1. The JMMC softwares to prepare AMBER observations AMBER Workshop - LAOG - 9 Nov 2004

2. The observing path from A to Z Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!! Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!!

3. The observing path from A to Z Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!! Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!!

4. The observing path from A to Z Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!! Have a great idea that needs VLTI- AMBER ! Make sure it is feasible and useful Write a good ESO proposal Get observing time with AMBER Prepare and perform observations Analyze data Publish a great paper !!!

5. JMMC’s mission JMMS is a network that gathers most of the French interferometric expertise Its goal is to help VLTI users throughout the process, except for what is taken care of by ESO or by the instruments’ team This is true for both the French and European community JMMC provides softwares and support JMMS is a network that gathers most of the French interferometric expertise Its goal is to help VLTI users throughout the process, except for what is taken care of by ESO or by the instruments’ team This is true for both the French and European community JMMC provides softwares and support

6. JMMC’s mission Pre-observing tools: software to simulate the proposed observations, evaluate their feasibility/usefulness and get ready for the observations themselves

7. JMMC’s mission Pre-observing tools: software to simulate the proposed observations, evaluate their feasibility/usefulness and get ready for the observations themselves Post-observing tools: software to model the calibrated visibilities and closure phases and extract as much science as possible Pre-observing tools: software to simulate the proposed observations, evaluate their feasibility/usefulness and get ready for the observations themselves Post-observing tools: software to model the calibrated visibilities and closure phases and extract as much science as possible

8. JMMC’s two main softwares ASPRO « Interferometer Simulator » (many arrays) Much broader than VLTI-AMBER Provides UV coverage, V 2 estimates, modelling ASPRO « Interferometer Simulator » (many arrays) Much broader than VLTI-AMBER Provides UV coverage, V 2 estimates, modelling

9. JMMC’s two main softwares ASPRO « Interferometer Simulator » (many arrays) Much broader than VLTI-AMBER Provides UV coverage, V 2 estimates, modelling SearchCalibrators Name is self-explanatory Only for < 2.5  m (for now) ASPRO « Interferometer Simulator » (many arrays) Much broader than VLTI-AMBER Provides UV coverage, V 2 estimates, modelling SearchCalibrators Name is self-explanatory Only for < 2.5  m (for now)

10. JMMC’s support services Users’ manual are available with the softwares

11. JMMC’s support services Users’ manual are available with the softwares An email contact has been set-up to answer all types of questions: user-support@mariotti.ujf-grenoble.fr Questions are either answered directly or redirected to the appropriate service/person Users’ manual are available with the softwares An email contact has been set-up to answer all types of questions: user-support@mariotti.ujf-grenoble.fr Questions are either answered directly or redirected to the appropriate service/person

12. JMMC’s support services Users’ manual are available with the softwares An email contact has been set-up to answer all types of questions: user-support@mariotti.ujf-grenoble.fr Questions are either answered directly or redirected to the appropriate service/person An FAQ webpage will be populated as questions come through the mailing list Users’ manual are available with the softwares An email contact has been set-up to answer all types of questions: user-support@mariotti.ujf-grenoble.fr Questions are either answered directly or redirected to the appropriate service/person An FAQ webpage will be populated as questions come through the mailing list

13. How to access the softwares For now, both softwares only runs remotely through a Java applet Accessible directly from the JMMC webpage http://mariotti.ujf-grenoble.fr For now, both softwares only runs remotely through a Java applet Accessible directly from the JMMC webpage http://mariotti.ujf-grenoble.fr

14. How to access the softwares For now, both softwares only runs remotely through a Java applet Accessible directly from the JMMC webpage http://mariotti.ujf-grenoble.fr ASPRO also exists in an ASPRO-VLTI version that is specific to the upcoming ESO Call for Proposal (once it is released). For now, both softwares only runs remotely through a Java applet Accessible directly from the JMMC webpage http://mariotti.ujf-grenoble.fr ASPRO also exists in an ASPRO-VLTI version that is specific to the upcoming ESO Call for Proposal (once it is released).

15. Principles of ASPRO ASPRO estimates the observability of a source given its coordinates (delay lines)

16. Principles of ASPRO ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like) ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like)

17. Principles of ASPRO ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like) It populates a UV table with a user-defined geometic model for the source ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like) It populates a UV table with a user-defined geometic model for the source

18. Principles of ASPRO ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like) It populates a UV table with a user-defined geometic model for the source It calculates visibilities and phases ASPRO estimates the observability of a source given its coordinates (delay lines) It provides an indicative PSF corresponding to the proposed UV coverage (radio-like) It populates a UV table with a user-defined geometic model for the source It calculates visibilities and phases

19. Principles of ASPRO ASPRO estimates errorbars on the observable quantities based on the performances of the instrument

20. Principles of ASPRO ASPRO estimates errorbars on the observable quantities based on the performances of the instrument It provides a modelling of the simulated datasets to see how constraining the proposed observations are ASPRO estimates errorbars on the observable quantities based on the performances of the instrument It provides a modelling of the simulated datasets to see how constraining the proposed observations are

21. Principles of ASPRO ASPRO estimates errorbars on the observable quantities based on the performances of the instrument It provides a modelling of the simulated datasets to see how constraining the proposed observations are It creates graphical outputs for proposals ASPRO estimates errorbars on the observable quantities based on the performances of the instrument It provides a modelling of the simulated datasets to see how constraining the proposed observations are It creates graphical outputs for proposals

22. Principle of SearchCalibrators To calibrate the system’s performance, observations of a good calibrator are required just before or after the scientific target

23. Principle of SearchCalibrators To calibrate the system’s performance, observations of a good calibrator are required just before or after the scientific target Good calibrator = similar brightness (visible and near-infrared) as well as nearby location in the sky (same instrumental set-up) To calibrate the system’s performance, observations of a good calibrator are required just before or after the scientific target Good calibrator = similar brightness (visible and near-infrared) as well as nearby location in the sky (same instrumental set-up)

24. Principle of SearchCalibrators To calibrate the system’s performance, observations of a good calibrator are required just before or after the scientific target Good calibrator = similar brightness (visible and near-infrared) as well as nearby location in the sky (same instrumental set-up) Important: the calibrator’s properties must be well known, especially its apparent size!! To calibrate the system’s performance, observations of a good calibrator are required just before or after the scientific target Good calibrator = similar brightness (visible and near-infrared) as well as nearby location in the sky (same instrumental set-up) Important: the calibrator’s properties must be well known, especially its apparent size!!

25. Principle of SearchCalibrators Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target

26. Principle of SearchCalibrators Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty

27. Principle of SearchCalibrators Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty Multiple and/or variable stars can be flagged Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty Multiple and/or variable stars can be flagged

28. Principle of SearchCalibrators Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty Multiple and/or variable stars can be flagged List of answers depends on users’ requirements Several catalogues at CDS (Strasbourg) are cross-searched for stars within a small radius and limited magnitude range around the target When photometry and coordiantes are well defined, an SED fit provides the object’s radius (and the extinction) with its uncertainty Multiple and/or variable stars can be flagged List of answers depends on users’ requirements