Transcript Slide 1
AP summary Corot Be star group GEPI, Meudon: Hubert, Floquet, Martayan, Frémat, Neiner Univ. Valencia: Fabregat, Gutiérrez-Soto, Suso Brazil: Janot-Pacheco, Andrade, Daflon in collaboration with the B stars group (Aerts et al.) CW9, ESTEC, Dec 2005 1 Search for faint Be stars in the exoplanet fields - Spectroscopy with the VLT/Giraffe - Hα and R photometry with the WFI/INT + Stromgren photometry - IR photometry with IRAC/Spitzer Program accepted for AO1 CW9, ESTEC, Dec 2005 2 Spectroscopy with Giraffe Hubert et al. - with VLT/Giraffe multifiber spectrograph - parts of first anticenter long run field - study B stars to detect emission in Hα 2 faint Be stars detected... see CW8 (Hubert et al.) CW9, ESTEC, Dec 2005 3 Optical photometry with the INT Fabregat et al. - with WFI/INT (La Palma) with Hα and Sloan R filters detect emission line stars - whole exoplanet field of the first long run towards the galactic center done in August 2005 (8 pointings * 4 CCDs) - more observations in December 2005 for the exoplanet field of the first long run toward the galactic anticenter CW9, ESTEC, Dec 2005 4 Figure shows 1/32 of the whole field (1917 stars with R<16.5) we expect to detect ~300 emission line stars in the whole field CW9, ESTEC, Dec 2005 5 Stromgren photometry Fabregat et al. - Stromgren photometry of the whole field already obtained, but not yet reduced - allows to perform a photometric spectral classification of the detected emission line stars detect Be stars (~30 for center field) among emission line stars Diagram without reddening [m1]-[c1] CW9, ESTEC, Dec 2005 6 IR photometry with Spitzer Neiner et al. - photometry in 4 IR bands with Spitzer/IRAC - half of first anticenter field observed in 2004 - ~30000 stars detected and identified in each band - cross-correlation with 2MASS, DENIS and Corotsky - analysis of SEDs to find OB stars with IR excess detection of 10 Be stars (in anticenter field) CW9, ESTEC, Dec 2005 7 Typical Be star SED Possible Be star observed with Spitzer 2MASS Be Black-body B B IR excess Spitzer colors CW9, ESTEC, Dec 2005 8 Faint Be stars discovered for Corot Anticenter field: - 2 Be stars with Giraffe - 10 Be stars with Spitzer - 4 Be stars with Calar Alto (see Fabregat et al., CW5) - a few Be stars with the INT (to be observed in 2 weeks...) Center field: - ~30 Be stars in the center field with the INT CW9, ESTEC, Dec 2005 9 Program accepted for AO1 collaboration Be stars group and B stars group Observed all faint Be stars (~40) + some B stars (~250) in the center and anticenter fields Search for signatures of rotational modulation and pulsations Perform seismic modelling of the stellar interior structure Statistical study to fine-tune the excitation mechanism in B stars and calibrate evolutionary models Study occurence of Be phenomenon and relation with pulsations, magnetic field, rotation Link between Be outbursts and pulsation beating CW9, ESTEC, Dec 2005 10