J/AJ/160/220 NIR light curve of 234 RR Lyrae in Messier 3 (Bhardwaj+, 2020)
Near-infrared census of RR Lyrae variables in the Messier 3 globular cluster and
the period-luminosity relations.
Bhardwaj A., Rejkuba M., de Grijs R., Herczeg G.J., Singh H.P., Kanbur S.,
Ngeow C.-C.
<Astron. J., 160, 220 (2020)>
=2020AJ....160..220B 2020AJ....160..220B
ADC_Keywords: Clusters, globular; Stars, variable; Photometry, infrared
Keywords: RR Lyrae variable stars; Stellar pulsations; Globular star clusters;
Distance indicators; Distance measure
Abstract:
We present new near-infrared (NIR), JHKs, time-series observations of
RR-Lyrae variables in the Messier-3 (NGC5272) globular cluster using
the WIRCam instrument at the 3.6m Canada-France-Hawaii Telescope. Our
observations cover a sky area of ∼21'x21' around the cluster center
and provide an average of 20 epochs of homogeneous JHKs-band
photometry. New homogeneous photometry is used to estimate robust mean
magnitudes for 175 fundamental-mode (RRab), 47 overtone-mode (RRc),
and 11 mixed-mode (RRd) variables. Our sample of 233 RR-Lyrae
variables is the largest thus far obtained in a single cluster with
time-resolved, multiband NIR photometry. NIR-to-optical amplitude
ratios for RR-Lyrae in Messier-3 exhibit a systematic increase moving
from RRc to short-period (P<0.6day) and long-period (P≳0.6day) RRab
variables. We derive JHKs-band period-luminosity relations for RRab,
RRc, and the combined sample of variables. Absolute calibrations based
on the theoretically predicted period-luminosity-metallicity relations
for RR Lyrae stars yield a distance modulus,
µ=15.041±0.017(statistical)±0.036(systematic)mag, to
Messier-3. When anchored to trigonometric parallaxes for nearby
RR-Lyrae stars from the Hubble Space Telescope and the Gaia mission,
our distance estimates are consistent with those resulting from the
theoretical calibrations, albeit with relatively larger systematic
uncertainties.
Description:
Our NIR observations were obtained using the WIRCam instrument mounted
on the 3.6m Canada-France-Hawaii Telescope (CFHT) on the summit of
Maunakea in Hawaii during four nights between 2019 May 26 and 29.
We requested JHKs time-series observations in queue mode centered on
the M3 cluster center, and obtained 22 epochs in J and 20 epochs in
the H and Ks bands. Each epoch consisted of on average 15 dithered
images obtained with an exposure time of 5s per image.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 34 13754 NIR time-series photometry of RRL in the M3 cluster
table4.dat 115 234 NIR pulsation properties of RRL in the M3 cluster
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See also:
V/150 : Updated catalog of variable stars globular clusters (Clement+ 2017)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/A+AS/121/95 : Giant stars abundances in 24 clusters (Carretta+ 1997)
J/AcA/50/221 : Astrometry of variable stars in M 3 (Bakos+, 2000)
J/AJ/129/267 : RR Lyrae variables in NGC 5272 (Cacciari+, 2005)
J/AJ/129/1596 : BVI photometric variability survey of M3 (Hartman+, 2005)
J/MNRAS/386/2115 : Type II Cepheid and RR Lyrae variables (Feast+, 2008)
J/AJ/142/187 : HST observations of 7 Pop.II variable stars (Benedict+,2011)
J/MNRAS/419/2173 : Long-term photometry of M3 RR Lyrae (Jursik+, 2012)
J/MNRAS/441/715 : Mid-infrared study of RR Lyrae stars (Gavrilchenko+, 2014)
J/PASP/126/521 : UBVRIJHK photometry of RR Lyrae in M4 (Stetson+, 2014)
J/MNRAS/447/3342 : Galactic & LMC Cepheids Fourier parameters (Bhardwaj+, 2015)
J/ApJS/219/25 : Light curves of RR Lyrae stars M3 (NGC5272) (Jurcsik+, 2015)
J/ApJ/807/127 : Properties of 70 RR Lyrae stars in LMC bar (Muraveva+, 2015)
J/AJ/150/129 : Swift UVOT stars survey.II. RR Lyrae M3 & M15 (Siegel+,2015)
J/AJ/151/88 : LMC NIR Synoptic Survey.II Wesenheit relat. (Bhardwaj+,2016)
J/MNRAS/458/4162 : Stromgren photometry of M3 (NGC5272) (Massari+, 2016)
J/AJ/153/154 : LMC NIR survey.IV. Type II Cepheid variab. (Bhardwaj+, 2017)
J/AJ/153/96 : Standard Galactic field RR LyraeI. Photometry (Monson+,2017)
J/ApJ/841/84 : Theoretical framework RR Lyrae II. MIR data (Neeley+, 2017)
J/AJ/155/137 : RRLs globulars. V.ωCentauri NIR photom. (Braga+, 2018)
J/A+A/616/A12 : Gaia DR2 sources in GC and dSph (Gaia Collaboration+, 2018)
J/A+A/625/A1 : RR Lyrae variables NIR light-curve templates (Braga+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- ID RR-Lyrae identifier (1)
7- 8 A2 --- Band Observational band used; H, J or Ks
10- 19 F10.4 d MJD [58629/58633] Modified Julian Date
21- 26 F6.3 mag mag [14.06/15.48] Apparent magnitude in Band
28- 32 F5.3 mag e_mag [0.004/0.13] Uncertainty in mag
34 A1 --- f_ID Quality flag (2)
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Note (1): Same as in the catalog of Clement+, 2001AJ....122.2587C 2001AJ....122.2587C.
Note (2): Flags as follows:
A = The extrema were well constrained so as to estimate accurate
amplitudes (8660 occurrences)
B = Remaining light curves (5094 occurrences)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- ID RR-Lyrea identifier (1)
7- 16 F10.6 deg RAdeg [205.38/205.71] Right Ascension (J2000) (1)
18- 26 F9.6 deg DEdeg [28.21/28.56] Declination (J2000) (1)
28- 34 F7.5 d Per [0.24/0.78] Pulsation period (1)
36- 39 A4 --- Type RRL type: ab, c or d (1)
41- 46 F6.3 mag Jmag [13.57/15.33] Mean J band magnitude
48- 53 F6.3 mag Hmag [13.02/15.13] Mean H band magnitude
55- 60 F6.3 mag Ksmag [12.88/15.17] Mean Ks band magnitude
62- 66 F5.3 mag e_Jmag [0.01/0.13] Uncertainty in Jmag
68- 72 F5.3 mag e_Hmag [0.01/0.08] Uncertainty in Hmag
74- 78 F5.3 mag e_Ksmag [0.01/0.13] Uncertainty in Ksmag
80- 86 F7.3 mag AJ [0.04/0.56]? J band amplitude
88- 94 F7.3 mag AH [0.04/0.42]? H band amplitude
96-102 F7.3 mag AKs [0.04/0.45]? Ks band amplitude
104-108 F5.3 arcsec Delta [0.002/1.19] Separation (2)
110-115 A6 --- f_ID Quality flag (3)
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Note (1): From Clement+, 2001AJ....122.2587C 2001AJ....122.2587C.
Note (2): Between coordinates of RRL from Clement+, 2001AJ....122.2587C 2001AJ....122.2587C
and our astrometric calibration.
Note (3): Flags as follows:
A = The extrema were well constrained so as to estimate accurate
amplitudes (140 occurrences)
B = Remaining light curves (83 occurrences)
C = Poor-quality light curves that exhibit large scatter or do not
show any distinct periodicity in one or more filters, due to
photometric contamination (11 occurrences)
Bl = Blazhko variation (90 occurrences)
I = Oosterhoff types I (91 occurrences)
II = Oosterhoff types II (15 occurrences)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 21-Jan-2021