RR Lyrae variables: visual and infrared luminosities, intrinsic colours and kinematics

Дамбис, А. К.; Бердников, Л. Н.; Kniazev, A. Y.; Kravtsov, V. V.; Rastorguev, A. S.; Sefako, Ramotholo; Vozyakova, O. V.

doi:10.1093/mnras/stt1514

Cited by 93 publications

(159 citation statements)

References 113 publications

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“…Photometry and metallicity for most of these stars is available in the literature, although sparse through many different papers and catalogues. Dambis et al (2013) (3.4 µm) passbands for 384, 403, and 398 stars, respectively. The pulsation periods are taken from the ASAS3 (Pojmanski 2002;Maintz 2005) and GCVS (Samus et al 2007(Samus et al -2015 catalogues.…”

Section: Rr Lyrae Starsmentioning

confidence: 99%

“…We adopt this value as the mean uncertainty of the extinction. The mean V magnitudes were calculated from nine overlapping sets of observations (see details in Dambis et al 2013, and references therein); the K s -band mean magnitudes were calculated from the 2MASS single-epoch observations of Cutri et al (2003) and by applying the phase-correction procedure described in Feast et al (2008) 10 . Mean magnitudes in the MIR W1 passband were calculated from the WISE single-exposure database.…”

Section: Rr Lyrae Starsmentioning

confidence: 99%

“…Mean magnitudes in the MIR W1 passband were calculated from the WISE single-exposure database. We cross-matched our sample of 364 RR Lyrae stars with TGAS parallaxes against the catalogue of Dambis et al (2013) and found 200 sources in common. They span the period range from 0.27 to 0.80 d. The error distribution of the TGAS parallaxes for these 200 RR Lyrae stars is shown by the blue histogram in Fig.…”

Section: Rr Lyrae Starsmentioning

confidence: 99%

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Gaia Data Release 1

Clementini¹,

Eyer²,

Ripepi³

et al. 2017

A&A

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Context. Parallaxes for 331 classical Cepheids, 31 Type II Cepheids, and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). Aims. In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, which involve astrometry collected by Gaia during the initial 14 months of science operation, we compared them with literature estimates and derived new period-luminosity (PL), period-Wesenheit (PW) relations for classical and Type II Cepheids and infrared PL, PL-metallicity (PLZ), and optical luminosity-metallicity (M V -[Fe/H]) relations for the RR Lyrae stars, with zero points based on TGAS. Methods. Classical Cepheids were carefully selected in order to discard known or suspected binary systems. The final sample comprises 102 fundamental mode pulsators with periods ranging from 1.68 to 51.66 days (of which 33 with σ / < 0.5). The Type II Cepheids include a total of 26 W Virginis and BL Herculis stars spanning the period range from 1.16 to 30.00 days (of which only 7 with σ / < 0.5). The RR Lyrae stars include 200 sources with pulsation period ranging from 0.27 to 0.80 days (of which 112 with σ / < 0.5). The new relations were computed using multi-band (V, I, J, K s ) photometry and spectroscopic metal abundances available in the literature, and by applying three alternative approaches: (i) linear least-squares fitting of the absolute magnitudes inferred from direct transformation of the TGAS parallaxes; (ii) adopting astrometrybased luminosities; and (iii) using a Bayesian fitting approach. The last two methods work in parallax space where parallaxes are used directly, thus maintaining symmetrical errors and allowing negative parallaxes to be used. The TGAS-based PL, PW, PLZ, and M V − [Fe/H] relations are discussed by comparing the distance to the Large Magellanic Cloud provided by different types of pulsating stars and alternative fitting methods. A79, page 2 of 29Gaia Collaboration (Clementini, G., et al.): Gaia Data Release 1Results. Good agreement is found from direct comparison of the parallaxes of RR Lyrae stars for which both TGAS and HST measurements are available. Similarly, very good agreement is found between the TGAS values and the parallaxes inferred from the absolute magnitudes of Cepheids and RR Lyrae stars analysed with the Baade-Wesselink method. TGAS values also compare favourably with the parallaxes inferred by theoretical model fitting of the multi-band light curves for two of the three classical Cepheids and one RR Lyrae star, which were analysed with this technique in our samples. The K-band PL relations show the significant improvement of the TGAS parallaxes for Cepheids and RR Lyrae stars with respect to the Hipparcos measurements. This is particularly true for the RR Lyrae stars for which improvement in quality and statistics is impressive. Conclusions. TGAS parallaxes bring a significant added value t...

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Section: Rr Lyrae Starsmentioning

confidence: 99%

Section: Rr Lyrae Starsmentioning

confidence: 99%

Section: Rr Lyrae Starsmentioning

confidence: 99%

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Gaia Data Release 1

Clementini¹,

Eyer²,

Ripepi³

et al. 2017

A&A

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“…2009b;Dambis et al 2013;Francis & Anderson 2014). As model 3 was adjusted for R 0 = 7.1 kpc, we rescaled all distances for model particles by a factor of k = 7.5/7.1.…”

Section: Catalogues and Modelsmentioning

confidence: 99%

Evidence of the Galactic outer ring R 1 R 2 ′ $R_{1}R_{2}'$ from young open clusters and OB-associations

Melnik

Rautiainen

Glushkova

et al. 2016

Astrophys Space Sci

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“…We begin by calculating (NUV−V ) 0 for 150 nearby RR Lyrae stars using the recent compilation by Dambis et al (2013), a sample for which we could easily obtain the necessary data. For this sample, we plot (NUV − V ) 0 against period for Table 2.…”

Section: The Identification Of Rr Lyrae and δ Scuti Stars In The Firsmentioning

confidence: 99%

THE IDENTIFICATION OF RR LYRAE AND δ SCUTTI STARS FROM VARIABLEGALAXY EVOLUTION EXPLORERULTRAVIOLET SOURCES

Kinman¹,

Brown²

2014

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We identify the RR Lyrae and δ Scuti stars in three catalogs of Galaxy Evolution Explorer (GALEX) variable sources. The NUV amplitude of RR Lyrae stars is about twice that in V, so we find a larger percentage of low-amplitude variables than catalogs such as Abbas et al. Interestingly, the (NUV − V ) 0 color is sensitive to metallicity and can be used to distinguish between variables of the same period but differing [Fe/H]. This color is also more sensitive to T eff than optical colors and can be used to identify the red edge of the instability gap. We find 8 δ Scuti stars, 17 RRc stars, 1 RRd star, and 84 RRab stars in the GALEX variable catalogs of Welsh et al. and Wheatley et al. We also classify 6 δ Scuti stars, 5 RRc stars, and 18 RRab stars among the 55 variable GALEX sources identified as "stars" or RR Lyrae stars in the catalog of Gezari et al. We provide ephemerides and light curves for the 26 variables that were not previously known.

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RR Lyrae variables: visual and infrared luminosities, intrinsic colours and kinematics

Cited by 93 publications

References 113 publications

Gaia Data Release 1

Gaia Data Release 1

Evidence of the Galactic outer ring R 1 R 2 ′ $R_{1}R_{2}'$ from young open clusters and OB-associations

THE IDENTIFICATION OF RR LYRAE AND δ SCUTTI STARS FROM VARIABLEGALAXY EVOLUTION EXPLORERULTRAVIOLET SOURCES

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