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J/AJ/153/104   Variables observed in the Galactic disk by AST3-1   (Wang+, 2017)

Variable stars observed in the Galactic disk by AST3-1 from Dome A, Antarctica. Wang L., Ma B., Li G., Hu Y., Fu J., Wang L., Ashley M.C.B., Cui X., Du F., Gong X., Li X., Li Z., Liu Q., Pennypacker C.R., Shang Z., Yuan X., York D.G., Zhou J. <Astron. J., 153, 104-104 (2017)> =2017AJ....153..104W (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Binaries, eclipsing ; Photometry, SDSS Keywords: binaries: eclipsing - catalogs - methods: data analysis - stars: variables: general - surveys - techniques: photometric Abstract: AST3-1 is the second-generation wide-field optical photometric telescope dedicated to time-domain astronomy at Dome A, Antarctica. Here, we present the results of an i-band images survey from AST3-1 toward one Galactic disk field. Based on time-series photometry of 92583 stars, 560 variable stars were detected with i magnitude ≤16.5mag during eight days of observations; 339 of these are previously unknown variables. We tentatively classify the 560 variables as 285 eclipsing binaries (EW, EB, and EA), 27 pulsating variable stars (δ Scuti, γ Doradus, δ Cephei variable, and RR Lyrae stars), and 248 other types of variables (unclassified periodic, multiperiodic, and aperiodic variable stars). Of the eclipsing binaries, 34 show O'Connell effects. One of the aperiodic variables shows a plateau light curve and another variable shows a secondary maximum after peak brightness. We also detected a complex binary system with an RS CVn-like light-curve morphology; this object is being followed-up spectroscopically using the Gemini South telescope. Description: Antarctic Survey Telescopes (AST3) was conceived as three telescopes, each equipped with one of three SDSS g, r, and i filters. Each telescope has an entrance pupil aperture of 0.5m and a wide FOV of 4.3deg2, and is equipped with a 10K*10K frame transfer STA1600FT CCD (charge coupled device) camera. Of the total of 3523 images obtained of our field, 65% had exposure times of 30s, and the remainder were 60s. The field is not crowded as the median distance between every star and its nearest neighbor from our reference frame is 11.14 pixels (note that the AST3-1 pixel scale is 1.0arcseconds/pixel). The stellar brightness profiles had a median Full Width at Half Maximum (FWHM) of 3.73pixels. During the eight days of observations, 3523 images were collected in total for our field and 96734 bright stars with S/N>30 were found on our reference image, which had the largest number of detections. We then rejected stars that were detected in fewer than 20% of the images. We ignored these objects, but they might be interesting. This left a final sample of 92583 stars. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 108 560 Variable stars table4.dat 76 221 Identifications for the 221 variables in common curves/* 31 560 *i band light curve
Note on curves/*: This supplementary material contains i-band light curves from the first AST3 (Antarctic Survey Telescopes) (AST3-1) for the 560 variable stars as tabulated in the Table2.
See also: B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013) B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014) II/336 : AAVSO Photometric All Sky Survey (APASS) DR9 (Henden+, 2016) I/312 : PPMX Catalog of positions and proper motions (Roeser+ 2008) II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005) J/AN/336/590 : Bochum Galactic Disk Survey: II (Hackstein+, 2015) J/AcA/63/115 : OGLE-III Galactic disk eclipsing binaries (Pietrukowicz+, 2013) J/AJ/146/139 : 2010 photometry of variable stars from Dome A (Wang+, 2013) J/AJ/142/155 : Variable stars photometry from Dome A (Wang+, 2011) J/A+A/503/651 : Variables in a VLT/VIMOS field in Carina (Pietrukowicz+ 2009) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 A8 --- AST3 Identification from the first of the Antarctic Survey Telescopes (AST3-1) in 2012 10- 11 I2 h RAh Hour of Right Ascension (J2000) (1) 13- 14 I2 min RAm Minute of Right Ascension (J2000) (1) 16- 20 F5.2 s RAs Second of Right Ascension (J2000) (1) 22 A1 --- DE- Sign of the Declination (J2000) (1) 23- 24 I2 deg DEd Degree of Declination (J2000) (1) 26- 27 I2 arcmin DEm Arcminute of Declination (J2000) (1) 29- 32 F4.1 arcsec DEs Arcsecond of Declination (J2000) (1) 34- 38 F5.2 mag <imag> [10.8/16.3] Mean AST3-1 SDSS i band magnitude (not an intensity mean) 40- 44 F5.2 --- L [0.65/16.22] Variability index L 46- 56 F11.9 d Per [0.074/7.83]? Median value of the period, when applicable 58- 68 F11.9 d e_Per ? Standard deviation of the main period in Markov Chain Monte Carlo (MCMC) simulation 70- 74 F5.2 --- chi2 [0.03/10.7]? Minimum χ2 per degree of freedom in Markov chain Monte Carlo (MCMC) simulation (2) 76- 79 F4.2 mag Amp [0.04/1.33] Peak-to-peak amplitude 81- 92 F12.6 d T0 [15427.8/15461.9]? Epoch of minimum light (T0) (3) 94- 98 A5 --- Cl1 Tentative classification of variable type (4) 100-102 A3 --- Cl2 Alternative tentative classification of variable type (4) 104-108 A5 --- Note Variability note (either A=AAVSO, O=OGLE-III, or G=GDS) (5)
Note (1): Matched to the Position and Proper Motions eXtended (PPMX; Roser et al. 2008, Cat. I/312) system. Note (2): Markov chain Monte Carlo (MCMC; Brooks 1998, Journal of the Royal Statistical Society. Series D (The Statistician) 47 69). Note (3): Epoch of minimum light since 1970-01-01 00:00:00 UTC, if possible. Note (4): The variable types are defined as follows: VAR = Objects with statistically significant variabilities, but not showing periodic behaviors; EW = W Urase Majoris-type binary; EB = β Lyrae-type binary; EA = Algol-type binary; EW-OC = EW binary with O'Connell effect; EB-OC = EB binary with O'Connell effect; DCEP = δ Cephei variable; DS = δ Scuti variable; GD = γ Doradus variable; PER = Unclassified periodic; MP = Multi-periodic; RRAB = RRab Lyrae variable; RRC = RRc Lyrae variable. Note (5): The notes are defined as follows: A = American Association of Variable Star Observer (AAVSO; https://www.aavso.org/) variable; O = Optical Gravitational Lensing Experiment (OGLE-III; see Pietrukowicz et al. 2013, Cat. J/AcA/63/115) variable; G = Bochum Survey of the Southern Galactic Disk (Hackstein et al. 2015, Cat. J/AN/336/590) variable.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 8 A8 --- AST3 Identification from the first of the Antarctic Survey Telescopes (AST3-1) in 2012 11- 16 I6 --- AAVSO ? Identification (OID) from AAVSO International Variable Star Index VSX (Watson et al. 2006, Cat. B/vsx) 20- 38 A19 --- GDS Identification (Variable ID) from Galactic Disk Survey (GDS; Hackstein et al. 2015, Cat. J/AN/336/590) 40- 51 A12 --- --- [OGLE-GD-ECL-] 52- 56 I5 --- OGLE-III ? Identification from OGLE-III (1) 58- 76 A19 --- OName Other source name (2)
Note (1): Eclipsing binary stars in the Optical Gravitational Lensing Experiment (OGLE-III) Galactic disk fields (Pietrukowicz et al. 2013, Cat. J/AcA/63/115). Note (2): Other identifiers: [PMF2009] = Pietrukowicz et al. 2009 (Cat. J/A+A/503/651); ASAS = All Sky Automated Survey variable stars (see Pojmanski et al. 2002-2005, Cat. II/264).
Byte-by-byte Description of file: curves/*
Bytes Format Units Label Explanations
1- 14 F14.8 d Time Days since 1970-01-01 00:00:00 UTC 16- 22 F7.4 mag imag AST3-1 SDSS i band magnitude 24- 31 F8.6 mag e_imag Uncertainty in imag
History: From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 04-Jul-2017
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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