lt _INTEGER gt BASELINEID 110 3 256 gt WAVELENGTH 32 3 DOUBLE WAVELENGTHERR 32 L 3 DOUBLE CHANWIDTH 32 3 lt _DOUBLE gt CHANWIDTHERR 32 3 lt _DOUBLE gt TRIPLE lt TABLE gt NUMTRIPLE lt _INTEGER gt OUTPUTBEAM 3 L 1 INTEGER BASELINE 3 L 1 lt _INTEGER gt NUMSPECCHAN 1 lt _INTEGER gt SPECCHAN 321 31L 1 lt _INTEGER gt GEOPARMS lt gt LATITUDE lt _DOUBLE gt LONGITUDE DOUBLE ALTITUDE lt DOUBLE EARTHRADIUS lt DOUBLE 12 lt DOUBLE SCANDATA lt gt NUMSCAN lt _INTEGER gt SCANID 1 lt _INTEGER gt NUMREC 1 INTEGER STARID 1 lt _CHAR 12 gt 171 172 APPENDIX D COBRA FILE STRUCTURE STARTTIME 1 DOUBLE STOPTIME 1 DOUBLE RAWDATA 1 TABLE TIME 42200 DOUBLE OUTPUTBEAM 3 lt gt SOFTDELAY
63. OYSTER Optical Interferometer Script Data Reduction Version 8 for IDL Christian A Hummel European Southern Observatory Karl Schwarzschild Str 2 85748 Garching Germany December 19 2014 Contents I OYSTER 1 General information tal OQ YS TER S s a Nel deos ou trt s edes dne AS Y E dr PS 1 2 About this guide 4 84 223 EU RUIT uu ei 1 3 Fonts used in the guide 2 Installing OYSTER 2 1 Compiling OYSTER ci uos a ko Y up BOE Dee Fo vom Gk e RC AO 2 2 Programmer s reference s 2 3 Earth orientation updates 3 Using OYSTER Salt Starting UPD ons see hk E non eese I ria Rue EC DA dcs 3 2 What to do next 52 e 7T We o3 dew p RI cl ei 3 3 Workingowith OYSTER way dopo a nen Pe eo 3 4 trouble iiu eie 22 AA EI ae qe ege de 3 5 Getting on line help 3 0 Finishing Ups a saci anii seen era eee be vee He ut E ORA 3 1 Using OySTERatNPOILT nam planden ee Ka 4 OySTERsupport for other interferometers 4 1 Motivation Oor wx mart et a SEE ESL PER EE EA NEN 4 2 OIBDUS fead r ues mica ye eR Ree x ERES BN usus 4 3 Programmer s reference 5 Plotting and editing 5 1 T terferometry ce A ne 5 1 1 The plot selection widget
64. R flat arrays e ScanData scan averaged data scans bgscans output from CHAMELEON as well as data used in AMOEBA velocities spectrosopy positions relative astrometry magni tudes photometry arrays of structures All flat array data have a pair of indices per group containing first and last elements for every corresponding scan loaded Depending on size due to sampling time some arrays have only data from a single scan others have all night s data In particular point data is meant to be loaded one star at a time overwriting the previous copy The scan data is always allocated for the whole night Tables are identical to arrays of structures in IDL but were not in PV WAVE Since the latter was the first language for CHAMELEON we still speak of tables Two tables accompany the interferometric scan data the scantable and the bgtable back ground table They exist for historical reasons related to being convenient containers for auxilliary scan related data when reading the point data but they could have been incorporated into the scan structures Aside from the flag tables and the station table the startable is the only other tables worth mentioning as it contains all stellar data and is subject to the manipulations through the STARBASE procedures 22 3 ARRAY CONFIGURATION 119 The interferometric configuration is stored in structures genconfig metroconfig geoparms and arrays of structures geninfo geoinfo The latter
65. This means you may have to specify a StopTime of 48 hours LogFile The observers log file usually named Y Y Y Y MMDD log If none is found none is included in the output ScnFile The star log file usually names YYYY MMDD XXXXXX starlog If none is none is included in the output OutFile The name of the output file should be YYYY MM DD con or YYYY MM DD coh The latter extension can be used as a memo for files which will have coherently integrated visibilities added later by OYSTER Please do not use other extensions Raw Write the raw data of every scan into a separate HDS file This can then be read by the COBRA scripts of OYSTER Off Lock Only average continuous locks Off Triple Compute and write the triple product On NumAv Number of samples in an incoherent integration 500 RefStation Which station to reference delays to Choose one which is common to all spectrometers 1 SmartFDLAverage Average the difference between measured and pred delays Off Metrology Decode and pass on metrology data On Nat Process NAT data On Here is an example of a CONSTRICTOR parameter file 24 4 SYSTEM CONFIGURATION 127 InFiles datacon11 2003 0330 104722 fringeData datacon11 2003 0330 105135 fringeData DirFiles 2003 03 30 1 dir 2003 03 30 2 dir 2003 03 30 3 dir 2003 03 30 4 dir 200 ir 2003 03 30 6 dir 2003 03 30 7 dir 2003 03 30 8 dir MaxPacket 5076 5059 4620 4943 5541 17518 193
66. arameters directly to any combination of data from interferometry spectroscopy photometry and astrometry e Stellar spectra and limb darkening atmospheric models which are used in bandwidth smearing computations and modeling Display of stellar spectra and line identifications e Stellar data base procedures for star catalog access Storage of data in a table and procedures for estimation of physical parameters of stars like diameters masses orbital elements e Planning of observations A set of procedures for computing visibility and simulating data for scheduling The stellar data base serves to aid in the selection of calibrator stars 13 14 CHAPTER 1 GENERAL INFORMATION OYSTER was created when three collections of scripts written first in PV WAVE Command Language PV WAVE is a trademark of Rogue Wave Software and then also in the Interactive Data Language IDL is a trademark of Exelis Visual Information Solutions were merged into one package for the purpose of providing a comprehensive data analysis package The PV WAVE version of OYSTER is however no longer supported while support for GDL Gnu Data Language has been added with version 8 of OYSTER no GUI support The three original collections CHAMELEON which reduces a single night of NPOI data AMOEBA which fits models to the calibrated visibility data of several nights and STARBASE which implements a stellar data base and provides catalog access are described in this Us
67. as such and arguments to the left then are compulsory Also remember that you have to enclose character strings in quotes unless you stored them in a variable of course 19 1 Accessing data files hds_open filename lt _char gt mode lt char gt status Opens a HDS data file Only one file can be open at a time mode READ UPDATE status returned 0 no error 1 error occurred hds_close Closes the current HDS file 19 1 1 Loading configuration and logs Several of these procedures have been modified to create the object for simulation purposes instead of reading it from an HDS file if that file is closed or if the appropriate input parameters are passed to the procedure get systemid system id Get Systemld from HDS file either NPOI or Mark llI If parameter is omitted Systemld will be stored in common block variable systemid If file is not open set default system ID NPOI 97 98 CHAPTER 19 COMMAND LINE PROCEDURES get datunm datum Read Date from HDS file Format yyyy mm dd If parameter is omitted date will be stored in common block variable date If file is not open set default date the next day get geoparms sysid datum Load GeoParms object from HDS file If file not open set default site coordinates corresponding to IDL variable systemid If sysid or datum are defined file is closed and obejct is created from inputs Also reads catalogs npoi mark3 dat for earth rotation information
68. ash situation IDL is in a debugging mode with operation stopped at the offending line in the code You can enquire about variables using the info variable structure command Under IDL just type retall and you will be returned to the main level 3 4 In case of trouble Unlike many programs compiled from C or FORTRAN code the OYSTER code being written in an interpreted language almost never crashes by returning to the operating system prompt What usually happens is that execution stops at the offending line in the script and an error message is printed At this point the fearless user can print values of variables enter IDL commands all within the current context in order to investigate the causes of the crash To resume the OYSTER session by backing out of the procedure it is best to return right away to the main level by typing retall 3 5 Getting on line help Click on the big OYSTER logo button to start a browser Firefox on OYSTER s main HTML help page oyster html oyster html These pages provide brief reminders of implemented features This page is under construction for the forseeable future Some of the widget routines provide HELP buttons At the IDL prompt type info for help help at the IDL prompt Type info for a list of currently defined IDL variables and available procedures and functions 3 6 FINISHING UP 19 3 6 Finishing up Before quitting OYSTER you will need to decide whether to save any calibrated data
69. ata file being worked on 17 4 Reduce the background data You should reduce this data of type scan before anything else REDUCE BG DATA examine and edit the data with PLOT Plot the background rate four channels at a time versus time Select channels 1 4 for the first panel don t forget to hit lt return gt after entering your selection and then the Next options in the data selection widget to plot all channels in groups of four Do this for all output beams i e spectrometers Remove scans taken on a star instead of on blank sky by identifying the scan number or time and then editing the data in a plot with ScanNo or Time along the Y axis Look out for the laser light in channel 11 the default is to delete this channel Remember that editing is only allowed in single plot windows i e a window containing only a single plot Save the BGFlagTable Use PROCESS BG if you want to replace edited scans with an average value from other valid scans in the same channel Use EXPAND BG to create new background scans for non existing ones by correlating the BGTable with the ScanTable Check the background form or use UTILITIES LIST BGSCANS to see missing background scans The reason for reducing the background data first is that average will not average the point data of a scan for which no background data exists 17 5 Reduce point data The point data loading widget already present on your desktop gives you the choice of loading
70. ative weights If weights need to be changed this can be done at any time after loading the data by simple selection if the corresponding data loading widget is displayed or if not by redisplaying it DATA INTERFEROMETRY Load visibility data ASTROMETRY Load p data SPECTROSCOPY Load radial velocity data PHOTOMETRY Load magnitude measurements SUMMARY Print summary of currently loaded data 8 2 Manipulation of a model The following menu bundles all routines related to reading and fitting of the hierarchical model The fit routine should not be confused with specialized and customized fitting routines to be found elsewhere in AMOEBA FIT 45 46 CHAPTER 8 BASIC WIDGET PROCEDURES MODEL READ Read and check a model file INFO CL info struct CALC Compute model data FIT General model fitting widget Results are stored in the model The general model fitting widget displays all components of the model and the parameters associated with each one of them Whether or not all or a subset of parameters are constrained by the data is not determined by AMOEBA but has to be decided by the user However since a SVD algorithm is used for the fitting no crash will occur if too many fit parameters are selected and the design matrix becomes singular Characteristics on control parameters of the non linear iterative fit can be modified using the FITICONTROL widget Data selection for the model fit comprises all data sets with a non zero weigh
71. ble GlassCode NumGlass integer ExFrac NumGlass double ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double ExtCatEyeConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser lt integer 163 Theta NumLaser lt _integer gt ThetaErr NumLaser lt _integer gt Phi NumLaser lt _integer gt PhiErr NumLaser lt _integer gt LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double
72. braries A Makefile is used to compile the C code whereas a command file c pro is used to compile the scripts Note that the compilation order in c pro has some significance as functions in general have to be compiled first that is before they are used in any procedure In the GUI source code directory idl type idl c to start up IDL and have it compile all procedures and functions The command file will also save the compiled code to oyster cpr and the common block definitions to oyster cmb If you would like to change the way a procedure works in your OYSTER session make a copy of the source code call it myfile pro for example modify it and recompile it using run myfile pro For your current session this compiled new code will replace the previous one It is a good idea to place modified routines into a file and compile them after startup 6 1 1 Script library files Here we list the files in italics which contain IDL code The itemization is not complete however and only intended to provide an overview of some 50 000 lines of code Note that except for the IDL specific widget libraries all code is in the same area common e OySTER oyster pro Contains the setup script and common data functions idlfunctions pro Functions which exist in PV WAVE CL but not IDL wavefunctions pro Functions which exist in IDL but not PV WAVE CL functions pro Math and miscellaneous functions time pro Date and time conversi
73. cing and calibrating the data scan data should be written to an output HDS file The filename is derived from the input filename except that the extension is now cha The input con file is closed automatically before opening the ouput file Note that if the file already exists objects are replaced with the new ones Data can also be written to a multi source FITS file It is the scans complexvis data being written calculate it after the calibration using CALIBRATE VISIBILITY SETCOMPLEX ACCESS WRITE cont d HDS Write all objects to HDS file FITS Write multi source FITS file SYSCONFIG GEOPARMS Write earth parameters GENCONFIG Write general configuration 90 CHAPTER 18 TABLES SCANTABLE BG TABLE Logs CoNLoa DATA SCANS 18 3 Reduce visibility data BASIC WIDGET PROCEDURES Write table of visibility scans Write table of background scans Observers log Constrictor log Write scan data The goal of this step and the next one concerning the reduction of the delay data for astrometry is to prepare the point data for averaging This involves editing the background and point data and the dispersion correction of the delay data if needed for astrometry It is recommended to first edit the background data which is always loaded for all stars due to the relatively small size of the corresponding object Thus when the point data for a specific star has been edited the averaging will make used of ba
74. ckground data that has been already processed The averaged data will be stored internally in an array of structures scans which is allocated the first time average is called This array will eventually hold all averaged scans Do not forget to average the point data before loading new point data as the old one will be overwritten REDUCE BG DATA PLOT PROCESS BG EXPAND BG DEFAULT BG FLAGTABLE SAVE LOAD APPLY CLEAR UNFLAG RESET POINTDATA IMAGING PLOT A R TRIPLE UNWRAP TRIPLE CLEAR DATA FLAGTABLE SAVE Plotting and editing Fix flagged data Fill in non existing scans Set default BG data Background flag table Store to disk file flg Read from disk file flg Fully apply flags from table Initialize flag table Specify flags to be removed Unflag all data Compute a new triple Unwrap the triple phase Deallocate memory for point data Point data flag table 18 4 REDUCE DELAY DATA 91 LOAD APPLY CLEAR UNFLAG RESET AVERAGE Average currently loaded point data 18 4 Reduce delay data For the reduction of astrometric delays corrections from atmospheric dispersion and array metrology have to be computed They are applied during averaging of the point data into scans Metrology correction can also be applied to the scan data later in which case one would initialize these data before averaging The procedure is as follows for the metrology open the appropriate INCHWORM output file and load a motion group us
75. components is built up incrementally between phase self calibrations The CLEAN algorithm is controlled with a slider widget to adjust the number of components to be added to the model updating the residual image for each component added or subtracted PEARL will work with the complex visibilities which have to be initialized with the observed visibility and closure phase data using the set_complexvis procedure For testing purposes if PEARL is called directly after computing model visibilities with calcmodel the complex visibilities used by PEARL correspond exactly to the model The PEARL widget has two HELP buttons for further information on how to use it The final PEARL image consists of a white light image and two maps one of the effective temperature and the other one of the surface gravity Together these fully constrain images of stellar surfaces and multiple stellar systems 29 2 Beam procedures and functions displaybeam starid lt _char gt Procedure compute the dirty beam for a given star and display it on the screen Example displaybeam FKV0621 contourbean starid lt _char gt Procedure plot a contour map of the dirty beam cleanbeam beam Function return parameters of an ellipse fitted to the half maximum points of the dirty beam Example print cleanbeam dirtybeam FKV0621 151 152 CHAPTER 29 INTRODUCTION Part XI Appendices 153 Appendix A Plot variables and their indices Some data selection
76. ctroscopic binary Single lined spectroscopic binary with astrometric orbit Triple with velocity curves of close pair Triple with velocity curves for all components 9 2 Model manipulation 9 3 Auxilliary data CONTENTS CONTENTS 5 10 Programmers reference 51 10 1 Organization of data 51 III STARBASE 53 11 Introduction 55 About STARBASE ee MUROS Te RUE PCR Gees 55 11 2 The format of 55 11 3 Available primary 58 11 4 Bueusage oi os ERG Eee Pe PL ewe 60 12 How to work with STARBASE 61 12 1 Introduction eins wed Br mut de Dae ubi A ue maed 61 12 2 Managing a calibrator 61 13 Command line procedures 63 13 1 Allocate l ad 5 63 13 2 Read entire primary catalogs 63 13 3 Print Hist Normalen ita ar Ege A rat ita y 64 134 ASS TT 64 13 5 Plot data from the 5 65 13 6 Stellar parameters from calibrations of spectral 65 13 6 1 Absolute visual magnitudes 65 13 6 2 Massa S ono eR ala Bar RS UC 66 13 60 97 Gravitles au xm uA Dx 66 13 6 4 Effective 66 13 6 5 Diameters e 222 on
77. cz models Only model atmosphere available so far is ip00k2 pck19 e Parameters used diameter LD pa ratio model teff logg Type 8 e Semi analytical transformation using stellar profiles directly from Aufdenberg models Models are only available upon request e Parameters used diameter LD pa ratio model teff logg 7 4 4 Miscellaneous stellar disks Type 9 e Numerical transformation of elliptical uniform disk for test purposes e Parameters used diameter pa ratio teff logg Type 10 e Elliptical Gaussian disk e Parameters used diameter pa ratio teff logg Type 11 e Pearson disk Produces exponentially decaying visibilities e Parameters used diameter pa ratio teff logg 42 CHAPTER 7 INTRODUCTION 7 4 5 Images OYSTER handles two types of images one being the classical type FITS image or image cube the other one being the PEARL image The latter is a parametric image assigning an effective temperature to each pixel Type 12 e FITS image cube The filename is given in model If a non zero positive diameter is specified its value position angle and axis ratio are used as CLEAN beam parameters which is deconvolved from the image i e the visibilities are divided by ther transform of the Gaussian CLEAN beam e Parameters used model diameter pa ratio Type 13 e PEARL image As described for type 12 visibilities can be normalized by a CLEAN beam e Parameters used model dia
78. dConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 double APPENDIX E INCHWORM FILE STRUCTURE WindDirConf NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt CrossEnv NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt SysLog lt _char gt ConstrictorLog lt _charx gt ScanData Table NumScan lt integer ScanID NumScan lt integer StartTime NumScan double StopTime NumScan lt double InchwormLog lt _charx gt NumMap lt integer Map NumMap SidMetMap NumPlate NumLaser lt integer LaunchEnd NumLaser MetAirTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer RetroEnd NumLaser MetAirTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer ExtCatEyeMap NumPlate NumLaser lt integer LaunchEnd NumLaser MetAi
79. data base widget Must own home directory 96 CHAPTER 18 BASIC WIDGET PROCEDURES CAL gt CHA Convert Mark III cal files to cha format List SUMMARY Summary SCANS Stars and scans BGSCANS BG Scans SCNLOG Scan log observer star log OBsLoa Observer log CoNLoG CONSTRICTOR parameters STARS StarTable information on star STAR Catalog information on star FORMS SCANFORMS Print scan and BG scan lists SPECFORMS Print spectrometer forms 18 6 1 Catalog access In order to obtain information on the observed stars click on UTILITIES LIST STARS If a scantable is loaded you will be presented a list of observed stars from which to select Otherwise you have to enter a star name Chapter 19 Command line procedures In this chapter we list some of the useful command line procedures Note that not all tasks e g plotting are be performed easily at this level for which therefore widget routines have been implemented However since all data is available at the command level feel free to analyze it using IDL In the following italic names e g value have to be replaced with variable names if no type is specified in the procedure usage description they will be allocated automatically and return the data requested If a type is specified e g value double the variable must be declared and initialized before Optional arguments are in square brackets e g status if several optional arguments are listed only one can be selected
80. dial velocity in km s Wavelengths The wavelengths corresponding to elements of the magnitudes array in the stellar parameter section Any number of elements is allowed In microns Name Component Single character string A B etc WMC WMC designation of component e g Aa Type Integer described in the following section Model Kurucz atmosphere model to use e g ip00k2 pck19 or name of Aufdenberg atmosphere without dat extension In case of images the filename 7 3 THE HIERARCHICAL STELLAR SYSTEMS MODEL FORMAT 39 SED Name of XDR file which restores wavelength and flux f in equal wavelength bins if to be used to define the SED of a component Mass In units of the solar mass Diameter In milliarcseconds Ratio Axial ratio minor major axis elliptical components or CLEAN beam PA Position angle of major axis Hole Disk hole in milliarcseconds Omega Ratio of axial rotation rate to breakup rate type 14 or ratio of axial rotation rate to orbital rate WD Tilt Inclination of rotation axis zero is pole on Teff Effective temperature in K 0 Set intrinsic flux to 1 0 Use blackbody law gt 0 Use model atmosphere Logg Logarithm of surface gravity gr Exponent in gravity darkening law convective envelopes 0 3 radiative 1 0 albedo alpha Temperature exponent in passive disks magnitudes Apparent visual magnitude These are converted to flux factors a
81. ding the data for stars you will be presented a widget listing all observed stars Click on the one whose data you need Under IDL press the control key when selecting the stars with the left mouse button This way the previous selections will not be undone Alternatively you can drag the mouse over the list and highlight a group of stars After selecting the stars click on Load and the loading commences The data will overwrite any point data currently loaded The widget will stay active The way to proceed is to fully reduce the data for one or more stars at a time editing dispersion correction and averaging The averaged data are stored in a structure which is allocated the first time you average data and which is sized so that it will eventually hold all the scan data of the night 18 2 4 Load scan data CHAMELEON can read its own output file Use AccEss LOADJINTERFEROMETRY if you need to re start CHAMELEON to work on averaged data This will read all relevant objects in a cha file get a startable for the observed stars and compute derived quantities CALIBRATE ASTROMETRY CALC Configuration items can also be read separately using but tons ACCESS LOAD SYSCONFIG 18 2 5 Load metrology data This button is used to load metrology data processed by INCHWORM These files have the inch extension ACCESS LOAD cont d METROLOGY Display widget for selection of metrology data to load inch file 18 2 6 Write data After redu
82. e NumPoint NumTripleChan lt real ComplTripleErr NumPoint NumTripleChan R I lt real SidMetData NumPlate NumData lt integer TimeStamp NumData lt integer Data NumData NumLaser plate integer OptAnchData NumPlate MaxNumCluster NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumLaserMax plate cluster lt _integer gt Pier2PierData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumLaser plate lt _integer gt ExtCatEyeData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumLaser plate lt _integer gt PlateExpData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumLaser plate lt _integer gt MetAirTempData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor plate lt _word gt MetSolidTmpData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor plate lt _word gt MetPressureData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor plate lt _word gt MetHumidityData NumPlate NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor plate lt _word gt LabAirTempData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _w
83. e Science Data Center 1982 NAME VAR BSC HDN RA DEC PMRA PMDEC RV PX MV BV UB RI SPECTRUM TYPE1 TYPE2 CLASS1 CLASS2 e BAT Eighth Catalog of the Orbital Elements of Spectroscopic Binaries Batten Fletcher amp MacCarthy 1989 NAME BAT HDN MV SPECTRUM TYPE1 TYPE2 CLASS1 CLASS2 A E LO N P T K1 K2 MF MISIN3I M2SIN3I AISINI A2SINI e FLN A Finding List for Observers of Interacting Binary Stars Wood et al 1980 FLN HDN MV SPECTRUM TYPE1 TYPE2 CLASS1 CLASS2 P T e WDS Fourth Catalog of Orbits of Visual Binary Stars Worley amp Heintz NAME WDS ADS RA DEC MV DMV SPECTRUM AELON ET 60 CHAPTER 11 INTRODUCTION 11 4 File usage STARBASE accesses the following primary star catalogs in catalogs o fk5 fk5 dat bsc4 bsc4 dat hipparcos hip_main dat hipparcos input hipp dat batten sb8 dat skycat hdn dat findlist findlist dat e sao sao dat e wds wdsorb dat STARBASE accesses the following secondary star catalogs in catalogs e hdn HDN xdr e mir MIR xdr e cal CAL xdr e bbc BBC xdr It also accesses lists in catalogs npoi namely e diameters bsc Compiled from various sources e ubv hdn Mermilliod 1991 e ubvri hdn Nagy amp Hill 1980 e uvbybeta hdn Hauck amp Mermilliod 1990 o jhk hdn 2MASS at IPAC e feh hdn Cayrel de Strobel e al 1985 e parallaz hdn van Altena et al 1991 e toe bsc from Bright S
84. e averaging the data Then use use CALIBRATE SYS TEM to bring up the system calibration widget Both squared visibili ties V2Bias and triple amplitudes TABias if two or more baselines are on the same detector need to be plotted but only for spectrometers without interpolated bias corrections from CON STRICTOR Plot all fits for all channels for every configuration The fit coefficients are stored in the genconfig v2bias and genconfig tabias variables If scan selection directive All is selected the fit coefficients will not be stored Then re load the back ground data get_bgdata and re average The bias coefficients will be written into the output file with the averaged data when done after the calibration Note that the triple amplitude bias correction currently is not handled in a strict fashion This is because it is the complex triple product which is biased CONSTRICTOR applies a correction to the complex triple product based on Poisson noise if all three baselines are from the same detector The remaining biases studied as mentioned above in the amplitude are due to non Poisson detector statistics If the amplitudes require additional bias compensation so would of course the closure phases But this is not currently done for lack of an analytical expression for the bias Another issue with the bias correction using incoherent scans is that they are currently com bined in a single fit whereas ideally each coherent scan would be
85. e component designation filter name the Julian date of observation and value and error of the magnitude measured The filter names must be one of Hp U B V R and I ABC V ABC V ABC V 2445249 299 2445249 304 2445249 313 2 60900 0 001 2 60000 0 001 2 59200 0 001 7 3 THE HIERARCHICAL STELLAR SYSTEMS MODEL FORMAT 37 7 3 The Hierarchical Stellar Systems Model Format In a hierarchical stellar system the separation between two neighboring stars is always much smaller than the separation of this pair from the next companion in the system be it another pair or a single star Hierarchical systems are dynamically stable and therefore by far the most common type encountered They are also numerically easier to handle than non hierarchical systems since each pair can be described with the standard orbital parameters and each star with a small number of physical parameters Because AMOEBA is designed to combine different data sets the HSSMF eliminates parameters only specific to one dataset in favor of replacing them with physical parameters such as masses luminosities etc It is important to not over determine the model i e to allow one or more parameters to be functions of others The following illustrates an example for a triple star Algol Global parameters starid 2 FKVO111 wavelengths 0 550 0 800 rv 4 0 3 Star parameters for each star name 0 gt A type 0 1 mass 0 3 67 diameter 0
86. e first entry in its packet but the sixth One word on the BeamCombinerID It is one for the 3 station combiner 2 for the 6 station combiner and 3 for the 6 station combiner used for astrometry The only difference between the last two cases is whether or not the white light a Lab fringe modulation needs to be doubled If BeamCombinerID 3 then the modulation has to doubled 24 5 Running CONSTRICTOR Type home cah constrictor constrictor You will see a prompt This is KEYIN communication you can modify parameters inter actively which you should NOT unless you edit the parameter file accordingly Type e g 1997 08 02 par and KEYIN will read the parameter file Type show and you will get the current setting of the parameters Then if everything is OK check carefully hit CON STRICTOR will now open all files create packet listings which are saved in the dir files or read a dir file if available from rawlist and process all data falling in between StartTime and StopTime At the end you will be returned to KEYIN at which point you should type quit to exit CONSTRICTOR 24 6 Programmer s reference Parts of CONSTRICTOR got fairly complicated over time due to pecularities of the raw data the requirement of backward compatibility and other issues Part VII INCHWORM 131 Chapter 25 Introduction INCHWORM written by N Elias II is not part of the OYSTER software but we document a few inst
87. ed NPOI raw data for analysis and display There is also a small class of procedures which read packets directly from a NPOI raw file These are described at the end of this part 26 1 Reading raw HDS scan files In the first implementation of optional raw data output in CONSTRICTOR NPOI raw data of a scan was written into a single HDS formatted file However long scans e g scans for atmospheric studies exceed 30 minutes and the advent of the 6 way fringe engine made the current logic necessary which is as follows Scans will be divided into sub scans which have an additional extension after the scan number identifiying the sequence number Sub scan files can still be read individually but the standard procedure is to read and concatenate at least the time stamps and delay line metrology data from all sub scans and then to read the fringe data individually get_rawdata file_spec lt _char gt Procedure to read raw time and delay data from one or more sub scan files specified by file spec Example get rawdata 2001 10 25 raw 013 Note that one does not include the sub scan extension as the procedure itself checks how many sub scan files are present on disk The data from all files found is read and concatenated If there is only one sub scan file it will be left open If no file is specified it is assumed that a file is open in which case the time and delay data of just this file will be read The file will be left open get_bincou
88. ed all phase bins are always selected Examples displayframe bincounts 0 0 displayframe bincounts 0 0 0 99 rotateframe c a g Function Apply rotation by group delay d and airpath a to fringe frame c and return rotated frame fringeframe a g l v n poisson Function Return a simulated fringe frame for a given path in air a delay tracking offset group delay g wavelength grid 1 visibility amplitude v and photonrate n Optionally include Poisson noise a and g can be arrays as well as v and n The number of bins is inferred from the genconfig numbin variable The default number of bins is 8 26 3 Visibilities fringevis bincounts K Function Return complex visibility for bincounts The parameter k selects a partic ular baseline i e fringe frequency Examples v fringevis bincounts 0 7 which returns the complex visibility of channel 1 and the baseline with the frequency number 7 If no sub array of bincounts is selected then the returned visibility array has the same dimensions as the input minus the bin index fringevissq bincounts lt real gt k n Function Return the averaged squared visibility amplitude for bincounts The parameter n selects how many samples will be averaged 26 4 FRINGE DELAYS visrotate v d Function Return rotated complex visibility for input visibility v wavelength scale l and group delay d 26 4 Fringe delays fdldelay baseline spectrometer
89. ed in a plot for each plot class is specified in the plot procedure associated with the new plot class Part VI CONSTRICTOR 121 Chapter 23 Introduction For completeness sake we include here a description of the raw data averaging software called CONSTRICTOR which produces the input files for OYSTER CONSTRICTOR is written in C but uses a mixed C and FORTRAN library for HDS file access This library is described in the OYSTER manual CONSTRICTOR reads NPOI raw data files and observation logs and decodes and integrates data such as visibilities delays photon rates etc NPOI raw data is written by the embedded system in form of packets with different types depending on which data they hold The packet definitions are contained in packetdefs h The packet headers all conforming to the same format contain information as to the type of the packet its length and a time stamp CONSTRICTOR first reads the packet headers from all raw files associated with one night of observing and creates a combined packet directory in which all packets are in chronological order Packet directories for the individual raw files are stored on disk working directory and can be read later for a faster restart on CONSTRICTOR should that become necessary More recently OYSTER has been upgraded to create these auxiliary files for CONSTRICTOR with the added benefit of additional data integrity checks CONSTRICTOR then reads the FILE HEADER and SYS CONF
90. ensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double LabPressConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 lt double LabHumConf NumSensor lt integer SampleInterval integer Chain NumSensor integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 double DLPressConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double 178 Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt CrossEnv NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt FBPressConf NumSensor lt _integer gt SampleInt
91. er s Guide in separate parts Also introduced are two new collections of scripts COBRA which provides functions for the interactive analysis of raw interferometry data NPOI only and PEARL which images interferometry data As of 2014 OYSTER has evolved into a package also supporting the reduction and analysis of data from interferometers other than NPOI This includes the GUI front ends MyMidiGui and MyAmberGui to the MIA EWS Attp wuww strw leidenuniv nl nevec MIDI indez html and amdlib http www jmme fr data_processing_amber htm data reduction softwares for MIDI and AMBER at VLTI respectively Also observation planning and advanced data analysis is available in OYSTER Stand alone reduction of data from other interferometers is not planned to be included in OYSTER since this involves obviously very instrument specific tasks Data of other interferometers can be read and modeled by OYSTERif they are stored using the OIFITS format http www mrao cam ac uk research OAS oi_data oifits html 1 2 About this guide This is not only a manual on how to use the OYSTER software but a reference as well on how the procedures work Study of the Programmer s reference sections should enable you to write and add your own procedures to the software or create modified copies of existing routines which replace the latter if they are compiled during a session 1 3 Fonts used in the guide In order to facilitate reading this manual various fonts
92. erferometer specific information is encoded in oyster pro Chapter 5 Plotting and editing We describe here all OYSTER plotting and editing procedures For calibrated visibility data as well as other data from e g astrometry the user will select plotting menus from the so called AMOEBA lower section of the main OYSTER GUI While AMOEBA is described later on in a dedicated part of this manual it is the general data analysis as compared to reduction facility of OYSTER The following plot menu is available PLOT INTERFEROMETRY Plot visibility data ASTROMETRY Plot p 0 data SPECTROSCOPY Plot radial velocity data PHOTOMETRY Plot magnitude measurements Each of the above buttons will display a widget designed for this class of plot Plotting of interferometry data is handled by the same routines as used in CHAMELEON see dedicated part on this NPOI data reduction facility 5 1 Interferometry Most of the plots of interferometric data in OYSTER are handled by one procedure plotdata Consequently there is one widget handling the plot selection ww plot Whenever a plot is requested a selection widget designed for that class of plot point scan astrom etc is opened replacing any currently displayed selection widgets from previous requests A second widget is created for the selection of which indices to plot if this input is required Plots can be 2 dimensional or 3 dimensional Therefore three data streams x y and
93. erometric data files handled by CHAMELEON use the HDS Hierarchical Data System format and have an extension con for point data files output by CONSTRICTOR and cha for scan averaged data output by CHAMELEON Think of the HDS format as a UNIX directory file tree contained within a single file Thus individual objects can be accessed and modified directly without having to read through the file until a specific section The con files are found in data npoi con on gemini Output files produced by CHAMELEON are always stored in the current working directory Aside from the data file three types of auxilliary files can be written files with extension flg XDR format contain the flag tables for interferometric data cal XDR format contain the calibration table and stn ASCII contain fitted station coordinates These files are only written 79 80 CHAPTER 16 INTRODUCTION by request never automatically As to auxilliary input files all these reside in the following directories of the OYSTER home directory The files used by STARBASE are listed in section 11 4 1 e usno mark3 dat the UT1 UTC and polarmotion data from the EO department of the US Naval Observatory e npoi stations config fdl config 3way config and 6way config array geometry configuration files and biasbase zdr obsbase rdr linear xdr and skycoord zdr the bias correction data base observation data base flux ratio file due to detector non linearity and star
94. erval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 lt double WxAirTempConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 lt double WxPressConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double WxHumConf NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 lt double WindSpee
95. es 120 22 5 2 Adding plot classes cia A Rob ee Rok ni 120 VI CONSTRICTOR 121 23 Introduction 123 24 How to use CONSTRICTOR 125 241 raw data files i sa caraga auca means ai RR UR PR S ROS 125 24 2 Preparation of parameter file 125 24 3 P r meters at 2 2 we GR A are Roe y Roue pL 126 24 A System config ration uk wann are Dada See uota Ba 127 24 5 Running CONSTRICTOR s 130 24 6 Programmer s reference 130 VII INCHWORM 131 25 Introduction 133 VIII COBRA 135 26 Introduction 137 26 1 Reading raw HDS scan files 187 20 2 Frames 75 5 4 o ti acad ml xe rS ida 138 263 Visibilities i iE tene a A en ae eee e WO ele RURSUS EUR RS 138 20 4 Fringe delays 2 20 2 au domo gos 5 Roh 139 26 5 Photon rates 2 04 cR BG RSS E hye xk EGRE EAR 139 20 6 NAT data x ars neo oer tre ees UR BLE GYF MOR la d 139 26 7 Compound plot procedures 140 27 NPOI raw packet data files 143 IX VOLVOX 145 28 Introduction 147 28 1 About VOLVOX 147 CONTENTS 9 X PEARL 149 29 Introduction 151 20 1 About PENRI Lira a A A a 151 29 2 Beam procedures and 151 XI Appendices 153 A Plot variables and their indices 155 B CONSTRICTOR
96. et NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 lt double LocErr NumSensor 3 lt double MetSolidTmpConf NumPlate NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 lt double LocErr NumSensor 3 double MetPressConf NumPlate NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3 lt double LocErr NumSensor 3 lt _double gt MetHumConf NumPlate NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt Cross NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt LabAirTempConf NumSensor lt _integer gt SampleInterval lt _intege
97. et is opened for a stream when the selected axis item requires further user input However if the NOTRACE option is de selected the default such a selection widget will not be activated for the x stream which will be assigned the selection of the y stream In the data selection widget input beam output beam and triple have to be specified depending on the selected axis item The selection for channels baselines and points are for this input output beam or triple only The ALL OB option is valid only for uv coverage plots where it implies that the data of all output beams channels and baselines shall be plotted A data selection for a specific index e g channel is made by combining a directive ALL NEXT CURRENT PREVIOUS SELECTED with a selection typed into the selection line A selection line entry is a series of numbers separated by commas and or number ranges consisting of a lower and upper value separated by a dash This entry is parsed into a vector of selected index values e g 2 3 6 9 is parsed into 2 3 6 7 8 9 Please do not forget to hit return after typing in your selection line entry NEXT and PREVIOUS return a selection of the next or previous n index values where n is the number of selected index values in the selection line Thus if the selection line reads 1 2 NEXT will select 3 4 for the next plot then 5 6 and so on It is not recommended to select these directives for m
98. etaErr NumLaser lt _integer gt Phi NumLaser lt _integer gt PhiErr NumLaser lt _integer gt LaunchInfo NumLaser NumGlass lt _integer gt NumAirGap lt _integer gt Loc 3 lt _double gt LocErr 3 lt _double gt GlassThick NumGlass lt _double gt GlassThickErr NumGlass lt _double gt GlassCode NumGlass lt _integer gt ExFrac NumGlass lt _double gt ExFracErr NumGlass lt _double gt AirGapThick NumAirGap lt _double gt AirGapThickErr NumAirGap lt _double gt RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt double ExFracErr NumGlass lt double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double MetAirTempConf NumPlate NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor lt double ScaleErr NumSensor double CrossEnv NumSensor lt double Loc NumSensor 3 double LocErr NumSensor 3 lt double MetSolidTmpConf NumPlate NumSensor lt integer SampleInterval integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor
99. fied and use the top hierarchical component if no component is specified If a component is specified so must be the epoch If com 1 compute relative to center of mass not center of brightness In the latter case one can specify lambda in meters for the wavelength to use If abs 1 return individual component positions instead of relative position In that case the component index is in the first dimension p 0 are in the second 49 50 CHAPTER 9 COMMAND LINE PROCEDURES modelk component lt _char gt Function Return velocity semi amplitude for component Examples PRINT MODELK A PRINT MODELK AB modelpx component lt _char gt Function Return parallax derived from parameters of the specified component Note that for systems higher than binaries the results could be inconsistent indicating an inconsistent set of model parameters 9 3 Auxilliary data set_parallax value error weight weight Set a value for the system parallax Set weight to zero to ignore stored value to positive value to re instate if neither value nor error are provided Set value to 1 to enforce the same parallax for all binary components without enforcing a specific value Chapter 10 Programmer s reference 10 1 Organization of data AMOEBA data is exclusively contained in the ScanData common area whereas the model data resides in the Model common block If some currently loaded data have been manipulated they have
100. file is given in sed and should restore variables and f which contain the wavelength in meters and the flux per wavelength interval respectively In many models specifying pa and ratio is used to rotate and stretch the u v coordinates The only exceptions are the images if a positive non zero diameter of the CLEAN beam have been specified 7 4 1 Uncorrelated flux component Type 0 e The correlated flux of this component is zero 7 4 2 Uniform disks Type 1 e The disk diameter is independent of wavelength e Parameters used diameter UD pa ratio Type 2 e The disk diameter scales with wavelength d 1 7u 15 1 1 3 where u is the linear limb darkening coefficient e Parameters used diameter LD pa ratio teff logg 7 4 3 Limb darkened disks Type 3 e The linear law is used for an analytical result The coefficients are from Van Hamme e Parameters used diameter LD pa ratio teff logg 7 4 STELLAR MODELS 41 Type 4 e The logarithmic law is used to produce maps which are then Fourier transformed e Parameters used diameter LD pa ratio teff logg Type 5 e Linear law with coefficients directly from Kurucz models e Parameters used diameter LD pa ratio teff logg Type 6 e Hestroffer law with coefficients directly from Kurucz models e Parameters used diameter LD pa ratio teff logg Type 7 e Semi analytical transformation using stellar profiles directly from Kuru
101. for the MaxPacket parameter in the parameter file Also check if the data at the tail of the listing is from the same night as the data at the beginning If the timestamps are not monotonically increasing in the entire listing this is an indication that DATAcon crashed and you are looking at data from a previous night at the end of the disk EXCEPTION for metrology data if there is no END OF DISK packet another file for the same siderostat see extension number might have it if the file was broken into two or more pieces 125 126 CHAPTER 24 HOW TO USE CONSTRICTOR 24 3 Parameters InFiles The order of the input files is irrelevant DirFiles These must be in the same order as InFiles and MaxPacket MaxPacket The maximum number of packets to process for each file DayNumber Even though this number is in the data some packet headers have the wrong number and it makes it a whole lot easier to have the user check and enter this number correctly If observations started before 0 UT choose the day number of that previous day CONSTRICTOR will add a multiple of 24 hours to the time tag when the day number changes Remember to set the StopTime to say 48 hours if you use a DayNumber of one less than the actual day number Start Time StopTime These times are for day number corrected time tags i e if the day number changes during the observations 24 hours are added to the tags and compared to the Start Time and StopTime parameters
102. ge area DATE Enter a date and display the position EDIT Edit data No flag tables used OPTIONS ERRORS Display error ellipses FLAGGED Display flagged data too ELLIPSE Superpose apparent ellipse ORBIT Superpose apparent orbit J2000 Precess observations to J2000 before plotting COLOR For hardcopies use color SUBMIT Submit hardcopy file to printer 5 3 SPECTROSCOPY 27 5 3 Spectroscopy UTIL IDENTIFY Identify data points WINDOW Change display area RANGE Enter new range of display EDIT Edit data OPTIONS ERRORS Display error ellipses FLAGGED Display flagged data too PHASE Plot as a function of phase instead of time Use the period of that orbit where the selected component appears alone Subtract the systemic velocity of that binary component ORBIT Superpose apparent orbit 5 4 Photometry UTIL IDENTIFY Identify data points WINDOW Change display area RANGE Enter new range of display EDIT Edit data OPTIONS ERRORS Display error ellipses FLAGGED Display flagged data too PHASE Plot as a function of phase instead of time Use the period of that orbit where the selected component appears alone Subtract the systemic velocity of that binary component ORBIT Superpose apparent orbit 28 CHAPTER 5 PLOTTING AND EDITING Chapter 6 Programmer s reference 6 1 Code All source code resides in oyster source subdirectories common idl and c as well as the directories for the HDS NOVAS FITSIO and WD code li
103. han beam NumScan lt _REAL gt BACKGNDRATE NumSpecChan beam NumScan lt _REAL gt per coherent integration BACKGNDERR NumSpecChan beam NumScan lt _REAL gt TRIPLE NumTriple lt EXTCOLUMN gt COMPLTRIPLE 2 NumTripleChan triple NumScan lt _REAL gt COMPLTRIPLEERR 2 NumTripleChan triple NumScan lt _REAL gt TRIPLEAMP NumTripleChan triple NumScan lt _REAL gt TRIPLEAMPERR NumTripleChan triple NumScan lt _REAL gt TRIPLEPHASE NumTripleChan triple NumScan lt _REAL gt TRIPLEPHASEERR NumTripleChan triple NumScan lt _REAL gt TRIPLEAMPC NumTripleChan triple NumScan lt _REAL gt TRIPLEAMPCERR NumTripleChan triple NumScan lt _REAL gt TRIPLEPHASEC NumTripleChan triple NumScan lt _REAL gt TRIPLEPHASECERR NumTripleChan triple NumScan lt _REAL gt INPUTBEAM FDLPOS FDLPOSERR GRPDELAY GRPDELAYERR DRYDELAY DRYDELAYERR WETDELAY WETDELAYERR NATJITTER NATJITTERERR NumSid lt EXTCOLUMN gt NumScan lt _DOUBLE gt NumScan lt _REAL gt NumScan lt _DOUBLE gt NumScan lt _REAL gt NumScan lt _DOUBLE gt NumScan lt _REAL gt NumScan lt _DOUBLE gt NumScan lt _REAL gt NumScan lt _REAL gt NumScan lt _REAL gt m relative to ReferenceStation m including group delay m dry air dispersion corrected m wet air dispersion corrected Appendix D COBRA file structure The HDS file format of raw data is described here SESSI
104. he previous session These files are not written automatically for reasons of greater flexibility Please also note that tables loaded are not automatically applied Look at the tables as logs containing information on flags and calibration entries If you want to load point data and apply flags from a previous session or want to undo specific actions on the scan data these tables are useful In order for them to be up to date you should load any existing table before you do additional editing or calibration If you want to start over with e g the calibration then you should also start a new calibration table by clearing any loaded table with UNDO RESET in the calibration widget which also initializes the calibrated data for the selected variable to be equal to the uncalibrated data 17 1 Open the data file FILE OPEN select a CONSTRICTOR file with a con extension Please do not double click Bug feature in the communication of IDL with X windows This can cause your session to crash 17 2 Read configuration information create tables and load data ACCESS LOAD INTERFEROMETRY will load Date SystemId GenConfig and GeoParms create the Scan Table and BGTable load the background scans and display the point data loading widget see below 83 84 CHAPTER 17 QUICK GUIDE 17 3 Print form sheets UTILITIES FORMS click on SCANFORMS and SPECFORMS to get printouts of form sheets They should be used to log information about the d
105. hich one can compute model values using calcmodel after reading a model file calcmodel will compute the complex visibilities scans complexvis and squared visibilities scans vissqm If one wants to write this data into a FITS file nothing needs to be copied since the procedure put_fits uses the complex visibilities to derive the FITS visibility 112 CHAPTER 20 DISCUSSION OF REDUCTION ISSUES variables amplitude and phase If noise is to be added to the visibilities it should be added to the real and imaginary parts of scans complexvis The data can then be mapped in AIPS with or without using phase self calibration Chapter 21 HDS procedures We list here all available procedures for the HDS access Italic names e g value have to be replaced with variable names they will be allocated automatically and return the data requested If a type is specified e g value lt _double gt the variable must be declared and initialized before Optional arguments are in square brackets e g status if several optional arguments are listed only one can be selected as such and arguments to the left then are compulsory Please refer to the HDS manual for explanations on the individual commands 21 1 hds_ hds_open name lt _char gt mode lt _char gt status hds_new filename lt _char gt name lt _char gt type lt _char gt status 21 2 cmp cmp_shape name lt _char gt ndim dims cmp_get0i name lt _char gt value cmp_get1i name lt _char g
106. ich increases to the left East The relationship between visibility and map is then 120 CHAPTER 22 PROGRAMMER S REFERENCE V u v J BE n ewp j2n u vn d dn 22 4 Command line procedures 22 5 Plotting 22 5 1 Adding plot variables Plot variables are identified by a sequence number in OYSTER and are defined in terms of OYSTER data variables in set plotdata and the corresponding function set ploterr The corresponding plot variable name is defined in the set_axitems function which should have exactly the same ordering The following additional information needs to be entered for each plot variable Each plot variable s ID is entered in set plotlabels for the index label it requires so that it is displayed together with the name in the plots In set plotloops the loop count is set to one for those indices which do not occur in the plot variable These functions and procedures are all found in plotting pro Finally the plot variable s ID need to be entered in ww setxaxis ww setyaxis and set zaxis if it s selection requires and additional index selection by the user 22 5 2 Adding plot classes A plot class is basically defined by the list of plot variables displayed in the x y and z axis selections of the plot selection widget The plot selection widget is recycled upon selecting a different plot class Any plot variable can be put on more than one selection list associated with a plot classes Variables are selected fo
107. idl to compile the IDL installation and make f Makefile gdl to prepare the GDL installation If you need to compile the C FORTRAN external library due to incompatibility of your OS with the pre compiled Linux 64 bit version unpack the src tar gz file to be obtained from the author in the oyster source folder Make sure your OS is either Linux or Darwin checking with the uname UNIX command The Makefiles will use uname to determine which of the pre installed Makefiles in the library directories are used for compilation The only part of the Makefile which still has to be edited manually before running make is Makefile lt uname gt in in source c which needs the path to the local IDL installation as well as the location of the libgfortran a library file Then run the make f Makefile src command in the home folder 2 2 Programmer s reference OYSTER uses an external library oyster so containing C and FORTRAN objects This library must be sharable in order for IDL to access it via the call_external command Aside from the OYSTER specific code written in C this library contains five external libraries These are e HDS Hierarchical Data System STARLINK e NOVAS Naval Observatory Vector Astrometry Subroutines USNO 15 16 CHAPTER 2 INSTALLING OYSTER FITSIO The Flexible Image Transport System I O package HEASARC WD Wilson Devinney binary light curve software U Florida ROCHE Gravity darkening in rotating stars Deane Pe
108. ime NumPar lt _double gt MotCorrFlags NumFlag lt _char gt AllBedrock NumPar lt integer NumPar 6NumPlate Par NumPar lt _charx gt NumCorr lt integer NumCorr NumPar NumPar 1 2 Corr NumCorr lt _char gt ReducedChi2 NumTime double XCorr NumTime NumCorr lt double NumSingVal NumTime integer SingValFlag NumTime NumPar integer WRatio NumTime NumPar lt double Par NumTime NumPar double ParFitErr NumTime NumPar lt _double gt 183 ParThErr NumTime NumPar lt _double gt
109. in a 73 74 CHAPTER 15 INTRODUCTION specific night and array configuration The date of observation is taken from the variable date and the array name from the variable systemid If these are not defined defaults are used for date the next night and for array NPOI As to the system configuration a list of stations can be passed to plotuptime which will then create a system configuration for them get_startable stars lt _char gt Create startable for stars specified read_obslist file lt _char gt Read observation list from file and create startable This procedure only reads the first i e the star column of the file It ignores lines containing an exclamation mark selectup from data nt mintime min Remove stars from startable which are not available Either compute predicted availability default or derive from currently loaded data from_data 1 Use keyword mintime default 3 hours to specify minimum availability after sunset and before sunrise selectnew dates nd scans ns Remove stars from startable which were observed before at least nd times with ns scans or more each The parameters default to nd 2 and ns 4 selectdone dates nd scans ns Remove stars from startable which have not been observed before at least nd times with ns scans or more each The parameters default to nd 2 and ns 4 addstar stars lt _char gt Add one or more stars to the startable Examples addstar FKV0193
110. ing INIT Initialize zero metrology corrections METROCORR Compute delay corrections from pivot point positions 92 ASTROCORR FLAGTABLE SAVE LOAD APPLY CLEAR UNFLAG RESET 18 5 Calibrate data CHAPTER 18 BASIC WIDGET PROCEDURES Obtain delay corrections from INCHWORM file Metro data flag table The CALIBRATE menu unites all procedures working with scan data in order to calibrate it or obtain calibration information The tasks range from calibrating the visibility amplitudes and closure phases to plotting of the channel sensitivities and fitting station coordinates CALIBRATE STARS SYSTEM VISIBILITY PLOT CALIBRATE SETERRORS SETCOMPLEX TRIPLE REWRAPTRIPLE DEWRAPTRIPLE MANUALUNWRAP FLAGTABLE SAVE LOAD APPLY CLEAR UNFLAG RESET 18 5 1 Scan data uv based plotting Channel sensitivities Plot ScanData Calibrate Apply calibration error Fill ComplexVis Unwrap triplephase Unwrap triplephase Unwrap triplephase Scan data flag table The CALIBRATE VISIBILITY CALIBRATE button is for the calibration of visibilities squared amplitudes triple amplitudes and closure phases You will be presented a widget in which to select the calibrator stars and system visibility indicators As for the calibrator stars there are three options to select all an unusual case select according to a flag in the startable derived from information contained in file diameter bsc or to select manually recommended
111. ing AccEss LoAb METROLOGY A motion group is a so lution for the siderostat pivot motion for all or a subset of the laser readings As part of the motion group two types of data are provided one being the x y z coordinates of the pivot the other one being the delay correction In CHAMELEON metrocorr uses the former to compute delay corrections whereas astrocorr only does the interpolation of the corrections computed by INCHWORM to the observed epochs of the data points The result is stored in only one variable metrodelay and can be plotted using the PointData plot widget The dispersion correction is computed from the observed variation of the visibility phase with wavelength Due to the low SNR of the blue channels REDUCE DELAYS PHASEEDIT can be used to flag these Also before computing the correction the closure relations have to be enforced using REDUCE DELAYS PHASECLOSE and the phases have to be unwrapped using REDUCE DELAYS PHASEWRAP After completion of dispcorr the corrections for the white light scans if present can be set to zero if these are too noisy and one would rather use the raw fdl delays REDUCE ASTROMETRY DELAYS PLOT Plotting and editing INITALL Initialize zero all stars INrrW Initialize white light scans only FK V0000 PHASEEDIT Flag channels 11 and 21 32 PHASECLOSE Enforce delay closure PHASE WRAP Unwrap the phases DIsPCORR Compute dispersion corrected delays METROLOGY PLOT Plotting and edit
112. l to the number of stations used a common mistake MAX SID like the other MAX parameters is used to tell CONSTRICTOR the number of places allocated but not necessarily used for the specifications in the KEYIN style system configuration For example OutputBeam StationID in the KEYIN file is a one dimensional array KEYIN does not recognize more than one dimension but needs to be converted to a two dimensional array which specifies for each output beam what stations it contains The MAX_SID parameter is used to determine where in the KEYIN vector the next output beam section begins here after the first 4 numbers Similarly the FRFREQ is used to decode the OutputBeam BiasMod numbers Again the actual number of baselines can be less but not more of course than this parameter allows 130 CHAPTER 24 HOW TO USE CONSTRICTOR Also note that the FDLTankID numbers are used to determine at which position in the FDL_POSITION packet one can find the delay data for a given station This is only true for 6 station data in the case of the 3 station data all three delay lines occupy the first three dimensions in the FDL_POSITION packet The same holds for SiderostatID which actually should have been called SidCon numbers This is because NAT SidModel and Motor counts are stored in the order of SidCon IDs not in the station order CONSTRICTOR uses SiderostatID to put the data into the right place Here for example the E02 NAT data is not th
113. length Baseline Triple Table A 4 Plot variables class metro and their indices IDL name metrotime parx pary parz metropath metropath inbeam ib ib ib ib ib outbeam triple channel baseline Table A 5 Miscellaneous plot variables and their indices IDL name genconfig wavelength inbeam outbeam triple ob ob ob tr channel ch ch point pt pt pt pt pt pt baseline bl bl 157 point 158 APPENDIX A PLOT VARIABLES AND THEIR INDICES Appendix B CONSTRICTOR output file structure The data are in an HDS Hierarchical Data System Starlink Project structure somewhat analogous to a directory structure It differs from a directory structure in that a directory can actually be an array Each element of the array will have the same set of sub directories Since the structure is like a directory tree the order of variables listed below is not meaningful Furthermore variables can be added or removed in the future Therefore this list amounts to a list of the data we think we want and of the names we have agreed to give them In addition to the natural array dimensions such as spectral channel number point number etc we use one more to label the real and imaginary parts of a complex number indicated by R I The uncertainties for complex numbers have three components which may be the major axis minor axis and position angle of the error ellipse For locations we
114. lly and use it instead of the SYS CONFIG packet Make sure this file does not exist in the current directory if you want to use the SYS CONFIG packet instead Here is an example of a system configuration MAX WAV 16 MAX FRFREQ 6 MAX SID 4 Latitude 35 0966666666667 Longitude 111 535 Altitude 2200 66 128 CHAPTER 24 HOW TO USE CONSTRICTOR TDTminusUTC 60 184 UTiminusUTC O InstrCohInt 2 NumBin 64 BeamcombinerID 2 InputBeam NumSid 6 InputBeam StationID E02 ACO AEO AWO WO7 ANO InputBeam SiderostatID 6 1 2 3 5 4 InputBeam Stroke 1 0e 6 3 0e 6 3 0e 6 3 0e 6 2 0e 6 2 0e 6 InputBeam FDLTankID 1 2 3 4 5 6 InputBeam BCInputID 1 2 3 4 5 6 InputBeam StationCoord 01 04 5 599326 1 792619 0 010397 8 429653 InputBeam StationCoord 05 08 0 499984 5 639917 0 000035 13 415900 InputBeam StationCoord 09 12 16 989235 12 896476 0 001264 31 406569 InputBeam StationCoord 13 16 20 389907 15 497607 0 000635 27 541854 InputBeam StationCoord 17 20 44 203123 32 988367 0 081429 56 867758 InputBeam StationCoord 21 24 0 627300 17 212581 0 008760 20 285819 OutputBeam NumOutBeam 2 OutputBeam BCOutputID 2 3 OutputBeam APDArrayID 2 3 OutputBeam NumSid 4 4 OutputBeam NumBiasFreq 1 3 OutputBeam NumSpecChan 16 16 OutputBeam BiasMod 01 06 8 7 10 5 3 5 OutputBeam BiasMod 07 12 1 7 10 8 3 5 OutputBeam StationI
115. lot the calibrated triple phase and fit a low order polynomial to a stretch which does not wrap use FIT The fit parameters are passed to the unwrapping algorithm which removes it from the data and then removes also the resulting steps The fit is then reapplied to the data The manual unwrapping utility MANUALUNWRAP will allow the user to place a box into a plot of phase vs time or channel and the data inside will be rotated 360 or 360 degrees as specified No calibrator stars need be specified for this operation Note that in this case the calibrated phase has to be plotted since this is the phase which is unwrapped 18 6 UTILITIES 95 18 5 4 Astrometry The CALIBRATE ASTROMETRY menu allows you to solve for station coordinates and star posi tions using the delay data Use PLOT to plot the O C data Select input beams higher than one since delays are referenced to the delay in input beam one Use SOLVE to display a selection widget for the astrometric solution A solution will be computed for the selected stations and stars using data only of the selected stars If no star is selected then no star position will be solved for but data of all stars will be used for the station coordinate solution As for the selected data either uncorrected FDL data can be used or the group delay and the dispersion corrected delays Remember that the latter can also include metrology corrections SAVE will write the stationtable to disk
116. mass from m sin i Calibrations are stored in files dwarfs masses spec_mass IV spec_mass III spec mass 11 spec mass I in oyster starbase mass stars Compute masses for stars in startable mass binaries Compute secondary mass mass star spectrum char Function Return mass for star with specified spectrum 13 6 3 Gravities Gravities for stars are derived from their spectral type and luminosity class Calibrations are stored in files spec_logg V spec_logg IV spec_logg III spec_logg II spec logg I in oyster starbase logg stars Compute log g for all stars in startable logg star spectrum char Function Return log g for star with specified spectrum 13 6 4 Effective temperatures Temperatures of stars are derived from their spectral type and luminosity class Calibrations are stored in files spec_par V spec_par IV spec_par III spec par 11 spec_par I in oyster starbase teff stars Compute effective temperature for all stars in startable teff star spectrum char Function Return effective temperature for star with specified spectrum 13 6 5 Diameters Compute stellar diameters in units of the Solar diameter from the spectral type diam stars Compute diameter for all stars in startable diam star spectrum char Function Return diameter for star with specified spectrum 13 7 Limb darkening Linear limb darkening coefficients are taken from tables published by Van Hamme 1993 AJ 106 2096
117. memorize all the commands and their parameters Widgets provide an easy way to set parameter values in common blocks which is how most of the information is passed between functions You may use both operation modes simultaneously Note that widget buttons which bring up another widget are labeled in all caps whereas the other type either displays a sub menu indicated by the arrow or executes a procedure upon selection At the command level you manipulate data using IDL This was one of the reasons to base OYSTER On a language like IDL Note that neither language is case sensitive An understanding of the language is very helpful when reducing data with AMOEBA tries to place the widgets in convenient places on the screen so that there is not too much overlap and so that the plot windows do not cover too many of the widgets The IDL version detects the dimensions of your screen and uses this information for the placements of the widgets OYSTER Procedures usually confirm proper completion of the task with a message terminated with a period In progress messages are not terminated Error messages usually contain the name of the procedure in which the error occurred In case of a crash inside a procedure under IDL click on the terminal window to make it active then try to return to successively higher levels by typing return until a con command causes IDL to resume In this case the widgets if previously displayed will be updated Note that in a cr
118. meter pa ratio 7 4 6 Rotating stars Type 14 e Includes Roche sphere computation and gravity darkening using code library written by D Peterson e Parameters used diameter pa omega tilt 7 4 7 Young stellar objects and disks Type 15 e Hillenbrand passive disk optically thick with temperature profile e Parameters used diameter hole pa alpha tilt Type 16 e DUSTY simulation Reads the radial intensity map scales the shell radii with the given diameter mas and computes the Fourier transform e Parameters used model diameter 7 5 FIT SCENARIOS 43 7 5 Fit scenarios 7 5 1 Single lined spectroscopic binary Select the appropriate orbital elements and the mass of the secondary The reason for not choosing the mass of the primary is that with decreasing primary mass the situation is asymp totically reached where the primary settles on a Keplerian orbit of a planet sized body and its velocity amplitude does not increase anymore This would prevent proper fitting of velocity curves of larger amplitudes If after fitting the corresponding velocity amplitude K is desired one uses the modelk function e g PRINT MODELK A 7 5 2 Double lined spectroscopic binary Add the primary mass as a fit parameter but remember as in the single lined case that these masses are not true masses since it is only the velocity amplitude as a function of several parameters including the masses that it efectively constrained
119. nd applied to the fluxes derived from the effective temperature parameter e Binary Component Name of component character string WDmode WD mode Method 1 Use orbital elements 2 Use p 0 parameters 3 Use p 0 parameters with orbital motion 4 Interacting binary use WD code Semimajoraxis in milliarcseconds Eccentricity Inclination in degrees Periastron in degrees of primary Apsidalmotion in degrees year Ascendingnode in degrees Period in days Epoch Full Julian date periastron passage Rho Separation in milliarcseconds 40 CHAPTER 7 INTRODUCTION Theta Position angle in degrees The model is checked upon reading to make sure all components are defined All wavelength dependent parameters are defined at a set of wavelengths given in the global parameter section and therefore all have to have the same number of elements Polynomials are used to interpolate intermediate values 7 4 Stellar models The type parameter allows to select from a range of stellar models either analytical or availbale as data files or FITS images Please note that a new numbering scheme was introduced with Version 6 12 2 Aug 2007 For all types from zero to 11 the flux distribution is computed as flat teff 0 a black body teff lt 0 or a stellar atmosphere teff gt 0 For all types specifying an arbitrary SED will override stellar spectra or fluxes derived from the images The XDR
120. nd elevation angle in de grees No GeoParms required equatorial2angle coord real Function Return hour angle in hours and declination in degrees for input equatorial coordinates No GeoParms required topostar times lt _real gt stars lt _char gt startable ra dec Compute apparent declinations and right ascensions for a list of times in seconds UTC and corresponding stars The arrays time and stars have to have the same number of elements therefore The startable is a standard STARBASE startable The geoparms structure has to be loaded calcastrom Procedure Compute astrometric variables in scans structure calcvis Procedure Compute estimated visibilities i e normalized visibilities referencestation station lt _char gt class lt _char gt Change reference station for data of specified class default all classes to station precess theta jy ra dec direction Precess J2000 position angles theta to current Julian Year epoch jy for direc tion 1 from current to J2000 for direction 1 see Heintz Double stars p 33 Input theta is in radians dec in degrees ra in hours output is in radians 19 8 Data base routines obsbase files lt _char gt Create if non existent or update observation data base catalogs npoi obsbase as a database of star tables from con or cha files File specification can be either through a string array or or a single wildcard e g files cha You have to have write
121. nfiguration table and raw data get_pointdata file lt _char gt Compound procedure Read point data for all scans Get auxilliary data Open file if necessary get_scandata file lt _char gt Compound procedure Read scan data and auxilliary data from cha file Do astrom etry This command is sufficient to read an entire cha file Open file if necessary get_metrodata file lt _char gt Compound procedure Read metrology data from inch file Also read general con figuration and scantable data Allocate and fill in startable get data file lt _char gt Compound procedure for all of the above Checks file format to see which of the above compound routines will be called to read the data 19 2 PointData manipulation 19 2 1 Astrometry The following procedures are specific to the reduction of point astrometry data dispinit stars lt _char gt class class Initialize the dispersion corrections In order for calibrated delays to be processed by average both dispersion and metrology corrections have to be initialized or computed Initialize zero the dispersion corrections for the specified stars Initial ization for all stars is the default A class ALL POINT SCAN can be specified using keyword class the default is all classes For scan data initialization means setting the dispersion corrected delays equal to the averaged FDL data dispf lag channels beams Flag the visibility phase for the specified
122. ng Two methods are used for phase unwrapping one able to detect the bimodal distribution of wrapped phases the other one using the rewraptriple procedure to remove phase drifts as a function of wavelength cause by excess dispersion in the interferometer 16 3 6 Logging and quality control Upon completion of the npoipipe command the log files will be examined by a npoipipeqc which extracts the most pertinent information of the log files Attention should be paid especially to the calibration errors 82 CHAPTER 16 INTRODUCTION Chapter 17 Quick Guide Here we describe briefly a sample session with CHAMELEON We include tips on how to get organized during the data reduction as this is a time consuming process We also assume that you are reducing output from CONSTRICTOR When re calibrating data however you will usually begin by reading the output of CHAMELEON After starting OYSTER type oyster at the IDL prompt In general we work our way from the top FILE to the bottom CALIBRATE in the displayed OYSTER main widget Also note that button labels are all caps if they bring up another widget All other buttons either open another button list if an arrow is displayed or immediately execute the associated procedure In order to restart CHAMELEON and to continue from where you left it or to get close to this point quickly it can be important that you have saved flag and calibration tables and if applicable the output file in t
123. nt level Store in parameter if given 19 6 DATE CONVERSION FUNCTIONS 103 list_tree List HDS tree beginning at current level list_scans indez List observed scans stars times stations and codes If indez is specified list only these scan IDs list_bgscans List stars and back ground scans list_stars stars lt _char gt List stars present in currently loaded data Store in parameter if given Also list scan numbers and embedded scan IDs The latter listed in parenthesis after the scan number are the scan numbers which were used by the embedded system during the observations list_stations stations lt _char gt List stations loaded Store in parameter if given list_summary_chameleon List summary for observations in CHAMELEON list_summary_amoeba List summary for loaded data in AMOEBA list_logs List all logs i e ObserverLog ConstrictorLog ChameleonLog list_flagreasons class lt _char gt List flag reasons for class specified 19 6 Date conversion functions All inputs for these functions and procedures can be arrays julian year lt _integer gt month lt _integer gt day lt _real gt Function returns Julian day including fraction Day can be fractional Example print julian 1998 12 16 2 jd2date jdf lt real gt year month day Procedure returns year month and day including fraction for input fractional Julian date 104 CHAPTER 19 COMMAND LINE PROCEDURES by2jd year lt _real gt
124. nteger ExFrac NumGlass lt _double gt ExFracErr NumGlass double AirGapThick NumAirGap double AirGapThickErr NumAirGap lt double ExtCatEyeConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser integer Theta NumLaser lt integer ThetaErr NumLaser lt integer Phi NumLaser lt integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass double ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass double ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double PlateExpConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser lt integer Theta NumLaser lt integer 176 Th
125. ntly selected item if other data items exist which depend on the selected one T his means that a particular point of data is unlikely to be valid if the item on which it depends is flagged Thus for example flagging a photon rate point will cause CHAMELEON to flag all visibilities where this photon rate point has a contribution Flagging information will be automatically entered into flag tables with a label attached to every entry specifying the reason for the flag The reason currently is derived from the system date time A list of these labels will be displayed if the UNFLAG button is selected Each entry is identified by the exact time of observation and the data selection Flag tables can be saved to disk for later retrieval The name of the disk file holding flag tables is made up of the body of the input data file name plus an extension flg 5 2 Astrometry UriL IDENTIFY Identify data points Program enters loop in which left mouse button click identifies right button click identifies and exits the loop WINDOW Change display area RANGE Enter new range of display ELLIPSE Interactively define an ellipse Use left mouse button to set or move either semi major axis end points the middle button to set or change the ellipticity and the right button to exit either mode and the utility upon clicking twice OnBIT Run Thiele Innes method to obtain inital estimate of orbital parameters The results are stored in a single orbit stora
126. nts spectrometer lt _int gt Read the bin count data for the specified spectrometer A raw HDS file must be open The spectrometer number i e the output beam is stored in a common block for shared reference get_data filename This standard procedure to read any kind of NPOI standard data files can be used to read a single raw file if the full filename is specified All spectrometers will be 137 138 CHAPTER 26 INTRODUCTION read and therefore the cautionary notes as to the spectrometer index in bincounts apply The file will be left open 26 2 Frames At NPOI a fringe frame is a two dimensional array of count rates whereby one dimension corresponds to the 8 or 64 phase bins across the fringe and the other dimension corresponds to the channel axis A frame is recorded every 2 m1997 05 15 chas The frames are stored in bincounts which can have dimensions in this order of the number of spectrometers number of bins number of channels and the number of frames This structure is the same whether or not one is using the 3 or 6 way beam combiners All COBRA functions are guaranteed to work if a single spectrometer is selected only a few accept frame or visibility variables with a spectrometer index as noted specifically below Therefore the default is that the bincounts array does not have a spectrometer index displayframe c Display frames on the TV Any index selections in the different dimensions can be dis played provid
127. of OYSTERis used to read edit average and calibrate output point data produced from raw fringe data by a standalone C program CONSTRICTOR The scripts are run interactively in the IDL environment with the data stored in IDL variables and therefore available at the command level Beginning with version 8 a pipeline has been implemented which produces averaged and calibrated data Data reduction and analysis are two steps separated by the average procedure In the classic NPOI 3 way reduction the squared visibility delay background and photonrate data are edited then averaged into scans For astrometry the emphasis is on the dispersion correction of the delay point data before the averaging step Calibration of the scan averaged visibilities is based on unresolved or nearly unresolved calibrator stars whereas the astrometric calibration is based on the application of constant term and pivot motion metrology data delivered by INCHWORM A new feature of the 6 way data reduction is the photometric and bias calibrations derived from the averaged data but used in a second averaging step in order for them to be applied Following the Introduction a Quick Guide will lead you through a sample session Basic widget procedures is a more comprehensive description of how to reduce data using the GUI Graphical User Interface Command line procedures lists some of the useful routines callable at the IDL prompt 16 2 Data and auxilliary files Interf
128. on Julian date formatting and parsing of date strings structure pro Allocation of data structures mainwidget pro All scripts related to the top level widgets of CHAMELEON and AMOEBA misc pro Miscellaneous unsupported procedures 29 30 CHAPTER 6 PROGRAMMER S REFERENCE e CHAMELEON chameleon pro Basic point data reduction and scan calibration access pro All higher level HDS data file access scripts hds pro All HDS CL wrappers These verify arguments and call the C wrappers which in turn call HDS library functions astrom pro Basic astrometric procedures plotwidget pro All plot widget scripts for AMOEBA and CHAMELEON plotting pro All general plot scripts e AMOEBA ameeba pro Basic data reading and model computation model pro Model data computation functions fitwidget pro Managing of fit widgets fitting pro Fitting of hierarchical models math pro Math routines in CL limb pro All limb darkening code filter pro Filter transmission functions e STARBASE starbase pro Basic data base routines catalogs pro Access of auxilliary secondary catalogs lists stars pro Estimation of stellar parameters starplot pro Miscellanous plot routines e COBRA cobra pro Raw data manipulation cobrawidget pro Raw data viewing e PEARL pearl pro Imaging 6 1 2 C libraries Each of the five direct
129. on to the target directories Then set environment variables STARLINK and INSTALL to point to the starlink installation direc tory In each of the ems chr cnf and hds sub directories hds must be processed last use the mk command with the targets in this order deinstall clean build and then install to compile the a library files which are automatically placed in the lib subdirectory of the starlink home 32 CHAPTER 6 PROGRAMMER S REFERENCE WD This is the Wilson Devinney code for the eclipsing binary model They were modified for use in OYSTER This proprietary library is not included in the standard distribution e fnl f e imic f e imlight f ROCHE This is Deane Peterson s code for the simulation of gravity darkening in rotating stars This proprietary library is not included in the standard distribution Part II AMOEBA Chapter 7 Introduction 7 1 About AMOEBA AMOEBA procedures and functions are used to fit parameters of hierarchical stellar system models to data from interferometry astrometry spectroscopy and photometry The data from the latter three methods are read from formatted ASCII files and stored in structure arrays Interferometric data however can only be stored in the scans structure one night at a time due to the complexity of the data and the varying configurations Therefore the different nights read by load_interferometry are buffered by a C function nightbuffer 7 2 Data files 7
130. onfiguration There is a command line function scanconfig which can be used for quick information regarding scan configurations as follows scanconfig Return list of different scan configurations used scanconfig scan Return scan configuration used for the specified scan ID scanconfig config lt char gt Return scan IDs which correspond to the specified scan configuration 20 2 Bias correction of visibilities Since Wittkowski et al 2001 the importance of improved bias corrections of the amplitudes has been recognized A good fraction of the non Poisson bias was removed from the 3 station data through the use of Dave s 2 correction in CONSTRICTOR For the new 6 station data 107 108 CHAPTER 20 DISCUSSION OF REDUCTION ISSUES CONSTRICTOR allows one to specify one two or three fringe modulation values k values at which the amplitude is measured and then used in a polynomial fit of order zero one or two respectively to compute a bias at other modulations through interpolation In the case of zero order bias correction in CONSTRICTOR a remaining bias can be studied by plotting the visibilities of incoherent scans i e fringe less data versus the photon rate Here is how After all editing of the point data has been done one should set the default back ground rate which is zero using defaultbg or REDUCE BG DATA DEFAULT BGi and zero bias coef ficients genconfig bias 0 only needed when starting over befor
131. or the siderostat mirror pointing has played a role in the visibility degradation Before the actual calculation of a solution it is required to select the data which is to be used for the computation of the calibration coefficients and is to be calibrated Clicking on CALIBRATE VISIBILITY PLOT will display the plot widget Please note that the star selection in this widget will now indicate the stars for which the data is to be calibrated It should also include the selected calibrator stars Since several calibrations can be applied sequentially to the same data appropriate selections are required here if calibrations differ from star to star Also note that the scan selection is used just as in the case of plotting scan data The calibration is only applied to valid visibilities By selecting the LOOP option selected channels and baseline will be calibrated independently rather than combined in a simultaneous fit This options was implemented to speed up calibration of an entire spectrometer Remember to work on all spectrometers and baselines In the case of NPOI 6 way data combine only scans of the same sub array configuration Unless the photometric calibration is very good sub arrays will differ in their system visibility Look at the normalized and calibrated visibilities to make sure they were not calibrated before if you want to start over with a new calibration This is because as mentioned above more than one calibration can be applied se
132. or your architecture This is because the crossindex files are binary files in XDR format To recompile the crossindices type get crossindex 1 exit the session type quit Finally it might be necessary to re create the binary ephemeris file used by NOVAS To do this go into the jpl subdirectory and follow the instructions in README 1st 2 3 Earth orientation updates Edit the file oyster usno cronjob to contain the proper path to the update shell script and then use the command crontab cronjob to install a job which fetches every Thursday the new UT1 and polar motion data from a computer at the US Naval Observatory Otherwise the database usno mark3 dat obtained with the download will not be updated and eventually will not provide Earth orientation data for the date observed In this case a warning message will be displayed which however can usually be ignored in all cases but astrometry Chapter 3 Using OYSTER 3 1 Starting up You invoke OYSTER at the UNIX prompt by typing the actual path may be different on your system idl home chummel oyster oyster or gdl home chummel oyster oyster Provided IDL version 5 0 or higher or GDL version 0 9 3 or higher is installed the language will start up and read and execute the commands in oyster oyster pro This procedure file will first determine the location of the oyster atmospheres and catalogs home directories then load the compiled procedures in oyster cpr
133. ord gt LabSolidTmpData 168 APPENDIX B CONSTRICTOR OUTPUT FILE STRUCTURE NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt LabPressData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt LabHumData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt DLPressData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt FBPressData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt WxAirTempData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt WxPressureData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt WxHumidityData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt WindSpeedData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt WindDirData NumData lt _integer gt TimeStamp NumData lt _integer gt Data NumData NumSensor lt _word gt Appendix C CHAMELEON file structure The file format of averaged data is described here It closely follows the format of the CON STRICTOR files DATASET
134. ore than one axis at a time as they will act simultaneously The CURRENT directive simply leaves the current selection unchanged which is not necessarily identical to the displayed selection It is not necessary to specify indices or alter the corresponding selection for axis items which do not contain those indices The pt and star selection address the same index Therefore the star selection is applied after the pt selection as displayed in the data selection widget When plotting scan data you can obtain information on which scans correspond to given stars from the UTILITIES LIST SCANS button 5 1 3 Flagging data Flagging data is allowed in only some plot classes point bg and scan and manual flagging only if the plot window contains a single plot remember to use the ALL IN 1 option to plot 26 CHAPTER 5 PLOTTING AND EDITING a selection of data into one plot Automatic flagging is recommended only for point data In the manual mode you will define a box on the plot by first clicking the left mouse button on the upper left corner then set the size shape of the box by moving the cursor and clicking the middle button then positioning the box Click on the left button to place another box or the right button to finish Finally you will be presented with a list of options of what to do with the boxed data Flagged data will be colored red 5 1 4 Logical editing and flag tables The scope of bad data flags can go beyond the curre
135. ories containing external code have make files Use the Makefile appropriate for your system to recompile them Use make clean first to prepare the compilation Please send copies of the Makefiles to the author if it was necessary to modify them 6 1 CODE 31 OYSTER e chameleon c e amoeba c e cobra c Raw packet data access e hds c HDS wrappers e writefits c The FITS writer e posprop c The Hipparcos epoch transformation e sidfuncs c NPOI siderostat model functions e nrutil c Numerical Recipes subroutines FITSIO A library containing functions for FITS I O OYSTER uses this package to write out interfero metric data in single source FITS format NOVAS A library containing function of the Naval Observatory Vector Astrometry Subroutines e novascon c e novas c e solsys2d c e jpleph f 6 1 3 Mixed and FORTRAN libraries HDS One of the libraries of the STARLINK UK astronomy software project These subroutines im plement the Hierarchical Data System used for NPOI data files They can usually be downloaded from the STARLINK web site and therefore do not need to be compiled e libhds a The HDS library if not appropriate for your system should be obtained directly from the STARLINK web site http star www rl ac uk following links to the Software Store Sub routine Libraries and HDS http star www rl ac uk cgi store storeform1 HDS Follow the instructions to unpack sh storeformhdr paying close attenti
136. ote that in this mode i e without parameter the procedure will prepare the table specifically for use by CHAMELEON This involves getting the stellar positions from the Hipparcos catalog diameters from diameters bsc and colors from the bright star catalog If a list of stars is specified just the catalog data available in the specified catalogs is loaded rename_starids from to lt _char gt Rename stars e g from FKV designation to BSC designation in which case from to would be fkv bsc 13 2 Read entire primary catalogs Note that your workstation has to have enough memory installed to hold the entire startable 63 64 get_bsc get_bat get_fkv get_fln get_sky get_wds 13 3 Print list information list star s tar CHAPTER 13 COMMAND LINE PROCEDURES 9096 entries 1469 entries 4652 entries 3564 entries 49418 entries 1635 entries Print some information from startable on star to screen For star the standard combination of catalog acronym and identifier can be used or the Flamsteed and Bayer names or a proper name Examples list star FKV0193 list_star alp aur list star Capella The second example works only if the NAME field was set list note s ar note Print notes to screen or save in note if specified Notes must have been read previously with read notes write stars Write startable to LATEX format output file write_npoi startable lt _char gt file lt _char gt Write
137. output file structure 159 C CHAMELEON file structure 169 D COBRA file structure 171 E INCHWORM file structure 173 10 CONTENTS Part I OYSTER 11 Chapter 1 General information 1 1 About oyster OYSTERis the original interactive data reduction package developed for the Navy Precision Optical Interferometer at Lowell NPOI OYSTER is an endeavor to combine all aspects of data reduction modeling astrometry and imaging including a stellar database with an interactive data language in one package Procedures are often shared It also tries to maximize ease of use by providing both command line procedures and widget routines e HDS data base access A full set of functions to access NPOI data files written in the Hierarchical Data System format developed by Starlink Individual objects can be accessed directly e Plotting and editing General plotting widgets with interactive display options and editing routines Flagtables are implemented for bookkeeping e Astrometry Multi color dispersion corrections metrology calibration astrometric func tions including the Naval Observatory Vector Astrometry Subroutines epoch conversions and polar motion data Solution for baseline and star coordinates e Calibration General multi dimensional visibility amplitude and phase calibration capa bility for several types of dependencies e Global modeling Use of a hierarchical stellar systems format which enables fitting physical p
138. pos Note that metrocorr and astrocorr store their results in the same variable since they should give very similar if not identical results 19 2 2 Other unwraptriple Unwrap triple phase as a function of time calcgeo Compute geometric delays for point data average Average point data currently loaded and place results in scan structure scans 102 CHAPTER 19 COMMAND LINE PROCEDURES 19 3 Writing HDS objects put_genconfig Write GenConfig to HDS file Erase existing object put_geoparms Write GeoParms to HDS file Erase existing object put_sysconfig Compound procedure put_observerlog put_constrictorlog put_date date put_userid user_id put systemid system id put_format format put_scandata filename Write entire scan data set to file Erase existing objects put_stationtable put_mark3data 19 4 Analysis procedures hb uvd real v2 lt _real gt Function Return diameter of star for given uv distance and squared visibility Uses calibration implemented in polynomial expressions caldiameter starid char calid char Function Return the diameter of a star using the calibrator and the uncalibrated estimated squared visibilities npoirates starid predictedrate Propagate the stellar flux through the atmosphere and NPOI and return the pre dicted count rate for every NPOI channel Configuration must be loaded 19 5 List procedures list_names names lt _char gt List HDS objects at curre
139. quentially and calibrated data is part of the data saved in the output Click on CALIBRATE in the calibration widget to compute a solution based on the calibrated estimated visibilities amplitudes or closure phases depending on your selection of the calibrator stars The calibrated visibilities are initialized as a copy of the uncalibrated visibility The results will be entered in the calibrations table strictly speaking an array of calibration entry structures and automatically applied to the data The entire calibration table can be stored to disk using ENTRIES SAVE and loaded from disk using ENTRIES LOAD A list of all calibration entries will be printed to screen by ENTRIES LIST Here we summarize again the calibration widget functions OPTIONS Loop Loop over channels and baselines 94 CHAPTER 18 BASIC WIDGET PROCEDURES ENTRIES SAVE Save all calibration entries to disk file LOAD Load entries from disk file replacing current entries APPLY Calibrate data using all calibration entries CLEAR Clear the list of calibration entries LisT List the entries UNDO UNDO Remove entries and corresponding calibration UNCAL Completely remove calibration from the selected data only RESET Reset calibration of all data for the selected variable data type UNDO UNDO will remove a specific calibration from the data as well as the corresponding entries in the calibration table You will be presented with a list of calibrations for the selec
140. r lt integer Phi NumLaser integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double 173 174 GlassCode NumGlass lt _integer gt ExFrac NumGlass lt _double gt ExFracErr NumGlass lt _double gt AirGapThick NumAirGap lt _double gt AirGapThickErr NumAirGap lt _double gt RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt double ExFracErr NumGlass lt double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double OptAnchConfig NumPlate MaxNumCluster NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser integer Theta NumLaser lt integer ThetaErr NumLaser lt integer Phi NumLaser lt integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass do
141. r a plot class because of a specific purpose of these plots Therefore the definition of a plot class requires the following information to be coded In ww plot the appropriate checkdata call and plot widget title need to be specified Furthermore in the same widget procedure the name of the new plot class needs to be added to each selection button if required Then in ww plotok an entry must be made for the new class for the plotting procedure associated with the new class Note that so far all plots in OYSTER are handled by just three different procedures plotdata plotncal and plotuv This is to have similar kinds of plots handled by the same procedure in order to make the plotting code shorter However some kinds of plots are sufficiently different in their logic so as to require a different plotting procdure to be written Finally as far as the plot widgets are concerned the new class needs to be added for each necessary index selection in ww indexsel Whereas the widget routines for plotting in OYSTER found in plotwidget pro the plot procedures and initialization functions are found in plotting pro Here we have to add an entry of the new class in init class for the definition of the auxilliary information which is displayed if the user selects the Identify button Then which plot variables are to be listed in the plot selection widget is defined in set axitems Finally the information of how multiple plots should be arrang
142. r gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt Cross NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt LabSolidTmpConf NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt 165 Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt Cross NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt LabPressConf NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt _double gt ScaleErr NumSensor lt _double gt Cross NumSensor lt _double gt Loc NumSensor 3 lt _double gt LocErr NumSensor 3 lt _double gt LabHumConf NumSensor lt _integer gt SampleInterval lt _integer gt Chain NumSensor lt _integer gt BRAD NumSensor lt _integer gt Offset NumSensor lt _double gt OffsetErr NumSensor lt _double gt Scale NumSensor lt double ScaleErr NumSensor double Cross NumSensor double Loc NumSensor 3
143. rTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer RetroEnd NumLaser MetAirTempSen integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer PlateExpMap NumPlate NumLaser lt integer LaunchEnd NumLaser MetAirTempSen integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer RetroEnd NumLaser MetAirTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer OptAnchMap NumPlate NumClusterMax NumLaser lt integer LaunchEnd NumLaser MetAirTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer 179 180 APPENDIX E INCHWORM FILE STRUCTURE RetroEnd NumLaser MetAirTempSen lt integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer Pier2PierMap NumLaser lt integer LaunchEnd NumLaser MetAirTempSen integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer RetroEnd NumLaser MetAirTempSen integer MetSolidTmpSen integer MetPressureSen lt integer MetHumiditySen lt integer NumAveGroup lt integer AveGroup NumAveGroup NumAveIn lt _integer gt NumAve0ut lt _integer gt TimeAveIn lt _integer gt TimeAveOut lt _integer gt NumTime lt _integer gt Time NumTime
144. raged using instrument specific data reduc tion packages they can if they have been stored in the OIFITS format be read by OYSTER for calibration if necessary and further analysis employing models and images In this way the vast number of data analysis procedures written for OYSTER can be used for any kind of inter ferometric data 4 2 OIFITS reader The primary access to OYSTER procedures is via the OIFITS reader get oifits which stores the data internally in the scans and other auxilliary IDL structures Alternatively VLTI MIDI and AMBER data can be reduced using the MyMidiGui and MyAmberGui front ends http www eso org chummel midi mymidigui mymidigut html http www eso org chummel amber myambergui myambergui html These provide easy to use GUIs for the externally developed data reduction softwares MIA EWS and amdlib and automatically store data internally using OYSTER s data structures as well as write data to disk in OIFITS format For data to be stored internally in OYSTER many requirements are to be met mostly for historical reasons of a data package first released over 15 years ago These procedures are handled in a mostly transparent way but need to be kept in mind in case of adaptations of the code to specific applications Here we point out relevant pecularities of OYSTER e Array information such as station names and coordinates are not strictly necessary to be present in the OIFITS data file and models
145. rectory Example p readpacket pdr 17 packetlist YYYY MMDD Open all raw packet files corresponding do embedded system date Y Y Y Y MMDD Create GUI displaying packetlistings for each file and a combined list of stars If one or more stars are selected click and or drag mouse cursor scans corresponding to the star selection are listed which in turn can be clicked to display the packets corresponding to a specific scan If packets are clicked i e selected the packet is read if that type is implemented and some information is displayed and or stored in OYSTER global variables like Date GenConfig etc The packet contents are made available in the common block variable packet 143 144 CHAPTER 27 NPOI RAW PACKET DATA FILES Part IX VOLVOX 145 Chapter 28 Introduction 28 1 About VOLVOX A small number of procedures dealing with global astrometric fits to interferometric delay data 147 148 CHAPTER 28 INTRODUCTION Part X PEARL 149 Chapter 29 Introduction 29 1 About PEARL A collection of procedures capable of imaging interferometric data These were written to develop an algorithm for combining multi channel data by accounting for the wavelength dependence of the image if composed of black body radiators or stellar atmospheres A corresponding multi channel CLEAN was implemented together with a self calibration routine following a difference mapping scheme In the latter a model list of CLEAN
146. rpose procedure to replace or add certain variables in con files 20 5 4 Dispersion correction OYSTER procedure dispcorr is used to compute group delays and dispersion corrections for the data read from the coh file The dispersion corrections are computed for every data point as well as the corrections due to the motions of the siderostat pivots The latter are solutions for the X Y and Z coordinates done by INCHWORM They are transformed into delays and interpolated to the time stamps of the data points by metrocorr Both are applied when the point data is averaged The delay corrections due to pivot motions are also available in the data file from INCHWORM in which case the astrocorr procedure is used to just do the interpolation The results of both procedures are stored in the same variable 20 5 5 Metrology corrections After averaging the point data the only remaining delay correction is the fringe position of the white light source used to monitor the feed system path length This is implemented as a toggle i e a procedure which applies the correction when called the first time then removes it when called again and so forth The procedure name is whitecorr For greater flexibility the siderostat metrology corrections can also be postponed until after the averaging in which case they are derived from the averaged XYZ pivot coordinates This is done by the procedure pivotcorr the scan data equivalent to the point data proced
147. ructions here on how to use it To create a inch file from a con file startup INCHWORM and then type inchworm inchl gemini npoi con 2003 03 15 con dir You can delete the inch1 object by typing inch1 delete Then open the file and go to Raw ScanData double click on sid 1 and go to Edit De glitch In this widget deselect tuple 1 2 4 and 1 3 5 and then click on Find Fix every glitch listed by double clicking the glitch and then judging by the plot the laser which glitched Select this laser Calc and click Fix Note that lasers 2 amp 4 as well as 3 amp 5 are degenerate since they are 180 degrees apart Also lasers 2 amp 5 and 3 amp 4 are on the same side of the plate and should therefore move in the same way You do not have to work on the glitches in sequence but note that of course every fix will shift all laser values from current to end by that amount Typically there is up to a three count difference between calculated and predicted values of the glitch 100 counts 0 5 um Any notes can be entered into the INCHWORM log using View Logs InchwormLog After fixing all glitches go to Average Re create ScanData then Calculate By Time then Calibrate and then Done To prepare the motion group go to Motion Re create Go Calculate Calculate Done Done To exit go to File Done 133 134 CHAPTER 25 INTRODUCTION Part VIII COBRA 135 Chapter 26 Introduction A collection scripts capable of reading HDS formatt
148. s for delays with and without metrology corrections for example The user has to keep track of the actual calibration status of the delays 20 5 2 CONSTRICTOR parameters for astrometric reductions Atmospheric dispersion corrections are based on the variation of the visibility phase with wave length In order to increase the SNR for these data we coherently integrate the complex visibility for typically 200 ms The coherent integration is done using the COBRA procedure cohstrictor In order to provide the necessary input file for this step the following CON STRICTOR parameters should be used OutFile YYYY MM DD coh The coh extension is standard for coherent integration e Raw On Write the raw data of every scan into a separate HDS file These files are needed by cohstrictor to compute the complex visibilities and fringe delays e NumAv 100 Integrate 100 2ms samples This seems to be a good trade off between SNR and possible systematic error at longer integration times Metrology On Pass on metrology data 20 5 3 Coherent integration As explained in the chapter on COBRA CONSTRICTOR no longer does coherent integrations due to the complexity of the steps involved Instead procedure cohstrictor is used with a 110 CHAPTER 20 DISCUSSION OF REDUCTION ISSUES single parameter telling it the file name of the CONSTRICTOR output Do not confuse this procedure with another COBRA procedure constrictor which is a general pu
149. s into account In order to do this run fakedata with dutycycle 0 1 and simulate a data set using the star table and selected configuration Then use plotuptime 1 to plot rise and set times derived from the data fakedata stations lt _char gt starids lt _char gt dutycycle dutycycle Simulate scan data for a full observation scan every hour while the star is up with NPOI using the stations given in the input character array Example fakedata NOO0 NO5 N10 W06 W08 W10 FKVO621 If stars are not specified the startable will be used instead Date and SystemID will default to the current date and NPOI unless set manually The dutycycle specifies the interval in hours between successive observations of the same star mockdata pearl pear poisson poisson triple triple init init Replace observed visibilities and triple data with model values in combination with fakedata or with real data sets Poisson noise can be added based on the photon rates of the data set To show the uv tracks for the simulated data on top of an image of the visibility ampli tude function first plot the uv coverage and read a model file with readmodel and then use uvimage uv to underlay the grey scale amplitude image 15 2 Observing list preparation The OYSTER scheduling routines assist in creating an observing list stored in the startable from scratch or from another list stored on disk and computing the visibility of the stars
150. scan Function Return residual FDL delay for specified baseline The baseline parameter can either be a string variable e g AW0 AEO or an integer in conjuction with the spectrometer number specifiying an entry in GenConfig Baselineld The scan keyword specifies whether or not all records belonging to the scan will be returned If not then only the records associated with the currently loaded bincount data if any will be returned The default is scan 1 visdft v l d Function Return complex Fourier transform of visibility with respect to wavenum ber computed at delay values d l are the channel wavelengths in the same units as d groupdelay p l d Function Return position of peak of amplitude of complex power spectrum p whitedelay v Function Return white light phase delay for complex visibility v Caution phases should be unwrapped before 26 5 Photon rates fringenphot bincounts real Function Return photonrate 26 6 NAT data natoffset c Function Return x and y offset in units of the airy disk of the image on the nat quad cell 139 140 CHAPTER 26 INTRODUCTION 26 7 Compound plot procedures These procedures use more elementary functions to produce diagnostic plots plot_fdldelay baseline lt int gt beam lt int gt slide Plot the residual FDL delay in microns If keyword slide is 1 then open a sliding plot widget plot fdlpower baseline int beam nt sf Plot a power
151. set the common blocks and call the procedure setup oyster to finish the setup At this point OYSTER procedures and functions are ready to use at the command line or through invoking the main widget by typing oyster If you are using remote login without the capability of displaying windows edit the oyster pro file to include the notv option Type quit to exit OYSTER If this is the first time you run OYSTER run the commands limbdata and kurudata ip00k2 to create files in the atmospheres folder necessary for using model atmospheres 3 2 What to do next More than a thousand procedures and functions available in OYSTER support three main tasks reducing and calibrating one night s interferometric data as well as scheduling and HDS file ac cess this collection is referred to as CHAMELEON computing stellar models and fitting them to the data AMOEBA and creating and managing stellar data bases and catalogs STAR BASE Please refer to that part of this guide which is appropriate for your task Note that many of the scripts are interdependent and share resources 17 pck19 18 CHAPTER 3 USING OYSTER 3 3 Working with oyster OYSTER procedures are called from within the IDL environment This is done from either the IDL command line by typing in the appropriate commands or by invoking a widget which provides buttons to click on for specific action The latter method is less flexible but has the advantage of not requiring you to
152. sor lt double Cross NumSensor double Loc NumSensor 3 double LocErr NumSensor 3 lt double WxHumConf NumSensor lt integer SampleInterval lt integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor double ScaleErr NumSensor lt double Cross NumSensor double Loc NumSensor 3 double LocErr NumSensor 3 double WindSpeedConf NumSensor lt integer SampleInterval lt integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor lt double Scale NumSensor double ScaleErr NumSensor lt double Cross NumSensor double Loc NumSensor 3 double LocErr NumSensor 3 double WindDirConf NumSensor lt integer SampleInterval lt integer Chain NumSensor lt integer BRAD NumSensor lt integer Offset NumSensor lt double OffsetErr NumSensor double Scale NumSensor double ScaleErr NumSensor lt double Cross NumSensor double Loc NumSensor lt double LocErr NumSensor 3 lt double BGScanData lt ExtTable gt NumBGScan lt integer ScanID NumBGScan integer Time NumBGScan lt double RA NumBGScan lt double Dec NumBGScan double OutputBeam NumOutBeam lt ExtColumn gt
153. spectrum or structure function if sf 1 of the delay The time stamps must be integer multiples of the instrumental coherent integration time 2 ms cur rently at Example plot delayseries fdlstamp fdldelay AEO AWO plot_vispower baseline lt int gt beam lt int gt nwmav numav Plot visibility power spectra in a special browser plot plot_fringepower channels channels numav numav Plot mean of squared visibility amplitude averaged over numav samples default 10 samples as a function of k frequency plot fringeimage channels channels Display image of fringes from the frame data plot images frames Display fringe frames in a special browser window Example plot images bincounts plot powerpeaks baseline int beam int scanfilec char numav numav Compute and plot scatter plots of primary and secondary peak heights in the fringe powerspectra plot spectrumpeaks baseline int beam int scanfilec char channels channels numav numav Compute fringe spectra of the squared visibility amplitude averaged incoherently over numav samples as a function of fringe frequency Make a scatter plot of the peak amplitude at the k value corresponding to the selected baseline versus the maximum peak amplitude over all the other fringe frequencies which are not supposed to contain any signal plot groupdelay baseline int beam int scanfilec char numav numawv classic classic
154. t In addition one can select single interferometry scans in the plot widget for the fit while others are ignored until the scan selection is set back to ALL 8 3 Fit routines Under this menu FIT are listed specialized fit routines for the different data types Results are not stored in the hierarchical model but either in separate areas or written to file 8 3 1 ASTROMETRYFIT This widget handles initial single orbit fits to improve the apparent ellipse or orbit as de termined by the ELLIPSE and ORBIT utilities in the ORBITPLOT widget The procedure is as follows the user defines an ellipse first then fits the apparent ellipse to the binary po sitions using ASTROMETRY ELLIPSE Then ORBITPLOT UTIL ORBIT is used to estimate the orbital elements which are then improved by ASTROMETRYFIT ORBIT If the fit was success ful ASFROMETRYFIT SETMODEL will store the elements in the appropriate model component 8 3 2 INTERFEROMETRYFIT This procedure is used to fit p 0 pairs to individual nights The list of nights is derived from the ones currently loaded and they are re loaded 1oad interferometry despite the overhead in order to allow data sets of the same night to be combined Initial estimates for p 0 are obtained from the orbital elements The results are written to file fitnights psn including fitted synthesized beam widths This file is in the standard astrometry format and can be read back into AMOEBA 8 3 3 CONTROL This menu
155. t char Date lt char SystemID char bserverLog lt char ConstrictorLog char GeoParms Latitude lt double Longitude lt double Altitude double EarthRadius lt double J2 lt double LeapSeconds integer EarthRotation double GenConfig InstrCohInt double BeamCombinerID lt integer NumLaserP2P integer P2PLaunchPlate NumLaserP2P integer P2PRetroPlate NumLaserP2P integer MasterPlateID lt _char gt NumPlate lt integer Plate NumPlate NumCluster integer PlateEmbedded lt integer PlateID lt _char gt PlateLoc 3 lt double PlateLocErr 3 lt double InputBeam Table NumSid integer StationID NumSid char SiderostatID NumSid integer DelayLineID NumSid integer BCInputID NumSid integer StarTrackerID NumSid integer 161 StationCoord NumSid 4 lt _double gt four coords incl delay OutputBeam Table NumOutBeam integer SpectrometerID NumOutBeam lt char NumBaseline NumOutBeam integer NumSpecChan NumOutBeam integer FringeMod MaxNumBaseline Num0utBeam integer BaselineID MaxNumBaseline NumDutBeam lt _char gt Wavelength MaxNumSpecChan NumDutBeam lt _double gt WavelengthErr MaxNumSpecChan NumOutBeam lt double ChanWidth MaxNumSpecChan Num0utBeam double ChanWidthErr MaxNumSpecChan Num0utBeam lt double Triple Table NumTriple lt integer Outpu
156. t num lt _long gt values cmp_getnd name lt _char gt ndim lt _long gt dims lt _long gt values cmp_getOd name lt _char gt value cmp_getid name lt _char gt num lt _long gt values cmp getnd name char ndim long dims long values cmp_get1r name lt char gt num lt long gt values cmp_getOc name lt _char gt data cmp_getic name lt _char gt num lt _long gt data cmp_getnc name lt _char gt data lt _char gt cmp_putOc name lt _char gt string lt _char gt cmp_put0i name lt _char gt value lt _long gt cmp_putOr name lt _char gt value lt _float gt cmp putOd name char value double cmp put1i name lt _char gt values lt _long gt cmp_putir name lt _char gt values lt _float gt cmp_putid name lt _char gt values lt _double gt 113 114 CHAPTER 21 cmp_putnd name lt _char gt ndim lt _long gt dims lt _long gt values lt _double gt cmp_putnr name lt _char gt ndim lt _long gt dims lt _long gt values lt _float gt cmp_putni name lt _char gt ndim lt _long gt dims lt _long gt values lt _long gt cmp_putnc name lt _char gt ndim lt _long gt dims lt _long gt values lt _char gt cmp_putic name lt _char gt data lt _char gt 21 3 dat dat_name name dat_type type dat_ncomp ncomp dat index inder long dat find name char dat annul dat cell ndimc long cell long dat_shape ndim dims dat_get1d num lt _long gt values dat_getir num lt _long gt values dat getli numc long gt values dat
157. t numbers NNNNNN for the large catalogs SAO HDN and HIC 12 2 Managing a calibrator catalog This section is dedicated to a topic not of common interest and therefore just serves as a container for the procedure developed to manage calibrators for ESO The secondary catalog holding calibrators submitted by the Pls of ESO programmes is CA L xdr To add calibrators use the compile cal procedure and then update_cat to add the entries to the catalog Using write_calvin a list of calibrators can be written in the format used by the CalVin database 61 62 CHAPTER 12 HOW TO WORK WITH STARBASE Chapter 13 Command line procedures In this section we list some command line procedures 13 1 Allocate load STARTABLE create_startable starids Allocate STARTABLE initialize star IDs read catalogs Read catalogs corresponding to CCC identifier get startable starids Compound procedure to allocate and read Example get startable FKV0193 BSC1412 HDN198217 Remember that the catalog iden tifier e g HDN determines which catalog is to be accessed for that particular star See next section for routines to rename stars and inquire cross indices list star star id char Print currently loaded information on star to screen Star is identified by catalog and number e g BSC1708 FKV0193 For more options see part on STARBASE get_startable Create startable and fill with catalog information for stars listed in scantable N
158. tBeam NumTriple 3 integer Baseline NumTriple 3 integer NumSpecChan NumTriple integer SpecChan NumTriple 3 integer SidMetConfig NumPlate NumLaser lt integer CountsPerWaveln integer LaserWavelength double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser lt integer Theta NumLaser lt integer ThetaErr NumLaser lt integer Phi NumLaser integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt double ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass lt _double gt ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double OptAnchConfig NumPlate MaxNumCluster NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser lt integer Theta NumLaser lt integer
159. ta NumTime lt _ DataErr NumTime LabPressData NumSens NumData NumTime Data NumTime DataErr NumTime A LabHumData NumSensor NumData NumTime Data NumTime DataErr NumTime DLPressData NumSenso NumData NumTime Data NumTime DataErr NumTime FBPressData NumSenso NumData NumTime Data NumTime DataErr NumTime WxAirTempData NumSen NumData NumTime Data NumTime lt _ DataErr NumTime WxPressData NumSenso NumData NumTime Data NumTime DataErr NumTime WxHumData NumSensor NumData NumTime Data NumTime lt _ DataErr NumTime WindSpeedData NumSen NumData NumTime Data NumTime DataErr NumTime WindDirData NumSenso NumData NumTime Data NumTime DataErr NumTime NumEnvCorrGroup lt integer EnvCorrGroup NumEnvCorrG AveGroup lt integer Map lt integer Refs lt _char gt SidMetData NumPlate EnvSensorFlag 8 integer 1 air temperature Data NumTime lt _ DataErr NumTime ExtCatEyeData NumPla EnvSensorFlag 8 integer 1 air temperature _double gt A Data NumTime DataErr NumTime PlateExpData NumPlat EnvSensorFlag 8 lt _integer gt 1 air temperature A Data NumTime lt _ DataErr NumTime OptAnchData NumPlate EnvSensorFlag 8 lt _integer gt 1 air temperature _double gt A Data NumTime DataErr NumTime Pier2PierData NumLas EnvSensorFlag 8
160. tar Catalogue e position hdn van Altena et al 1991 Chapter 12 How to work with STARBASE 12 1 Introduction At this time STARBASE is used to perform two different tasks namely reading primary and secondary catalogs and computing astrophysical quantities from the collected information The data is stored in different fields of a table STARTABLE see next section Primary catalogs reside in subdirectories of catalogs and are read by the C function catalog Stars in the primary catalogs have unique ID numbers Entries are in the order of these numbers Information found in the primary catalogs replaces existing information in STARTABLE The available data for each primary catalog is listed below Secondary catalogs are lists of specific data on stars e g UBV photometry They were derived from various astronomical catalogs by extracting the ID number usually the HDN and the desired data Secondary catalogs reside in catalogs npoi and have an extension indicating the identifier for the ID numbers e g HDN They are read by PV WAVE procedures command dc read free and are used to replace information in STARTABLE Any star in STARTABLE is defined through a string of format CCCNNNNNN or CCC NNNN where CCC indicates the primary catalog and NNNNNN NNNN the ID number in that catalog Valid catalog identifiers are FKV BSC FLN BAT SAO HDN and HIC Please use 4 digits numbers NNNN for the small catalogs FKV BSC FLN and BAT Use 6 digi
161. te the astrometry 19 1 3 Loading data 99 Note that there are some procedures which package several tasks e g get_pointdata includes loading of the configuration scantable etc and the loading of point data for all scans get_records Read raw data from HDS file Since there is only one scan per file no scan number needs to be specified Note that all records all loaded get_points scans lt _integer gt Read point data for list of scans First scan number is always 1 Note that configu ration and table data must have been read prior to this call The default is to load point data for all scans get_scans Read scan data into scans Note that configuration and table data must have been read prior to this call get_bgscans Read background scan data into bgscans Note that configuration and table data must have been read prior to this call get motiongroup group lt integer gt Read motion group data from inch file get_astromcorrgroup group lt integer Read astromcorr group data from inch file get_metrogroup group lt _integer gt Compount procedure for get_motiongroup and get_astromcorrgroup Note that the first group is index 1 100 CHAPTER 19 COMMAND LINE PROCEDURES get_star star lt _char gt Read point data for star e g FKV0193 Note that configuration and table data must have been read prior to this call get_rawdata file lt _char gt Compound procedure Open file if necessary and read co
162. ted variable from which to choose the calibration to be removed The data selection is provided by the information stored in the calibration table To remove a calibration only from the table use the ENTRIES EDIT function UNDO UNCAL will remove all calibrations for the selected data and all stars scans UNDO RESET resets the calibration table for amplitudes or phases depending on your selection and remove all calibrations from all data 18 5 2 Calibrating amplitude errors The errors on the amplitudes of the visibility and the triple can be recomputed based on their formal uncertainties and the calibration error The latter is derived from the variation of the calibrator visibilities and the comparison to their formal errors Both are added in quadrature This procedure requires the selection of calibrator and program stars 18 5 3 Unwrapping triple phases There are three unwrapping algorithms available under CALIBRATE VISIBILITY TRIPLE For the first two REWRAP TRIPLE and DEWRAPTRIPLE you have to have calibrator stars selected first since they unwrap only the data for these stars for the time being Rewrapping here shall mean the rotation of the complex visibility by a specified angle so that the entire range of phases fits into the interval 180 180 degrees The the phases are recomputed and backrotation is applied to the complex quantities but merely subtracted from the phases If the phase is wrapping more rapidly one should p
163. terson SUNY e SHADOW VLTI shadowing computations 1997 05 15 cha After the standard installation procedure described above manual re compilation can be performed by going into the C source directory source c and editing Makefile Please note that the Makefile is the result of a concatenation of Makefile all in and Makefile lt uname gt in performed by the standard installation procedure Then run make clean and make to compile the library which is named oyster so Copy this file into the sub directory of the OYSTER home directory corresponding to your operating system using the provided shell scripts release Darwin or release Linux into the OYSTER home directory Please send a copy of the Makefile to the author if you had to modify it This procedure should work for LINUX and DARWIN OYSTER wil detect your OS and then know the path to the shared library and the binary JPL ephemeris file which differs between MAC and PC based work stations residing in directories linux and darwin under the main OYSTER directory To recompile and install the IDL procedures start up IDL in the idl directory with the com mand file c pro i e idl c which will then compile the IDL code and save it into files oyster cmb and oyster cpr The command file will then end the session You should use OYSTER first to recompile the crossindex subdirectory of the catalog directory if the code and catalog data distri bution tape was not specifically assembled f
164. there are no normalized quantities When writing calibrated data into a cha output file both the uncalibrated and calibrated visibilities are written but not the normalized data This is because normalization is done every time the data is read from the output file The calibration table which can be used to undo specific calibration and which is updated during the calibration process is only needed for this purpose any calibration can be reset without it and thus start over for a new calibration 20 5 Astrometry data reduction 20 5 1 Introduction Astrometry with NPOI is based on the measurement of fringe delays which are related to the baseline orientation and star position There are three different corrections to the uncalibrated FDL delays which are due to atmospheric refractive index fluctuations path length variations in the feed system and motions of the siderostat pivots We call the application of these corrections to the raw FDL delays calibration of the delays OYSTER similar to the visibility calibration has storage for three calibrated delays i e group dry and wet delays These are the result of the dispersion correction procedure dispcorr which computes cumulative corrections based on the white light fringe position group delay the dry and wet air dispersion constants respectively All subsequent metrology corrections are only applied to these three calibrated delays Note that OYSTER does not have separate variable
165. uble ExFracErr NumGlass double AirGapThick NumAirGap double AirGapThickErr NumAirGap lt double RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc 3 lt _double gt LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass integer ExFrac NumGlass double ExFracErr NumGlass double AirGapThick NumAirGap lt double AirGapThickErr NumAirGap lt double Pier2PierConfig NumLaser lt integer CountsPerWaveln integer LaserWavelength lt double SampleInterval lt integer IFBox NumLaser lt integer Channel NumLaser integer Theta NumLaser lt integer ThetaErr NumLaser lt integer Phi NumLaser integer PhiErr NumLaser lt integer LaunchInfo NumLaser NumGlass integer APPENDIX E INCHWORM FILE STRUCTURE 175 NumAirGap lt _integer gt Loc 3 lt _double gt LocErr 3 lt _double gt GlassThick NumGlass lt _double gt GlassThickErr NumGlass lt _double gt GlassCode NumGlass lt _integer gt ExFrac NumGlass lt _double gt ExFracErr NumGlass lt _double gt AirGapThick NumAirGap lt _double gt AirGapThickErr NumAirGap lt _double gt RetroInfo NumLaser NumGlass integer NumAirGap lt integer Loc lt double LocErr 3 lt double GlassThick NumGlass double GlassThickErr NumGlass lt double GlassCode NumGlass i
166. ure metrocorr It too is implemented as a toggle It is important however to use pivotcorr before whitecorr since pivotcorr will have to correct the white light delays too This is because the white light fringe position not only depends on the feed system path but also on the pivot motion If one decides to apply pivot and constant term corrections after the data has been averaged so that the changes may be studied more easily the situation may arise where raw pivot coordinates from the INCHWORM file have to be averaged this can be done using the inchav procedure 20 5 6 standard recipe So here are the steps for a standard astrometry reduction get_data 2001 03 16 coh Read a CONSTRICTOR file with coherent integrations hds close REDUCE BG DATA DEFAULT BG To make sure every scan has a back ground rate and set it to zero since we don t care about the visibility calibration REDUCE POINT DATA ASTROMETRY PHASEEDIT Flag all channels higher than 20 as well as the laser channel 11 Data after about May 2002 only need channel 12 of spectrometer 1 flagged This is done automatically 20 6 IMAGING SIMULATIONS 111 flagphase 2 1 chan indgen 16 1 Optional flagging of baseline 1 in beam 2 in this example This is needed if the same baseline occurs twice in the data In the case of a reference baseline the one in the first beam would be overwritten by the one in the second beam and so on in the dispersion correction procedure
167. utton is used to clear the HDS status to zero if an HDS error occurred This button will also close the file FILE OPEN Open HDS file for read only access CLOSE Close HDS file CLRST Close file and clear HDS status 18 2 Access a data file 18 2 4 Browse through an HDS file Since an HDS file is a binary file no editor can be used to look at it or extract data Special HDS routines have to be used instead to access an HDS file CHAMELEON provides a set of procedures which are wrappers for C functions contained in hds c which themselves call the appropriate HDS functions These procedures have names identical to the HDS routines and are simple to use at the command level Please refer to appendix A for a list of these procedures ACCESS TREE prints the HDS file directory to the screen recursively starting at the current level Click on the terminal window and hit a key to get the next page until the message Listing 87 88 CHAPTER 18 BASIC WIDGET PROCEDURES complete is displayed Note that for array objects the procedure will descend only through the first array element ACCESS BROWSE allows you to navigate through an HDS file and obtain information about the components in an object At any level you can jump up several levels just by closing a parent widget or clicking on an object displayed in a parent widget AccEss BROWSE always starts at the current level You have to close the top level browse widget before you can click on
168. velength whereby special attention needs to be payed to the averaging corresponding to what the instrument actually does The grid chosen is usually appropriate for the selected interferometer if the spectral reso lution is high the grid wavelengths correspond exactly to the channel center wavelengths The choice of grid is made in function calcmodel for each spectrometer 44 CHAPTER 7 INTRODUCTION Chapter 8 Basic widget procedures This section describes the complete line of model computation and fitting procedures within the widget environment To invoke the main widget type the following command at the IDL prompt IDL gt oyster 8 1 Load data AMOEBA is designed to handle data input from interferometry astrometry spectroscopy and photometry The data for the first type including configuration information is buffered i e loaded one night at a time into the ScanData section from the buffer This procedure was necessary since CHAMELEON procedures handling the data cannot handle more than one night at a time The loading of the data is handled by widgets which also allow to set flags and weights to be used in the subsequent data analysis The files are selected from a list option LIST of files with the proper extension found in the current directory and displayed in the widget or from a file giving the file names option FILE The DATA SUMMARY button gives information about the currently loaded data sets and their rel
169. vs Time for this However there are usually no outliers if 17 6 AVERAGE 85 they have been removed from the DelayJitter data so this step may be skipped and returned to if upon examination of the averaged delays outliers are found If reducing 6 way data and photometric and bias corrections are desired set a default back ground before averaging i e set all background scans to zero using the defaultbg procedure or the REDUCE BG DATA DEFAULT button After averaging all data perform the calibrations by using CALIBRATE CHANNELS and then re average the data but do not forget to reload and expand the back ground data and apply any flag tables 17 6 Average REDUCE AVERAGE averages all the data currently contained in the point data arrays The corresponding scans in the scans array it will be automatically created when non existent will be updated average will print out messages as to invalid flagged data encountered and non existing background scans If you are reducing the data on a star by star basis go back to load the next star and process it If for any reason you want to postpone the following calibration of the scan data you can write these data to a cha file now see below 17 7 Astrometry CALIBRATE ASTROMETRY this is the first calibration step of the uv coordinates that is you should take Here we examine the averaged delay data with PLOT select FDL_O C before attempting to fit station coordinates with SOLVE
170. why D for the west arm stations is reduced by that amount In the file stations config D contains the path from the siderostat pivot point to the mirror at the intersection of the N and E arms but excluding the vertical path in the elevator can which belongs to the delay line based path In file fdl config the paths do not include about 86m of path from the mirror at the inter section of the N and E arms through the feed system to the FDL entrance In file 6way config about 4m of path through the beam combiner are not included That is to say that the delays in this file and the previous one are relative paths This is a result from their having been created using the npoiconfig procedure from measurements of the white light fringe positions in different configurations 22 3 2 Basic definitions and sign conventions This section is partially derived from Basic definitions for the USNO and NRL Optical Inter ferometers by D Buscher A baseline vector is oriented from telescope 1 to telescope 2 i e the baseline coordinates are the coordinates of station 2 minus the coordinates from station 1 In the aperture plane the u coordinate increases to the East and the v coordinate increases to the North Remember though that uv coverages are plotted in OYSTER as seen on the sky so that the source structure and visibility function can be easily superposed In PEARL a map on the sky is allocated with the z coordinate corresponding to RA wh
171. widgets for plotting display more indices than needed for some of the plot variables in order to avoid recycling of the data selection widget if the variables change In the following tables an overview is presented over the indices applicable to the plot variables They are organized by class even though strictly speaking an OYSTER plot class refers only to a specific selection of variables listed in a plot selection widget More precisely the integration interval if applicable is the same for all variables for a table Also note that the IDL variables in italic font denote a derivation from this variable i e the data is not exactly identical to the variable contents Where the IDL variable field is left blank the formula is more complicated and might involve more than one variable Table A 1 Plot variables class point and their indices Plot variable IDL name inbeam outbeam triple channel baseline point Time pointtime pt PointNo pt VisSq vissq ob ch bl pt VisAmp visamp ob ch bl pt VisPhase visphase ob ch bl pt TripleAmp tripleamp tr ch pt TriplePhase triplephase tr ch pt PhotonRate photonrate ob ch pt FDLPath fdlpos ib pt FDLDelay fdlpos ib pt Delay Jitter delayjitter ob bl pt NAT Jitter natjitter ib pt GrpDelay erpdelay ib pt DryDelay drydelay ib pt WetDelay wetdelay ib pt VacDelay ib pt MetroDelay metropos ib pt 155 156 APPENDIX A PLOT VARIABLES AND THEIR INDICES Table A 2 Plot variables class bg and their
172. xed variable Im this example the variable NumScan is in the ScanData object that contains ComplexVis so the source for NumPoint is suppressed but NumOutBeam is in the GenConfig object so the source for NumBaseline is indicated We use the C convention where the last index listed is the most rapidly varying Tables are not part of the HDS system but they are easily implemented A table such as ScanData is simply a structure like any other containing a set of substructures each of which is an array What makes it a table is our agreement that the items a primitive a structure or a sub array pointed to by the first index of each array correspond with one another e g PointData 1 where PointData is itself a complicated structure was taken between StartTime 1 and StopTime 1 while we observed StarID 1 and so on We use two kinds of table here Table and ExtTable Both are slightly different from the table type described in the previous paragraph Both types contain one integer scalar quantity giving the number of rows e g NumData followed by the contents of the table ie one or more arrays of variables for which the first index runs from 1 to NumData 1 The ExtTable extended table type also allows array variables whose first index does not correspond with row number However the primitives that make up that variable must be array primitives whose first index does correspond with row number Session Format l

Manual

Contents

Download Pdf Manuals

Related Search

Related Contents