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

G. Bono, G. Iannicola, V. F. Braga, I. Ferraro, P. B. Stetson, D. Magurno, N. Matsunaga, R. L. Beaton, R. Buonanno, B. Chaboyer, M. Dall'Ora, M. Fabrizio, G. Fiorentino, W. L. Freedman, C. K. Gilligan, B. F. Madore, M. Marconi, M. Marengo, S. Marinoni, P. M. MarreseC. E. Martinez-Vazquez, M. Mateo, M. Monelli, J. R. Neeley, M. Nonino, C. Sneden, F. Thevenin, E. Valenti, A. R. Walker

Resultado de la investigación: Article

5 Citas (Scopus)

Resumen

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 ω 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]∼-1.98 and a standard deviation of σ = 0.54 dex. The spread is, as expected, metal-poor ([Fe/H] ≤ -2.3) objects. The current metallicity distribution is ∼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 μ = 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 1σ. The metallicity dependence of distance diagnostics agrees with theory and observations, but firm constraints require accurate and homogeneous spectroscopic measurements.

Idioma originalEnglish
Número de artículo115
PublicaciónAstrophysical Journal
Volumen870
N.º2
DOI
EstadoPublished - 10 ene 2019

Huella dactilar

metallicity
near infrared
stars
metal
estimates
standard deviation
spatial variation
metals
harmonics
method
test
luminosity
distribution
firm

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Bono, G. ; Iannicola, G. ; Braga, V. F. ; Ferraro, I. ; Stetson, P. B. ; Magurno, D. ; Matsunaga, N. ; Beaton, R. L. ; Buonanno, R. ; Chaboyer, B. ; Dall'Ora, M. ; Fabrizio, M. ; Fiorentino, G. ; Freedman, W. L. ; Gilligan, C. K. ; Madore, B. F. ; Marconi, M. ; Marengo, M. ; Marinoni, S. ; Marrese, P. M. ; Martinez-Vazquez, C. E. ; Mateo, M. ; Monelli, M. ; Neeley, J. R. ; Nonino, M. ; Sneden, C. ; Thevenin, F. ; Valenti, E. ; Walker, A. R. / 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. En: Astrophysical Journal. 2019 ; Vol. 870, N.º 2.
@article{9af3954634f54983a6d59e78b2a89e21,
title = "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",
abstract = "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 ω 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]∼-1.98 and a standard deviation of σ = 0.54 dex. The spread is, as expected, metal-poor ([Fe/H] ≤ -2.3) objects. The current metallicity distribution is ∼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 μ = 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 1σ. The metallicity dependence of distance diagnostics agrees with theory and observations, but firm constraints require accurate and homogeneous spectroscopic measurements.",
keywords = "globular clusters: individual (Centauri), stars: distances, stars: horizontal-branch, stars: variables: RR Lyrae",
author = "G. Bono and G. Iannicola and Braga, {V. F.} and I. Ferraro and Stetson, {P. B.} and D. Magurno and N. Matsunaga and Beaton, {R. L.} and R. Buonanno and B. Chaboyer and M. Dall'Ora and M. Fabrizio and G. Fiorentino and Freedman, {W. L.} and Gilligan, {C. K.} and Madore, {B. F.} and M. Marconi and M. Marengo and S. Marinoni and Marrese, {P. M.} and Martinez-Vazquez, {C. E.} and M. Mateo and M. Monelli and Neeley, {J. R.} and M. Nonino and C. Sneden and F. Thevenin and E. Valenti and Walker, {A. R.}",
year = "2019",
month = "1",
day = "10",
doi = "10.3847/1538-4357/aaf23f",
language = "English",
volume = "870",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

Bono, G, Iannicola, G, Braga, VF, Ferraro, I, Stetson, PB, Magurno, D, Matsunaga, N, Beaton, RL, Buonanno, R, Chaboyer, B, Dall'Ora, M, Fabrizio, M, Fiorentino, G, Freedman, WL, Gilligan, CK, Madore, BF, Marconi, M, Marengo, M, Marinoni, S, Marrese, PM, Martinez-Vazquez, CE, Mateo, M, Monelli, M, Neeley, JR, Nonino, M, Sneden, C, Thevenin, F, Valenti, E & Walker, AR 2019, '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', Astrophysical Journal, vol. 870, n.º 2, 115. https://doi.org/10.3847/1538-4357/aaf23f

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. / Bono, G.; Iannicola, G.; Braga, V. F.; Ferraro, I.; Stetson, P. B.; Magurno, D.; Matsunaga, N.; Beaton, R. L.; Buonanno, R.; Chaboyer, B.; Dall'Ora, M.; Fabrizio, M.; Fiorentino, G.; Freedman, W. L.; Gilligan, C. K.; Madore, B. F.; Marconi, M.; Marengo, M.; Marinoni, S.; Marrese, P. M.; Martinez-Vazquez, C. E.; Mateo, M.; Monelli, M.; Neeley, J. R.; Nonino, M.; Sneden, C.; Thevenin, F.; Valenti, E.; Walker, A. R.

En: Astrophysical Journal, Vol. 870, N.º 2, 115, 10.01.2019.

Resultado de la investigación: Article

TY - JOUR

T1 - 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

T2 - ω Centauri as a First Test Case

AU - Bono, G.

AU - Iannicola, G.

AU - Braga, V. F.

AU - Ferraro, I.

AU - Stetson, P. B.

AU - Magurno, D.

AU - Matsunaga, N.

AU - Beaton, R. L.

AU - Buonanno, R.

AU - Chaboyer, B.

AU - Dall'Ora, M.

AU - Fabrizio, M.

AU - Fiorentino, G.

AU - Freedman, W. L.

AU - Gilligan, C. K.

AU - Madore, B. F.

AU - Marconi, M.

AU - Marengo, M.

AU - Marinoni, S.

AU - Marrese, P. M.

AU - Martinez-Vazquez, C. E.

AU - Mateo, M.

AU - Monelli, M.

AU - Neeley, J. R.

AU - Nonino, M.

AU - Sneden, C.

AU - Thevenin, F.

AU - Valenti, E.

AU - Walker, A. R.

PY - 2019/1/10

Y1 - 2019/1/10

N2 - 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 ω 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]∼-1.98 and a standard deviation of σ = 0.54 dex. The spread is, as expected, metal-poor ([Fe/H] ≤ -2.3) objects. The current metallicity distribution is ∼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 μ = 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 1σ. The metallicity dependence of distance diagnostics agrees with theory and observations, but firm constraints require accurate and homogeneous spectroscopic measurements.

AB - 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 ω 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]∼-1.98 and a standard deviation of σ = 0.54 dex. The spread is, as expected, metal-poor ([Fe/H] ≤ -2.3) objects. The current metallicity distribution is ∼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 μ = 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 1σ. The metallicity dependence of distance diagnostics agrees with theory and observations, but firm constraints require accurate and homogeneous spectroscopic measurements.

KW - globular clusters: individual (Centauri)

KW - stars: distances

KW - stars: horizontal-branch

KW - stars: variables: RR Lyrae

UR - http://www.scopus.com/inward/record.url?scp=85060204327&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aaf23f

DO - 10.3847/1538-4357/aaf23f

M3 - Article

AN - SCOPUS:85060204327

VL - 870

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 115

ER -