Ground Based Observations for the ESP V-1 1.Existing data and catalogues 2.Planned observations 3.Needed observations 4.Telescopes 5.Questions Sources: D. Barrado, R. Blomme, J.-C. Bouret, Y. Frémat, A. Lanzafame, C. Martayan, Y. Nazé, C. Neiner, V. Straizys Ground-Based Observations for GAIA (Meeting 1) – September 2006

Why Ground Based Observations ? - To calibrate the spectrophotometry. Important for ESP because of a loss of accuracy in the Blue and Violet. Need for faint comparison stars observations. - To validate the model atmospheres in the NIR at HR and in the whole optical range at lower resolution (photometry). - Measurement of radial velocities and orbit determination of massive Binaries. (CU4, CU6) + APs (CU8) - Variability status of emission line stars in the NIR. Is there a way to make a “clever” time-average of the RVS spectra for these stars ? - What models can we use for emission line stars ? How complex should they be ? - To validate the model atmospheres in the NIR at HR and in the whole optical range at lower resolution (photometry). - Find the best algorithm to classify them. - Calibration of the Ca IRT stellar activity index in cool stars. - Define the type of cool stars that need additional treatment. Find benchmarks for K and M stars. - Study cool stars with circumstellar material. - Classification of anomalous abundance stars. - Find benchmarks and detect missing atomic data in chemically peculiar stars.

Existing data and catalogues ftp://vizier.cfa.harvard.edu/pub/cats/III/217 Atlas of nm spectral region  = 840 nm – 880 nmR ~ 5000CARELEC Only a very few late-O type stars ! High-resolution spectroscopy over 8500 – 8750 A for GAIA  = 850 nm – 875 nmR ~ 20000ECHELLE Paper catalogue – the spectra need to be digitized A survey of Be stars in the 7500 – 8800 A region (Andrillat et al.)  = nm – nmR ~ 5000OHP193 ROUCAS + RETICON  = nm – nmR ~ 3000OHP193 ROUCAS + RETICON Ground-Based Observations for GAIA (Meeting 1) – September 2006 B & O stars FEROS archive  = 360 nm – 920 nmR ~ 48000ECHELLE Reed, B.C. 2003, AJ, 125, 2531 UVB  photometry of galactic OB stars Maiz-Apellaniz, J. et al. 2004ApJS Galactic O star catalog (photometry, stromgren)

Busa et al., A&A, in press The Ca II Infrared Triplet as a stellar activity diagnostic II. Test and Calibration with high resolution observations  ~ 840 nm – 880 nmHigh ResolutionSARG/TNG and Mc Donald « … Observations of 40 stars with different activity level … » Existing data and catalogues « …, we have large collections of spectral energy distributions for hundreds of stars. They include both normal (solar composition) stars and stars of various peculiarities. However, most of them are brighter than the 10th magnitude... They are collected from all available (mostly published) sources. » Ground-Based Observations for GAIA (Meeting 1) – September 2006

The NIRSPEC Brown Dwarf Spectroscopic Survey  = 960 nm – 2310 nmR ~ 2000, 20000NIRSPEC The Spectra of T Dwarfs I: NIR Data and Spectral Classification  = 1000 nm – 2500 nmR ~ 60, 120 NIRC  = 1200 nm – 2350 nmR ~ 1200 OSIRIS Sandy Leggett – M, L and T dwarf data archive  = 612 nm – 740 nmR ~ 1750, 900  = 1100 nm – 2350 nmR ~ Photometry H, J, K Keck LRIS spectra of late-M, L and T dwarfs  = 600 nm – 1000 nmR ~ Ultracool Dwarf Catalog  = 380 nm – 980 nmR ~ T dwarfs Photometry « … first get an homogeneous list, which should include a fair amount of objects in each spectral subclass, and try to get additional data when needed … » Existing data and catalogues Ground-Based Observations for GAIA (Meeting 1) – September 2006

Planned observations or proposals On-going service mode observations OHP: Telescope 1.52: AURELIE: Grating 4: R ~ 6000:  = 800 nm – 890 nm ESO: NTT: EMMI: Ech. 9 + Cross4, R ~ 9700:  = 580 nm – 990 nm Sample of O and W-R stars « … at least one star per spectral type/luminosity class combination + some binaries + a few ON/OC stars … » If everything is going right with the proposal, the data should be reduced and analyzed next year and used to test the model atmospheres. Will be released in 1 or 2 years. (078.D-0114) Ground-Based Observations for GAIA (Meeting 1) – September 2006 Sample of cool stars (planned proposal submissions) … at different level of activity to fill gaps in the data available and to refine the calibration of the activity level based on Ca IRT. Also to test other CU8 algorithms. « Proposal for TNG/SARG, … but difficult to get time there … » Nazé et al.

 Well known LBVs  Of stars (HD108, HD66811 …)  Oe, Be, Ae (HD53367, HD32991, XX Oph, …)  Other classes of stars with emission (B[e], Novae, Symbiotic stars, T Tauri …)  Follow-up of a massive binary. (CU4, CU6, CU8) Ground-Based Observations for GAIA (Meeting 1) – September 2006 Needed observations Sample of cool stars  Cool stars with circumstellar material.  We also need to establish what star can be used as benchmark for K and M type stars.  We need RVS data for different kind of chemically peculiar stars.  A target list have been prepared. Unfortunately, they contain mostly "bright" stars, since faint stars (10-14 mag) usually have no accurate classification and physical parameters available. So, spectral energy distributions of these "bright" stars may be used only for synthetic photometry and evaluation of possibilities to detect stars of various peculiarities. For direct calibration of the Gaia spectra we need stars fainter than 10 mag. The list of such stars with various peculiarities will be prepared before the planned ground-based observations.  Available qualified man power, but missing money for travel. Also needs an observatory with good astro-climate.

Not available but they should exist somewhere … CCD Observations from Andrillat, Jaschek et al.  = 400 nm – 900 nm B[e] stars. II. MWC 349 A Andrillat Y., Jaschek M., Jaschek C. =1996A&AS A B[e] stars. III. MWC 645 Jaschek M., Andrillat Y., Jaschek C. =1996A&AS J B[e] stars. IV. HD = MWC 142 Andrillat Y., Jaschek C., Jaschek M. =1997A&AS A B[e] stars. V. HD = MWC 158 Jaschek C., Andrillat Y. =1998A&AS J B[e] stars. VI. MWC 297 = IRAS Andrillat Y., Jaschek C. =1998A&AS A Interesting and yet existing data, but where could we get them ? B[e] stars. I. HD (=OY Gem) Jaschek C., Andrillat Y., Jaschek M. = June(I) 1996 Ground-Based Observations for GAIA (Meeting 1) – September 2006 Needed observations

Best suited telescopes and instruments Ground-Based Observations for GAIA (Meeting 1) – September 2006 OHP – 1.52 – AURELIE ESO – 2.2 – FEROS ESO – NTT – EMMI La Palma – NTG – SARG Pic du Midi – TBL – NARVAL Data from small telescopes (some Italian facility could be considered) VLT-FLAMES to derive APs for the faint calibration stars ?

Questions … 1.Will there be a database for the observations ? In which framework and how will it be build ? 2.What kind of data will it contain ? 3.What will be the policy adopted regarding new data as well as data retrieved from existing archives ? 4.Accessibility of the database … ? 5.Where can we have access to low dispersion CCD photometry ? (See the mail sent by Vytas Straizys to Caroline: urgent need for spectrophotometry of faint standard stars. Also need for accurate AP determination of these stars.) Ground-Based Observations for GAIA (Meeting 1) – September 2006