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J/ApJ/807/127  Properties of 70 RR Lyrae stars in the LMC bar  (Muraveva+, 2015)

New near-infrared Period-Luminosity-Metallicity relations for RR Lyrae stars and the outlook for Gaia. Muraveva T., Palmer M., Clementini G., Luri X., Cioni M.-R.L., Moretti M.I., Marconi M., Ripepi V., Rubele S. <Astrophys. J., 807, 127 (2015)> =2015ApJ...807..127M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Magellanic Clouds ; Abundances, [Fe/H] ; Photometry, infrared Keywords: astrometry - distance scale - Magellanic Clouds - methods: data analysis - stars: statistics - stars: variables: RR Lyrae Abstract: We present results of the analysis of 70 RR Lyrae stars located in the bar of the Large Magellanic Cloud (LMC). Combining the spectroscopically determined metallicity of these stars from the literature with precise periods from the OGLE III catalog (Soszynski et al. 2009, J/AcA/59/1) and multi-epoch Ks photometry from the VISTA survey of the Magellanic Clouds system, we derive a new near-infrared period-luminosity-metallicity (PLKsZ) relation for RR Lyrae variables. In order to fit the relation we use a fitting method developed specifically for this study. The zero-point of the relation is estimated two different ways: by assuming the value of the distance to the LMC and by using Hubble Space Telescope parallaxes of five RR Lyrae stars in the Milky Way (MW). The difference in distance moduli derived by applying these two approaches is ∼0.2 mag. To investigate this point further we derive the PLKsZ relation based on 23 MW RR Lyrae stars that had been analyzed in Baade-Wesselink studies. We compared the derived PLKsZ relations for RR Lyrae stars in the MW and LMC. Slopes and zero-points are different, but still consistent within the errors. The shallow slope of the metallicity term is confirmed by both LMC and MW variables. The astrometric space mission Gaia is expected to provide a huge contribution to the determination of the RR Lyrae PLKsZ relation; however, calculating an absolute magnitude from the trigonometric parallax of each star and fitting a PLKsZ relation directly to period and absolute magnitude leads to biased results. We present a tool to achieve an unbiased solution by modeling the data and inferring the slope and zero-point of the relation via statistical methods. Description: In order to derive mean Ks magnitudes for the RR Lyrae stars in our sample we used data from the VMC survey (Cioni et al. 2011A&A...527A.116C). Started in 2009, the VMC survey covers a total area of 116 deg2 in the LMC with 68 contiguous tiles. The survey is obtaining YJKs photometry. The Ks-band photometry is taken in time-series mode over 12 (or more) separate epochs and each single epoch reaches a limiting Ks magnitude ∼19.3 mag with a signal-to-noise ratio (S/N) ∼5 (see Figure 1 of Moretti et al. 2014, J/MNRAS/437/2702). On the bright side, VMC is limited by saturation at Ks∼11.4 mag. The majority of RR Lyrae stars in our sample are located within the VMC tile LMC 5_5. Observations of the tile LMC 5_5 were performed in 15 epochs taken in the period from 2010 October 30, to 2012 January 11. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 89 70 Properties of the 70 RR Lyrae Stars in the Bar of the LMC Analyzed in This Paper
See also: J/A+AS/145/11 : AGAPEROS: variable stars in the LMC Bar (Melchior+, 2000) J/AcA/53/93 : OGLE RR Lyrae in LMC (Soszynski+, 2003) J/A+A/421/937 : Metal abundances of LMC RR Lyrae (Gratton+, 2004) J/A+A/430/603 : BVI photometry of LMC bar variables (Di Fabrizio+, 2005) J/A+A/502/505 : Ks photometry of LMC RR Lyrae (Borissova+, 2009) J/AcA/59/1 : VI light curves of LMC RR Lyrae stars (Soszynski+, 2009) J/MNRAS/437/2702 : MC Cepheids, RR Lyrae stars and binaries (Moretti+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Star Star identification from Di Fabrizio et al. (2005, J/A+A/430/603) (ANNNNN, BNNNNN) (1) 8- 27 A20 --- OGLE OGLE identification (2) 29 I1 h RAh Hour of Right Ascension (J2000) 31- 32 I2 min RAm Minute of Right Ascension (J2000) 34- 38 F5.2 s RAs Second of Right Ascension (J2000) 40 A1 --- DE- Sign of the Declination (J2000) 41- 42 I2 deg DEd Degree of Declination (J2000) 44- 45 I2 arcmin DEm Arcminute of Declination (J2000) 47- 50 F4.1 arcsec DEs Arcsecond of Declination (J2000) 52- 55 A4 --- Type [RRc RRab] Subtype of RR Lyr star 57- 61 F5.2 [Sun] [Fe/H] Metallicity from Gratton et al. (2004, J/A+A/421/937) 63- 66 F4.2 [Sun] e_[Fe/H] Uncertainty in [Fe/H] 68- 76 F9.7 d Per Period (2) 78- 83 F6.3 mag Ksmag Dereddened mean Ks magnitude (3) 85- 89 F5.3 mag e_Ksmag Uncertainty in Ksmag
Note (1): [DCM2005] A-NNNNN and [DCM2005] B-NNNNN in Simbad. Note (2): From the OGLE III catalog (Soszynski et al. 2009, J/AcA/59/1). Note (3): From the VMC data (Cioni et al. 2011A&A...527A.116C), determined from the analysis of the light curve with GRATIS (custom software developed at the Observatory of Bologna by P. Montegriffo; see, e.g., Clementini et al. 2000AJ....120.2054C).
History: From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 20-Sep-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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