J/AJ/150/107 Variable stars from TNTS. I. 2012-2014 (Yao+, 2015)
Photometry of variable stars from the THU-NAOC transient survey.
I. The first two years.
Yao X., Wang L., Wang X., Zhang T., Chen J., Yuan W., Mo J., Li W., Jin Z.,
Wu X., Nie J., Zhou X.
<Astron. J., 150, 107 (2015)>
=2015AJ....150..107Y 2015AJ....150..107Y (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Binaries, eclipsing
Keywords: binaries: eclipsing - stars: evolution - stars: variables: general -
stars: variables: RR Lyrae
Abstract:
In this paper, we report the detections of stellar variabilities from
the first two years of observations of a sky area of about 1300 square
degrees from the Tsinghua University-NAOC Transient Survey. A total of
1237 variable stars (including 299 new ones) were detected with a
brightness <18.0mag and a magnitude variation ≳0.1mag on a timescale
from a few hours to a few hundred days. Among such detections, we
tentatively identified 661 RR Lyrae stars, 431 binaries, 72
semi-regular pulsators, 29 Mira stars, 11 slow irregular variables, 11
RS Canum Venaticorum stars, 7 Gamma Doradus stars, 5 long-period
variables, 3 W Virginis stars, 3 Delta Scuti stars, 2 Anomalous
Cepheids, 1 Cepheid, and 1 nova-like star based on their time-series
variability index Js and their phased diagrams. Moreover, we found
that 14 RR Lyrae stars show the Blazhko effect and 67 contact
eclipsing binaries exhibit the O'Connell effect. Since the period and
amplitude of light variations of RR Lyrae variables depend on their
chemical compositions, their photometric observations can be used to
investigate the distribution of metallicity along the direction
perpendicular to the Galactic disk. We find that the metallicity of RR
Lyrae stars shows large scatter at regions closer to the Galactic
plane (e.g., -3.0<[Fe/H]<0) but tends to converge at [Fe/H]~-1.7 at
larger Galactic latitudes. This variation may be related to the fact
that the RRAB Lyrae stars in the Galactic halo come from globular
clusters with different metallicities and vertical distances, i.e.,
OoI and OoII populations, favoring the dual-halo model.
Description:
We report the detections of stellar variabilities from the first two
years of observations of a sky area of about 1300 square degrees from
the Tsinghua University-NAOC Transient Survey (TNTS).
The TNTS is conducted with a 0.6m Schmidt telescope equipped with a
4k*4k CCD. The CCD has a pixel scale of 1.3arcsec/pixel and a field of
view (FOV) of 1.5°*1.5°. It was designed to operate for four
years starting from 2012 October. About 85000 images were accumulated
from our survey performed during the period from 2012 October to 2014
August, and these images cover about 1800 square degrees of the
northern sky.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 107 1237 Variable stars
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See also:
B/vsx : AAVSO International Variable Star Index VSX (Watson+, 2006-2014)
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)
J/MNRAS/446/2251 : Southern Catalina Survey type-ab RR Lyrae (Torrealba+, 2015)
J/ApJS/213/9 : Catalina Surveys periodic variable stars (Drake+, 2014)
J/AJ/146/101 : LINEAR. III. Catalog of periodic variables (Palaversa+, 2013)
J/AJ/132/1202 : RR Lyrae in Northern Sky Variability Survey (Kinemuchi+, 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Field Survey field identifier
6- 10 I5 --- Star Identifier within the field
12- 13 I2 h RAh Hour of Right Ascension (J2000) (1)
15- 16 I2 min RAm Minute of Right Ascension (J2000) (1)
18- 22 F5.2 s RAs Second of Right Ascension (J2000) (1)
24- 26 I3 deg DEd Degree of Declination (J2000) (1)
28- 29 I2 arcmin DEm Arcminute of Declination (J2000) (1)
31- 35 F5.2 arcsec DEs Arcsecond of Declination (J2000) (1)
37- 42 F6.2 mag [9.3/141.2] Mean unfiltered magnitude (2)
44- 47 F4.2 mag Av [0.01/1.2] Line-of-sight extinction (3)
49- 52 F4.2 mag Amp [0/3.8] Amplitude of variation (4)
54- 58 F5.2 --- Js [0.31/30] Welch-Stetson variability index Js
(Stetson, 1996PASP..108..851S 1996PASP..108..851S)
60- 71 F12.8 d Per1 [0.1/730]? Period from our measurement (Tsinghua
University-NAOC Transient Survey; TNTS)
73- 75 A3 --- Meth Period calculate method (LS, PDM, or VSX) (5)
77- 86 F10.6 d Per2 [0.2/730]? Period from International Variable
Star Index (VSX; cat. B/vsx)
88- 94 F7.3 --- T0 [121/882]? Epoch when primary eclipse or minimum
light occurs
96-102 A7 --- Type Tentative classification about the variable star
whenever possible (6)
104 A1 --- VSX [V] Indicates a VSX variable (7)
105 A1 --- CSS [C] Indicates a CSS variable (7)
106 A1 --- New [N] Indicates a new variable
107 A1 --- LIN [L] Indicates a LINEAR variable (7)
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Note (1): Based on reference images from Tsinghua University-NAOC Transient
Survey (TNTS).
Note (2): Calibrated with the R-band magnitudes of the Position and Proper
Motions eXtended (PPMX; cat. I/312) catalog.
Note (3): Based on Schlafly & Finkbeiner (2011ApJ...737..103S 2011ApJ...737..103S).
Note (4): Magnitude from maximum to minimum.
Note (5): The methods are defined as below:
LS = Lomb-Scargle method;
PDM = Phase Dispersion Minimization method;
VSX = From International Variable Star Index (VSX; cat. B/vsx) catalogs.
Note (6): Including previous identification of variables from VSX (cat. B/vsx)
database and GCVS (cat. B/gcvs), defined as follows:
ACEP = Anomalous Cepheids;
RS = RS Canum Venaticorum;
EC = Contact binary;
ES = Semi-detached binary;
ED = Detached binary;
CWA = W Virginis;
RR = RR Lyrae variable;
BL = "Blazhko effect";
CEP = Cepheids;
GDOR = Gamma Doradus star;
DSCT = Delta Scuti star;
SR = Semiregular pulsator;
M = Mira variable;
LPV = Long Period Variable;
L = Slow irregular variable.
Note (7): Information flag defined as below:
V = Variable in International Variable Star Index (VSX; cat. B/vsx) of the
Association of Variable Star Observers (AAVSO);
C = Variable in Catalina Sky Survey (CSS) sample (Drake et al. 2014,
cat. J/ApJS/213/9);
L = Variable in Lincoln Near-Earth Asteroid Research (LINEAR) survey sample
(Palaversa et al. 2013, cat. J/AJ/146/101);
N = New variable.
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 23-Oct-2015