New near-infrared JHKs light-curve templates for RR Lyrae variables

被引：23

作者：

Braga, V. F. ^{[1
,2
]}

Stetson, P. B. ^{[3
]}

Bono, G. ^{[4
,5
]}

Dall'Ora, M. ^{[6
]}

Ferraro, I ^{[5
]}

Fiorentino, G. ^{[7
]}

Iannicola, G. ^{[5
]}

Inno, L. ^{[8
,9
]}

Marengo, M. ^{[10
]}

Neeley, J. ^{[11
]}

Beaton, R. L. ^{[12
]}

Buonanno, R. ^{[13
]}

Calamida, A. ^{[14
]}

Ramos, R. Contreras ^{[15
]}

Chaboyer, B. ^{[16
]}

Fabrizio, M. ^{[17
]}

Freedman, W. L. ^{[18
]}

Gilligan, C. K. ^{[16
]}

Johnston, K., V ^{[19
]}

Lub, J. ^{[20
]}

Madore, B. F. ^{[12
]}

Magurno, D. ^{[4
]}

Marconi, M. ^{[6
]}

Marinoni, S. ^{[17
]}

Marrese, P. M. ^{[17
]}

Mateo, M. ^{[21
]}

Matsunaga, N. ^{[22
]}

Minniti, D. ^{[1
,2
,23
]}

Monson, A. J. ^{[12
]}

Monelli, M. ^{[24
]}

Nonino, M. ^{[25
]}

Persson, S. E. ^{[12
]}

Pietrinferni, A. ^{[13
]}

Sneden, C. ^{[26
,27
]}

Storm, J. ^{[28
]}

Walker, A. R. ^{[29
]}

Valenti, E. ^{[30
]}

Zoccali, M. ^{[15
]}

机构：

[1] Inst Milenio Astrofis, Santiago, Chile

[2] Univ Andres Bello, Dept Fis, Fac Ciencias Exactas, Fernandez Concha 700, Santiago, Chile

[3] Natl Res Council Canada, Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[4] Univ Roma Tor Vergata, Dept Phys, Via Ric Sci 1, I-00133 Rome, Italy

[5] INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy

[6] INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy

[7] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy

[8] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[9] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[10] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

[11] Florida Atlantic Univ, Dept Phys, 777 Glades Rd, Boca Raton, FL 33431 USA

[12] Carnegie Inst Sci, The Observatories, 813 Santa Barbara St, Pasadena, CA 91101 USA

[13] INAF Osservatorio Astron Abruzzo, Via Mentore Maggini Snc, I-64100 Loc Collurania, Teramo, Italy

[14] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[15] Pontificia Univ Catolica Chile, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago, Chile

[16] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA

[17] Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

[18] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA

[19] Columbia Univ, Dept Astron, 550 W 120th St, New York, NY 10027 USA

[20] Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands

[21] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[22] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[23] Vatican Observ, I-00120 Vatican City, Vatican

[24] Inst Astrofis Canarias, Calle Via Lactea S-N, Tenerife 38205, Spain

[25] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[26] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA

[27] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA

[28] Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany

[29] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, Casilla 603, La Serena, Chile

[30] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 625卷

基金：

美国国家科学基金会;

关键词：

stars: variables: RR Lyrae; methods: data analysis; globular clusters: individual: M 4; globular clusters: individual: omega Cen; Magellanic Clouds; BAADE-WESSELINK METHOD; PHOTOMETRIC STANDARD STARS; PERIOD-LUMINOSITY RELATION; ABSOLUTE MAGNITUDES; GLOBULAR-CLUSTERS; METAL-RICH; RADIAL-VELOCITIES; OMEGA-CENTAURI; CCD PHOTOMETRY; FIELD STARS;

D O I：

10.1051/0004-6361/201834893

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We provide homogeneous optical (UBVRI) and near-infrared (NIR, JHK) time series photometry for 254 cluster (omega Cen, M 4) and field RR Lyrae (RRL) variables. We ended up with more than 551 000 measurements, of which only 9% are literature data. For 94 fundamental (RRab) and 51 first overtones (RRc) we provide a complete optical/NIR characterization (mean magnitudes, luminosity amplitudes, epoch of the anchor point). The NIR light curves of these variables were adopted to provide new light-curve templates for both RRc and RRab variables. The templates for the J and the H bands are newly introduced, together with the use of the pulsation period to discriminate among the different RRab templates. To overcome subtle uncertainties in the fit of secondary features of the light curves we provide two independent sets of analytical functions (Fourier and periodic Gaussian series). The new templates were validated by using 26 omega Cen and Bulge RRLs. We find that the difference between the measured mean magnitude along the light curve and the mean magnitude estimated by using the template on a single randomly extracted phase point is better than 0.01 mag (sigma = 0.04 mag). We also validated the template on variables for which at least three phase points were available, but without information on the phase of the anchor point. We find that the accuracy of the mean magnitudes is also similar to 0.01 mag (sigma = 0.04 mag). The new templates were applied to the Large Magellanic Cloud (LMC) globular cluster Reticulum and by using literature data and predicted PLZ relations we find true distance moduli mu = 18.47 +/- 0.10 (rand.) +/- 0.03 (syst.) mag (J) and 18.49 +/- 0.09 +/- 0.05 mag (K). We also used literature optical and mid-infrared data and we found a mean mu of 18.47 +/- 0.02 +/- 0.06 mag, suggesting that Reticulum is similar to 1 kpc closer than the LMC.

引用

页数：19