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J/AJ/153/252  Photometric variability of BeSS-KELT stars  (Labadie-Bartz+, 2017)

Photometric variability of the Be star population. Labadie-Bartz J., Pepper J., McSwain M.V., Bjorkman J.E., Bjorkman K.S., Lund M.B., Rodriguez J.E., Stassun K.G., Stevens D.J., James D.J., Kuhn R.B., Siverd R.J., Beatty T.G. <Astron. J., 153, 252-252 (2017)> =2017AJ....153..252L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, Be ; Stars, variable ; Photometry, VRI ; Spectral types ; Photometry, infrared Keywords: stars: emission-line, Be - stars: oscillations - stars: variables: general - techniques: photometric - techniques: spectroscopic Abstract: Be stars have generally been characterized by the emission lines in their spectra, and especially the time variability of those spectroscopic features. They are known to also exhibit photometric variability at multiple timescales, but have not been broadly compared and analyzed by that behavior. We have taken advantage of the advent of wide-field, long-baseline, and high-cadence photometric surveys that search for transiting exoplanets to perform a comprehensive analysis of brightness variations among a large number of known Be stars. The photometric data comes from the KELT transit survey, with a typical cadence of 30 minutes, a baseline of up to 10 years, photometric precision of about 1%, and coverage of about 60% of the sky. We analyze KELT light curves of 610 known Be stars in both the northern and southern hemispheres in an effort to study their variability. Consistent with other studies of Be star variability, we find most of the stars to be photometrically variable. We derive lower limits on the fraction of stars in our sample that exhibit features consistent with non-radial pulsations (25%), outbursts (36%), and long-term trends in the circumstellar disk (37%), and show how these are correlated with spectral sub-types. Other types of variability, such as those owing to binarity, are also explored. Simultaneous spectroscopy for some of these systems from the Be Star Spectra database allow us to better understand the physical causes for the observed variability, especially in cases of outbursts and changes in the disk. Description: Kilodegree Extremely Little Telescope (KELT) is a photometric survey using two small-aperture (42 mm) wide-field (26°x26°) telescopes, with a northern location at Winer Observatory in Arizona in the United States, and a southern location at the South African Astronomical Observatory near Sutherland, South Africa. The Be Star Spectra (BeSS) database is a continually updated catalog that attempts to include all known Be stars, as well as their stellar parameters. This catalog is based primarily on the catalog of classical Be stars published by Jaschek et al. (1982, Cat. III/67) but also includes more recently discovered Be stars from a variety of sources (e.g., Neiner et al. 2005ApJS..156..237N; Martayan et al. 2006A&A...445..931M). From the BeSS database, we compiled a list of all the classical Be stars with 7<V<13, which included 1362 unique objects. This magnitude range was chosen to align with KELT's magnitude limits. This subset was then cross-matched with the KELT catalog, and 610 unique objects that exist in both data sets were recovered. Of the 610 stars in this sample, 374 are observed by KELT North, 206 are observed by KELT South, and 30 are observed by both KELT North and South (the joint field J06). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 282 610 Table of BeSS-KELT stars with variable type classifications
See also: III/67 : Catalogue of Be stars (Jaschek+, 1982) VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006) J/A+A/335/565 : Be stars variability (Hubert+ 1998) J/AJ/149/7 : SDSS-III/APOGEE. I. Be stars (Chojnowski+, 2015) http://basebe.obspm.fr : The BeSS database Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- BKNum [0/609] Internal identifier 5- 12 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000) (1) 14- 21 F8.4 deg DEdeg Declination in decimal degrees (J2000) (1) 23- 27 F5.2 mag Vmag [6.03/12.81] V band magnitude (1) 29- 38 A10 --- SpType Spectral type (1) 40- 61 A22 --- ID Common identifier (1) 62- 65 I4 --- NSpec [0/3317] Number of archival BeSS spectra 67- 70 I4 km/s vsini [5/500]? BeSS rotational velocity 72-106 A35 --- KeID KELT eastern orientation data file identifier 108-142 A35 --- KwID KELT western orientation data file identifier 144-148 F5.2 mag Kemag [8.69/18.16]? KELT eastern orientation instrumental magnitude 150-154 F5.2 mag Kwmag [8.29/16.14]? KELT western orientation instrumental magnitude 156-163 F8.4 deg GLON Galactic longitude 165-172 F8.4 deg GLAT Galactic latitude 174-179 F6.3 mag Jmag [4.303/11.927] 2MASS J band magnitude (2) 181-186 F6.3 mag Hmag [3.546/11.822] 2MASS H band magnitude (2) 188-193 F6.3 mag Ksmag [3.326/11.686]? 2MASS Ks band magnitude (2) 195-200 F6.3 mag W1mag [3.138/11.525]? WISE 3.4µm band magnitude (3) 202-207 F6.3 mag W2mag [1.585/11.32]? WISE 4.6µm band magnitude (3) 209-214 F6.3 mag W3mag [-0.653/11.207]? WISE 12µm band magnitude (3) 216-221 F6.3 mag W4mag [-2.078/9.408]? WISE 22µm band magnitude (3) 223-227 F5.2 mag NUVmag [10.55/19.1]? GALEX NUV band magnitude (4) 229-233 F5.2 mag FUVmag [11.80/17.81]? GALEX FUV band magnitude (4) 235-245 F11.7 d Per1 [0.14205/205.99]? First period 247-256 F10.6 d Per2 [0.20635/192.70125]? Second period 257-266 F10.6 d Per3 [6.57901/127.10082]? Third period 268-282 A15 --- VType Variable type(s) (5)
Note (1): Celestial coordinates, identifiers, spectral types, and V-band magnitudes are gathered from the BeSS database (http://basebe.obspm.fr). Note (2): Skrutskie et al. (2006, Cat. VII/233). Note (3): Wright et al. (2010AJ....140.1868W). Note (4): Martin et al. (2005ApJ...619L...1M). Note (5): Variable types followed by "?" indicate some uncertainty in the ascribed characteristic. Variable type as follows: ObV = Outburst Variation - outbursts are present in the raw light curve; SRO = Semi-Regular Outbursts - outbursts occur with some regularity; LTV = Long Term Variation - long term variability in the raw light curve; NRP = Non-Radial Pulsator candidate - shows periodic variability at timescales of less than 2 days; IP = Intermediate Periodicity - shows periodic variability at timescales greater than 2 days; EB = Eclipsing Binary; DW(S/I) = Double Wave - indicates double-waved modulation at (S)hort or (I)ntermediate periods; SAT = Saturated - saturation issues in the KELT photometry make analysis of this star intractable at the present time.
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 30-Apr-2018
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

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