1 / 21

Chair : M. Deleuil

Exoplanets Complementary Observations Working Group. Chair : M. Deleuil. Goal:. organise and coordinate observational efforts for programs using the exoplanet channel. prepare the targets selection + mask allocation. prepare the scientific analysis.

zavad
Download Presentation

Chair : M. Deleuil

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Exoplanets Complementary Observations Working Group Chair : M. Deleuil

  2. Goal: organise and coordinate observational efforts for programs using the exoplanet channel. prepare the targets selection + mask allocation prepare the scientific analysis prepare follow-up observations of transit candidates: confirmation & characterization Who is concern? People who intend to use exo-channel data: exoplanet core program + add. programs

  3. Focal plane: N 3.5º Secondary targets mv < 9 2.8º Exoplanet field Main target mv  6 stars with 11 < mv < 16 in principle .. 6000 photometric windows per CCDs : targets should be selected.

  4. A0 F0 G2 K2 M2 Magnitude Spectral type 11 12 13 14 15 characterization of all the stars needed! Targets selection  Scientific: - Favourite: late type dwarves Criteria:  Environmental: - crowding effects • Instrumental: - the shape of the PSF changes as a function of: • the location of the stars on the CCD • star’s colors • star’s magnitude

  5. Targets selection  Scientific: - Favourite: late type dwarves Criteria:  Environmental: - crowding effects • Instrumental: - the shape of the PSF changes as a function of: • the location of the stars on the CCD • star’s colors • star’s magnitude stars with 11 < mv < 16 at low galactic latitude : no catalogue provides the spectral classification

  6. Preparatory Observations - Step 1 Exoplanet domain ~20 HD 171834: Potential main target for the astero. program

  7. Preparatory Observations - Step 1 Catalogues: • Used for the spectral classification • will be used for the targets selection for short runs • DENIS/2Mass • USNO-A2 • Hipparcos/Tycho Long runs: (~ 20□)  ~ 4 106 stars with mv < 16 UBVRI Photometry - since 2001 - 2.5 INT/La Palma : 24 nights Will be complete at the end 2005 - CFHT/12K  a few deep exposures in R filter in order to characterize background stars.

  8. Data gathered in EXODAT Ground-based Observations - Status

  9. The ExoDat Data Base scientific DB for exoplanet channel • Archive the ground-based observations • Cross-correlate these data with existing catalogues • Perform the spectral classification • Validate algorithms: - allocation of the best photometric mask - estimate the contamination for each potential target • Prepare the scientific analysis • Validate the data provided to CoRotSky for the Exoplanet channel

  10. Spectral Classification 1) Dwarf / Giant sorting : Ground – based observations cross-correlated with 2Mass and/or DENIS data

  11. i < 16 AND V-i >1.0 Giants i < 16 AND V-i < 1.0 V-i MS MS i Spectral Classification: exemple HD174866 field Giants V - i Main Seq. i

  12. Spectral Classification 1) Dwarf / Giant sorting : From ground – based observations cross-correlated with 2Mass and/or DENIS data  luminosity class – good level of confidence for stars brighter than 15 in R 2) UBVRIJHK data compared with SEDs from a spectral library : Estimate of the spectral type of each star – the 3 “best” solutions are saved. Potential binarity is included.

  13.  Typical pre-selected field in the center direction: Typical pre-selected field in the anti-center direction: Additional informations on the target selection process for additional programs.. density of stars with R ≤ 15: ~ 6000 (HD 177552) % overlapping : ~ 30%  4200 potential targets / deg2 i.e. 5880 potential targets per CCD density of stars with R ≤ 15: ~ 3100 (HD 49434) % overlapping : ~ 20%  2480 potential targets / deg2 i.e. 3470 potential targets per CCD

  14. Spectroscopic observations Preparatory Observations - Step 2 Once CCDs position will be fixed .. • GIRAFFE/VLT : observations Dec 2004 & Jan 2005 (Guaranteed time + Open time)  A.M. Hubert on monday • VIMOS/VLT  V. Repipi on tuesday • Brazilian observational facilities  discussion on tuesday Goal : for stars with mv < 15 check & improve the spectral classification identify binaries derive stellar parameters: Teff, logg, vsini .. identify hot Jupiter in COROT fields

  15. Photometric survey: Complementary photometric observations: X-rays observations Preparatory Observations - Step 2 BEST (H. Rauer ) monitoring of the Exo-fields (mv < 14.5) 1 or 2 field per season Interest : binaries identification variable stars identification Geneva system (C. Aerts ) Goal : classification of variable stars BUT FOV 6.5’x6.5’ ! Interest and feasibility to be demonstrated (next CW) (F. Favata ) Interest: stellar activity, identify young stars .. (under study)

  16. ExoDat Data Base Contamination Mask design α,δ + error mag_R … Background mV > 16 Spect. type Logg, vsini, Radius, metal... Spectroscopic obs. α,δ + error mag_U+err mag_B+err mag_V+err mag_R+err mag_I+err mag_J+err mag_H+err mag_K+err Colors Images Spect. type Lum. class Binarity Broad Band Photom. Spect. Classif. Soft. Variability, X-rays.. Ground Surveys + Add Prog. Contamination CoRoTSky catalogues mv < 11

  17. α,δ + error mag_R Background mV > 16 Exo-stars in CoRoTSky Contamination Spect. Type Lum. Class Binarity V_min/V_max α,δ + error mag_B+err mag_V+err mag_R+err mag_I+err + star type catalogues mv < 11 Star type = information from add. programs

  18. Follow-up Observations • Necessary in order to • remove ambiguities, • better characterize the nature of the detected planet • derive accurate spectral parameters of the parent star. Radial velocity measurements

  19. Radial velocity follow-up strategy - 1 • SOPHIE – 1.93m OHP/France Fiber-fed cross-dispersed Echelle spectrograph 1st commissioning by the end of 2005 3 m/s in 1 hour for mv = 12.5 • 2m TLS - TAUTENBOURG Germany • Remove ambiguities • HR Spectrocopy of the parent star • Characterization of all the companions with masses  Jupiter • Filter the targets for HARPS and UVES+FLAMES

  20. Radial velocity follow-up strategy - 2 • HARPS – 3.6m La Silla • 3 – 30 M (10 M - 0.1 AU - G0 - mv=14) • 50 nights already allocated in HARPS guaranteed time • Possibility to follow-up immediately a detected transit • Additional nights  ESO proposals • UVES+FLAMES – 8.2m Paranal • 0.1 – 1 MJup (0.3 MJup - 0.1 AU - G0 - mv=16) • ESO proposal  ~ 12 months of delay…

  21. data analysis - spectral classification observational facilities In conclusion .. We are dealing with a large set of data A lot of work has already been done but help is very welcome

More Related