J/AJ/146/136 BEST-II catalog of variables. I. Southern fields (Fruth+, 2013)
The Berlin Exoplanet Search Telescope II catalog of variable stars.
I. Characterization of three southern target fields.
Fruth T., Cabrera J., Chini R., Csizmadia SZ., Dreyer C., Eigmuller P.,
Erikson A., Kabath P., Kirste S., Lemke R., Murphy M., Pasternacki T.,
Rauer H., Titz-Weider R.
<Astron. J., 146, 136 (2013)>
=2013AJ....146..136F 2013AJ....146..136F
ADC_Keywords: Binaries, eclipsing ; Photometry
Keywords: binaries: eclipsing - stars: variables: general -
techniques: photometric
Abstract:
A photometric survey of three southern target fields with BEST II
yielded the detection of 2406 previously unknown variable stars and an
additional 617 stars with suspected variability. This study presents a
catalog including their coordinates, magnitudes, light curves,
ephemerides, amplitudes, and type of variability. In addition, the
variability of 17 known objects is confirmed, thus validating the
results. The catalog contains a number of known and new variables that
are of interest for further astrophysical investigations, in order to,
e.g., search for additional bodies in eclipsing binary systems, or to
test stellar interior models. Altogether, 209070 stars were monitored
with BEST II during a total of 128 nights in 2009/2010. The overall
variability fraction of 1.2%-1.5% in these target fields is well
comparable to similar ground-based photometric surveys. Within the
main magnitude range of R∈[11, 17], we identify 0.67(3)% of all
stars to be eclipsing binaries, which indicates a completeness of
about one third for this particular type in comparison to space
surveys.
Description:
BEST II (Berlin Exoplanet Search Telescope II) is located at the
Observatorio Cerro Armazones, Chile. Since 2007, it has been operated
continuously by the Institute of Planetary Research of the German
Aerospace Center (DLR) in robotic mode from Berlin. The system
consists of a 25cm Baker-Ritchey-Chretien telescope. The photometric
data presented here were obtained with a 4k*4k Finger Lakes
Instrumentation CCD (IMG-16801E1) in white light, i.e., without any
photometric filter. The CCD is most sensitive at λ∼650nm, and
the photometric system is roughly comparable to the Johnson R-band.
Three target fields, named F17, F18, and F19, were monitored
intensively with BEST II in 2009 Apr 20-2009 Jul 22, 2009 Aug 19-2009
Oct 27, and 2010 Mar 24-2010 Sep 21 respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 122 17 Known variable stars in data sets F17-F19
table5.dat 137 3083 Catalog of variable stars in three southern
BEST-II target fields
--------------------------------------------------------------------------------
See also:
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)
I/322 : UCAC4 Catalogue (Zacharias+, 2012)
II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/AJ/143/140 : BEST-II periodic variables in CoRoT LRa02. II. (Fruth+, 2012)
J/AcA/62/67 : ASAS photometry of ROSAT sources (Kiraga, 2012)
J/AJ/137/3911 : BEST periodic variable stars in LRc2 field (Kabath+, 2009)
J/A+A/506/569 : BEST-II periodic variables in CoRoT LRa02 field (Kabath+, 2009)
J/AJ/136/654 : BEST periodic variable stars in LRa1 field (Kabath+, 2008)
J/AJ/134/766 : BEST variable stars in LRc1 field (Karoff+, 2007)
J/AJ/134/1560 : BEST periodic variable stars in IR01 field (Kabath+, 2007)
J/A+A/446/785 : Catalogue of eclipsing variables (Malkov+, 2006)
J/AcA/50/177 : All Sky Automated Survey Catalog (Pojmanski+, 2000)
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- BESTII BEST II identifier (FNN_FNNNNN or FNN_NNNNNN)
12 A1 --- f_OName Revised cross_identification (a) (1)
14- 32 A19 --- OName Name in reference
34- 37 F4.1 mag Rmag BESTII instrumental magnitude
39- 45 F7.5 d Per1 ? BEST II variability period
47- 53 F7.5 d e_Per1 ? Uncertainty in Per1
54- 62 F9.5 d Per2 ? Period from reference
63- 68 F6.4 d e_Per2 ? Uncertainty in Per2
70- 72 A3 --- Type1 BEST II variable type (G1)
74 A1 --- u_Type2 [:?] Uncertainty flag on Type2 (: or ?)
75- 79 A5 --- Type2 Variable type from reference
81-122 A42 --- Ref Reference
--------------------------------------------------------------------------------
Note (1): Meinunger (1970MitVS...5..156M 1970MitVS...5..156M) assigns the variability of NU Nor to
the star 2MASS 16274939-5533450 (BEST II F19_045485). However, in BEST II
data, the variability can clearly be assigned to the
object 2MASS 16275033-5533400 (BEST II F19_045321), which is located at an
angular distance of 9" to the former.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Field Field identifier (F17, F18, F19)
5- 14 A10 --- BESTII BEST-II identifier (FNN_FNNNNN or FNN_NNNNNN)
16- 18 A3 --- f_BESTII Variability flag (c=contaminated, s=suspected,
k=known) (1)
20- 35 A16 --- 2MASS 2MASS identifier (HHMMSSss+DDMMSSs; J2000) (2)
37- 38 I2 h RAh Hour of Right Ascension (J2000) (3)
40- 41 I2 min RAm Minute of Right Ascension (J2000) (3)
43- 46 F4.1 s RAs Second of Right Ascension (J2000) (3)
48 A1 --- DE- Sign of the Declination (J2000)(3)
49- 50 I2 deg DEd Degree of Declination (J2000) (3)
52- 53 I2 arcmin DEm Arcminute of Declination (J2000) (3)
55- 58 F4.1 arcsec DEs Arcsecond of Declination (J2000) (3)
60- 64 F5.2 mag Rmag BESTII instrumental magnitude (4)
66- 72 F7.3 d T0 ? Time of minimum brightness; HJD-2455000
74- 83 F10.6 d Per ? Variability period
85- 93 F9.6 d e_Per ? Uncertainty in Per
95-100 F6.4 mag Amp ? Amplitude
102-106 F5.3 mag e_Amp ? Uncertainty in Amp
108-109 I2 % y [0/99]? Contamination parameter γ (5)
111-117 A7 --- Type Variable type (G1)
119-137 A19 --- OName Other name
--------------------------------------------------------------------------------
Note (1): Flag meaning:
c = Contaminated light curve, i.e., variability of the same type and period
has also been measured for a nearby target;
s = Suspected variable;
k = Previously known variable (see also Section 5.2 and Table 4).
Note (2): Stars have been matched with the closest 2MASS object within
a radius of 2 arcseconds.
Note (3): Coordinates are derived by an astrometric match of CCD to UCAC3
(Zacharias et al., 2009, cat. I/315; obsoleted by UCAC4, Zacharias et al.,
2012, cat. I/322) coordinates.
Note (4): Given magnitudes are instrumental and reflect the CCD sensitivity,
as observations have been obtained without filter.
Note (5): Parameter approximates the fraction of light in the target's
aperture coming from other objects than the target itself (see Section 4).
--------------------------------------------------------------------------------
Global notes:
Note (G1): The classes are identified as follows:
EA = Algol-type Eclipsing binary (prototype β Per). For eclipsing binary
systems with light curves showing clear eclipses and almost no variation
in between (detached binary)
EB = Eclipsing Binary systems (prototype β Lyr) with ellipsoidal
components, phase variations are significant and hinder an exact
determination of the beginning/end of eclipses (semi-detached binary);
EW = Eclipsing binary systems at orbital periods below one day, both objects
are in contact, eclipses are of equal depth and are fully blended with
the phase variation (prototype W UMa; contact binary);
ROT = ROTating variable star. Stellar rotation can introduce flux variations,
e.g. due to stellar spots, magnetic fields, or ellipsoidal components.
Since BEST II photometry alone is usually not sufficient to distinguish
these cases, they are grouped under a general "ROT" classification;
VAR = Inconclusive case. Stars showing clear variability that cannot be
assigned a type according to the classification scheme from photometry;
further observations are needed to better constrain the physical origin
of variability;
LP = Long Periodic variable. Non-periodic variables or stars variable on time
scales comparable to/larger than the observational coverage;
DSCT = δ SCuTi variable (pulsating variable star with period p≤0.2d);
RR = RR Lyrae (pulsating variable star with period P=0.2-1d, characteristic
shape);
CEP = CEPheid (pulsating variable star with period p>1d, amplitude 0.01-2mag);
GDOR = γ DORadus star (pulsating variable star);
SR = Semi-Regular variable (pulsating variable star, p≥20d, with
irregularities).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Klagyivik et al. Paper II. 2016AJ....151..110K 2016AJ....151..110K, Cat. J/AJ/151/110
Dreyer et al. Paper III. 2018AJ....156..204D 2018AJ....156..204D
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 21-Jul-2014