Evaluation of the Corot candidate fields including secondary candidates for long runs E. Michel COROT field evaluation mai 04, IAS E. Michel COROT field evaluation mai 04, IAS Objectives: Using Corotsky + complementary information on secondary candidates, Go through the list of candidate fields (ref document january/04) in order to estimate to which extent:  information on Corot fields is sufficient to evaluate their scientific interest  the present list can satisfy scientific expectations  We can propose more precise fields  eventually what should/could be added, how and when…

E. Michel COROT fields evaluation mai 04 IAS E. Michel COROT fields evaluation mai 04 IAS

E. Michel COROT fields evaluation E. Michel COROT fields evaluation

E. Michel COROT, E. Michel COROT, HD49933+HD49434

Field HD HD  3 early Be stars outside the CCDs with this position of the CCDs

E. Michel COROT, E. Michel COROT, HD49933+HD49434 For this field, the objects of specific interest mentioned: -Primary cand.: HD49933, HD HD50209 Be showing photometric variability with 2 close periods - HD (G) solar-like cand (Vsini=7.5 alph=14mas,Mv= ,Teff=5800K,Fe/H=-0.11 mV=7.9 - HD49330 early Be (1 period) - HD49585 early Be (1 period) RQ: The rest of the objects available in the field should be useful to complete HR diagramme exploration for variability

E. Michel COROT, E. Michel COROT, HD49933+HD49434 As an example, we scan the content of the field for the following position of the CCDs HD49933+HD49434

E. Michel COROT, E. Michel COROT, HD49933+HD49434

E. Michel COROT, E. Michel COROT, HD49933+HD49434 Selection aiming at HR diagramme coverage  Reasonably rich, but Fundamental parameters ?

E. Michel COROT, E. Michel COROT, HD49933+HD49434 Numerous objects with mV>8  need for complementary observations for parameters determination. How & when?

E. Michel COROT, E. Michel COROT, HD43587

E. Michel COROT, E. Michel COROT, HD43587

E. Michel COROT, E. Michel COROT, HD43587

E. Michel COROT, E. Michel COROT, HD43587

E. Michel COROT, E. Michel COROT, HD43587 Exo: we used “no constraints” After discussion with Magali: low density in the south, i.e. go rather north… For this field, the objects of specific interest mentioned: - Primary cand.: HD HD43856 a solar-like cand.(F Vsini=7.3km/s,alph=12.55,mV=8,MV= ,Teff=6100K,Fe/H= HD delta Sc slow rot.(F,Vsini=58.3km/s,alph=10.78,mV=7.56,MV= ,Tef=6900K,Fe/H=-0.25) - HD delta Scuti, slow rot (19km/s), TAMS - HD a B9 MS Hipp variable - HD a new Be star - HD Be star, weak phot. Var (Hipparcos) and spectro. Var (same period) RQ: All these objects cannot be put together on the CCD, but 6 of them can, leading to choose between HD (Be), HD (d Scu) and HD (Be) The rest of the objects available in the field should be useful to complete HR diagramme exploration for variability

E. Michel COROT, E. Michel COROT, HD43587 As an example, we scan the content of the field for the following position of the CCDs

E. Michel COROT, E. Michel COROT, HD43587 Selection aiming at HR diagramme coverage  Reasonably rich, but Fundamental parameters ?

E. Michel COROT, E. Michel COROT, HD43587 Numerous objects with mV>8  need for complementary observations for parameters determination. How & when?

E. Michel COROT, E. Michel COROT, HD52265

E. Michel COROT, E. Michel COROT, HD52265

E. Michel COROT, E. Michel COROT, HD52265

E. Michel COROT, E. Michel COROT, HD52265

E. Michel COROT, E. Michel COROT, HD52265 Exo:we used “no special problem”. Magali suggestions: in favor of the south for higher density For this field, the objects of specific interest mentioned: - Primary cand.: HD HD51332 a solar-like cand.(F Vsini=23.6km/s, alph=10.9, mV=7.12, MV= , Teff=6958K, Fe/H=0) - HD a d Scu (Vsini 17km/s) evolved ? - HD Be star (B0) (spectroscopic var, no photom) - HD Be (B0), phot. Var. (1 period) - HD Be (B1), phot. Var. (1 period) - HD Be, Var. (1 period) RQ: The rest of the objects available in the field should be useful to complete HR diagramme exploration for variability

E. Michel COROT, E. Michel COROT, HD52265 As an example, we scan the content of the field for the following position of the CCDs HD52265

E. Michel COROT, E. Michel COROT, HD52265

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD170580

E. Michel COROT, E. Michel COROT, HD Exo: we used “no special problem”; Magali: rather in favor of the north; low density in the south For this field, the objects of specific interest mentioned: - Primary cand.: HD Beta Ceph (multiperiodic,,but multiple system) - HD a d Scu (fast rotator, blue border) - HD d Scu unevolved fast rot - HD B Hipp var. - HD , Be - HD solar-like cand. F Vsini 20.6km/s, alph=10.75, mV=7.5, MV= , Teff=6500K, Fe/H=-0.27) - HD solar-like cand, F Vsini 11.9km/s, alph=15.24, mV=7.6, MV= , Teff=6300K, Fe/H=-0.23) RQ: The rest of the objects available in the field should be useful to complete HR diagramme exploration for variability

E. Michel COROT, E. Michel COROT, HD As an example, we scan the content of the field for the following position of the CCDs HD170580

E. Michel COROT, E. Michel COROT, HD Not rich in CCD A2, but objects with mV <8

E. Michel COROT, E. Michel COROT, HD171834

E. Michel COROT, E. Michel COROT, HD171834

E. Michel COROT, E. Michel COROT, HD171834

E. Michel COROT, E. Michel COROT, HD Exo: no special problem; Magali confirms For this field, the objects of specific interest mentioned: - Primary cand.: HD HD (G*)solar-like cand - HD (F*) solar-like cand - HD HGMN * belonging a cluster - HD dScu in eclipsing binary belonging to cluster - HD solar-like cand. F Vsini 20.6km/s, alph=10.75, mV=7.5, MV= , Teff=6500K, Fe/H=-0.27) - HD solar-like cand. F, Vsini=174, alph=16.9,mV=7.6, MV= , Teff=6400K, Fe/H= HD solar-like cand, F, Vsini=14km/s, alph=29, mV=5.39, MV= , Teff=6600, Fe/H= HD , solar-like cand, F, Visni 13.5km/s, alph=13.97, mV=7.5, MV= , Teff=6400K, Fe/H=-0.24 RQ: The rest of the objects available in the field should be usefull to complete HR diagramme exploration for variability

E. Michel COROT, E. Michel COROT, HD As an example, we scan the content of the field for the following position of the CCDs HD171834

E. Michel COROT, E. Michel COROT, HD171834

E. Michel COROT, E. Michel COROT, HD HD177552

E. Michel COROT, E. Michel COROT, HD

E. Michel COROT, E. Michel COROT, HD Exo:“north too crowded” For this field, the objects of specific interest mentioned: - Primary cand.: HD HD A variable, but dScu ? - HD MS B star.(for survey) - HD HGMN - HD Beta Lyrae ecl. Binary - HD , G, Vsini=6.3km/s, alph=15.7, mV=7.96, MV= , Teff=5500K, Fe/H=-0.21 (geante)

E. Michel COROT, E. Michel COROT, HD For information, content of the field for an arbitrary position of the CCDs. As an example, we scan the content of the field for the following position of the CCDs HD177552

E. Michel COROT, E. Michel COROT, HD177552

E. Michel COROT, E. Michel COROT, HD HD180642

E. Michel COROT, E. Michel COROT, HD HD180642

E. Michel COROT, E. Michel COROT, HD HD180642

E. Michel COROT, E. Michel COROT, HD HD180642

E. Michel COROT, E. Michel COROT, HD HD Exo: we used: “not very good, not too south”, After check with Magali: very dense, to be checked on specific position. For this field, the objects of specific interest mentioned: -Primary cand.: HD delta Sc. - Primary cand HD Beta Ceph, slow rot. - HD (F) solar-like cand, Vsini=18.2km/s, alph=14, mV=7.65, MV= , Teff=6300K, Fe/H= HD , solar-like cand, F, Vsini=21.1km/s, alph=20.21, mv=6.57, MV= , Teff=6300K, HD unevolved dScu - HD Be/Am visual bina ??? - HD Be - HD Be

E. Michel COROT, E. Michel COROT, HD HD As an example, we scan the content of the field for the following position of the CCDs HD HD

E. Michel COROT, E. Michel COROT, HD HD180642

THE LOWER PART OF THE INSTABILITY STRIP : the DSCT bookmarks ZAMS : 1 HD primary target 2 HD HD43587 UNEVOLVED : 3 HD HD HD HD HD HD HD >200 HD ZIGZAGS (TAMS) 7 HD HD HD EA HD171834

12 B stars with accurate parameters 12 B stars with accurate parameters

+ 2 Be stars in the CCDs + 2 Be stars HR diagram of Be secondary targets Real Location = in the CCDs

Conclusions E. Michel COROT field evaluation mai 04, IAS E. Michel COROT field evaluation mai 04, IAS Using Corotsky + complementary informations on secondary candidates,+ exo-field criteria  For each field: 6-8 “specific” objects,  among which ~3-6 observable together  to be completed to 10, for ~ half of it with:  mV<8 informations avaliables  8<mV<9.5 information not yet available  can the present list can satisfy scientific expectations? Yes  We can propose more precise fields: Yes, SOON, for some of them  Proposal for summer 04 based on available infos (seismo+exo)   eventually what should/could be added, how and when…: Stromgren photometry for complementary stars with mV-> 9.5 available mid 2005, To confirm the choice