1. Corot Week 61 Targets selection Be stars Paris-Meudon Observatory: A.-M. Hubert, M. Floquet, C. Neiner Univ. of Valencia: J. Fabregat, J. Gutierrez-Soto, J. Suso Univ. of Sao Paulo: E. Janot-Pacheco, L. Andrade, S. Daflon Royal Observatory of Belgium: Y. Frémat ESA, Estec, RSSD: C. Neiner

2. Corot Week 62 Early and late Be stars: 2 science goals  Early Be stars (B0-B3): pulsations and multiperiodicity already detected from the ground  Is the beating effect of close pulsation periods the cause of the Be phenomenon i.e. the presence of a disk around Be stars?  Effects of fast rotation and magnetic field on the pulsations  Late Be stars (B4-B9): pulsations predicted by theory but the amplitude is too small to be detected from the ground  detection of pulsations with Corot!

3. Corot Week 63 Photometric variability: Hipparcos (Hubert & Floquet )  Some of the targets observed by Hipparcos: periodicity found!

4. Corot Week 64 Ground-based photometry + variability (Fabregat, Gutierrez-Soto, Suso)  Stromgren photometry at the 0.9m in Granada (6 weeks) for variability: detection of variability, periodicity and even multiperiodicity for HD 168797 and HD 179405  uvby photometry + narrow filters (H , H  ) at the 1.5m in Calar Alto (3 weeks) to search for faint Be stars in the exoplanet fields See Gutierrez-Soto et al. 2003 and posters!

5. Corot Week 65 Spectroscopy: GAUDI  for 6 < V < 8  spectra in GAUDI  17 new Be stars discovered in GAUDI (Neiner, Hubert & Catala, 2004) But:  No spectrum if V > 8  Does not allow variability study

6. Corot Week 66 Additional spectroscopy + variability (Hubert, Janot-Pacheco, Andrade)  Spectroscopic observations at the 1.5m at OHP (6 weeks)  Spectroscopic observations at the 1.6m at LNA (1 week)  Spectrum for Be stars with V > 8  Detection of variability

7. Corot Week 67 Determination of stellar parameters ( Frémat, Neiner, Daflon, Andrade)  Data : GAUDI + OHP + LNA  2 independent determinations: Frémat & Neiner + Daflon & Andrade  ~70 Be stars in the eyes of Corot (See Frémat, Neiner et al. 2004) 26000 3.75 253

8. Corot Week 68 Centre Main targetBe targetTypeVvsiniTefflog gVariability HD 171234+170580HD 171219B8e7.65300135903.07 HD 171834HD 171219B8e7.65300135903.07 HD 175726HD 175869B9IIIe5.56164118103.25 HD 177552- HD 181555+180642HD 181231B9Ve8.58250136583.73 HD 181367B8e9.36279135003.65  Only late Be stars in these primary targets fields. Results for primary fields

9. Corot Week 69 Anticentre Main targetBe targetTypeVvsiniTefflog gVariability HD 43318- HD 43587HD 43285B6Ve6.07240140003.780.45 d HD 43913A0e7.88 HD 45067- HD 46558HD 45901B2Ve8.8164265183.73phot HD 46484B1Ve7.74120270003.603.29 d HD 47359B0.5Ve8.87 HD 49933+49434HD 49330B0e8.92300270003.820.28 d HD 49585B0.5Ve9.13253260423.750.61 d HD 50209B9Ve8.33180118093.620.66 + 0.59 d HD 50696B1Ve8.83350213003.450.31 d HD 52265HD 50891B0pe8.880.54 d HD 51193B1Vnne8.06215229943.620.61 + 5.5 d HD 51404B3e9.3342225004.20.37 d HD 51452B0IIIne8.08298298873.88spec

10. Corot Week 610 Centre:  5 possible late Be stars including 3 well positioned next to the primary targets  no early Be stars Anticentre:  3 possible late Be stars including 3 well positioned next to the primary targets  10 possible early Be stars including 3 well positioned next to HD 52265 TOTAL: 18 possible Be stars (8 late, 10 early) including 9 well positioned (6 late and 3 early)

11. Corot Week 611 Field HD 171234 + HD 170580 171219

12. Corot Week 612 Field HD 175726 175869

13. Corot Week 613 Field 181555 + HD 180642 181367 181231

14. Corot Week 614 Field HD 43587 43285 43913 + HD 43913

15. Corot Week 615 Field HD 46558 + HD 47359 46484 45901 47359 46484

16. Corot Week 616 Field HD 49933 + HD 49434 50209 49330 49585 50696  3 early Be stars outside the CCDs with this position of the CCDs

17. Corot Week 617 Field HD 52265 + HD 50891 51404 51193 51452 50891

18. Corot Week 618 HR diagram of Be secondary targets Apparent Location + 4 Be stars

19. Corot Week 619 HR diagram of Be secondary targets Rotation effect  c = 0.95 + 4 Be stars

20. Corot Week 620 + 2 Be stars in the CCDs + 2 Be stars HR diagram of Be secondary targets Real Location = in the CCDs

21. Corot Week 621 Results for exploratory fields  ~ 60 possible Be targets for exploratory fields  It is better to concentrate on early Be stars, since we have very few early Be stars as secondary targets  2 already detected with multiperiodicity (Fabregat et al.) : HD 168797 (B3e) and HD 179405 (B5e)  Targets in non-selected primary fields have been well studied  easier candidates

22. Corot Week 622 Conclusions  We need early and late Be stars as secondary targets: 2 different science goals  We found variability, periodicity and even multiperiodicity in most of the Be stars, in spectroscopy and in photometry  We plan to search for magnetic fields with Espadons (CFHT) for the Be secondary targets (starting Feb. 2005)  We have 9 out of 18 Be stars (possible secondary targets) which are well positioned in the CCDs, but 6 late and only 3 early  We need to concentrate on early Be stars for the exploratory fields  We already have 2 very interesting exploratory candidates