2015A&A...576A..80L


Query : 2015A&A...576A..80L

2015A&A...576A..80L - Astronomy and Astrophysics, volume 576A, 80-80 (2015/4-1)

Gaia-ESO Survey: Analysis of pre-main sequence stellar spectra.

LANZAFAME A.C., FRASCA A., DAMIANI F., FRANCIOSINI E., COTTAAR M., SOUSA S.G., TABERNERO H.M., KLUTSCH A., SPINA L., BIAZZO K., PRISINZANO L., SACCO G.G., RANDICH S., BRUGALETTA E., DELGADO MENA E., ADIBEKYAN V., MONTES D., BONITO R., GAMEIRO J.F., ALCALA J.M., GONZALEZ HERNANDEZ J.I., JEFFRIES R., MESSINA S., MEYER M., GILMORE G., ASPLUND M., BINNEY J., BONIFACIO P., DREW J.E., FELTZING S., FERGUSON A.M.N., MICELA G., NEGUERUELA I., PRUSTI T., RIX H.-W., VALLENARI A., ALFARO E.J., ALLENDE PRIETO C., BABUSIAUX C., BENSBY T., BLOMME R., BRAGAGLIA A., FLACCOMIO E., FRANCOIS P., HAMBLY N., IRWIN M., KOPOSOV S.E., KORN A.J., SMILJANIC R., VAN ECK S., WALTON N., BAYO A., BERGEMANN M., CARRARO G., COSTADO M.T., EDVARDSSON B., HEITER U., HILL V., HOURIHANE A., JACKSON R.J., JOFRE P., LARDO C., LEWIS J., LIND K., MAGRINI L., MARCONI G., MARTAYAN C., MASSERON T., MONACO L., MORBIDELLI L., SBORDONE L., WORLEY C.C. and ZAGGIA S.

Abstract (from CDS):

The Gaia-ESO Public Spectroscopic Survey is obtaining high-quality spectroscopy of some 100000 Milky Way stars using the FLAMES spectrograph at the VLT, down to V=19 mag, systematically covering all the main components of the Milky Way and providing the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. Observations of young open clusters, in particular, are giving new insights into their initial structure, kinematics, and their subsequent evolution. This paper describes the analysis of UVES and GIRAFFE spectra acquired in the fields of young clusters whose population includes pre-main sequence (PMS) stars. The analysis is applied to all stars in such fields, regardless of any prior information on membership, and provides fundamental stellar atmospheric parameters, elemental abundances, and PMS-specific parameters such as veiling, accretion, and chromospheric activity. When feasible, different methods were used to derive raw parameters (e.g. line equivalent widths) fundamental atmospheric parameters and derived parameters (e.g. abundances). To derive some of these parameters, we used methods that have been extensively used in the past and new ones developed in the context of the Gaia-ESO survey enterprise. The internal precision of these quantities was estimated by inter-comparing the results obtained by these different methods, while the accuracy was estimated by comparison with independent external data, such as effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. A validation procedure based on these comparisons was applied to discard spurious or doubtful results and produce recommended parameters. Specific strategies were implemented to resolve problems of fast rotation, accretion signatures, chromospheric activity, and veiling. The analysis carried out on spectra acquired in young cluster fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products. These include targets in the fields of the Oph, ChaI, NGC2264, γ Vel, and NGC2547 clusters. Stellar parameters obtained with the higher resolution and larger wavelength coverage from UVES are reproduced with comparable accuracy and precision using the smaller wavelength range and lower resolution of the GIRAFFE setup adopted for young stars, which allows us to provide stellar parameters with confidence for the much larger GIRAFFE sample. Precisions are estimated to be ≃120K rms in Teff, ≃0.3dex rms in logg, and ≃0.15dex rms in [Fe/H] for the UVES and GIRAFFE setups.

Abstract Copyright:

Journal keyword(s): open clusters and associations: general - surveys - methods: data analysis - stars: pre-main sequence - stars: fundamental parameters

Simbad objects: 15

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Number of rows : 15
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * tau Cet PM* 01 44 04.0834226 -15 56 14.926552 4.43 4.22 3.50 2.88 2.41 G8V 1144 1
2 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 3121 0
3 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2793 0
4 NGC 2264 OpC 06 40 58 +09 53.7           ~ 1642 0
5 Ass Vel OB 2 As* 08 09 22.478 -47 21 03.46           ~ 227 0
6 * gam02 Vel WR* 08 09 31.95013 -47 20 11.7108 0.64 1.58 1.83 1.85 2.00 WC8+O7.5III-V 858 0
7 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 336 0
8 IC 2602 OpC 10 42 58 -64 24.0           ~ 585 0
9 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1031 1
10 * rho Oph ** 16 25 35.11766 -23 26 49.8150 4.30 4.85 4.63 4.27 3.96 B2IV+B2V 625 0
11 NAME rho Oph Cluster Cl* 16 26 22 -24 23.7           ~ 55 0
12 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 971 2
13 NGC 6705 OpC 18 51 05 -06 16.2   6.32 5.8     ~ 371 0
14 * 61 Cyg A BY* 21 06 53.9396100677 +38 44 57.897024357 7.50 6.39 5.21 4.19 3.54 K5V 974 0
15 NAME Local Group GrG ~ ~           ~ 7392 0

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2021.10.21-05:18:58

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