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1. File Help Curent DB Parameters Name Value Default Range gt amber amber_p2vm dummy Add to pool Request Pool Input Frames Filename Classification _ Je AMBER 2006 02 11T00 25 39 341 fits Locate Display Ja _ JAMBER 2006 02 11T00 25 51 000 fits Locate J Display AMBER 2006 02 11T00 26 08 457 fits_ Locate Display AMBER 2006 02 11T00 26 39 319 fits Locate Display JAMBER 2006 02 11T00 26 54 079 fits Locate Display J AMBER 2006 02 11T00 27 18 478 fits Locate Display Zz Product Naming AADADDAH J gt JT_aj __ AAA Product Root Directory home tlicha amalitest products Browse Naming Scheme Numeric v gt za Ee Output Frames rLog Messages Save Clear Figure 6 7 1 The recipe amber_raw_to_fitsimage when launched in GASGANO Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Teang Issue 0 8 Date Date 2006 09 18 Page 26 of 46 The recipe will store the FITS image at the location tmp amber_raw_to_fitsimage fits It can be dis played by any capable FITS viewer i e the FV amber_p2vm v20001 File Help Curent reir Parameters Name Value Default Range amber amber_p2vm dummy Add to pool Request Pool _ rlnput Frames DADRA lt _
2. Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Tue SUS Oe Date Date 2006 09 18 Page 37 of 46 DO category Type Explanation Required SCIENCE_REDUCED product frame OI FITS file J CALIB_REDUCED product frame OI FITS file J Table 7 7 1 Input files for the amber_selector recipe ESO Doc VLI MAN ESO 19500 XXXX AMBER Pipeline User Manual Sue Soie ng Date Date 2006 09 18 Page 38 of 46 8 Product Data Description Products can be distinguished in intermediate product and scientific product These products are classified by the DO of by Gasgano 7 according to their own DO category keyword PRO CATG assigned to them at creation time For this reason no classification keyword is listed in this section The name of the recipe or recipes used to create a given product is given here 8 1 8 2 Intermediate Products e Flat Field DO category AMBER_FLATFIELD Created by amber_detector Association keywords DET NTEL Bad Pixel Map DO category AMBER_BADPIX Created by amber_detector Association keywords DET NTEL Pixel To Visibility Matrix P2VM DO category P2VM_REDUCED Created by amber_p2vm Association keywords DET NTEL Scientific Products OI Product DO category SCIENCE_REDUCED Created by amber_SciCal Association keywords DET NTEL
3. colours MIDAS_00 graph_0 2006 02 11703 04 43 Total number of frames 1000 Vis 2 lt 0 2 0000 plotted 1000 Vis 2 gt 12 0000 sur 0000 snr gt 2 1000 T T 4 Fringe SNR Fringe SNR gt T T de EN N G t APA 2 Visibility 2 60 10 2 SARA 100 160 800 2860 11860 11980 11400 11420 11440 Fringe_SNR time 5 MIDAS_00 graph_0 Total number of frames 1500 Vis 2 lt 0 2 0000 plotted 1600 Vis 2 gt 12 0000 sar lt 2 0140 snr gt 2 1360 Bl 0458 Be 0461 B3 0441 Visibility 2 j 1 1 11460 11480 11600 time a MR_K_alfori Medium_K_1_2 1 17 Wavelength 2005 02 26709 07 56 Del Vel Wittkowski Cal Medium_K_1_2 1 Wavelength 0 04 Lila ace 208 ai als Su Wavelength Note that three baselines are present and displayed in Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual aso Issue Oe Date Date 2006 09 18 Page 31 of 46 7 Pipeline Recipes Interfaces 7 1 amber raw to fitsimage The AMBER pipeline recipe amber_raw_to_fitsimage is used to create a primary image from AMBER rawfiles which do contain tables of numbers only This image can be regarded as a recreation of the active area of the CCD sensor It is useful to check if the interferometric channel is actually showing fringes and if flux is present i
4. Explanation X the x position of the beam centroid Y the y position of the beam centroid SIZX the size in x direction of the beam SIZY the size in y direction of the beam FLUX the flux count of the beam Table 7 3 2 QC values written by amber_beampos recipe Depending on the type of the frame there will be a prefix written to identfy the specific optics used Example for a complete QC parameter including the prefix HIERARCH ESO OC CLDSTP SIZX 23 45 Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue issue Date Date 2006 09 18 Page 33 of 46 QC Prefix Explanation CLDSTP cold stop A K A in K band B K B in K band C K C in K band A H A in H band B H B in H band C H C in H band AJ A in J band B J B in J band CJ C in J band BCD A K_ BCD and A in K band BCD B K BCD and B in K band BCD CK BCD and C in K band BCD A H BCD and A in H band BCD B H BCD and B in H band BCD C H BCD and C in H band BCD A J BCD and A in J band BCD B J BCD and B in J band BCD C J BCD and C in J band OUTF A OUTF and A OUTF B OUTF and B OUTF C OUTF and C Table 7 3 3 OC value prefixes written by amber_beampos recipe File name DO category Type Explanation amber_beampos_xxxx fits BEAMPOS_REDUCED FITS FITS file with primary image of the beam and the QC pi 7 4 amber p2vm Table 7 3 4 Product of the amber_beampos recipe
5. The AMBER pipeline recipe amber_p2vm is used to create a pixel to visibility matrix P2VM This P2VM is containing the translation matrix for the interferometric channel to be able to calculate visibilities from scientific observations This recipe is able to handle 2 and 3 telescope P2VMs The DET NTEL keyword from the first rawfile s header will determine the mode The raw files are actually containing all possible variations of the shutter positions of the photometric channels and the response of the interferometric channel for the standard lamps used during that process Because in 3 telescope mode there is one more photometric channel compared The only product of the amber_p2vm recipe is the P2VM file as shown in Table 7 4 2 Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soie nS Date Date 2006 09 18 Page 34 of 46 DO category Type Explanation Required AMBER_BADPIX Calibration frame Bad Pixel Map of the detector y AMBER_FLATFIELD Calibration frame i Field of the detector y and the instrument s optical train AMBER_2P2V Raw frame 2 telescopes P2VM 5 frames are needed y AMBER_2WAVE Raw frame 2 telescopes P2VM spectral calibration AMBER_3P2V Raw frame 3 telescopes P2VM 10 frames are needed J AMBER_3WAVE Raw frame 3 telescopes P2VM spectral calibration Table 7 4 1 Input files for the amber_p2vm recipe File name DO category Type Explanat
6. 24 of 46 The basic format for using EsoRex is as follows esorex esorex_options recipe_name recipe_options set_of_frames A list of all the available recipes each with a one line description can be obtained using the command sorex recipes To get help for an individual recipe in the subsequent examples vmbias is used the following is used esorex help amber_SciCal In order to display the current parameters setting of a recipe either the recipe configuration file located under SHOME esorex may be viewed if present or the following command may be used esorex params amber_SciCal If the default recipe configuration file is not found or a particular value is not configured within this file then the system defaults will be shown and used A recipe can be run by specifying its name to EsoRex together with the name of a SOF see Section 6 3 page 22 For instance the following command line would be used to run the recipe amber_SciCal for processing the files specified in the SOF amber_SciCal sof esorex amber _SciCal amber_SciCal sof A recipe configuration file different from the default one see Section 6 4 page 23 can also be specified on the command line sorex recipe config my_alternative_config rc amber_SciCal amber_SciCal sof The recipe parameters can be modifyed either by editing directly the used configuration file or by specifying new parameter values on the command line usi
7. 11 Do not forget to activate the AMBER rul in your Gasgano preferences to make it calssify the AMBER files correctly LE ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 45 of 46 B Troubleshooting Guide Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue issue Date Date 2006 09 18 Page 46 of 46 C Geometrical distortions models The reduction of AMBER scientific data made by the AMBER pipeline is not based on a set of predefined mod els of the optical distortions affecting the instrument However it relies on the P2VM to correct for distortions 212
8. 2006 09 18 Page 29 of 46 6 10 Plotting the scientific results It is possible to plot the scientific results from previously stored products GASGANO will group the product at the end of the raw files of the observation so that they can easily be identified The particular product must be selected and right clicked In the menu Run must be chosen Selecting amber_gasgano_plot sh will start the plotting Please make sure that MIDAS is installed and that the amber_gasgano_plot prg resides in the same path as the script does A GASGANO Version 2 1 2 tlicha Linux Jal File Selected files Tools Help BSA Default grouping collapse Find entry y fina 1 File CLASSIFICATION DER TEE TPL ID ORIGFILE TPL EXPNO TPL NEXP ME AMBER ZUU6 UZ TITUZTS OSS SSIS VEH TEE mehr AMBER GET y H AMBER 2006 02 11T02 36 47 364 fits UNCLASSIFIED CPTPIST BASE12 AMBER_2Tstd_ AMBER_BASE1 21 6 ml H AMBER 2006 02 11T02 36 57 501 fits UNCLASSIFIED FRNSRC BASE12 AMBER_2Tstd_ AMBER_BASE1 22 7 El AMBER 2006 02 11T02 37 09 067 fits UNCLASSIFIED CPTPIST BASE12 AMBER_2Tstd_ AMBER_BASE1 23 7 H AMBER 2006 02 11T02 37 19 178 fits UNCLASSIFIED FRNSRC BASE12 AMBER_2Tstd_ AMBER_BASEL 24 8 H AMBER 2006 02 11T02 37 37 774 fits UNCLASSIFIED CPTPIS
9. Browse Naming Scheme Numeric Y E Execute Selected Figure 6 8 1 The recipe amber_p2vm when launched in GASGANO ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 28 of 46 6 9 Calculating the scientific results TODO Description selecting proper frame types mandaotry and optional frames amber_SciCal v20001 File Help Current OUEN a Parameters Name ak amber amber_SciCal str_option lamber amber_SciCal int_binning Input Frames Filename AMBER 2006 02 11T05 13 36 596 fits A AMBER 2006 02 11T06 11 30 007 fits AMBER 2006 02 11T06 13 29 571 fits AMBER 2006 02 11T06 14 57 175 fits AMBER 2006 02 11T06 16 48 723 fits AMBER 2006 02 11T06 18 24 260 fits AMBER_BPM_fuzzy_img fits AMBER_FFM_img fits Pro du Nai _ _ _ _ Product Root Directory nome fulicha arnolio test products H Browse Naming Scheme Numeric Y O Beaute S y Request Pool Display 30 Display Display Display Display v Execute Selected Figure 6 9 1 The recipe amber_SciCal when launched in GASGANO Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Teang Issue 0 8 Date Date
10. CPLDIR and OFITSDIR are properly set or the CPL and qfits have been installed into one of the system s standard directories This should keep the following example commands as simple as possible Please note also that the usage of the default installation prefixes in the example below is just for demon stration purposes Any directory for which one has write access can be used although it is not recom mended to use the distribution s source directory as the installation s target directory The simplest way to set up the package is to run the following command at the system prompt from the source tree s top level directory configure prefix usr local pipeline Alternatively if using the environment variable is preferred PIPE_HOME may be defined in the shell s startup file If the Bourne or a compatible shell i e sh bash ksh zsh etc is used to the file profile or bashrc if bash is used it should be added PIPE_HOME usr local pipeline export PIPE_HOME If the the C shell i e csh or tesh is used the commands above translate into setenv PIPE_HOME usr local pipeline and should be added to the C shell startup file cshrc To activate these settings one may either logout and login again or source the startup script manually 4 To compile and install the AMBER pipeline on the system run the following sequence of commands from the source tree s top level directory make
11. Note Number of Telescopes used Note Number of Telescopes used Note Number of Telescopes used Note Number of Telescopes used Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Boeng Date Date 2006 09 18 Page 39 of 46 9 Algorithms In this section the data reduction procedures applied by the 23 pipeline recipes currently in use see Section 6 2 are described in some detail Common algorithms as cosmic rays removal or bad pixel cleaning are described separately 9 1 General Algorthms 9 1 1 Dark subtraction Dark frames are taken during the actual observation run If no dark was taken though the dark channel left most on CCD chip will be taken as a substitute with less accuracy 9 1 2 Flat field correction The flat field correction merely consists of dividing the frame to be corrected by a given master lamp flat field frame produced by the recipe amber_detector It is currently under discussion if the flat field is implicit with the p2vm correction 9 1 3 fringe search TODO 9 2 Recipes Algorithms 9 2 1 recreation of active CCD sensor area TODO Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue issue Date Date 2006 09 18 Page 40 of 46 A Installation This chapter gives generic instructions on how to obtain build and install the AMBER pipeline Even if this chapter is kept as up to date as much as possible it
12. S make install Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e Seeng Date Date 2006 09 18 Page 43 of 46 The configure script provides a variety of command line options to customise the AMBER pipeline installation The list of available options can be obtained by running configure help Using a command line option always takes precedence over any previously set environment variable However it is important to include the options enable type prefix nable float to force the fftw subsystem to compile correctly In case your box has already the package scisoft pre installed you also have to add the F77 for proper compilation of AMBER pipeline A typical configuration could look like that configure prefix SCPLDIR nable type prefix nable float F77 After the installation has been completed the source tree is no longer needed and can be removed AA Configuring the pipeline recipe front end applications In this section an outline is given how to set up the recipe front ends EsoRex and Gasgano so that the just installed AMBER pipeline recipes can be executed by these applications For detailed instructions on how to configure the two currently available front end applications EsoRex and Gasgano please refer to their documentation available at http www eso org cpl esorex html and http www eso org gasgano respectively In the following it is assumed that the AMBER pi
13. ii ii Filename Classification AMBER 2006 02 11T00 25 39 341 fits Locate Display E EI AMBER 2006 02 11T00 25 51 000 fits Locate J Display j AMBER 2006 02 11T00 26 08 457 fits Locate Display AMBER 2006 02 11T00 26 39 319 fits Locate Display EI AMBER 2006 02 11T00 26 54 079 fits Locate J Display AMBER 2006 02 11T00 27 18 478 fits Locate j Display IE Product Naming Product Root Directory home tlicha amadlib_test products H Browse Naming Scheme Numeric Y a Execute Selected Secre Q Dd Clear Log Messages Save Clear Figure 6 7 2 Example FITS image ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 27 of 46 6 8 Calculating the Pixel To Visibility Matrix TODO Description selecting proper frame types mandaotry and optional frames amber_p2vm v20001 File Help Current MOTE Ra Parameters Kap Name Default amber amber_p2vm durnmy DS Request Pool Filename Classification AMBER 2006 02 11T00 25 39 341 fits AMBER 2006 02 11T00 25 51 000 fits AMBER 2006 02 11T00 26 08 457 fits AMBER 2006 02 39 319 fits_ 54 079 fits 18 478 f1ts Product Naming Product Root Directory home tlichafamalib_test products H
14. may not be fully applicable to a particular release This might especially happen for patch releases One is therefore advised to read the installation instructions delivered with the AMBER pipeline distribution These release specific instructions can be found in the file README located in the top level directory of the unpacked AMBER pipeline source tree The supported platforms are listed in Section A 1 It is recommended reading through Section A 2 3 before starting the installation A bundled version of the AMBER pipeline with all the required tools and an installer script is available from ftp ftp eso org pub cpl amber for users who are not familiar with the installation of software packages The AMBER pipeline can also be downloaded from http www eso org projects dfs dfs shared web vlt vlt instrument pipelines html or http www eso org observing gasgano amber pipe recipes html A 1 Supported platforms The utilisation of the GNU build tools should allow to build and install the AMBER pipeline on a variety of UNIX platforms but 1t has only been verified on the VLT target platforms e HP UX 11 00 or later e Linux glibc 2 1 or later e Sun Solaris 2 8 or later using the GNU C compiler version 3 2 or newer A 2 Building the AMBER pipeline This section shows how to obtain build and install the AMBER pipeline from the official source distribution A 2 1 Requirements To compile and install the AMB
15. the parameter names has currently no effect Although it is not used at the moment it is envisaged that this feature will be used in future releases to avoid potential name clashes The shorter parameter aliases are made available for use on the command line The parameter names belonging to the recipe specific configuration files are described in the corresponding recipe sections More than one configuration file may be maintained for the same recipe but in order to be used a configuration file not located under HOME esorex or having a name different from the recipe name should be explicitly specified when launching a recipe see next section 6 5 Running a recipe using EsoRex The AMBER pipeline recipes are implemented as plugins used by front end applications like EsoRex or Gasgano 7 to execute the recipes The file organiser Gasgano 7 provides an intuitive GUI for launching the recipes applying the same rules used by the DO for the available data frames classification whereas EsoRex is the most basic way for executing the pipeline recipes from the shell prompt that shall be described here The plugin concept allows the implementation of different front end applications with specific functionalities For a complete description on how to create a pipeline recipe launcher please refer to the CPL User Manual 6 Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e Seeng Date Date 2006 09 18 Page
16. will only contain the matching frames which passed the filter This means the resulting product can be plotted by the same tools like all other AMBER OI FITS files Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soene Date Date 2006 09 18 Page 35 of 46 DO category Type Explanation Required AMBER_BADPIX Calibration frame Bad Pixel Map of the detector J AMBER_FLATFIELD cross ee deedor i n J and the instrument s optical train AMBER_P2VM Calibration frame eee ey Ma me J of the instrument s optical train AMBER SCIENCE DARK Raw frame dark frame from scientific observation AMBER SCIENCE SKY Raw frame sky frame from scientific observation AMBER_SCIENCE Raw frame science object frame from scientific observation y AMBER_CALIB Raw frame calibrator object frame from scientific observation AMBER_SCIENCE_CALIB Raw frame standard calibrator object frame Table 7 5 1 Input files for the amber_SciCal recipe File name DO category Type Explanation amber_xxxx fits SCIENCE_REDUCED FITS OI FITS file with xxxx corresponding to the file s number Table 7 5 2 Product of the amber_SciCal recipe There is various different algorithms to select and filter data The algorithms can be selected and controlled by the parameters selection_method and selection_x selection_method First x Frames This method will filter the first number of x frames o
17. 0 XXXX ESO AMBER Pipeline User Manual e Soene Date Date 2006 09 18 Page 42 of 46 For example if the CPL has been installed into somewhere and therefore the CPL header files are located in somewhere include and the libraries are in somewhere lib the argument of the option with cpl or the path assigned to the variable CPLDIR must be somewhere Le the root directory of the CPL installation The same is true for the option or environment variable corresponding to gfits If command line options are used the argument of with cext is usually the same as the one passed to with cpl since both packages install together This is also reflected by the fact that there is no separate environment variable for the cext package By default the configuration seript will setup the installation path of the package as usr local This means that root privileges would be required to complete the installation If one does not have sufficient privileges or the default installation path is just not appropriate it is possible to change this default There are two possibilities using the scripts prefix option or defining the environment variable PIPE_HOME Using the option will override a possibly defined variable In either case the provided path is used for the installation of the AMBER pipeline All its components will be located in the directory tree rooted at this path The following example assumes that the variables
18. 2006 09 18 Page 8 of 46 Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Sse ng Date Date 2006 09 18 Page 9 of 46 1 Introduction 1 1 Purpose The AMBER pipeline is a subsystem of the VLTI Data Flow System DFS Its target user is ESO Data Flow Operations DFO in the generation of master calibration data in the reduction of scientific exposures and in the data quality control It should also serve as a quick look tool for Paranal Science Operations PSO Additionally the AMBER pipeline recipes are made public to the user community to allow a more personalised processing of the data from the instrument This manual is a complete description of the data reduction recipes used by the the AMBER pipeline reflecting the status of the AMBER pipeline as of June 30 2006 version 2 0 5 1 2 Acknowledgements The software package on which the AMBER pipeline is based was in large parts developed by the AMBER Consortium and it is still the foundation of the current AMBER interferometry data reduction 1 3 Scope This document describes the AMBER pipeline used at ESO Garching and ESO Paranal for the purpose of data assessment and data quality control 1 4 Applicable documents 2 VLT Data Flow System Specifications for Pipeline and Quality Control VLT SPE ESO 19600 1233 3 Data Flow for VLT instruments Requirement Specification VLT SPE ESO 19000 1618 2 0 4 DFS Pipeline amp Qu
19. 6 4 Recipe configuration Each pipeline recipe may be assigned a configuration file containing the default values of the parameters related to that recipe The possibility to create recipe configuration files and the way information is conventionally stored in such files depends on the front end application used for launching the pipeline recipes In this section the recipe configuration files created and handled by EsoRex are described Please refer to the Gasgano User s Manual 7 for information about saving recipe configuration parameters An EsoRex recipe configuration file can be generated in the directory SHOME esorex by EsoRex see Section 6 5 on page 23 at installation time and has the same name as the recipe to which it is related with the filename extension rc For instance the recipe amber_SciCal has its EsoRex generated configuration file named amber_SciCal rc Without a recipe configuration file the recipe will use the default values The definition of one parameter of a recipe may look like this Binning Binning of frames default 1 amber Parameters binning 10 In this example the parameter amber Parameters binning is setto the value 10 In the configuration file generated by EsoRex one or more comment lines are added containing information about the possible values of the parameter and an alias that could be used as a command line option see again Section 6 5 on page 23 The hierarchy introduced in
20. ER pipeline one needs e the GNU C compiler version 3 2 or later e the GNU gzip data compression program e aversion of the tar file archiving program and Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Seeng Date Date 2006 09 18 Page 41 of 46 e the GNU make utility An installation of the Common Pipeline library CPL must also be available on the system Currently the CPL version 2 0 or newer is required The CPL distribution can be obtained from http www eso org cpl Please note that CPL itself depends on an existing qfits installation The qfits sources are available from the CPL download page or directly from the qfits homepage at http www eso org projects aot qfits In conjunction with CPL 2 0 qfits 5 2 0 must be used In order to run the AMBER pipeline recipes a front end application is also required Currently there are two such applications available a command line tool called EsoRex and the Java based data file organizer Gasgano which provides an intuitive graphical user interface At least one of them must be installed The EsoRex and Gasgano packages are available at http www eso org cpl esorex html and http www eso org gasgano respectively For installation instructions of any of the additional packages mentioned before please refer to the documentation of these packages A 2 2 Downloading the AMBER pipeline source distribution From the ESO ftp server ftp f
21. EUROPEAN SOUTHERN OBSERVATORY Organisation Europ enne pour des Recherches Astronomiques dans 1 H misph re Austral Europ ische Organisation fiir astronomische Forschung in der s dlichen Hemisph re VERY LARGE TELESCOPE AMBER Pipeline User Manual VLT MAN ESO 19500 XXXX Issue 0 8 Date 2006 09 18 e J Prepared ESO AMBER Pipeline Team 2006 09 18 Name 0 Date Signature Approved P Ballester M Peron Name oe Date Signature Released P Quinn Name Date Signature This page was intentionally left blank ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 3 of 46 Change record Issue Rev Date Section Parag affected Reason Initiation Documents Remarks 1 0 09 07 2004 All First version This page was intentionally left blank Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual E Soie ng Date Date 2006 09 18 Page 5 of 46 Contents 1 Introduction 9 FPU OSE dt a a Sk see E o a a cada 9 1 2 Acknowledgements AEN a ee 9 EI SCOPE Ah i te e ee Taataa a Ay aaa aa eee he peak bdo od a Mew uty de 9 L Applicable documents ao o o bare a a a Le Wak ae ed 9 1 5 Reference documents 9 1 6 Abbreviations and acronyms 10 L7 GLOSSARY aleni sea As NN EE 10 2 Overview 11 3 AMBER Instrument Description 12 3il MOVERVIEW ha E A 2h hE Sy Te E A e de ee
22. M Processed by amber_SciCal Classification keywords DPR CATG CALIB DPR TYPE P2VM DPR TECH DO category AMBER_BADPIX Processed by amber_SciCal Classification keywords DPR CATG CALIB DPR TYPE BADPIX DPR TECH DO category AMBER_FLATFIE Processed by amber_SciCal Classification keywords DPR CATG CALIB DPR TYPE FLATFIELD DPR TECH Association keywords DET NTEL Association keywords DET NTEL Association keywords DET NTEL Note Number of Telescopes used Note Number of Telescopes used Note Number of Telescopes used ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 20 of 46 5 Ancillary Data Description Currently there is no static calibration data Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e DSe nS Date Date 2006 09 18 Page 21 of 46 6 Data Reduction In this section the usage of the AMBER pipeline recipes is described In particular typical data reduction sessions for each instrument operating mode are presented in Sections and 6 1 Reduction Cascade VLTI pipeline DO and RBS je reduction rules SOF raw frame classification BDD EHR as ol Display RTD Y y y boy amb
23. T BASE12 AMBER_2Tstd_ AMBER_BASE1 25 8 H AMBER 2006 02 11T02 42 01 884 fits AMBER_SCIENC DARK AMBER_2Tstd_ AMBER_2TSTD 1 Hd H AMBER 2006 02 11T02 44 37 415 fits UNCLASSIFIED COHERENC 2TEL AMBER_2Tstd_ AMBER_CAL_C 2 8 H AMBER 2006 02 11T02 44 52 879 fits UNCLASSIFIED COHERENC 2TEL AMBER_2Tstd_ AMBER_CAL_C 3 s H AMBER 2006 02 11T02 45 08 403 fits AMBER_SCIENCE OBJECT AMBER 2Tstd_ AMBER_2TSTD 4 9 H AMBER 2006 02 11T02 47 20 109 fits UNCLASSIFIED COHERENC 2TEL AMBER_2Tstd_ AMBER_CAL_C 5 10 H AMBER 2006 02 11T02 47 48 132 fits AMBER_SCIENCE OBJECT AMBER_2Tstd_ AMBER_2TSTD 6 10 H AMBER 2006 02 11T02 49 59 909 fits UNCLASSIFIED COHERENC 2TEL AMBER_2Tstd_ AMBER_CAL_C 7 11 E AmBER 2006 02 11T02 50 16 725 fits AMBER_SCIENCE OBJECT AMBER_2Tstd_ AMBER_2TSTD 8 11 DH AMBER 2006 02 11T02 52 28 984 fits UNCLASSIFIED COHERENC 2TEL AMBER_2Tstd_ AMBER_CAL_C 9 12 E AmBeR 2006 02 11T03 05 02 417 fits AMBER_SCIENCE OBJECT AMBER 2Tstd_ AMBER_2TSTD 1 4 H AMBER 2006 02 11T03 07 08 042 fits AMBER_SCIENCE OBJECT AMBER 2Tstd_ AMBER_2TSTD 2 4 H AMBER 2006 02 11T03 09 15 497 fits AMBER_SCIENCE OBJECT AMBER_2Tstd_ AMBER_2TSTD 3 4 i AMBER 2006 02 11T03 11 28 918 fits AMBER_SCIENC SKY AMBER_2Tstd_ AMBER_2TSTD 4 bh G amber_0000_0000 fits SCIENCE_REDU OBJECT AMBER_2Tstd_ 2 4 Bamber_0001_0000 firs SCIENCE_REDU OBJECT AMBER_2Tstd_ 3 4 Q GB 200155385 MR_K bellatrix El 4mser 2006 02 117T03 25 24 5 Run the fo
24. ality Control User Manual VLT MAN ESO 19500 1619 5 ESO DICB Data Interface Control Document GEN SPE ESO 00000 0794 6 Common Pipeline Library User Manual VLT MAN ESO 19500 2720 7 Gasgano User s Manual VLT PRO ESO 19000 1932 8 AMBER Calibration Plan VLT PLA AMB 15830 0004 1 5 Reference documents 2 X Yyyyyy and Z Zzzzzz 1996 TODO A amp A Supp v 117 p 393 404 ESO AMBER Pipeline User Manual E Doc VLT MAN ESO 19500 XXXX Issue 0 8 Date Date 2006 09 18 Page 10 of 46 1 6 Abbreviations and acronyms ADF ADM AMBER AT CPL CRV DFS DMD DO DRS ESO MIDAS FITS HR ICS IDS IRAF IWS LR MMU MOS MR P2VM PAF PWS QC RB RBS SAO SNR SOF TCS UT VLT VLI WCS 1 7 Glossary Aperture Definition File Aperture Definition in mm Astronomical Multi BEam combineR Auxilliary Telescope Common Pipeline Library Spectral curvature model Data Flow System Data Management Division Data Organiser Data Reduction System ESO s Munich Image Data Analysis System Flexible Image Transport System High Resolution Instrument Control Software Inverse Dispersion Solution Image Reduction and Analysis Facility Instrument WorkStation Low Resolution Mask Manufacturing Unit Multi Object Spectroscopy Medium Resolution Pixel To Visibility Matrix VLT PArameter File Pipeline WorkStation Quality Control Reduction Block Reduction Block Scheduler Smithsonian Astrophysical Observatory S
25. and 3 telescopes Optionally it will also perform a spectral calibration amber_SciCal This recipe calculates the visibilities along with additional information like the SNR error bars and the closure phase for the given band amber_selector This recipe can select or filter the visibilities by various algorithm such as Fringe Contrast SNR In the next sections a general description on the use of recipes is given together with more detailed information on the individual recipes First there will be a description of how to use the recipes with EsoRex and later how to use them with GASGANO 6 3 Set of frames Each pipeline recipe is run on a set of input FITS data files The filenames are listed together with their DO category in an ASCII file the Set of Frames SOF that is required when launching a recipe SOF files containing the frames selected by the user are automatically created by Gasgano 7 Here is an example of SOF valid for the amber_SciCal recipe AMBER 2003 02 04T16 31 53 012 fits AMBER_FLATFIELD AMBER 2003 02 04T16 31 54 014 fits AMBER_BADPIX AMBER 2003 02 04T16 31 55 038 fits AMBER_P2VM AMBER 2003 02 04T16 31 56 040 fits AMBER_SCIENCE_DARK AMBER 2003 02 04T16 31 57 045 fits AMBER_SCIENCE AMBER 2003 02 04T16 31 57 050 fits AMBER_SCIENCE_SKY The pipeline recipe will access the listed files when required b
26. be the frame A copy of the product will always be stored at the location tmp amber_raw_to_fitsimage fits with a fixed name to make it easier to write scipts for automation purposes Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soie ng Date Date 2006 09 18 Page 32 of 46 There are no amber_raw_to_fitsimage parameters A description of the algorithms used in this recipe is given in Section 9 2 1 page 39 7 2 amber detector The AMBER pipeline recipe amber_detector is used to create the bad pixel map and the master flat field for the AMBER instrument Recipe currently under development DO category Type Explanation Required AMBER_DETECTOR_DARK Raw frame dark exposure y AMBER_DETECTOR_FLAT Raw frame flat exposure y Table 7 2 1 Input files for the amber_detector recipe 7 3 amber beampos The AMBER pipeline recipe amber_beampos is used to monitor the beam alignment for the AMBER instru ment A technical template will create the 22 necessary files DO category Type Explanation Required AMBER_BEAMPOS Raw frame exposures with various optics settings y Table 7 3 1 Input files for the amber_detector recipe From these files the recipe will derive an image of the detector as well as QC parameters and write them to a product as well as to the QC log For each of the frames the following values are written QC Parameter
27. bstantially lower than the figures mentioned above Another example is differential interferometry If the source is not resolved i e substantially smaller than the lambda B limit then the differential phase still yields the displacement of the source photocenter with wavelength which in many cases has been shown to be able to provide decisive spatial information The accuracy on the photocenter displacement is typically the lamda B resolution divided by the fringe SNR For example in the case of AGN BLRs proposal 4 it has been shown that in 20 minutes of actual observations on K 12 object with tracked fringes we can achieve a 10 mas accuracy on the photocenter displacement 3 4 Flux Sensitivity Concerning the limits in sensitivity these depend on a large number of factors observing modes that correspond to the elementary exposure time high sensitivity 50ms high precision 10ms and long exposures any Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soie ng Date Date 2006 09 18 Page 15 of 46 but with fringe tracking the type of telescopes the spectral resolution the seeing etc Some of these are relatively well identified by the design of AMBER for instance transmission efficiency fiber coupling detector characteristics etc while many others are more diffcult to characterize at this time for instance the quality of fringe tracking and adaptive optics correction AA Field Of V
28. ctrograph Raw Data Figure 3 1 2 Left panel Sketch of the AMBER instrument The light enters the instrument from left Right panel Reconstituted image from AMBER raw data in three telescopes mode DK corresponds to a dark region of the detector Pk are vertically dispersed spectra from each telescope and IF is the spectrally dispersed interferogram Resolution Mode Abbreviation Description Low Resolution JHK LR The J H and K bands are covered simultaneously Medium Resolution JH MR The J and H bands are covered simultaneously Medium Resolution HK MR The H and K bands are covered simultaneously High Resolution J HR The J band is covered High Resolution H HR The H band is covered High Resolution K HR The K band is covered Table 3 2 1 AMBER modes for observations resolution will depend also on the signal to noise ratio SNR available which is in turn a function of the source brightness as well as of many factors mentioned below Under conditions of very high SNR it is in principle feasible to obtain higher resolutions than the broad limit given above This applies in particular to cases in which a source model is available and determinations of the visibility before the frst zero are suscient to constraint the size of the object for instance angular diameters and binary stars Reversely conditions of low SNR for instance for very faint sources will limit the actual maximum resolution to values which can be su
29. de Nice MPI fiir Radioastronomie Bonn and Osservatorio Astrofisico di Arcetri The instrument has been made available to the community and started operations in Paranal on October 1 2005 In this chapter a brief description of the AMBER instrument is given A more complete documentation can be found in the AMBER User Manual downloadable from http www eso org instruments amber 3 1 Overview AMBER is the first generation near infrared three way beam combiner This instrument provides simultane ously spectrally dispersed visibility for three baselines and a closure phase at three different spectral resolutions AMBER has been designed to investigate the milli arcsec surrounding of astrophysical sources like young and evolved stars active galactic nuclei and possibly detect exoplanet signal The main new feature of the instrument compared to other interferometric instruments is the simultaneous use of modal filters optical fibres and a dispersed fringe combiner using a spatial coding The AMBER team has therefore investigated carefully a data processing strategy for this instrument and is providing a new type of data reduction method Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual aso SUSO Date Date 2006 09 18 Page 13 of 46 Figure 3 1 1 The complex instrument AMBER consists of various optical and mechanical components to allow interferometric and spectroscopic observations at the same
30. e tnd 12 3 2 Observation Modes sup ek adh en yd A a ee EE EE a 13 3 3 Angular Resolution 1 MA ia A ted ae gO Ee OM gd 13 3 4 Flux Sensitivity 2 eea aia a a e el ee Ee ee eS 14 Ss O URI sects ate Sea e Bae el eae Bed en ae eta ae oath ae ba ia ek 15 4 Instrument Data Description 16 4l Calibration Frames oa aeta ca kal ana eee Wa AEN a A on ae aoe e A 16 4 2 Scientific Framnes coa ae as A de GER o oe Ba e dea ee Ha hoe Ea 18 5 Ancillary Data Description 20 6 Data Reduction 21 6 1 Reduction Cascade ati do es E Wao n BEE Gee ke eo aE he eed 21 6 2 AMBER pipeline recipes 2 21 6 35 Setool frames Ce SUS we cl eb Aen he EEN ne te te ed Ae i ee 22 6 4 Recipeconfiguration 23 6 5 Running a recipe using EsoRex 2 23 6 6 Running a complete data reduction using GASGANO e 25 Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue URES Date Date 2006 09 18 Page 6 of 46 6 7 Creating a primary FITS Image of the Channels o o e 25 6 8 Calculating the Pixel To Visibility Matrix 27 6 9 Calculating the scientific results e 28 6 10 Plotting the scientific results e 29 7 Pipeline Recipes Interfaces 31 Il amber raw to fitsimage i osei oreo ee 31 7 2 Samber det ctor csta ie ee ee A a A RO i a 32 Tea amber DESEAMOS ss yee fe weet a ae eile e Re earth a a ER eg eld Baar Bh hota tats 32 TAs bet BE ck a oh Re YT eet Be ee bh ws ee Ss tho eed 33 T thermal e
31. ecipe with the same exceptions mentioned above In the automatic pipeline environment a product data frame alone wouldn t trigger the launch of any recipe In the following all raw and product AMBER data frames are listed together with the keywords used for their classification and correct association The indicated DO category is a label assigned to any data type after it has been classified which is then used to identify the frames listed in the Set of Frames see Section 6 3 page 22 Raw frames can be distinguished in calibration frames and science frames Their intended use is implicitly defined by the assigned recipe 4 1 Calibration Frames These are frames that are used for instrument calibration e Detector Calibration and Flat Field These raw frames are for the creation of a master flat field and a bad pixel map DO category AMBER_DETECTOR_DARK Processed by amber_detector Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE DETDARK DPR TECH DO category AMBER_DETECTOR_FLAT Processed by amber_detector Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE DETFLAT DPR TECH Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e Soie ne Date Date 2006 09 18 Page 17 of 46 e Pixel To Visibility Matrix and Spectral Calibration These frames are f
32. er_init prg SA Display Raw Frames creates MIDAS Ca a I amber_detector prg amber_p2vm prg p amber_SciCal prg dra RTD displays prg keeps last P2VM E tmplamber_xxxx fits A pixel to visibility matrix 2 and 3 telescopes Itmplcurrent_P2VM fits amber_SciCal amber_display creation of image out of the raw tables amber_detector bad pixel map and science visibilities IAU exchange standard flatfield dark 3 phot generation inerferometric channel amdlib cfitsio mie cpllib MPIbonn_lib Figure 6 1 1 lt AMBER Association Map 6 2 AMBER pipeline recipes The current AMBER pipeline is based on a set of stand alone recipes assigned to different fundamental opera tions Creation of general calibration data or informational output amber_raw_to_fitsimage The AMBER raw frames are containing tables of numbers only This recipe is re creating an image of what the detector has recorded amber_detector This recipe creates the master flat field and the bad pixel map for the optical train and detector of the instrument Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e Sse ng Date Date 2006 09 18 Page 22 of 46 amber_p2vm Calculation of the Pixel To Visibility Matrix to be able to disentangle the interferometric channels for 2
33. f the observation in other words the earliest frames The purpose of this method is a more technical one It can be used to check the if the instrument is porperly supressing the very first few frames after switching the detector to on These frames usually contain garbage due to the design of the redout eletronics of the detector selection_method Fringe SNR gt x This method will filter all the frames where the Signal To Noise Ratio of the fringes is greater than the value of x Useful values of x could be 2 and above selection_method Fringe SNR percentage x This method will filter the frames where the Signal To Noise Ratio of the fringes is highest and leaving x percent of frames Le example if x 20 this method will filter the 20 percent of frames with the highest Fringe SNR and drop the other 80 percent selection_method Flux gt x This method will filter all the frames where the flux of is greater than the value of x Useful values of x could be and above selection_method Flux percentage x This method will filter the frames where the flux of is highest and leaving x percent of frames I e example if x 20 this method will filter the 20 percent of frames with the highest flux and drop the other 80 percent Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Toue E Date Date 2006 09 18 Page 36 of 46 Parameter Possible values Explanation 0 to 9999 binnin 8 ma
34. i he hae aisle EN e eae eS Be die ee ee db des 34 RO amber selector at ee A Ma o Ad ae ped ahd ta dead le ada 34 Le amper divider os a a Ae ees AA ee Boe ee EE 36 8 Product Data Description 38 8 1 Intermediate Products rsi se ak AA ee A ee eet A ae 38 8 2 Scientific Products mite eer cha Bek RA ee Re Eee Ae a E N a 38 9 Algorithms 39 HI General Algorthms lt a Sark Si Yee er EO A Een nd Pe Pa 39 OAT Dark SUDAH iro eea tare Sa A NEEN A la Pk Rack ea ea a 39 HL Plat meld correctiOn y cia lo we aA da ee be ER es 39 HE lt fringe seateh ea a A Ne a A ee BS 39 Hi Recipes Algorithms EN a a a ae Se oe bab ae ae 39 9 2 1 recreation of active CCD sensor area 39 A Installation 40 AT Supported platforms 4 40424 ir AA ee A A A A erter 40 A 2 Building the AMBER pipeline naaa 40 AL Requirements NEEN hae Boe we Se Se ba A 40 A 2 2 Downloading the AMBER pipeline source distribution 41 A 2 3 Compiling and installing the AMBER pipeline o a 41 Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue SSNS Date Date 2006 09 18 Page 7 of 46 A 3 Configuring the pipeline recipe front end applications 43 A 3 1 Setting up the EsoRex command line tool 43 A 3 2 Setting up Gasgano e 44 B Troubleshooting Guide 45 C Geometrical distortions models ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date
35. iew AMBER is a single mode instrument therefore theoretically the field of view is limited to the Airy disk of each individual aperture i e 250 mas for the ATs in K and 60 mas for the UTs in K Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soene Date Date 2006 09 18 Page 16 of 46 4 Instrument Data Description AMBER data can be separated into raw frames and product frames Raw frames are the unprocessed output of the AMBER instrument observations while product frames are either the result of the AMBER pipeline processing as reduced frames master calibration frames etc or are the result of the calculation of the Pixel To Visibility Matrix P2VM Any raw or product frame can be classified on the basis of a set of keywords read from its header Data classification is typically carried out by the DO or by Gasgano 7 that applies the same set of classification rules The association of a raw frame with calibration data e g of a science frame with a master falt field frame can be obtained by matching the values of a different set of header keywords Each kind of raw frame is typically associated to a single AMBER pipeline recipe i e the recipe assigned to the reduction of that specific frame type In the pipeline environment this recipe would be launched automatically A product frame may be input to more than one AMBER pipeline recipe but it may be created by just one pipeline r
36. ignal to Noise Ratio Set Of Frames Telescope Control Software Unit Telescope Very Large Telescope Very Large Telescope Interferometer World Coordinate System Optional section Remove if necessary Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soie ng Date Date 2006 09 18 Page 11 of 46 2 Overview The AMBER pipeline is a collection of data reduction recipes administrated by the higher level programs of the VLT Data Flow System DFS 1 The VLT Data Flow System provides an environment where the definition and the execution of the data reduction steps can be made entirely automatic The fundamental DFS software components making up the required functionality are the Data Organiser DO and the Reduction Block Scheduler RBS The DO applies some defined instrument dependent rules for the classification of the incoming frames for their association to suitable calibration data and for launching the appropriate recipe for their standard reduction The product of the DO is the Reduction Block RB an ASCII file containing all the necessary information for the specific data reduction The RB is executed by the RBS which calls the assigned pipeline recipe with the appropriate parameters and makes the data reduction products available to the Data Handling Server DHS The AMBER pipeline recipes can also be used outside the pipeline context as stand alone programs In this way they may be ea
37. ion amber_p2vm fits P2VM_REDUCED FITS Pixel to Visibilty Matrix Table 7 4 2 Product of the amber_p2vm recipe There are no amber_p2vm parameters A description of the algorithms used in this recipe is given in Section page 7 5 amber SciCal The AMBER pipeline recipe amber_SciCal is used to calculate visibilities from interferometric observations This recipe is able to handle 2 and 3 telescope observations The DET NTEL keyword from the first rawfile s header will determine the mode It can also handle all of the different bands in any resolution If there is more than one band present in the raw frame the recipe will split the bands and create a separate product for the J H and K band All the files that must be included in the input SOF are listed in Table 7 4 1 In addition to the frames marked as required there must be at least one frame of the DO categories AMBER_SCIENCE AMBER_CALIB or AMBER_SCIENCE_CALIB For each of them corresponding product will be created The only product of the amber_SciCal recipe is a OI file as shown in Table 7 5 2 The amber_SciCal parameters are listed in Table 7 5 3 A description of the algorithms used in this recipe is given in Section page 7 6 amber selector The AMBER pipeline recipe amber_selector is used to select matching frames from AMBER products created by amber_SciCal The output is again an AMBER product same OI FITS format like the input but
38. l replace the path to the recipes in the EsoRex configuration file If EsoRex has already been used for running recipes from other instruments the path to the AMBER recipes must be appended to the existing configuration file To do this edit the configuration file SHOME esorex esorex Go to the entry starting with esorex caller recipe dir This is a colon separated list of directories searched by EsoRex for recipes To add the AMBER recipes just append the AMBER recipe installation directory separated by a colon to the end of this list To verify the updated configuration execute the following command at the shell s prompt esorex recipes This should display a list of the available recipes on the terminal screen At the EsoRex homepage http www eso org cpl esorex html a detailed description of the application can be found A 3 2 Setting up Gasgano The AMBER recipe set can be incorporated into Gasgano s configuration using the Preferences dialog from the File menu Select the tab labeled Recipe Configuration and press the Add Recipe button A file selection dialog pops up where the recipes to add can be selected The selection has to be confirmed and Gasgano must be restarted to activate the new recipe configuration Now the recipes are seamlessly integrated into the application and the files to process can be passed to the recipes using drag n drop for details please have a look into the Gasgano User Manual
39. llowing command 7 Ei AmBeR 2006 02 11703 27 56 8 E AMBER 2006 02 11703 2 P home tlicha gasgano scripts AMBER amber_gasgano_plotsh E 9 El Amser 2006 02 11T03 3 d home tlicha amdlib_test products amber_0001_0000 fits d 10 El amser 2006 02 11703 30 42 el No 10 El amser 2006 02 11T03 35 11 0 AER 8 2 E amber_0001_0000 fits lt unknown orig name gt SCIENCE REDUCED Extension HEADER Y Find in header DPR v fina toad Fitter O Fitter Auto Display DATE 2006 02 24T 17 15 23 060 f TELESCOP FESO WITI A1 z Figure 6 10 1 Starting the plotting script from GASGANO To finish the plot and return to GASGANO one has to type bye in the window named inmidas After the plot has completed on screen there is a corresponding post script file available named tmp amber_0000 ps However this will be overwritten by the next plot so one has to copy it to a safe place for further usage ESO AMBER Pipeline User Manual Doc VLT MAN ESO 19500 XXXX Issue Issue 0 8 Date Date 2006 09 18 Page 30 of 46 The plots are different for the 2 and 3 telescopes case of course while in the 2 telescope case there is only one In the 3 telescopes case there are 3 baselines In the upper left of the plot there is the statistics of how many frames the observation contained and how many of them have been reduced giving a SNR greater than 2 Figure 6 10 3 Example plot for the 3 telescopes mode
40. n all photometric channels It can handle raw files taken in 2 and 3 telecope mode The image shows the vertically dispersed channels of the AMBER instrument as follows Dark Channel Photometric Channel Telescope 1 Photometric Channel Telescope 2 Photometric Channel Telescope 3 Interferometric Channel all Telescopes Figure 7 1 1 Example image for the 3 telescopes mode At least one of the files listed below must be included in the SOF If there are more files only the first one will be displayed DO category Type Explanation Required AMBER_2P2V Raw frame 2 telescopes P2VM AMBER_2WAVE Raw frame 2 telescopes P2VM spectral calibration AMBER_3P2V Raw frame 3 telescopes P2VM AMBER_3WAVE Raw frame 3 telescopes P2VM spectral calibration AMBER_SCIENCE_DARK Raw frame dark frame from scientific observation AMBER_SCIENCE_SKY Raw frame sky frame from scientific observation AMBER_SCIENCE Raw frame science object frame from scientific observation AMBER_CALIB Raw frame calibrator object frame from scientific observation Table 7 1 1 Input files for the amber_raw_to_fitsimage recipe Any of the AMBER raw frames can be displayed with that recipe This recipe is only creating an intermediate product namely a FITS file containing the primary image of the reconstructed image of the active regions of the detector In addition the header is completed with a copy of the raw frame s header to descri
41. nd a Bad Pixel Map For improved SNR it is useful to input the optional frames for sky and dark detector illumination DO category AMBER_SCIENCE Processed by amber_SciCal Classification keywords Association keywords Note DPR CATG SCIENCE DPR TYPE OBJECT DET NTEL Number of Telescopes used DPR TECH DO category AMBER_SCIENCE_DARK Processed by amber_SciCal Classification keywords Association keywords Note DPR CATG SCIENCE DPR TYPE DARK DET NTEL Number of Telescopes used DPR TECH DO category AMBER_SCIENCE_SKY Processed by amber_SciCal Classification keywords Association keywords Note DPR CATG SCIENCE DPR TYPE SKY DET NTEL Number of Telescopes used DPR TECH DO category AMBER_CALIB Processed by amber_SciCal Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE OBJECT DET NTEL Number of Telescopes used DPR TECH DO category AMBER_SCIENCE_CALIB Processed by amber_SciCal Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE STD DET NTEL Number of Telescopes used DPR TECH Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e Soe nS Date Date 2006 09 18 Page 19 of 46 DO category AMBER_P2V
42. ng the command line options defined for this purpose Such command line options should be inserted after the recipe name and before the SOF name For instance to set the amber_SciCal recipe binning parameter to 10 the following should be typed esorex amber_SciCal binning 10 amber_SciCal sof There are also parameters used to configure the EsoRex launcher that may be listed in an esorex rc con figuration file located under HOME esorex On the command line the EsoRex options must be inserted before and not after the specified recipe name The EsoRex options are those that are recipe independent as for instance the verbosity level the directory where the recipe products should be written or the permission to overwrite old products with new ones For more information on EsoRex see http www eso org cpl esorex html Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual aso issue Date Date 2006 09 18 Page 25 of 46 6 6 Running a complete data reduction using GASGANO For AMBER we need a two step data reduction First we must create a P2VM and with it we can reduce the scientific data taken with the same optical train 6 7 Creating a primary FITS Image of the Channels This recipe can display one AMBER raw frame at a time Select any of the following frames TO DO Table of classifications By right clicking and choosing amber_raw_to_fitsimage one can run the recipe amber_p2vm v20001
43. or calculation of a Pixel To Visibilty Matrix Optionally the 2WAVE amd 3WAVE files can be send to the recipe In this case the the recipe will also perform a new spectral calibration DO category AMBER_2P2V Processed by amber_p2vm Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE 2P2V DET NTEL Number of Telescopes used DPR TECH DO category AMBER_2WAVE Processed by amber_p2vm Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE WAVE 2TEL DET NTEL Number of Telescopes used DPR TECH DO category AMBER_3P2V Processed by amber_p2vm Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE 3P2V DET NTEL Number of Telescopes used DPR TECH DO category AMBER_3WAVE Processed by amber_p2vm Classification keywords Association keywords Note DPR CATG CALIB DPR TYPE WAVE 3TEL DET NTEL Number of Telescopes used DDR TECH Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual e SSe nS Date Date 2006 09 18 Page 18 of 46 4 2 Scientific Frames e Scientific Observation These frames are for scientific observations For the calculation of visibilities there is at least one science object frame needed In addition there must be a valid P2VM as well as a Flat Field a
44. peline was installed as described in Section A 2 3 i e that the AMBER recipes have been copied into usr local pipeline lib amber plugins amber X Y Z X Y and Z indicate the version number of the recipes A 3 1 Setting up the EsoRex command line tool The general syntax for the EsoRex front end is the following esorex esorex_options recipe_name recipe_options set_of_frames In order to execute a recipe EsoRex must be told where the recipes can be found This location can be passed to the tool using its command line option recipe dir followed by the complete path to the recipes In this scenario the command to be executed at the shell s prompt will look like esorex recipe dir gt usr local pipeline lib amber plugins amber X Y Z However the path to the recipe location s can also be set in the EsoRex configuration file If an EsoRex configuration file does not already exist it can be created by executing the command esorex create config recipe dir gt usr local pipeline lib amber plugins amber X Y Z Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual E E Date Date 2006 09 18 Page 44 of 46 In addition to just creating the configuration file in its standard location SHOME esorex esorex rc the path to the recipes is also added by this command This way for updating the configuration can be re peated whenever a new version of the recipes is installed It wil
45. sily used by astronomers at their home institutes or taken as building blocks for different data reduction strategies However the pipeline recipes being designed to operate within the DFS environment do not repeat the checks already performed by the DO In other words data classification and appropriate association are not proofed in any way within a recipe being taken for granted The Gasgano 7 data browser that is capable of classifying the data frames in the same way as the DO does greatly assist in the administration of a large quantity of different data frames The AMBER instrument and the different types of AMBER raw frames are briefly described in Sections 3 and 5 while the usage of the available reduction recipes is presented in Section 6 More detailed descriptions of the data reduction algorithms used by the individual pipeline recipes can be found in Sections C and 9 In Section an overview of what s new on AMBER Pipeline release 2 0 7 is given In Appendix A the installation of the AMBER pipeline recipes is described Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue issues Date Date 2006 09 18 Page 12 of 46 3 AMBER Instrument Description AMBER has been developed under ESO contract by the AMBER Consortium headed by the Laboratoire d Astrophysique de Grenoble with contributions from Observatoire de la Cote dSAzur Laboratoire Univer sitaire dS Astrophysique
46. time 3 2 Observation Modes AMBER offers three different modes of resolutions and three different bands in the following combinations One should note that the spectral coverage of the high spectral resolution does not cover the entire bands Depending on the type of science required one can choose to observe with AMBER in classical way or in differential mode The differential mode involves slight diffrences in the observing procedures but allows to obtain larger precision on the differential phase The expected accuracy are typically 1 for the high sensitivity mode 0 1 for the high precision mode and 0 01 for the phase in the high precision mode in the differential configuration This can be used either to obtain angular information on very unresolved objects or to aim at very high accuracy like in the extrasolar planets programs 3 3 Angular Resolution Angular resolution is set by the maximum available baseline which is about 200 meters for the ATs and about 130 meters for the UTs Accordingly the limit will be about 2 milliarcseconds mas for the ATs and about 3 mas for the UTs in the K band These values must be roughly halved for the J band Of course the actual Doc VLT MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Tene Scion Date Date 2006 09 18 Page 14 of 46 Spatial filtering Recombination Spectral dispersion Wavelength 50 100 Pixels Single mode fibers Output pupils Spe
47. tp eso org pub cpl amber the latest release of the AMBER pipeline distribution is available The AMBER pipeline sources are distributed as a gzipped tar archive named like amber X Y Z tar gz where X and Y are the major and minor release numbers and Z indicates the patch level which might be missing if no patch has been released A 2 3 Compiling and installing the AMBER pipeline It is recommended to read through this section before starting with the installation 1 First if an appropriate version of CPL c f section A 2 1 does not already exist on the system compile and install the CPL libraries and their dependencies For detailed instructions on how to install the CPL libraries please refer to the CPL documentation 2 Unpack the AMBER pipeline sources in a choosen directory using S zcat d amber X Y Z tar gz tar xf at the system prompt This will create a directory called amber X Y Z containing the source tree 3 Run the configuration script configure which is located in the top level directory of the AMBER pipeline source tree If the CPL or qfits have not been installed into one of the system s standard directories the configuration script must be told where the dependent libraries CPL qfits etc can be found This is either done using the command line options with cpl with cext and with qfits of the script or by defining the two environment variables CPLDIR and QFITSDIR Doc VLI MAN ESO 1950
48. ximum number of frames per observation the number of frames to be averaged for each of the visibility calculations Table 7 5 3 amber_SciCal parameters DO category Type Explanation Required SCIENCE_REDUCED product frame OI FITS file J CALIB_REDUCED product frame OI FITS file J Table 7 6 1 Input files for the amber_selector recipe selection_method Exclude Frames by ASCII File This method is an interface to any external tools which are able to identify frames to be excluded Simply store a file called tmp amber_exclude txt conatining the frame index There shall be only one frame index per line If you want to exclude frame number 13 20 25 and 255 the file should look like 13 20 25 255 Table 7 6 2 example of tmp amber_exclude txt As aresult the output OI FITS file will contain all frames but not the four numbered above selection_method Include Frames by ASCII File This method is the same like the exclude described above It just works the other way round It will leave the frames with the given index numbers and drop all the rest The file must be called tmp amber_include txt 7 7 amber divider The AMBER pipeline recipe amber_divider is used to create calibrated visibilities from AMBER two products created by amber_SciCal One product must be from calibrator and the other from a science object The output is currently undefined Recipe currently under development
49. y the reduction algorithm Note that the AMBER pipeline recipes do not proof in any way the correctness of the classification tags specified in the SOF In the above example the recipe amber_SciCal will treat the frame AMBER 2003 02 04T16 31 53 012 as a AMBER_FLATFIELD the frame AMBER 2003 02 04T16 31 54 014 fits AMBER_BADPIX as a AMBER_BADPIX etc even when they do not contain this type of data However the recipe will check all frames if the optical train is the same like it has been during recording the P2VM files It will also check if all the contained regions are consistent which each other Otherwise the usage of a particular P2VM file will result in useless data The reason of this lack of control is that the AMBER recipes are just the DRS component of the complete pipeline running on Paranal where the task of data classification and association is carried out by the Data Organiser On the other side using Gasgano 7 as an interface to the pipeline recipes will permit to classify the data frames exactly as the DO does A recipe handling an incorrect SOF may stop with not immediately understandable error messages at best In the worst cases the recipe would apparently run without any problem producing results that may look reasonable while they are instead flawed Doc VLI MAN ESO 19500 XXXX ESO AMBER Pipeline User Manual Sue Soie ng Date Date 2006 09 18 Page 23 of 46

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