On a New Method to Estimate the Distance, Reddening, and Metallicity of RR Lyrae Stars Using Optical/Near-infrared (B, V, I, J, H, K) Mean Magnitudes: ω Centauri as a First Test Case

被引：25

作者：

Bono, G. ^{[1
,2
]}

Iannicola, G. ^{[2
]}

Braga, V. F. ^{[3
,4
]}

Ferraro, I. ^{[2
]}

Stetson, P. B. ^{[5
]}

Magurno, D. ^{[1
]}

Matsunaga, N. ^{[6
]}

Beaton, R. L. ^{[7
]}

Buonanno, R. ^{[8
]}

Chaboyer, B. ^{[9
]}

Dall'Ora, M. ^{[10
]}

Fabrizio, M. ^{[11
]}

Fiorentino, G. ^{[12
]}

Freedman, W. L. ^{[13
]}

Gilligan, C. K. ^{[9
]}

Madore, B. F. ^{[7
]}

Marconi, M. ^{[10
]}

Marengo, M. ^{[14
]}

Marinoni, S. ^{[2
,11
]}

Marrese, P. M. ^{[2
,11
]}

Martinez-Vazquez, C. E. ^{[15
]}

Mateo, M. ^{[16
]}

Monelli, M. ^{[17
,18
]}

Neeley, J. R. ^{[19
]}

Nonino, M. ^{[20
]}

Sneden, C. ^{[21
,22
]}

Thevenin, F. ^{[23
]}

Valenti, E. ^{[24
]}

Walker, A. R. ^{[15
]}

机构：

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

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

[3] Inst Milenio Astrofis, Santiago, Chile

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

[5] Domin Astrophys Observ, NRC Herzberg, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[6] Univ Tokyo, Sch Sci, Inst Astron, Kiso Observ, Kisogun,3, Nagano 970101, Japan

[7] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[8] INAF Osserv Astronomico Abruzzo, Via Mentore Maggini Snc, I-64100 Teramo, Italy

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

[10] INAF Osserv Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy

[11] SSDC, Via Politecn Snc, I-00133 Rome, Italy

[12] INAF Osserv Astrofis & Sci Spazio Bologna, Via Piero Gobetti 93-3, I-40129 Bologna, Italy

[13] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

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

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

[16] Univ Michigan, Dept Astron, 1085 S Univ, Ann Arbor, MI 48109 USA

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

[18] Univ La Laguna, Dept Astrofis, Tenerife, Spain

[19] Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA

[20] INAF Osserv Astron Trieste, Via GB Tiepolo,11, I-34143 Trieste, Italy

[21] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

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

[23] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange, BP 4229, F-06304 Nice, France

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

来源：

ASTROPHYSICAL JOURNAL | 2019年 / 870卷 / 02期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

globular clusters: individual (Centauri); stars: distances; stars: horizontal-branch; stars: variables: RR Lyrae; PERIOD-LUMINOSITY RELATION; GLOBULAR-CLUSTERS; PULSATING STARS; CHEMICAL ABUNDANCES; CLASSICAL CEPHEIDS; RADIAL-VELOCITY; AGES EXPERIMENT; CATALOG; PHOTOMETRY; MODELS;

D O I：

10.3847/1538-4357/aaf23f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We developed a new approach to provide accurate estimates of the metal content, reddening, and true distance modulus of RR Lyrae stars (RRLs). The method is based on homogeneous optical (BVI) and near-infrared (JHK) mean magnitudes and on predicted period-luminosity-metallicity relations (IJHK) and absolute mean magnitude-metallicity relations (BV). We obtained solutions for three different RRL samples in omega Cen: first overtone (RRc, 90), fundamental (RRab, 80), and global (RRc+RRab) in which the period of first overtones were fundamentalized. The metallicity distribution shows a well defined peak at [Fe/H]similar to-1.98 and a standard deviation of sigma = 0.54 dex. The spread is, as expected, metal-poor ([Fe/H] <= -2.3) objects. The current metallicity distribution is similar to 0.3 dex more metal-poor than similar estimates for RRLs available in the literature. The difference vanishes if the true distance modulus we estimated is offset by -0.06/-0.07. mag in true distance modulus. We also found a cluster true distance modulus of mu = 13.720 +/- 0.002 +/- 0.030 mag, where the former error is the error on the mean and the latter is the standard deviation. Moreover, we found a cluster reddening of E(B-V) = 0.132 +/- 0.002 +/- 0.028 mag and spatial variations of the order of a few arcmin across the body of the cluster. Both the true distance modulus and the reddening are slightly larger than similar estimates available in the literature, but the difference is within 1 sigma. The metallicity dependence of distance diagnostics agrees with theory and observations, but firm constraints require accurate and homogeneous spectroscopic measurements.

引用

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