J/ApJ/931/131 Metallicity of Gal. RRLyrae from opt & IR LCs. II. (Mullen+, 2022)
Metallicity of Galactic RR Lyrae from optical and infrared light curves.
II. Period-Fourier-Metallicity relations for first overtone RR Lyrae.
Mullen J.P., Marengo M., Martinez-Vazquez C.E., Bono G., Braga V.F.,
Chaboyer B., Crestani J., Dall'Ora M., Fabrizio M., Fiorentino G.,
Monelli M., Neeley J.R., Stetson P.B., Thevenin F.
<Astrophys. J., 931, 131 (2022)>
=2022ApJ...931..131M 2022ApJ...931..131M
ADC_Keywords: Stars, variable; Abundances, [Fe/H]; Photometry; Optical;
Infrared sources
Keywords: RR Lyrae variable stars ; RRc variable stars ;
Pulsating variable stars ; Globular star clusters ; Metallicity
Abstract:
We present new period-φ31-[Fe/H] relations for first-overtone
RRL stars (RRc), calibrated over a broad range of metallicities
(-2.5≲[Fe/H]≲0.0) using the largest currently available set of
Galactic halo field RRL with homogeneous spectroscopic metallicities.
Our relations are defined in the optical (ASAS-SN V band) and,
inaugurally, in the infrared (WISE W1 and W2 bands). Our V-band
relation can reproduce individual RRc spectroscopic metallicities with
a dispersion of 0.30dex over the entire metallicity range of our
calibrator sample (an rms smaller than what we found for other
relations in literature including nonlinear terms). Our infrared
relation has a similar dispersion in the low- and
intermediate-metallicity range ([Fe/H]≲-0.5), but tends to
underestimate the [Fe/H] abundance around solar metallicity. We tested
our relations by measuring both the metallicity of the Sculptor dSph
and a sample of Galactic globular clusters, rich in both RRc and RRab
stars. The average metallicity we obtain for the combined RRL sample
in each cluster is within ±0.08dex of their spectroscopic
metallicities. The infrared and optical relations presented in this
work will enable deriving reliable photometric RRL metallicities in
conditions where spectroscopic measurements are not feasible; e.g., in
distant galaxies or reddened regions (observed with upcoming Extremely
Large Telescopes and the James Webb Space Telescope), or in the large
sample of new RRL that will be discovered in large-area time-domain
photometric surveys (such as the LSST and the Roman space telescope).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 65 617 Derived photometric properties of the RRc sample
--------------------------------------------------------------------------------
See also:
II/328 : AllWISE Data Release (Cutri+ 2013)
II/357 : The Dark Energy Survey (DES): Data Release 1 (Abbott+, 2018)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
II/366 : ASAS-SN catalog of variable stars (Jayasinghe+, 2018-2020)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/A+A/312/111 : [Fe/H] from RR Lyrae light curves (Jurcsik+, 1996)
J/A+AS/121/95 : Giant stars abundances in 24 clusters (Carretta+ 1997)
J/AJ/128/2239 : JHKs photometry of 92 LMC Cepheids (Persson+, 2004)
J/MNRAS/363/734 : Sculptor dSph variables metal abundances (Clementini+, 2005)
J/ApJ/699/1742 : LCID project. I. Cetus and Tucana variables (Bernard+, 2009)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/AJ/137/4377 : List of SEGUE plate pairs (Yanny+, 2009)
J/ApJ/712/1259 : LCID project. II. Variables in IC1613 (Bernard+, 2010)
J/MNRAS/432/3047 : LCID project VIII. Cepheids of Leo A (Bernard+, 2013)
J/MNRAS/435/3206 : Properties of field RR Lyrae variables (Dambis+, 2013)
J/AJ/145/160 : Variables in LMC globular clusters. III. Ret (Kuehn+, 2013)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/AcA/64/177 : VI LCs of Galactic Bulge RR Lyrae (Soszynski+, 2014)
J/ApJ/814/71 : Carina project IX: UBVI of Carina variables (Coppola+, 2015)
J/ApJ/808/11 : RR Lyrae stars in M4. II. Spitzer/IRAC phot. (Neeley+, 2015)
J/MNRAS/462/4349 : Variable stars in Sculptor dSph (Martinez-Vazquez+, 2016)
J/ApJ/850/137 : ISLAndS project. III. Var. stars (Martinez-Vazquez+, 2017)
J/ApJ/842/60 : Var. stars in Logal Group galaxies. III. (Monelli+, 2017)
J/ApJ/841/84 : Theoretical framework for RR Lyrae. II. MIR (Neeley+, 2017)
J/A+A/619/A8 : Cepheid period-luminosity-metallicities (Groenewegen, 2018)
J/MNRAS/481/1195 : GaiaDR2 RR Lyrae stars as standard candles (Muraveva+, 2018)
J/A+A/622/A60 : Gaia DR2 misclassified RR Lyrae list (Clementini+, 2019)
J/ApJ/913/38 : Compilation of Cepheids in the MW and MCs (Breuval+, 2021)
J/ApJ/908/20 : Field RR Lyrae as Galactic probes. II. (Crestani+, 2021)
J/ApJ/914/10 : Field RR Lyrae as Gal. probes. III. Abund. (Crestani+, 2021)
J/ApJ/912/144 : Metallicity of Gal. RRL from opt. & IR LCs (Mullen+, 2021)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 I19 --- GaiaDR3 Gaia DR3 identification number
21- 29 F9.7 d Per [0.2/0.43] Period of the fundamental
pulsation mode (1)
31- 35 F5.3 rad phi31c(V) [0.17/6.1]? V band Fourier decomposition
parameter φ31 - Cosine decomposition
37- 41 F5.3 rad e_phi31c(V) [0.002/0.12]? One sigma error in phi31c(V)
43- 47 F5.2 [Sun] [Fe/H](V) [-2.92/-0.04]? Photometric metallicity
[Fe/H] from V band Fourier parameter
49- 53 F5.3 rad phi31s(MIR) [0.48/6.3]? Mid-IR Fourier decomposition
parameter φ31 - Sine decomposition
55- 59 F5.3 rad e_phi31s(MIR) [0.005/0.2]? One sigma error in phi31s(MIR)
61- 65 F5.2 [Sun] [Fe/H](MIR) [-2.7/-0.3]? Photometric metallicity
[Fe/H] from mid-IR Fourier parameter
--------------------------------------------------------------------------------
Note (1): When both V-band and mid-IR (WISE) data is present, the period
included was calculated from ASAS-SN (V-band) data as the period is
usually more accurate due to the higher amplitude and steeper light
curve.
Period accuracies are quoted to an accuracy on the order of
10-6days, corresponding to a readily detectable ∼1% shift in phase
for a typical 0.32d period RRc star when phased over the large
temporal (>8yrs) baseline of our datasets.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Mullen et al. Paper I. 2021ApJ...912..144M 2021ApJ...912..144M Cat. J/ApJ/912/144
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Apr-2024