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AP summary Corot Be star group

AP summary Corot Be star group. GEPI, Meudon : Hubert, Floquet, Martayan, Fremat, Neiner Univ. Valencia : Fabregat, Guti é rrez-Soto, Suso Brazil : Janot-Pacheco, Andrade, Daflon in collaboration with the B stars group (Aerts et al.). Search for faint Be stars in the exoplanet fields.

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AP summary Corot Be star group

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  1. AP summary Corot Be star group GEPI, Meudon: Hubert, Floquet, Martayan, Fremat, Neiner Univ. Valencia: Fabregat, Gutiérrez-Soto, Suso Brazil: Janot-Pacheco, Andrade, Daflon in collaboration with the B stars group (Aerts et al.)

  2. 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

  3. 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.)

  4. 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 donein August 2005 (8 pointings * 4 CCDs) • more observations in December 2005 for the exoplanet field of the first long run toward the galactic anticenter

  5. 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

  6. 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]

  7. 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)

  8. 2MASS Be Black-body B B IR excess Spitzer colors Possible Be star observed with Spitzer Typical Be star SED

  9. Faint Be stars discovered for Corot • Anticenter field: • - 2 Be stars with Giraffe • 10 Be stars with Spitzer • a few Be stars with the INT (to be reduced...) • Center field: • ~30 Be stars in the center field with the INT

  10. 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

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