METALLICITY DISTRIBUTION FUNCTIONS OF THE OLD POPULATIONS OF THE MAGELLANIC CLOUDS FROM RR Lyrae STARS

Haschke, Raoul; Grebel, Eva K.; Duffau, S.; Jin, Shoko

doi:10.1088/0004-6256/143/2/48

Cited by 92 publications

(163 citation statements)

References 84 publications

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“…larger dispersion in the various relationships mentioned above. To verify if different choices about the inclined disc parameters could improve the results, we have carried out the de-projection using several results present in the literature (see Haschke et al 2012;Rubele et al 2012;Subramanian & Subramaniam 2013, and references therein). Under no circumstances the dispersion of the P W s decreased (we used P W s as reference because they are reddening-free).…”

Section: J Ks-band Period-luminosity Period-luminosity-colour and Pmentioning

confidence: 99%

“…We decided to evaluate the relations for α=1.5±0.5 (to encompass reasonable values for α) and [Fe/H]=−1.5±0.3 dex as an average value for the LMC old population (see, e.g. Borissova et al 2004Borissova et al , 2006Gratton et al 2004;Haschke et al 2012). The uncertainties on these parameters were taken into account in re-deriving the ZP of the predicted P L and P W relations in the VISTA system.…”

Section: Comparison With the Literaturementioning

confidence: 99%

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The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

Ripepi

Moretti

Marconi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The VISTA survey of the Magellanic Clouds System (VMC) is collecting deep K s -band time-series photometry of the pulsating variable stars hosted in the system formed by the two Magellanic Clouds and the Bridge connecting them. In this paper we have analysed a sample of 130 Large Magellanic Cloud (LMC) Type II Cepheids (T2CEPs) found in tiles with complete or near complete VMC observations for which identification and optical magnitudes were obtained from the OGLE III survey. We present J and K s light curves for all 130 pulsators, including 41 BL Her, 62 W Vir (12 pW Vir) and 27 RV Tau variables. We complement our near-infrared photometry with the V magnitudes from the OGLE III survey, allowing us to build a variety of PeriodLuminosity (P L), Period-Luminosity-Colour (P LC) and Period-Wesenheit (P W ) relationships, including any combination of the V, J, K s filters and valid for BL Her and W Vir classes. These relationships were calibrated in terms of the LMC distance modulus, while an independent absolute calibration of the P L(K s ) and the P W (K s , V ) was derived on the basis of distances obtained from Hubble Space T elescope parallaxes and Baade-Wesselink technique. When applied to the LMC and to the Galactic Globular Clusters hosting T2CEPs, these relations seem to show that: 1) the two population II standard candles RR Lyrae and T2CEPs give results in excellent agreement with each other; 2) there is a discrepancy of ∼0.1 mag between population II standard candles and Classical Cepheids when the distances are gauged in a similar way for all the quoted pulsators. However, given the uncertainties, this discrepancy is within the formal 1σ uncertainties.

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Section: J Ks-band Period-luminosity Period-luminosity-colour and Pmentioning

confidence: 99%

Section: Comparison With the Literaturementioning

confidence: 99%

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

Ripepi

Moretti

Marconi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…It should be noted that some authors (e.g. Deb & Singh , hereinafter DS10; Haschke et al , hereinafter HGDJ) have used I ‐band data to derive metal abundances and physical parameters of RR Lyrae stars. As thoroughly discussed in Paper I, although the I ‐band light curves may produce similar average metallicities to those derived from the V ‐band light curves, discrepancies are revealed in metallicities of individual stars and their distributions.…”

Section: Data Analysis and Fourier Decompositionmentioning

confidence: 99%

RR Lyrae variables in the Small Magellanic Cloud - II. The extended area: chemical and structural analysis

Kapakos

Hatzidimitriou

2012

Monthly Notices of the Royal Astronomical Society

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We have performed the Fourier decomposition analysis of 8‐ and 13‐yr V‐band light curves of a carefully selected sample of 454 fundamental‐mode RR Lyrae variables (RRab type), detected in an ≃14 square degree area of the Small Magellanic Cloud (SMC) and listed in the Optical Gravitational Lensing Experiment, phase III, Catalogue of Variable Stars. The Fourier decomposition parameters were used to derive metal abundances and distance moduli, following the methodology described by Kapakos, Hatzidimitriou & Soszyński. The average metal abundance of the RRab stars on the new scale of Carretta et al. was found to be 〈[Fe/H]C09〉 = −1.69 ± 0.41 dex (std, with a standard error of 0.02 dex). A tentative metallicity gradient of −0.013 ± 0.007 dex kpc−1 was detected, with increasing metal abundance towards the dynamical centre of the SMC, but selection effects are also discussed. The distance modulus of the SMC was re‐estimated and was found to be 〈μ〉 = 19.13 ± 0.19 (std) in a distance scale where the distance modulus of the Large Magellanic Cloud (LMC) is μLMC = 18.52 ± 0.06 (std). The average 1σ line‐of‐sight depth was found to be σ int =5.3±0.4 kpc (std), while spatial variations of the depth were detected. The SMC was found to be deeper in the north‐eastern region, while metal‐richer and metal‐poorer objects in the sample seem to belong to different dynamical structures. The former have smaller scale height and may constitute a thick disc, its width being 10.40 ± 0.02 kpc, and a bulge whose size (radius) is estimated to be 2.09 ± 0.81 kpc. The latter seem to belong to a halo structure with a maximum depth along the line of sight extending over 16 kpc in the SMC central region and falling to ∼12 kpc in the outer regions.

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“…For example, on global scales they are one of the key parameters in the study of the luminosity-metallicity and massmetallicity relations of galaxies, their evolution with time, and their dependence on environment or star formation rate (e.g., Lequeux et al 1979;Grebel et al 2003;Tremonti et al 2004;Erb et al 2006;Panter et al 2008;Zahid et al 2012;Sánchez et al 2013;Peng & Maiolino 2014;Zahid et al 2014;Izotov et al 2015, to just name a few of the many studies). Local measurements within galaxies reveal the position-dependent metallicity of the chosen tracer population and may show abundance gradients, which in turn hold clues about galaxy evolution (e.g., Searle 1971;Janes 1979;Maciel & Quireza 1999;Harbeck et al 2001;Andrievsky et al 2002;Chen et al 2003;Mehlert et al 2003;Cioni 2009;Haschke et al 2012;Boeche et al 2013Boeche et al , 2014Pilyugin et al 2014Pilyugin et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

New calibrations for abundance determinations in H ii regions

Pilyugin¹,

Grebel²

2016

Mon. Not. R. Astron. Soc.

277

250

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Simple relations for deriving the oxygen abundance in H ii regions with intensities of the three strong emission lines R 2 , R 3 , and N 2 (R calibration) or S 2 , R 3 , and N 2 (S calibration) in their spectra are suggested. A sample of 313 reference H ii regions of the counterpart method (C method) is used as calibrating data points. Relations for the determination of nitrogen abundances, the R calibration, are also constructed. We find that the oxygen and nitrogen abundances in high-metallicity H ii regions can be estimated using the intensities of the two strong lines R 2 and N 2 (or S 2 and N 2 for oxygen) only. The corresponding two-dimensional relations are provided. There are considerable advantages of the suggested calibration relations as compared to the existing ones. First, the oxygen and nitrogen abundances estimated through the suggested calibrations agree with the T e -based abundances within ∼ 0.1 dex over the whole metallicity range, i.e., the relative accuracy of the calibration-based abundances is 0.1 dex. Although we constructed distinct relations for high-and low-metallicity objects, the separation between these two can be simply obtained from the intensity of the N 2 line. Moreover, the applicability ranges of the high-and low-metallicity relations overlap for adjacent metallicities, i.e., the transition zone disappears. Second, the oxygen abundances produced by the two suggested calibrations are in remarkable agreement with each other. In fact, the R-based and S -based oxygen abundances agree within ∼0.05 dex in the majority of cases for more than three thousand H ii region spectra.

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METALLICITY DISTRIBUTION FUNCTIONS OF THE OLD POPULATIONS OF THE MAGELLANIC CLOUDS FROM RR Lyrae STARS

Cited by 92 publications

References 84 publications

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

RR Lyrae variables in the Small Magellanic Cloud - II. The extended area: chemical and structural analysis

New calibrations for abundance determinations in H ii regions

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