J/A+A/472/577 NGC 330 Be stars and binaries (Martayan+, 2007)
Be stars and binaries in the field of the SMC open cluster NGC 330
with VLT-FLAMES.
Martayan C., Floquet M., Hubert A.M., Gutierrez-Soto J., Fabregat J.,
Neiner C., Mekkas M.
<Astron. Astrophys., 472, 577-586 (2007)>
=2007A&A...472..577M 2007A&A...472..577M
ADC_Keywords: Magellanic Clouds ; Stars, Be ; Stars, double and multiple
Keywords: stars: early-type - stars: emission-line, Be -
galaxies: Magellanic Clouds - stars: binaries: spectroscopic -
stars: binaries: eclipsing - stars: oscillations
Abstract:
Observations of hot stars belonging to the young cluster SMC-NGC 330
and its surrounding region were obtained with the VLT-GIRAFFE
facilities in MEDUSA mode. We investigated the B and Be star
properties and proportions in this environment of low metallicity. We
also searched for rapid variability in Be stars using photometric
databases.
Using spectroscopic measurements, we characterized the emission
and properties of Be stars. By cross-correlation with photometric
databases such as MACHO and OGLE, we searched for binaries in our
sample of hot stars, as well as for short-term variability in Be
stars. We report on the global characteristics of the Be star sample.
Description:
Spectra of a significant sample of the B star population in the young
cluster SMC NGC 330 and its surrounding field have been obtained with
the ESO VLT-FLAMES facilities, as part of the Guaranteed Time
Observation programs of the Paris Observatory (P.I.: F. Hammer). The
multi-fiber spectrograph VLT-FLAMES has been used in MEDUSA mode (132
fibres) at medium resolution.
Observations (ESO runs 72.D-0245A and 72.D-0245C) were carried out on
October 21-23, 2003 (blue and red spectra) and on September 9 (blue
spectra) and 10, 2004 (red spectra).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 131 135 Observational characteristics of Be stars
in the SMC
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See also:
J/A+A/462/683 : Velocities in SMC field of NGC 330 (Martayan+, 2007)
J/A+AS/134/489 : Be stars in MC young clusters (Keller+ 1999)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Source name (MHF[S9] NNNNN or SMC5_NNNNNN) (1)
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 26 F6.3 s RAs Right ascension (J2000)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination (J2000)
32- 33 I2 arcmin DEm Declination (J2000)
35- 39 F5.2 arcsec DEs Declination (J2000)
41- 45 F5.2 mag Vmag ?=- V magnitude
47- 52 F6.2 0.1nm EWHa ? Halpha equivalent width
54- 58 F5.2 --- I(V) ? Maximum intensity of the violet peak for
double-peak emission
59 A1 --- u_I(V) [:?] Uncertainty flag on I(V)
61- 65 F5.2 --- I(R) ? Maximum intensity of the red peak for
double-peak emission
66 A1 --- u_I(R) [:?] Uncertainty flag on I(R)
67- 73 F7.2 --- Imax ? Maximum intensity for a single peak emission
74 A1 --- u_Imax Uncertainty flag on Imax
78- 80 I3 km/s FWHMHa ? Full width at half maximum of the
circumstellar Hα emission
82- 86 A5 --- KWBBE kXXX number of the star in Keller et al.
(1999, Cat. J/A+AS/134/489).
Cl* NGC 330 KWBBE NNNN in Simbad
88-131 A44 --- Rem Remarks (2)
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Note (1): Name of the Be star in the EIS catalogue, or following our
catalogue if the star is not found in the EIS catalogue.
(MHF[S9] NNNNN or SMC5_NNNNNN).
Note (2): Remarks as follows:
cl = the star belongs to a cluster
bin = the star is a binary
sh = the star shows shell lines
Fe II = (red or blue lines) indicate that the corresponding lines
present emission components
He I = (red lines) indicate that the corresponding lines present
emission components
dble = when the corresponding emission is a double peak one
w = when the corresponding emission is weak peak one
noneb = no nebular lines have been detected
α(CS+neb) = the nebular line is present at Hα but cannot be
disentangled from the CS emission, and
αCS+αneb = the Hα CS and nebular lines can be disentangled
** = indicates that the star was pre-selected from the ESO-WFI
slit-less study Martayan et al. (2006, SF2A-2006, 481).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 16-Nov-2007