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The JMMC softwares to prepare AMBER observations

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

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The JMMC softwares to prepare AMBER observations

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  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 !!!

  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 !!!

  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 !!!

  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

  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

  8. JMMC’s two main softwares • ASPRO • « Interferometer Simulator » (many arrays) • Much broader than VLTI-AMBER • Provides UV coverage, V2 estimates, modelling

  9. JMMC’s two main softwares • ASPRO • « Interferometer Simulator » (many arrays) • Much broader than VLTI-AMBER • Provides UV coverage, V2 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

  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

  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

  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).

  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)

  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

  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

  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

  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

  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)

  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!!

  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

  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

  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

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