J/AJ/146/139 2010 photometry of variable stars from Dome A (Wang+, 2013)
Photometry of variable stars from Dome A, Antarctica: results from the 2010
observing season.
Wang L., Macri L.M., Wang L., Ashley M.C.B., Cui X., Feng L.-L., Gong X.,
Lawrence J.S., Liu Q., Luong-Van D., Pennypacker C.R., Shang Z.,
Storey J.W.V., Yang H., Yang J., Yuan X., York D.G., Zhou X., Zhu Z., Zhu Z.
<Astron. J., 146, 139 (2013)>
=2013AJ....146..139W 2013AJ....146..139W
ADC_Keywords: Stars, variable ; Photometry, SDSS
Keywords: site testing - stars: variables: general
Abstract:
We present results from a season of observations with the Chinese
Small Telescope ARray, obtained over 183 days of the 2010 Antarctic
winter. We carried out high-cadence time-series aperture photometry of
9125 stars with i≲15.3mag located in a 23deg2 region centered on
the south celestial pole. We identified 188 variable stars, including
67 new objects relative to our 2008 observations, thanks to broader
synoptic coverage, a deeper magnitude limit, and a larger field of
view. We used the photometric data set to derive site statistics from
Dome A. Based on two years of observations, we find that extinction
due to clouds at this site is less than 0.1 and 0.4mag during 45% and
75% of the dark time, respectively.
Description:
The region surrounding Dome A (elevation: 4093m above mean sea level)
in the Antarctic plateau is likely the best astronomical site on
Earth. We developed an observatory capable of year-round operations
called PLATO, and a quad-telescope called CSTAR (the Chinese Small
Telescope ARray). The observatory is part of the Chinese Kunlun
station, located at Dome A. Observations were carried out using CSTAR
(unit#3), which we described in detail in Wang et al. (2011, cat.
J/AJ/142/155). Briefly, it is a Schmidt-Cassegrain wide-field
telescope with a pupil entrance aperture of 145mm, a Sloan i-band
filter, and a 1K*1K frame-transfer CCD with a plate scale of
15.7"/pixel, giving a field of view 4.5° on a side. Scientifically
useful images were acquired from 2010 March 29 to 2010 September 27
(Antarctic winter season).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 97 188 Variable stars observed with CSTAR in 2010
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)
I/305 : The Guide Star Catalog, Version 2.3.2 (GSC2.3) (STScI, 2006)
J/AJ/142/155 : Variable stars photometry from Dome A (Wang+, 2011)
J/PASP/122/347 : Chinese Small Telescope ARray (CSTAR) (Zhou+, 2010)
J/AcA/50/177 : All Sky Automated Survey Catalog (Pojmanski+, 2000)
http://casdc.china-vo.org/data/cstar : Chinese Virtual Observatory
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name CSTAR identification from 2010 observations (1)
9- 14 I6 --- Name2 ? CSTAR identification (2008 observations) (2)
16- 25 A10 --- GSC2.3 Identification from Guide Star Catalog (3)
27- 28 I2 h RAh Hour of Right Ascension from GSC2.3 (J2000)
30- 31 I2 min RAm Minute of Right Ascension from GSC2.3 (J2000)
33- 37 F5.2 s RAs Second of Right Ascension from GSC2.3 (J2000)
39 A1 --- DE- Sign of the Declination from GSC2.3 (J2000)
40- 41 I2 deg DEd Degree of Declination from GSC2.3 (J2000)
43- 44 I2 arcmin DEm Arcminute of Declination from GSC2.3 (J2000)
46- 49 F4.1 arcsec DEs Arcsecond of Declination from GSC2.3 (J2000)
51- 55 F5.2 mag Mean i band magnitude
57- 61 F5.2 mag dimag The 90% magnitude range of i band light curve
63- 67 F5.2 --- J Welch-Stetson variability index J (4)
69- 77 F9.6 d Per ? Main period if applicable
79- 81 A3 --- r_Per Method of period determination (LS or BLS) (5)
83- 90 F8.4 d T0 ? Epoch of primary eclipse or minimum light
(JD-2454500), when applicable
92- 93 A2 --- Type Tentative classification of variable type (6)
95- 97 A3 --- Ref Additional reference (7)
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Note (1): A letter "n" is added at the beginning to avoid confusion with 2008
CSTAR (Chinese Small Telescope ARray) identifiers from our previous work.
Note (2): From Wang et al. (2011, cat. J/AJ/142/155), if applicable.
Note (3): From Version 2.3.2 (GSC2.3, cat. I/305) except for #n116380 (based on
CSTAR master frame).
Note (4): See Section 2 of Stetson (1996PASP..108..851S 1996PASP..108..851S);
Note (5): Technique of period determination as follows:
LS = Lomb-Scargle method (Lomb, 1976Ap&SS..39..447L 1976Ap&SS..39..447L;
Scargle, 1982ApJ...263..835S 1982ApJ...263..835S);
BLS = box fitting algorithm (Kovacs et al., 2002A&A...391..369K 2002A&A...391..369K).
Note (6): Variable type as follows:
DS = δ Scuti (DSCT);
EC = Eclipsing Contact binary (EW);
ED = Eclipsing Detached binary (EA);
ES = Eclipsing Semi-detached binary (EB);
LT = Long-Term variation (LPV);
PR = unclassified PeRiodic;
RL = RR Lyrae;
GD = γ Doradus;
MP = Multi-Periodic;
IR = IRregular;
TR = TRansit-like eclipse.
Note (7): Reference as follows:
A = Previous identification of the variable by the All Sky Automated Survey
(Pojmanski et al., 2000, cat. J/AcA/50/177);
G = Inclusion in the General Catalog of Variable Stars (B/gcvs).
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 22-Jul-2014