ASPRO-VLTI User's Manual - Observation and Data Reduction with
Contents
1. GREG i a Anti Aliasing U kh 2 40 1 10 0 10 210 200 240 nna Setup for Observation of T_TAU at MIDI_UT Close Help Back to Source def Source Observability GO Show Add UV Tracks Proceed to Visibility Panel Help on MIDI Enter Observing Wavelength Wavelength microns 49 0 kam d wmd Ei Telescope 1 Name 1 ul o iz 2 A e 2 Telescope 2 Name gt uz 4 E j i gt gt RESET FRAME start a new plot V Parameters for the MIDI instrument of VLTI Star magnitude in band N q Beam Combiner HIGH SENS l B 100 1 10 Spectrograph PRISM Observing Sampling Periodicity min 60 200 200 100 0 100 200 Declination 19 5 i Ze U meters Model C DISK lick here t lidate Ent M U1 U2 DL set 127 00000 rr 2 10 Wavelength 10 090 microns Figure 11 The default Setup For Observation panel left and the resulting UV coverage plot for a E_Gauss model right UV PLOTS see Sect 3 7 Note that ASPRO VLTI refuses to move on to the next module if the button has not been clicked after the last modification of the instrumental setup D GREG 1 Anti Aliasing Day 13 DEC 2005 LEC Obs 70 24 11 642 24 37 33 117 0 3 6 9 12 15 18 21 E EE 7 CSC OBSERVABILITY OF T_TAU Go Close Help Min El2. Es on JMMC Calibrator Group 3 1 SHOW ALL RESULTS RESET SHOW DETAILS HIDE DETAILS 7 Science star NAME RAJ2000 DEJ2000 MagN Base max Lambda DiamVK T_TAU 04 21 59 43 19 32 6 4 0 56 5685 10 Results Number of stars 7 found 7 with coherent diameter and 6 without variability and multiplicity vis vis2 e_di A ZS Wb Fa a gt Catalog Origin 1 280 Slam E BR URE SR charm __B denis g Confidence Index BN Medium Hon A SAVE oO EXPORT ESSE o o Figure 10 The window presenting the results of the Search Calibrators tool Once the user has retrieve a calibrator list or has confirmed that good calibrators are available for his her target both panels can be dismissed by clicking on the CLOSE buttons If the defined does not appear in the proposed list of targets repeat the object definition step and make sure to click on that button Revision 6 0 Page 16 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual 3 6 OBSERVATIONAL SETUP menu The Observational Setup menu brings up the Setup For Observation panel see left part of Fig 11 in which the user indicates its intended instrumental setup Some basic information about the capabilities of MIDI and AMBER during Periods 77 and 78 can be obtained by clicking on the button The default assumption is that the target will be followed during its entire transit as long as it re mains at an elevation of at least 30 d
3. 14 The default Setup For Observation panel left and the resulting UV coverage plot for a Eae FAG ke EHH MES EE OK EEM isio CDE MES PEA SA 16 The Observability panel left and the resulting time coverage plot right 16 The Setup For Observation panel with the Less Used Observing Constraints left and Additional Plotting Constraints right sub panels 17 The Interferometric Observables Explorer panel left and a visibility plot right 18 UV fit control panel left and result windows right for the Fit UV Data procedure for two different models fitted to the same synthetic dataset 2 02 00 84 20 Current setup panel left and UV table listing right obtained from the MISC menu 21 eee ss eee hE Re eee GS 24 Re ning The Select s Ae ec EN Re ee Kea ee eRe RE A ee 20 Field Selecion Tool lt a eee Rhee eee eee ee eth eee eee eA 26 Maximum magnitude difference Selection Tool 0 0 a 0 eee ene 26 Spectral Types Selection Tool 26 Luminosity class Selection Tool A a a ee Seek ee Sete nite dee et eSesetaa Suz 2r Maximal expected accuracy Selection Tool noa a aa a a 27 Variability Selection Tool aoaaa e a 27 Revision 6 0 Page 4 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual 25 Multiplicity Selection Tool a a aa 27 Revision 6 0 Page 5 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual 1 Introduction 1 1 Object This document describes the usage of ASPR
4. 3 5 2 Get CDS Object By Name Selecting Get CDS Object By Name under the OBJECT menu or clicking on the button in the Manual Object Entry panel brings up the Get Source Coordinates panel see Fig 8 Enter a case insensitive target name Enter CDS Source Name with no more than 24 characters and no embedded lt space gt use lt underscore gt instead and click on the button If the requested object name is not resolved by SIMBAD a pop up window presents an error message click on and enter a new object name or click on and select Manual Object Entry in the OBJECT menu If the object name was resolved by SIMBAD the panel is dismissed and an All About My Source panel appears with the coordinates retrieved from CDS The object name cannot be modified in this panel but its coordinates can be Because of possible errors in the CDS database it is recommended to check that the coordinates are correct and if necessary to modify them fe J 20 0 All About My CDS Source Parametric Model Close Help User Provided Model Redo CDS Query Back to Manual Proceed to Observational Setup 1 Found CDS Source T_TAU RA 2000 4 21 59 4345 DEC 2000 19 32 06 429 Relevant object photometry for instrument MIDI STANDARD Mag N q Mag V for Adaptive Optics 9 6000003814697 Choose a Parametric Model for the Source Number of Functions 4 E Function 1 Cc DISK NON GET SOURCE COORDIN
5. 2 0 File Exchange Remote File System Local File System OO File Exchange Remote File System Update mme File Update Removi Update L Work Name amp Date Modified Admin Friday January 28 2005 12 28 PM Atlases Thursday January 6 2005 2 07 AM Data Thursday July 29 2004 8 26 PM Docs Friday November 12 2004 7 04 PM mensen 1 JMMC ASPRO Thursday March 17 2005 11 14 AM Observ Monday November 8 2004 3 53 PM Proposals Tuesday February 1 2005 7 13 PM Publis Wednesday August 18 2004 9 01 AM Science Friday September 10 2004 1 46 PM Teaching Tuesday February 22 2005 4 44 PM File Format All Files Cancel O Cancel Enable File Management E Enable File Management List transfered successfully Figure 4 The File Exchange windows to upload and download files from a personal ASPRO VLTI account 3 2 The ASPRO package Once the user has launched the ASPRO package he is presented with two GUI windows see Fig 5 the graphic window in which plots will be presented when running ASPRO VLTI and the start up control window At this stage the start up control window contains only a Choose menu from which the user actually selects the JMMC software he wants to use for this session The possible choices are AMBER 3T Period 78 and 77 AMBER 2T Period 78 and 77 MIDI on UTs Period 78 and 77 MIDI on ATs Period 78 and 77 F
6. 3 Using ASPRO VLTI 6 3 1 Launching the ASPRO package 444 56 ee eee Oe wa HE EE A E we ee Se 6 Olek DO Lange applet e ct Se ew He ERE ERD ED EH EHO ES mE 6 3 1 2 Anonymous vs authenticated login on the ASPRO server 0 4 7 3 1 3 Setting a personal account on the ASPRO server 02 a 7 3 1 4 Starting the ASPRO package cae sew ee eed et E deeds caw 7 3 1 5 Uploading and downloading files to from the ASPRO server 7 de AREA PERO DD eee sabia ADSENSE HEE BE SS 8 3 3 First contact with ASPRO VLTI 0 0 00200 ee eee 9 Do eee RN ceo eee Bee eS REESE ee E ESE EG SEER GEES a da 10 J9 DESCON e s ere REREAD Cw OEE OS He RES Kw 10 3 5 1 Manual Object Entry 2 6 lt 6 48 6 wee Peds ade eee Sd O eee eS 10 3 9 2 Get CDS Object By Name 0 00002 eee ee 13 Dod SPS eaat aeea hee ee Bee eben dae et go kG eae s Ree 13 3 6 OBSERVATIONAL SETUP menu 0 a 15 Oe UY Re E ee PERS EOE SCHERER SESE Ee 17 Do FIT MODEL rie hs cc tw tee Ee E EES HSH HESS EOE SESE SA 18 eek Fna UY Daia ge ewe ERR hE ERR Ow eee eee SS 18 3 8 2 Model Parameter Errors Calculator 004 20 Oe SOLAR ok eee ERR eee KR EPR eGR Ee Oh ee REE Re 20 CAUS i e RE ORE GEOR AS OY EER ERG RRS ERAS 20 3 10 1 Show Current Setup 20 3 10 2 Plot Current Interferometer Setup 02 0 0048 2 3 10 3 Reset Marker Szen 21 3 10 4 Use Big MB sssbrceresiska EEE HACE LTS ACE E DE
7. 4 2 Refining the selection To refine the selection do e list SELECT CALIBRATORS Selection parameters Maximal distance in RA and DEC Maximal distance in RA and DEC Maximal Magnitude Separation mag Spectral Type Luminosity Class Maximal expected accuracy on the calibrator squared visibility CO Variability Multiplicity Figure 18 Refining the selection Click on the arrow left of SELECT CALIBRATORS to open the list of selection parameters fig 18 Select the parameter See http www ivoa net Documents latest VOT html for more information about this format Revision 6 0 Page 27 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Click on SELECT CALIBRATORS button to open a specific choice panel Enter the value of the selection parameter Click on button to start the selection The new result is displayed in the Result window Click the RESET button to return the previous result 1 Field around the Science Object Maximal distance in RA and DEC Maximal RA Separation nm 0 O Maximal DEC Separation legre o OOOO O O DL E Figure 19 Field Selection Tool 2 Maximum magnitude difference Science Object Calibrator Maximal Magnitude Separation S Close Help Maximal Magnitude Separation magjo Ok Figure 20 Maximum magnitude difference Selection Tool 3 Spectral Types Temperature class of the Calibrators spectral Type Figure 21 S
8. At the bottom of that window the result of the fit is summarized as follows with one line per model parameter Model Name Variable Name Best Fit Uncertainty If the parameter was held fixed the Uncertainty entry reads fixed instead of a numerical value In the example presented in the top right part of Fig 15 an E Disk function with three free parameters FWHM along the semi major and semi minor axes and position angle was fitted to a synthetic set of visibilities created with a C Disk function The result window indicates that both axes which should in principle be equal are only poorly recovered and the position angle is obviously not at all constrained This can be interpreted as evidence that the actual geometry of the source is not elongated in a particular direction prompting the user to try fitting a C Disk function rather The result of this second fit which has only one free parameter FWHM gives a satisfactory 30 8 0 3 milli arcsecond result whereas the input model was constructed using a value of 30 milli arcsecond The quality of the fit can be estimated with the RMS residual flux value indicated just above the best fit parameters values in the Result window In the example above using a Gauss function rather than a C Disk function gives a residual standard deviation almost twice as large suggesting that the C Gauss Revision 6 0 Page 21 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual laral
9. com ASPRO VLTI can be used in anonymous or authenticated mode Authenticated mode permits to exchange files with the server and retrieve previously stored user preferences and files When launching ASPRO VLTI anonymously the user connects to one of the 16 ASPRO VLTI visztor accounts available If all accounts are already being used the application will not start and the user must try again later All Revision 6 0 Page 7 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual connections use one IP port in the range 50000 52500 In case of systematic failure to start the application the user must check that he she is not working in front of a firewall that blocks part of this port range An alternative method to start ASPRO VLTI is to launch it as a Java Webstart application also available from the JMMC website This only requires the installation of Java Runtime Tool Kit on the user s computer also available from http java sun com The ASPRO VLTI GUI has been created by JMMC based on Java and XML technologies The use of the GUI should be totally transparent to the user if necessary a document describing the basic principles of the XML based GUI is available from the JMMC website 3 Using ASPRO VLTI This section describes how to launch the ASPRO package and to use ASPRO VLTI which is a part of this package If problems occur while running ASPRO VLTI check here for possible errors in selecting options or providing information to the soft
10. is running Open File Exchange Panel file Users qaspardduchene JavaGui cfa EXIT file Users qaspardduchene JavaGui cfal EXIT Figure 3 The new tabs appearing in the Application Applet window after ASPRO VLTI has been launched 3 1 5 Uploading and downloading files to from the ASPRO server If the user has started the application with an authenticated login the Open File Exchange Panel button in the File Management tab allows him her to upload download files from his her personal ASPRO Revision 6 0 Page 9 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual VLTI account Clicking on this button opens a File Exchange window see left part of Fig 4 that lists all files currently present on the user s account it is empty when the account has just been created Checking the Enable File Management box opens a second sub panel in the File Exchange window see right part of Fig 4 that lists and allows to browse the files and directories present on the user s personal computer To upload a file on the JMMC servers highlight the file in the Local File System sub panel and click on the button the file should appear in the Remote File System sub panel Reversely to download a file from the JMMC servers select the file and click on the button after selecting the appropriate download directory Click on the button in the Remote File System sub panel to dismiss the File exchange window g D 2
11. the arrow in the Additional Plotting Constraints sub panel see right part of Fig 13 For instance it is possible to modify the size of the UV plot to produce U V range to plot to remove the Fourier Transform of the object model by unchecking the Underplot a Model Image box or to change the quantity to be plotted Plot What visibility amplitude phase or any derivative with respect to the model parameters and the color scale stretch Use Image to Pixel Conversion linear which is default logarithmic or equalization The name of the output file to store the image in GILDAS format This Image Filename and its size This Image Size can also be modified by the user Once new values of these parameters have been entered click on the Click Here to Validate Entries to record them and then repeat the UV coverage calculation Click again on the arrow to dismiss the Additional Plotting Constraints sub panel 3 7 UV PLOTS menu This menu brings up the Interferometric Observables Explorer panel see left part of Fig 14 in which plots of the synthetic visibilities and other interferometric quantities can be created The Fourier Transform of the model which has been calculated in the OBJECT module is sampled at the UV points determined by the array and instrument setup defined in the OBSERVATIONAL SETUP module Since the target and the instrumental setup are defined in the previous modules there is little to choose here and a default plo
12. wavelength The scientific target brightness Science Object Magnitude in Search Band is carried over from the object definition panel it is used by the software to search for calibrators of appropriate brightness for MIDI observations For AMBER observations the user must specify the range of magnitudes for the calibrators Magnitudes min max to search entered as two real numbers separated by a lt space gt character Then a first set of selection criteria must be provided by the user concerning the distance to the object within which calibrators should be searched for the default values are considered a good default choice Finally the maz baseline used is indicated to the user if no array configuration has been selected yet then a default value is provided Once the search criteria are selected click on the button to start the search eee SEARCH CALIBRATORS Science Object Name 7 Tay E Observing wavelength microns 10 Science Object MagnitudeinSearchig OOO CO Search Radius in R A minutes of tir 120 Search Radius in DEC degrees 5 info max baseline used 56 56854 Figure 9 The Search Calibrators panel opened by the Calibrator s menu Once the search is over the results are presented in a new window illustrated in Fig 10 A detailed description of the window presenting the results and of the available methods to refine the search for the most appropriate calibrators is presented in Appendix A
13. 4 3 4 13 327 17573 024959 27153 0 974 0 004 0 436 0 030 B8Vn E Catalog Origin 280 1z Confidence Index Ds Di D e File SAVE Oe Pi ES Figure 17 Result Panel A 4 1 Initial selection The panel consists in three sections the Science Star window the Results window and a set of subpanels allowing a refinement of the selection of the calibrators based on various selection parameters The Science Star window shows the parameters of the Science object name position RA DEC N magnitude and maximum baseline computed angular diameter K Band Revision 6 0 Page 26 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual The Results window shows the list of the calibrators without any indication of variability or multiplicity Only some selected parameters are given see table 5 for JHK results 4 for N Band results unless the SHOW DETAILS button has been activated By clicking on the name of the column and dragging the column it is possible to personalize their order The top border of the panel presents 4 buttons RESET button to show the full list of the potential calibrators SHOW ALL RESULTS button to display the full list of the potential calibrators including those which are variable multiple of that have inconsistent diameters which are excluded from the default list SHOW DETAILS button to display the full li
14. ATES J SS SSS Parameters 0 0 1 0 029999999329448 00 L Go Let Close Help _ Function 2 F POINT E Enter CDS Source Name 1 TAU Parameters 001000 Figure 8 The Get Source Coordinates panel opened by the Get CDS Object By Name menu left and the resulting All About My Source panel right The remainder of the object definition process is identical to that described in Sect 3 5 1 and is not repeated here 3 5 3 Calibrator s Selecting Calibrator s in the OBJECT menu brings up the Search Calibrators panel see Fig 9 The basic principle of this tool is to provide the user with a list of stars that can be considered as good interferometric calibrators These calibrators must fulfill a number of conditions that include proximity to the target similar brightness as the target and well defined radius hence visibility A more detailed description of the methods used by this piece of software is provided in Appendix A Calibrators are search for around the last target that has been defined by the user in the OBJECT menu The user must provide the desired Observing Wavelength between 8 and 13 um for MIDI observa tions and between 1 8 and 2 5 um for AMBER observations to calculate the calibrators properties at the The definition of a new object is only validated once the user clicks on the Proceed to Observational Setup button Revision 6 0 Page 15 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual relevant
15. Brief functional description ASPRO VLTI is designed to allow effortless usage by any astronomer in particular no detailed knowl edge of optical interferometry is required The only prior information that the user should provide is the instrument he she would like to use and the physical properties of his her target ASPRO VLTI provides tools to determine the optimal VLTI configuration and interferometric calibrators to achieve the user s as trophysical goals The optimization is performed through estimating synthetic interferometric observables visibilities as well as through fitting theoretical models on these quantities The fitting process takes into account the measurement errors of the interferometric signal based on the instrument s ETC ASPRO VLTI is organized as a suite of four main successive modules see Fig 1 which are briefly presented below and described in more details later in Sect 3 The four modules are OBJECT to define the target properties name coordinates photometry and model of its geometry OBSERVATIONAL SETUP to define the VLTI configuration to be used in the observations this includes defining both the telescope array and the instrumental setup UV PLOTS to calculate and plot interferometric observables and their associated uncertainties FIT MODEL to fit parametric models to the synthetic interferometric signal that are created by the UV PLOTS module Object Definition Instrumental Set
16. JMMC MAN 2100 002 Revision 6 0 Date 02 05 2006 JMMO ASPRO VLTI USER S MANUAL Authors Gaspard Duch ne lt Gaspard Duchene obs ujf grenoble fr gt LAOG JMMC Gilles Duvert lt Gilles Duvert obs ujf grenoble fr gt LAOG JMMC Daniel Bonneau lt Daniel Bonneau obs azur fr gt OCA JMMC Olivier Chesneau lt Olivier Chesneau obs azur fr gt OCA JMMC Author Gaspard Duch ne Institute LAOG JMMC Approved by G rard Zins Institute LAOG JMMC Released by Gilles Duvert Institute LAOG JMMC Signature Date 02 05 2006 Signature Date 02 05 2006 Signature Date 02 05 2006 JMMC MAN 2100 002 ASPRO VLTI User s Manual Change record Remarks aa User s Manual for preparation of observations during P75 DEE User s Manual for preparation of observations during P76 DEE User s Manual for preparation of observations during P76 and P77 mean Updated for SearchCal 3 3 36 08 20 User s Manual for preparation of observations during P77 and P78 a New version of SearchCal software Revision 6 0 Page 2 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Table of contents 1 Introduction 4 Sa D ses ses SARTRE NESSA TESS SPAS DES RS RA E 4 la Relerence dA a me bee BER we EEE HBR EELS EESC SEE DG 4 Lo Ave and acronyms ck ee ES OCR ELAS RSS Os 4 2 Overview 5 2 1 Brief functional description 5 2 2 System requirements kh eR OEE ERR DD DERE RE RSE EES 5
17. MAN 2100 002 ASPRO VLTI User s Manual Post processing of the calibrators A coherence test of the photometry is done by comparison of the computed diameters from the different color index The star is rejected if one of the computed diameter differs more than 20 from the mean value A 3 Further selection of the calibrators It is possible once the list of calibrators has been constructed to refine the choice of the calibrators using several selection criteria field size around the science object object calibrator magnitude difference spectral type and luminosity class accuracy on the calibrator visibility information regarding the calibrator variability and multiplicity A 4 Results of the SearchCalibrators tool Once the CDS request is answered a Result Panel pops up fig 17 Close Help RESET SHOW ALL RESULTS SHOW DETAILS HIDE DETAILS Science star NAME RAJ2000 DEJ2 000 Magk Base max Lambda ETATAU Gamm 2406 185 0000 102 45 210 H X Results e ag Number of stars 13 found 8 with coherent diameter and 4 without variability and multiplicity Number dis HD R4 2000 DEJ2000 vis2 vis2Err aam e ediamve SpTye 1 0 462 23408 03 45 49 24 22 0 0 974 0 004 0 435 0 030 Bei EX 2 0 598 23302 034452 2406 4 0 976 10 003 0 423 0 029 Bell 3 3 9 397 19787 03 1137 19433 0 622 10 042 1 817 0 125 K2llvar
18. O VLTI a software derived from the JMMC general soft ware for preparing interferometric observations ASPRO ASPRO VLTI allows users to simulate VLTI observations with the setups offered by ESO for Period 77 and 78 1 2 Reference documents 1 JMMC MAN 2100 001 Revision 2 0 ASPRO User s Manual 1 3 Abbreviations and acronyms AMBER Astronomical Multi Beam Recombiner ASPRO Astronomical Software to PrepaRe Observations AT Auxiliary Telescope CDS Centre de Donn es astronomiques de Strasbourg CHARA Center for High Angular Resolution Astronomy COAST Cambridge Optical Aperture Synthesis Telescope DFT Discrete Fourier Transform ESO European Southern Observatory ETC Exposure Time Calculator FAQ Frequently Asked Questions FITS Flexible Image Transport System FWHM Full Width at Half Maximum GI2T Grand Interf rometre 2 T lescopes GILDAS Grenoble Image and Line Data Analysis System GUI Graphic User Interface IOTA Infrared Optical Telescope Array IRAM Institut de RadioAstronomie Millim trique JMMC Jean Marie Mariotti Center MIDI MID infrared Instrument PDF Portable Document Format PS PostScript PTI Palomar Testbed Interferometer RMS Root Mean Square SIMBAD Set of Identifications Measurements and Bibliography for Astronomical Data UT Unit Telescope VLTI Very Large Telescope Interferometer XML eXtensible Markup Language Revision 6 0 Page 6 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual 2 Overview 2 1
19. Radial velocity 22 RadVel radial velocity km s 23 RotVel rotation velocity v sini km s Measured angular diameter from CHARM Richichi and Percheron 2002 24 LD limb darkened disc diameter mas 25 e_LD error on limb darkened disc diameter mas 26 UD uniform disc diameter mas 27 e UD error on uniform disc diameter mas 28 Meth method of measurement 29 lambda wavelength Computed angular diameter from Catalogue of calibrators stars for LBSI Bord et al 2002 30 UDDK uniform disc diameter in K band mas 31 e UDDK error on uniform disc diameter mas Photometry 32 41 B Vires N Johnson s magnitudes U B V R I J H K L M N Photometry corrected for interstellar absorption 42 Ay visual interstellar absorption Revision 6 0 Page 32 30
20. S 21 3 10 5 Exit From Error Loop 21 3 10 6 Ignore Error 444 4486865668 SO Ee A wee eee EE RH OEE SEEDS 21 3 10 7 List UV Table Content 22 A SearchCalibrators Tool 23 DA Se ee te hee eR eR Ree ee Eee eee eB ER ee RR 23 ae ONE 23 A21 NA O e eb he wee CELESC EDER ETR ES 23 Boge AMB DONOS i ah eee SEEKER REE AE ARERR EASE ERER A DEE 23 A 3 Further selection of the calibrators oaoa a a 24 AA Results of the SearchCalibrators tool aoa aoa a a a 24 Aal DAR os oa a cee deeb os ee ESSA RES ES A 24 A 4 2 Refining the selection wwe aaa eee Se dane ee REM Ge ww 25 A 5 Description of columns in the Search Calibrator result panel 0 27 A 5 1 Short list column description N Band case ooa a 27 A 5 2 Short list column description JHK Band case o oo a a a 28 Revision 6 0 Page 3 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual A 5 3 Full table description N Band case aoa a a 29 AAA Full table description JHK Band case 29 List of Tables Im oP WNW Fi List of available analytical models and the parameters that describe them 12 Quantities that can be selected to plot the results of the simulated observations 19 Magnitude Search Range vs Flux of Object 2 0 00 0 ee 25 Short list column description N Band case aoao a a a a 28 Short list column description JHK Bands case 2 28 Column description N Band case oao a a a a 29 Column description JHK b
21. Source Info 2 0 All About My Source User Model Source name STAR 1 Ke See Close Help RA 2000 1 00 00 000 DEC 2000 0 00 00 000 Parametric Model Query CDS by Name Proceed to Observational Setup Relevant object photometry for instrument MIDI STANDARD DS Mag N Enter Source Info g 0 E Mag V for Adaptive Optics o ee STAR 1 Choose a Parametric Model for the Source RA 2000 1 00 00 000 Number of Functions 4 ES DEC 2000 0 00 00 000 Relevant object photometry for instrument MIDI STANDARD Function 1 C DISK 43 ESR y ea ho Parameters 0 0 1 0 029999999329448 0 0 Mag V for Adaptive Optics q Function 2 POINT hy l User Provided Model Fits File for the Source Your Model Data FITS file Browse Parameters 001000 Figure 7 The All About My Source panel opened by the Manual Object Entry menu in the case of a parametric model of the source default left and of a user provided FITS model right appear after modifying the instrumental configuration as well In addition the V band magnitude of the object is requested as the interferometer is fed by an adaptive optics system using an optical wave front sensor The coordinates of the object can also be retrieved from the CDS database by clicking on the button see Sect 3 5 2 In the bottom half of the panel the user must define the geometrical model of the target The default option to do this is to select one or the w
22. a RESULT E z Help 2 0 MIDI UT 76 UV FIT control panel E Close Help E DISK Dec 0 00000 fixed 00 00 00 0000 zen _ _ E_DISK Flux 1 00000 fixed O E S E_DISK Major 0 03705 0 00480 l Back to Source def Back to Obs Setup Back to Visibility Panel GO Perform Fit E DISK Minor 0 02758 0 03314 4 zm lt E Disk Pos Ang 81 95957 78 96639 Y re JV visibilities d Number of Functions 1 B E 7 en ONON RESULT Function 1 f C_DISK ISS e Close Help Parameters 0 0 1 0 029999999329448 0 0 Starting range 900000 numb of starts 1 1 1000 r m s U U4U8 Jy Function 2 POINT zl C_DISK R A 0 00000 fixed 00 00 00 0000 TLD C_DISK Dec 0 00000 fixed 00 00 00 0000 O Parameters 001000 C_DISK Flux 1 00000 fixed Starting range 000000 C_DISK Diam 0 03078 0 00031 e numb of starts 000000 Figure 15 UV fit control panel left and result windows right for the Fit UV Data procedure for two different models fitted to the same synthetic dataset model is an unlikely fit to the synthetic visibilities Once again because of the random process included in the fitting process it is strongly recommended to run the fit a number of times and to average the values of the residual RMS for instance 3 8 2 Model Parameter Errors Calculator This menu provides an alternative though not realistic method to fit a parametric model on the synthetic visib
23. ands case onoo a 30 List of Figures 1 10 11 12 13 14 15 16 17 18 13 20 2l 22 23 24 Outline of the usage of ASPRO VLTI Users go through each of these four main modules and obtain some quantitative results indicated below each module 5 The Application Applet window for anonymous left and personal account right login tO ASPRO VLIL eresas srra Ree E ER e EN E EEN E a 6 The new tabs appearing in the Application Applet window after ASPRO VLTI has been RAs BRS H ESR AER EERE RG EERE ESTEE RESET EERE HS 7 The File Exchange windows to upload and download files from a personal ASPRO VLTI MM sanere a ac a ae on a me ae ae ee ae 8 The two GUI windows that are automatically opened upon launching the ASPRO package the start up control window top and the graphical window bottom left 9 The appearance of the main control window GUI once the user has selected a version ASPRO SA ee nm a a a ee ee ee ee 9 The All About My Source panel opened by the Manual Object Entry menu in the case of a parametric model of the source default left and of a user provided FITS model right 11 The Get Source Coordinates panel opened by the Get CDS Object By Name menu left and the resulting All About My Source panel right 13 The Search Calibrators panel opened by the Calibrator s menu 14 The window presenting the results of the Search Calibrators tool
24. as been selected by the user so far Note that many variables have default values so that no parameter presents an empty field even at the time ASPRO VLTI is launched the only exception being Model File which represent the name of the user provided FITS model of the object Click on after reviewing the parameters the panel will be automatically dismissed once another module is opened Revision 6 0 Page 22 30 JMMC MAN 2100 002 STATUS Go Close Help User Info Observatory Status Current Interferometer Focal Instrument Min Length of current Baselines Max Length of current Baselines aspro0 17 MAR 2005T15 22 53 MIDI UT 76 MIDI STANDARD 56 568542480469 56 568542480469 ASPRO VLTI User s Manual Stations Used U1 U2 Field Calculator Max u v radius is 202m with a min spacing of 8m At Lambda equals10 microns images should be roughly 26x26 pixels and cover an angular size of 0 25783100129551 arc seconds 1 2499999684223E 06 radians with a resolution of 0 010211129177739 arc seconds 4 9504951249446E 08 radians r 7 x nny Source Information Current Source Catalog oipt sources sou Close Help Current Source is T TAU RA 04 21 59 4345 DEC 19 32 06 42900 r SS lt J Wavelength microns 10 Wi Wi Wi Obs Times Telat Tele Vere Vim Weil E 4 423078 32 73196 45 92445 2 000000 3600 000 1 000000 2 000000 0 7410625 0 000000 0 1111594 Fi
25. atedly this option will not increase the marker size every time his can be overridden by selecting Reset Marker Size 3 10 5 Exit From Error Loop Selecting this option forces the command interpreter to return to its default idle status i e green icon in the main GUI window without executing the remainder of an aborted command This is to be used when ASPRO VLTI is stuck with a red or fixed orange icon in the main GUI window in the latter case check in the LOG window that the last output is indeed an error message In some cases it may be necessary to select this option several times consecutively to unwind the command stack 3 10 6 Ignore Error Selecting this option forces the command interpreter to ignore step over the current error and to try to complete the remainder of the command This usually does not solve problems but it may be useful in some specific cases We strongly recommend using Exit From Error Loop and analyzing the error message s in LOG window check for missing files unproper parameter selection instead Revision 6 0 Page 23 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual 3 10 7 List UV Table Content Selecting this option displays in a pop up window the current content of the UV table corresponding to the observations simulated by ASPRO VLTI see right part of Fig 16 The file contains one line per measurement and per individual baseline Each line contains the UVW projected baseline coordinat
26. ay time The black horizontal segment indicates the period of the day during which the target is above the requested minimum elevation whereas the red segment indicates the period during which the VLTI delay lines allow observation of the target Normally with current VLTI technical information it is be always possible to observe the target through its transit This tool is therefore more appropriate to determine whether the entire transit occurs during night time To determine the actual UV coverage of his her proposed observations the user must first provide the wavelength of interest Wavelength between 7 and 15 um for MIDI and 1 46 and 2 54 um for AMBER values outside these ranges are rejected and a default value is automatically selected Note that with both MIDI and AMBER a large wavelength range is covered with a single observation however plots created by ASPRO VLTI apply to a single wavelength which can be selected to be that of a spectral feature of interest for instance The user then specifies the VLTI stations to be used Telescope N Name The checked Reset Frame box means that only the current array configuration is calculated Unchecking this box and requesting a second set of telescopes results in the combination of the two arrays in a single observation The object magnitude Star magnitude in Band N cannot be modified in this module if necessary click on the button to go back to the OBJECT module and modif
27. d for improving the quality of the graphical display on your computer screen 3 4 EXIT menu The only command under the EXIT menu Exit From ASPRO MIDI UT quits the ASPRO VLTI software after confirmation in a pop up window After the software is shut down the GUI windows are dismissed the Application Applet window remains in the user s screen but the ASPRO tab has now disappeared The configuration of the applet window is identical to its status after the user has first started the applet see Hie 21 in particular if the user had logged in with his her personal account information he she has been automatically logged out Clicking on the button terminates the current ASPRO VLTI session 3 5 OBJECT menu This menu brings up the first main module constituting ASPRO VLTI the object definition module Here the user must provide all properties that define the interferometric target its name coordinates brightness and a model of its geometry The coordinates of the object can be entered by hand see Sect 3 5 1 or retrieved from the CDS database see Sect 3 5 2 Also ASPRO VLTI provides a tool to find the most appropriate calibrators for a given scientific target taking into account the required accuracy on the visibilities see Sect 3 5 3 3 5 1 Manual Object Entry Selecting Manual Object Entry under the OBJECT menu brings up the All About My Source panel illustrated in the left part of Fig 7 In the upper half of the panel t
28. e color indicates ASPRO VLTI status when it is green the software is up and running and waiting for commands from the user when it is orange it is executing a command when it is red the software has run into an error and stopped Commands can only be executed when this icon is green If it is orange wait for the command to be completed If it is red or stuck on orange for at least a couple of minutes try using a few times if necessary Exit From Error Loop in the MISC menu see Sect 3 10 5 Revision 6 0 Page 11 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual If this is not enough to restore a normal running state for ASPRO VLTI then there has been a severe crash it is then recommended to quit ASPRO VLTI and restart if from scratch If the same problem occurs repeatedly checking the content of the LOG window may provide an indication of the nature of the problem The buttons located in the top left corner of the graphical window represent the following from left to right Refresh Plot redraws the last plot requested in case it did not show up automatically or if the displays contains only a red square crossed by two thin white diagonals Zoom In increases the zoom factor and provides scrolling bars to move around in the plot Zoom Out decreases the zoom factor Toggle Scrolling Bars On and Off adjusts the window size to the current zoom while removing the scrolling bars the Anti Aliasing option can be use
29. e provide a secondary estimate of the uncertainty on the model parameters which Revision 6 0 Page 20 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual should be close to the one provided by a single fit This fitting approach is in principle a close match to the actual observing and analysis processes that would be conducted by the user on actual datasets and should therefore provide a good estimate of the constraint on the models provided by the proposed observations Table 2 Quantities that can be selected to plot the results of the simulated observations Variable Description U Fourier coordinate corresponding to the East West axis V Fourier coordinate corresponding to the North South axis ANGLE Position angle in the Fourier plane RADIUS Radius in the Fourier plane AMP Amplitude visibility V of the Fourier Transform of the model AMP 2 Squared amplitude V2 of the Fourier Transform of the model PHASE Phase V of the Fourier Transform of the model REAL Real part Re V of the Fourier Transform of the model IMAG Imaginary part Im V of the Fourier Transform of the model SIG V2 Uncertainty on the squared visibility o V TIME Time of observation DATE Date of observation SCAN Sequential number of scan NUMBER Sequential number of observation Clicking on the GO Perform Fit button launches the fit and a Result window that presents the results of the fit automatically appears see right part of Fig 15
30. egrees This can be modified in the Less Used Observing Con straints sub panel see below To check the actual observability of a target at a certain date click on the Source Observability button This brings up the Observability panel illustrated in the left part of Fig 12 The user must enter the Min Elevation in degrees above which he she plans on observing the previously defined target and the Date to be tested format should be DD MMM YY using decimal numbers for days and years and English 3 letter abbreviation for months The telescope stations which have been defined in the Setup For Observation panel is reminded but cannot be changed in this panel If the Time stamp DL Availability Zones box is checked the earliest and latest time at which the limited range of the delay lines will allow observation of the target Once all parameters have been set click on the button The Observability panel will be dismissed the Setup For Observation panel brought back and a new plot will appear in the graphical window see right part of Fig 12 The horizontal axis represents time local standard time and universal time are indicated on the top and bottom axes respectively Also indicated around the plot are the Moon phase as a percentage of illumination and brightness apparent magnitude the date of observations and reminder of the VLT coordinates The night and twilight periods are indicated with dark and light shades of gray the white are is d
31. eighted sum of two simple parametric models for which the Fourier Transform can be calculated analytically This choice is provided with the Number of Function scroll down menu The list of functions along with the appropriate sets of parameters can be found in Table 1 Provide the name of the desired functions Function 1 and Function 2 and their associated parameters Parameters Important Be sure to provide 6 parameters for each function even though less parameters are needed to describe some of them fill in the list with Os if necessary The first two parameters for all models Aa and Ao represent the angular offset from the coordinate center i e the values entered for RA 2000 and Dec 2000 This is useful when using a model that sums two parametric functions that represent spatially separated components of the object for one function models these parameters should be set to O O F represents the normalized flux associated to the model when using only one analytical model set this to 1 and when using the sum of two models make sure that fyi fy2 1 D and D1 2 represent the diameter and FWHM of the model respectively The subscripts M and m indicate the major and minor axis respectively whereas 7 and o indicate the inner and outer diameters 0 is the position angle of the major axis models E Gauss and E Disk or of the binary system model Binary Finally FR is the flux ratio of the binary and Cy and Cy are the coefficients defini
32. er provided FITS file should have 2 or 3 dimensions The third dimension if present represents independent spectral channel This capability is not yet fully implemented in ASPRO VLTI and the software currently processes only the first slice of an input datacube The two spatial dimensions must have the same number of pixel i e square image The FITS file header must contain a certain type of information so that ASPRO VLTI can deal with it properly In particular the pixel scale must be provided Here is a possible beginning for a valid FITS file header NAXIS 2 2 minimum NAXIS1 512 size ist axis NAXIS2 512 size 2nd axis CRVAL1 0 0000000000000E 00 center is at O CRPIX1 0 2560000000000E 03 reference pixel is 256 in Alpha CDELT1 0 4848136811095E 09 increment is 0 001 in radians and astronomy oriented negative CRVAL2 center is at O O 0000000000000E 00 Revision 6 0 Page 14 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual CRPIX2 CDELT2 0 2560000000000E 03 reference pixel is 256 in Delta 0 4848136811095E 09 increment is 0 001 in radians In this example the coordinate center i e the point where the object coordinates apply is located at the center of the 512x512 image and each pixel is 1 milli arcsecond or 0 48 x 107 radian on the side Once the object has been entirely defined click on the button to move on to the second main module of ASPRO VLTI UV PLOTS see Sect 3 6
33. es a dummy observation date the time since the beginning of observations in seconds the code for the two telescope stations the real and imaginary part of the complex visibility and its weight i e its uncertainty A text file uvtable txt containing the same information is automatically stored in the user s ASPRO VLTI account the user can then retrieve it and use custom plotting routines to create different plots than those provided by ASPRO VLTI Revision 6 0 Page 24 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual A SearchCalibrators Tool A l Goals SEARCH CALIBRATOR builds a dynamical catalogue of stars with all useful information for the selection of the calibrators most adapted to the requirement of the astrophysical program A 2 Method Two methods are used one specific for the N band e g the MIDI instrument of ESO one used for the VJHK bands suitable for the AMBER instrument in J H and K A 2 1 N Band case Definition of calibrator field The maximum angular distance in RA and DEC of calibrators from the object is given by the user Flux constraints Three cases are considered for the range of magnitude of the calibrators following the object brightness see Table 3 Fob Jy Ei Rial mag Nyan Mag N maa lt 10 5 20 10 100 5 50 gt 100 5 100 Table 3 Magnitude Search Range vs Flux of Object List of possible calibrators he program finds the possible calibrat
34. evation 30 0 E SS Time stamp DL availability zones V Date DD MMM YYYY 13 DEC 2005 i i harom o 3 6 9 12 15 18 21 24 Telescope 1 Name ui LST Telescope 2 Name y2 Figure 12 The Observability panel left and the resulting time coverage plot right If the default type of observation i e following the target for an entire transit at elevations above 30 degrees does not match the user s goal intention click on the arrow in the Less Used Observing Constraints sub panel to open it and make some modifications see left part of Fig 13 There it is possible to change the minimum and maximum hour angles Hour Angle Start and Hour Angle End and elevations Min Elev To Plot and Maz Elev To Plot Only observations that satisfy both the hour angle and elevation requests are plotted Once new values of these parameters have been entered click on the Click Here to Validate Entries to record them and then repeat the UV coverage calculation by clicking on the GO Show Add UV Tracks button Click again on the arrow to dismiss the Less Used Revision 6 0 Page 18 30 JMMC MAN 2100 002 Observing Constraints sub panel r 2 0 Setup for Observation of T_TAU at MIDL UT Close Help Back to Source def Help on MIDI Enter Observing Wavelength avelength microns 10 0 ource Observability GO Show Add UV Tracks Proceed to Visibility Panel K
35. ferometric Observables Explorer Close Help Back to Source def 1 Back to Obs Setup GO Refresh Plot Proceed to UV Fitting Y data ampa2 a d p X data RADIUS L oxprad Plot Model Curve s i 17 M R 2005 Leg p Add ErrorBars To Plot y an FE Plot limits 4 reals all zeroes auto 9 9 00 0000 ES UN radius meters Figure 14 The Interferometric Observables Explorer panel left and a visibility plot right If the plotted visibilities or other quantities appear unsatisfactory to the user for instance because they do not change enough with time or because they are too small to be confidently measured click on the button to return to the OBSERVATIONAL SETUP module and try another instrumental configuration Otherwise the user can click on the Proceed to UV Fitting button to try to fit the synthetic visibilities with parametric models and to estimate the resulting parameter uncertainties 3 8 FIT MODEL menu In this menu the user can fit the synthetic visibilities created by the UV PLOTS module with parametric models in order to estimate the constraints provided by the proposed observations on the geometry of the object At any time the user can return to any of the other three main ASPRO VLTI modules by clicking on the buttons 3 8 1 Fit UV Data This menu brings up the MIDLUT UV Fit Control Panel see left part of Fig 15 which is also automatically opened when the
36. he user must provide the target name Source Name with no more than 24 characters and no embedded lt space gt use lt underscore gt instead its J2000 coordinates RA 2000 and DEC 2000 format should be HH MM SS SSS and DD MM SS SSS and its N JHK band magnitude Mag N Mag J H K the relevant filter s for MIDI AMBER observations If the brightness of the object is below the minimum required by ESO for observations during Period 78 a warning window will pop up when proceeding to the OBSERVATIONAL SETUP module note that the limiting magnitude is a function of instrument set up spectral resolution for instance so that a new pop up warning window may Note that the minimum brightness indicated by ESO applies to the correlated flux of the object i e basically the product of the object total flux by its interferometric visibility Since the visibilities are only calculated in the UV PLOTS module only the total flux can be tested against the required minimum brightness at this stage Remember however that if the object visibility is V 0 25 or 25 then its correlated flux is about 1 5 mag fainter than its total flux for instance Revision 6 0 Page 12 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual r 3 2 0 All About My Source Parametric Model Close Help User Provided Model Query CDS by Name Proceed to Observational Setup W Seu le D Enter
37. ilities created in the UV PLOTS module Its usage is almost identical as that of the MIDI UT UV Fit Control Panel panel see Sect 3 8 1 except for the absence of the Starting Range and for the fact that the Numb of Starts entries is replaced by Masked Parameters This can only take values of O free parameter or 1 fixed parameter The fit is performed iteratively from the initial guess Parameters entries in a way that does not take into account the visibility uncertainties It is therefore not representative of an actual observation analysis procedure and should not be considered as a strong result by the user We strongly recommend using the Fit UV Data menu rather 3 9 PLOT menu Selecting Show Plot in Browser PS PDF File under the PLOT menu creates a PS PDF file con taining the current content of the ASPRO VLTI graphic window The file is automatically displayed by the user s browser and simultaneously stored in the user s ASPRO VLTI account where it can later be retrieved 3 10 MISC menu 3 10 1 Show Current Setup This menu opens a Status window in which the basic properties of the observation being simulated are sum marized see left part of Fig 16 The information provided includes the interferometer instrument array configuration current object wavelength and name of a few key files for ASPRO VLTI No modifications to the setup can be performed from this panel it is exclusively informative but provides an overview of what h
38. io KE Start application using my account informatio Login Password Login 4 _ogout Gi E Remember passwort EXIT EXIT Figure 2 The Application Applet window for anonymous left and personal account right login to ASPRO VLTI To start a new ASPRO VLTI session click on the Start the Application Launcher Applet icon link in the ASPRO webpage If the appropriate Java2 applet is installed see Sect 2 2 an Application Ap plet window will appear on the user s screen see left part of Fig 2 Select Help under the menu for Revision 6 0 Page 8 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual a basic description of the usage of the applet Note that at this stage ASPRO VLTI has not yet been started the Java applet has only initiated a new session from which it is possible to start the entire suite of JMMC softwares including ASPRO VLTI 3 1 2 Anonymous vs authenticated login on the ASPRO server The user can decide to launch ASPRO VLTI either anonymously default option offered by the Applica tion Applet window or using a pre defined username First or one time ASPRO VLTI users can usually accommodate using the anonymous login option For frequent ASPRO VLTI users and or for repeated use of some custom input setup files the use of a personal account is usually more appropriate Note that it is not possible to upload files such as FITS files representing object models to the JMMC servers using anonymo
39. ion Aa Ad E C Gauss Circularly symmetric Gaussian distri Aa Ao Fy pe bution E Gauss Elliptical Gaussian distribution Aa Ad F D D d C Disk Circular disk a k a uniform disk Aa Ad F D E Disk Elliptical uniform disk i e inclined Aa Ad L Dm Da d C Disk Ring Uniform ring with finite width Aa Ao Fy D Do U Ring Unresolved infinitely narrow ring Aa Ad Fy D a Exp Exponential brightness distribution Aa AAA F D 2 Power 2 1 r brightness distribution Aa Ad Fy Die Power 3 1 r brightness distribution Aa Ad Fy Dt LD Disk Limb darkened disk resolved star Aa Ad F D Cy Cy Binary Binary point source Aa Ao Ff FR p d format below Either indicate the file name or if it has not yet been uploaded on the user s personal ASPRO VLTI account click on the button which opens the Select One File window whose use is much similar to that of the File Exchange window described in Sect 3 1 5 in case of anonymous login to ASPRO VLTI the user must upload his her files at every login since they cannot be stored on the server Once the FITS file is uploaded highlight it in the Remote File System sub panel and click on to validate the choice the upload window is automatically dismissed and the filename now appears in the Your Model Data entry of the All About My Source panel If the user has no adequate FITS file click on the and select a parametric model from the available list instead The us
40. ist column description JHK Band case Table 5 Short list column description JHK Bands case entry index calibrator object angular distance in degrees HD HD number RAJ2000 right ascension J2000 DEJ2000 declination J2000 vis2 squared visibility Ve ErrVis2 estimated error on Ve diam_vk estimated dk from the V V K calibration e_diam_vk estaimted error on dy K Sp Type MK spectral type mag V mag J mag H mag K Revision 6 0 Page 30 30 JMMC MAN 2100 002 HD RAJ2000 DEJ2000 vis2 vis2Err Dial2 e_Dial2 orig F12 N vis2 A and vis2Err A Calib Mflag Vflag d H e_plx pmRA pmDE AN Chi2 Sp Typ Teff ASPRO VLTI User s Manual A 5 3 Full table description N Band case Table 6 Column description N Band case index calibrator object angular distance in degrees identification by HD number right ascension J2000 dclinaison J2000 computed squared visibility Vi estimated error on Ve computed angular diameter at 12um error on the angular diameter source of the IR flux IRAS or MSX mid infrared flux Jy at 12 m relative error on F12 MK spectral type N magnitude computed from F12 using the relation Nmag 4 1 2 5 log F12 0 89 computed visibility and estimates error for the limits of the N band A Sum and 13um c for stars selected as spectro photometric calibrators indication of binarity angular separation 2 from Hipparcos catalog indica
41. le for Period 78 and with future VLTI instruments allowing observations with 4 and 8 telescope arrays This version of the software is not described here a specific Users Manual is available from JMMC 3 3 First contact with ASPRO VLTI Once a specific version of ASPRO VLTI has been selected the main control window offers seven menus see Fig 6 The EXIT menu allows to quit ASPRO VLTI The OBJECT OBSERVATIONAL SETUP UV PLOTS and FIT MODEL menus allow the user to enter the four main modules constituting ASPRO VLTI see Fig 1 The PLOT and MISC modules offer several helpful commands that can be used at any time while running ASPRO VLTI All menus are described in more detail in the remainder of this document J ASS JAVA XMLBased GUI EXIT OBJECT OBSERVATIONAL SETUP UV PLOTS FIT MODEL PLOT MISC tj Help Log do Figure 6 The appearance of the main control window GUI once the user has selected a version ASPRO VLTI In addition to these main menus the main control window contains an button and a button to open the LOG window in which ASPRO VLTI prints out messages as it executes commands The content of the LOG window can be useful while troubleshooting To the left of these two buttons is a white background window in which ASPRO VLTI provides short statements about its status while running commands it is usually empty when the software is idle Finally to the left of this window is a roundish icon whos
42. les used by ASPRO 12 63858 33 48358 43 80772 2 000000 7200 000 1 000000 2 000000 0 7009596 0 000000 0 1051439 uvfile list of u v positions oipt psf 19 99279 34 92108 39 75936 2 000000 10800 00 1 000000 2 000000 0 6329305 0 000000 0 949395 S e 25 98452 36 94650 34 05525 2 000000 14400 00 1 000000 2 000000 0 5540922 0 000000 0 831138 User Providen model 30 20545 39 42183 27 08413 2 000000 18000 00 1 000000 2 000000 0 4805217 0 000000 0 720782 gt 32 36793 42 17835 19 32106 2 000000 21600 00 1 000000 2 000000 0 4229630 0 000000 0 634444 4 model image file oipt lastmodel gdf Figure 16 Current setup panel left and UV table listing right obtained from the MISC menu 3 10 2 Plot Current Interferometer Setup Selecting this options results in a new plot that represents a sketch of the selected interferometer along with the name of the offered stations 3 10 3 Reset Marker Size Selecting this option forces ASPRO VLTI to use the default dot like markers when plots are created This overrides the selection of Use Big Markers 3 10 4 Use Big Markers Selecting this option forces ASPRO VLTI to use larger markers when creating plots This can be useful when plotting visibilities with their uncertainties for instance since the errorbar is as large as the default dot like marker and it is therefore sometimes difficult to determine from the plot the actual visibilities There is only one big marker size selecting repe
43. mg Telescope 1 Name un ul ES Telescope 2 Name y2 E RESET FRAME start a new plot V CO Parameters for the MIDI eng T VLTI Beam Combiner HIGH_SENS Spectrograph PRISM Observing Sampling Periodicity min 60 Eg K Click here to validate Entries Hour Angle Start 456 Hour Angle End gt 0 Min Elevation degrees 30 0 Max Elevation degrees 90 0 ASPRO VLTI User s Manual COO Setup for Observation of T_TAU at MIDI_UT Close Help Back to Source def Enter Observing Wavelength Wavelength microns 490 Help on MIDI Proceed to Visibility Panel GO Show Add UV Tracks Telescope 1 Name ui ui ES aU Telescope 2 Name gt u2 Jl RESET FRAME start a new plot Y Parameters for the MIDI instrument of VLTI tar magnitude in band N Beam Combiner HIGH SENS aal Spectrograph prism Observing Sampling Periodicity min en EEE SEET Click here to validate Entries U V range to plot 595 9 Underplot a model image v Plot what AMP Use image to pixel conversion AUTOMATIC oipt lastmodel gdf B This image size pixels 256 256 Figure 13 The Setup For Observation panel with the Less Used Observing Constraints left and Additional Plotting Constraints right sub panels It is also possible to change the default plotting options by clicking on
44. ng the limb darkening profile This profile is defined such that the Fourier Transform of the limb darkened disk is G u v a Jy x x 1 253 b J3 x x 2 c Jo x x s where z tD u v7 Ji x and Jo x are Bessel functions J3 x 0 637 zx sing x cosa a 1 Cy Cy b Cy 2Cy c Cy and s a 2 b 3 c 4 All angular distances must be given in arcseconds even though milli arcseconds usually is a more natural unit for optical interferometry The position angle is expressed in degrees following the usual astronomical convention i e measured East from North If none of the parametric models adequately describe the geometry of the target the user can decide to use a FITS file instead for which ASPRO VLTI can calculate the Fourier Transform using a DFT This can be done by clicking on the button which brings a new All About My Source panel see right part of Fig 7 The top part of the panel is unchanged and previously entered information source name coordinates and magnitude is still present Only the bottom part has changed and now contains a single entry Your Model Data in which the user indicates his her FITS model see the adequate Revision 6 0 Page 13 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Table 1 List of available analytical models and the parameters that describe them Name Description Par 1 Par 2 Par A Par 4 Par 5 Par 6 Point Point Source Dirac funct
45. ors in the list of mid infrared interferometric calibration sources established by van Boekel et al 2005 The result is a list of stars with known parameters in astrometry equatorial and galactic positions proper motion parallax spectral classification photometry as well as indication of variability and multiplicity and computed value of the measured angular diameter For each calibrator the squared visibility V2 AVZ2 is computed as function of the angular diameter wavelength and maximum baseline A 2 2 Other Bands Definition of calibrator field The search is based upon user specified criteria of angular distance and magnitude around the Scientific Object List of possible calibrators The program sends a request to the CDS database using scenarios based upon the selected photometric band K The result is a list of stars with known parameters in astrometry equatorial and galactic positions proper motion parallax spectral classification photometry Johnson magnitudes as well as indication of variability and multiplicity and known value of the measured angular diameter For each star the angular diameter is computed using a surface brightness method and color index calibration using V magnitude and B V V R and V K color index For each star the squared visibility V2 AV2 is computed as function of the angular diameter wavelength and maximum baseline Y Yeal cal 8 Revision 6 0 Page 25 30 JMMC
46. pectral Types Selection Tool 4 Luminosity class of the calibrators Revision 6 0 Page 28 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Luminosity Class Close Help Figure 22 Luminosity class Selection Tool 5 Maximal expected accuracy on the calibrator visibility AV2 V2 in Close Help aximal expected relative accuracy 0100 Ok Figure 23 Maximal expected accuracy Selection Tool 6 Variability Variability ese ome Figure 24 Variability Selection Tool 7 Multiplicity Multiplicity Multiplicity Forbidden v Ok Figure 25 Multiplicity Selection Tool A 5 Description of columns in the Search Calibrator result panel A 5 1 Short list column description N Band case Revision 6 0 Page 29 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Table 4 Short list column description N Band case entry index calibrator object angular distance in degrees HD HD number RAJ2000 right ascension J2000 DEJ2000 declination J2000 vis2 squared visibility Vo I vis2Err estimated error on Ve Dial2 computed angular diameter in band e_Dial2 error on the angular diameter F12 mid infrared flux Jy at 12um 11 MK spectral type 12 N N magnitude computed from F12 using the relation Nmag 4 1 2 5 log F12 0 89 13 to 16 vis2 A and computed visibility and estimates error for the limits of the N band A Sum and 13um vis2Err A A 5 2 Short l
47. st of measurements returned by the program All available parameters are given in Tables 6 and 7 for N and JHK band search respectively HIDE DETAILS button to display only the principal measurements returned by the program Only some selected parameters are given Tables 5 and 4 The lower part of the panel is a set of selection tools used to refine the list of calibrators and load save results SELECT CALIBRATORS is described below in sect A 4 2 DELETE to delete a star of the list Click the arrow enter the number of the line to be suppressed click the DELETE button LOAD to load a result saved as a file Click the arrow enter the name of the File name scl click the LOAD button SAVE to save in a file all the information of the list of calibrators Click the arrow enter the name of the File name scl click the SAVE button Retrieving this file is possible within the File Exchange Panel see sect 2 EXPORT CSV to save in a file the list of calibrators as displayed in the results window Click the arrow enter the name of the File name csv click the EXPORT button Retrieving this file is possible within the File Exchange Panel see sect 2 EXPORT VOT to save in a file the list of calibrators as displayed in the results window in the VOTable format Click the arrow enter the name of the File name vot click the EXPORT button Retrieving this file is possible within the File Exchange Panel see sect A
48. t see right part of Fig 14 appears at the same time as the panel appears on the user s screen The user can decide which quantities to plot X data and Y data for the horizontal and vertical axis respectively the possible choices are listed in Table 2 along with a brief description Selecting V for Y data and U forX data will produce a plot very much similar to the one obtained at the end of the OBSERVATIONAL SETUP module Checking the Add Errorbars to Plot box enables uncertainties to be plotted they are automatically calculated by ASPRO VLTI based on the object brightness with an instrument specific ETC The limits of the plot along both axes Plot limits Xmin Xmax Ymin Ymax in that order can either be chosen by the user or automatically computed which is achieved with the default O O O O selection The user can also choose to check the Plot Model Curve box which superimposes on the calculated visibilities the theoretical visibilities as a set of continuous red curve s If the model is axisymmetric only one curve appears when plotting AMP 2 as a function of RADIUS if the model is non axisymmetric or when plotting quantities as a function of ANGLE numerous curves appear corresponding to different position angles or radii in the Fourier domain Revision 6 0 Page 19 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual GREG 1 Anti Aliasing Sayre T TAU Madel OISK A ss 10 np VW vs RADIUS yZ S 2 0 inter
49. tion of variability from SIMBAD SB or eclipsing B V magnitude H magnitude trigonometric parallaxes error on plx proper motion in RA proper motion in DE visible interstellar absorption Chi2 value for the model fitting of spectro photometric data spectral type from adopted modelling effective temperature A 5 4 Full table description JHK Band case Revision 6 0 Page 31 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual Table 7 Column description JHK bands case Col Identifier Explanation Num 1 Number index 2 dist calibrator object angular distance in degrees Computed squared visibility from measured angular diameter or computed diameter 3 vis2 computed squared visibility ae 4 vis2Err estimated error on Ve Estimated photometric angular diameters 5 diam bv diameter b from V B V calibration 6 diam_vf diameter yr from V V R calibration T diam vk diameter yk from V V K calibration 8 e diam vk estimated error on dyk Identificators 9 HIP HIP number 10 HD HD number 11 DM DM number Astrometric data 12 RAJ2000 right ascension J2000 13 DEJ2000 declination J2000 14 pmDec proper motion in declination 15 pmRA proper motion in right ascension 16 plx trigonometric parallax Spectral Class 17 SpType MK spectral type Variability Multiplicity 18 VFlag Variability Flag 19 MFlag Multiplicity Flag Galactic coordinates 20 GLAT galactic latitude 21 GLON galactic longitude
50. ull ASPRO Interface The first four choices represent the specific versions of ASPRO VLTI available for preparing obser vations for Period 77 or 78 They allow the user to choose the instrument MIDI or AMBER and the type UTs or ATs for MIDI AMBER is only offered with UTs for Periods 77 and 78 or number 2 or 3 for AMBER MIDI only allows 2 telescope interferometry of telescopes Note that the technical details of both AMBER and MIDI instruments are unchanged between Period 77 and 78 The appearance and usage of ASPRO VLTI is essentially the same for all versions with only minor details varying from one to the other such as the instrument sensitivities or the observing wavelength In the remainder of this document Revision 6 0 Page 10 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual e a a a GREG 8 3 Ala JAVA XMLBased GUI Choose A Help Log 1 Figure 5 The two GUI windows that are automatically opened upon launching the ASPRO package the start up control window top and the graphical window bottom left we describe the usage of MIDI on UTs Period 78 and 77 and only explicitly discuss the specificities of other versions when needed The Full ASPRO Interface choices starts up the wider scope ASPRO software which allows simula tions of observations with other interferometers CHARA COAST GI2T IOTA IRAM s Plateau de Bure PTI as well as configuration of VLTI with MIDI and AMBER that are not availab
51. up Betinitlon Simulation of Observations Model Flttng Observabllity of Object Syntheti Interferometric Observables Model Parameters Constralnts UY Coverage of Object Assoc lated Uncertalntles Discrimination Between Models Figure 1 Outline of the usage of ASPRO VLTI Users go through each of these four main modules and obtain some quantitative results indicated below each module The UV coverage of the object with VLTI is provided by the OBSERVATIONAL SETUP module With the UV PLOTS module the user can readily estimate if observing the target in the requested configuration will yield visibilities that are accurately measurable and that vary significantly as a function of time for instance The FIT MODEL module allows the user to estimate whether the observations would yield tight constraints on the geometrical model of the source possibly leading to the exclusion of some models for instance In addition to these outputs ASPRO VLTI also provides a tool to search for adequate interferometric calibrators the user is provided with a list of objects along with a number of relevant properties from which the most appropriate ones can be selected 2 2 System requirements ASPRO VLTI is run remotely through the JMMC website It is normally run as a Java2 applet which means that the appropriate Java plug in version 1 1 2 or higher must be installed If it is not installed please install the computer specific plug in first see http java sun
52. us login nor is it possible to retrieve files created or used during previous use of ASPRO VLTI It is however possible to save any plot generated by ASPRO VLTI as a PS or PDF file with either type of login 3 1 3 Setting a personal account on the ASPRO server Setting a personal account can be done simply by subscribing to the aspro users mailing list After sending an email to sympa mariotti ujf grenoble fr with sub aspro users in the subject line the user will receive a confirmation email containing his her username and password These are the entries to provide in the Application Applet window after checking the Start application using my account informations box see right part of Fig 2 3 1 4 Starting the ASPRO package To start the entire ASPRO package which includes ASPRO VLTI either anonymously or after logging in with a valid username password combination do not forget to click on the button once after filling the username and password fields simply select ASPRO in the Start menu of the Application Applet When ASPRO VLTI is launched one or two new tab s appear in the Application Applet window ASPRO and if the user has used an authenticated login File Management see Fig 3 The ASPRO tab should indicate that ASPRO VLTI is now running E Sl ANOO Application Applet SON Application Applet d er Account File Management ASPRO User Account File Management ASPRO e Your application
53. user click on the button in the Interferometric Observables Explorer panel The user only needs to define the parametric model to be fit which can be one or the weighted sum of two simple parametric models Use Number of Functions Function 1 Function 2 and Parameters in the same way as in defining the object model see Sect 3 5 1 In addition the user can provide a range of possible values for the model parameters Starting Range and a number of evenly spaced values to test throughout that range Numb of Starts 1 means that the parameter is fixed to its prescribed value and 0 provides an automatic fit If a variable is not fixed then the value listed in Parameters and the Starting Range around them is a series of first guess es from which the iterative fitting process starts In this fitting process the fit is actually not performed on the synthetic visibilities created in the UV PLOTS module but rather on a noise added dataset a random quantity is added to each simulated visibility based on its associated uncertainties assuming a Gaussian distribution for the uncertainties Therefore the fitting process never recovers exactly i e with infinite accuracy the original model parameters This also means that repeating the fitting process yields different results every single time because of the random treatment of uncertainties Making a series of 10 fits and calculating the standard deviation of the resulting parameters can therefor
54. ware Furthermore right clicking lt CTRL gt click for Macintosh users on a variable parameter name in any panel brings up a brief explanation of its nature and possible values In addition use the buttons available in each ASPRO VLTI panel If no solution to a problem can be found there or in the ASPRO VLTI FAQ webpage on the JMMC website please send an email to the JMMC User Support group user support mariotti ujf grenoble fr with a detailed description of the problem including input parameters and error messages appearing in the LOG window if any Each of the OBJECT OBSERVATIONAL SETUP UV PLOTS and FIT MODEL panels which are described below contains a button to dismiss it However navigation between modules of ASPRO VLTI should normally be performed with the and buttons a method which ensures that the four main modules of ASPRO VLTI are used in the appropriate order Note ASPRO VLTI generates several files as commands are executed and uses them in other modules The naming convention of these files which can be retrieved by the user from his her ASPRO VLTI account 1s automatic and cannot be modified by the user 3 1 Launching the ASPRO package 3 1 1 The launcher applet r l r 2 Application Applet aaa Application Applet Start a User Account k pm User Account Authentication is made on mariotti fr Authentication is made on mariotti fr __ Start application using my account informat
55. y the target brightness The instrumental configuration must then be selected for MIDI observations the user must choose the Beam Combiner High Sens or Sci Phot and the Spectrograph Prism or Grism for AMBER observations the user must select the Spectral Resolution High Medium or Low Finally the user must specify at what frequency he she plans on obtaining calibrated visibilities Observing frequency The default value proposed in ASPRO VLTI is the ESO selected normal observing frequency If longer or more sparse observations are required modify this entry Once all parameters are set click on the button to visualize the UV cov erage resulting from the requested setup see right part of Fig 11 The module of the Fourier Transform of the object model i e the interferometric visibility is automatically underplotted on a linear stretch which provides a visual indication of the relevance of the selected setup In the example given in Fig 11 the selected UV coverage appears to sample a range of visibilities from relatively high to low values If the UV coverage appears inappropriate for the object model the telescope stations and or wavelength of interest can be modified and the UV coverage recalculated Once a satisfactory coverage has been found click on the Proceed to Visibility Panel button to reach the next main module of ASPRO VLTI Revision 6 0 Page 17 30 JMMC MAN 2100 002 ASPRO VLTI User s Manual
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