Access to Astronomical Catalogues

← Click to display the menu
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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 131 135 Observational characteristics of Be stars in the SMC
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
Bytes Format Units Label Explanations
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)
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).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 16-Nov-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service