J/AJ/129/1596 BVI photometric variability survey of M3 (Hartman+, 2005)
BVI photometric variability survey of M3.
Hartman J.D., Kaluzny J., Szentgyorgyi A., Stanek K.Z.
<Astron. J., 129, 1596-1606 (2005)>
=2005AJ....129.1596H 2005AJ....129.1596H
ADC_Keywords: Binaries, eclipsing ; Clusters, globular ; Stars, variable ;
Photometry
Keywords: binaries: eclipsing - δ Scuti -
globular clusters: individual (M3) - stars: variables: other - surveys
Abstract:
We have conducted a three-band (BVI) variability survey of the
globular cluster M3. This is the first three-band survey of the
cluster using modern image subtraction techniques. Observations were
made over nine nights in 1998 on the 1.2m telescope at the F. L.
Whipple Observatory in Arizona. We present photometry for 180 variable
stars in the M3 field, 12 of which are newly discovered. New
discoveries include six SX Phoenicis-type variables that all lie in the
blue straggler region of the color-magnitude diagram, two new
first-overtone RR Lyrae variables, a candidate multimode RR Lyrae
variable, a detached eclipsing binary, and two unclassified variables.
We also provide revised periods for 52 of the 168 previously known
variables that we observe.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table23.dat 139 180 Catalog of M3 variables
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See also:
J/AJ/129/267 : RR Lyrae variables in NGC 5272 (Cacciari+, 2005)
V/97 : Updated 3rd Cat Variable Stars in Globular Clusters (Clement+ 1997)
Byte-by-byte Description of file: table23.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Variable identification number (1)
5 I1 --- 2MASS [0/1] The 2MASS flag (2)
7- 8 I2 h RAh Hour of Right Ascension (J2000) (3)
10- 11 I2 min RAm Minute of Right Ascension (J2000) (3)
13- 17 F5.2 s RAs Second of Right Ascension (J2000) (3)
19 A1 --- DE- Sign of the Declination (J2000) (3)
20- 21 I2 deg DEd Degree of Declination (J2000) (3)
23- 24 I2 arcmin DEm Arcminute of Declination (J2000) (3)
26- 29 F4.1 arcsec DEs Arcsecond of Declination (J2000) (3)
31 I1 --- f_Vmag Flag on Vmag (4)
33 I1 --- f_Bmag Flag on Bmag (4)
35 I1 --- f_Imag Flag on Imag (4)
37- 42 F6.3 mag Vamp ? Observed V band full-amplitude (5)
44- 49 F6.3 mag Vmag ? Flux averaged mean V band magnitude (6)
51- 56 F6.3 mag Bamp ? Observed B band full-amplitude (5)
58- 63 F6.3 mag Bmag ? Flux averaged mean B band magnitude (6)
65- 70 F6.3 mag Iamp ? Observed I band full-amplitude (5)
72- 77 F6.3 mag Imag ? Flux averaged mean I band magnitude (6)
79- 86 F8.6 d Per ? Observed best period of variability (7)
88- 95 F8.6 d PerPub ? Published period (8)
97 A1 --- f_PerPub [01] Flag on PerPub (9)
99-112 F14.6 d T0 ? First minimum Julian Date (10)
114-121 F8.6 --- Bphase ? Phase of minimum B (11)
123-130 F8.6 --- Iphase ? Phase of minimum I (11)
132-135 A4 --- Class Classification of variability (12)
137-139 A3 --- Rem Additional remarks (13)
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Note (1): V1-V285 is taken from Clement et al. (2001AJ....122.2587C 2001AJ....122.2587C).
New identifications are denoted by "NV."
The ID number roughly corresponds to discovery order.
Note (2): The 2MASS flag, defined as follows:
0 = no variable matches to 2MASS sources.
1 = variable matches a 2MASS source.
Note (3): This value is taken from the 2MASS catalog for sources with a 2MASS
match, otherwise it is obtained from the rectangular to equatorial
transformation derived using the Bakos et al. (2000AcA....50..221B 2000AcA....50..221B)
catalog.
Note (4): Flag on Vmag, Bmag, Imag, defined as follows:
0 = no B- or I-band detection.
1 = observation could be converted to magnitudes.
2 = observation was left in differential count units.
Note (5): Defined to be the faintest observed magnitude minus the brightest
observed magnitude on the cleaned light curve.
Note (6): For the eclipsing binary this is the out of eclipse magnitude
determined with EBOP (see Section 4).
Note (7): Derived using the ANOVA statistic of Schwarzenberg-Czerny
(1996ApJ...460L.107S 1996ApJ...460L.107S). In cases where aliasing allowed for a number of
acceptable periods, we chose the period corresponding to the peak in
the periodogram nearest to the published period, where available.
Note (8): Taken from Clementini et al. (2004AJ....127..938C 2004AJ....127..938C), Corwin & Carney
(2001AJ....122.3183C 2001AJ....122.3183C) or Clement et al. (2001AJ....122.2587C 2001AJ....122.2587C) in that
order of priority.
Note (9): Integer denoting whether or not the observed best period should be
taken as a revision of the published period. This determination is
based on a visual comparison between the light curve phased with the
published period and the light curve phased with the observed best
period. Values are 0=no revision, 1=revision.
Note (10): Of the first minimum in V-band to occur after the first observation.
This field is null for unclassified variables.
Note (11): Where 0 phase is set to the minimum in V-band.
Note (12): Classification of variability, defined as follows:
RR0 = fundamental mode RR Lyr (RRab).
RR1 = first overtone RR Lyr (RRc).
RR01 = candidate multi-mode RR Lyr (RRd). Note that the possible presence
of multiple periods was determined by eye and was not the result of
a systematic search.
SXP = SX Phe type variable.
N/A = Unclassified variable.
EB = Eclipsing binary.
Note (13): Here we denote the possible presence of multiple modes (mp) for SXP
variables as well as the presence of the Blazhko effect (Bl) within
the observations.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 31-Jan-2006