The VMC Survey

Ripepi, V.; Moretti, M. I.; Marconi, M.; Clementini, G.; Cioni, M-R.L.; Grijs, Richard de; Emerson, J. P.; Groenewegen, M. A. T.; Ivanov, V. D.; Muraveva, T.; Piatti, Andrés E.; Subramanian, Smitha

doi:10.1093/mnras/stu2260

Cited by 60 publications

(103 citation statements)

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“…They were calculated according to the following procedure: for the classical Cepheids we adopted the PM K s and PW(V, I) relations derived for the LMC variables by Fouqué et al (2007) (rows 4 and 2 from the bottom of their Table 8) and the PW(V, K s ) relation by Ripepi et al (2012) (their Table 4). For the Type II Cepheids we used the LMC relations in Table 5 of Ripepi et al (2015). Finally, for the RR Lyrae stars we applied the relations from Muraveva et al (2015) and Clementini et al (2003).…”

Section: Comparison Of Results From Different Relations and Conclusionmentioning

confidence: 99%

“…6 in Benedict et al 2011, and the discussion below), in contrast with the Type II Cepheids being expected to lay on the extrapolation to longer periods of the RR Lyrae star PM K relation (see e.g. Ripepi et al 2015, and references therein). Benedict et al (2011) explain this discrepancy either as being due to the wide range in absolute magnitude spanned by the short-period Type II Cepheids or as being caused by some anomaly in VY Pyx itself.…”

Section: Comparison With Other Parallax Measurementsmentioning

confidence: 97%

“…They have been studied by several authors (Wallerstein & Cox 1984;Gingold 1985;Harris 1985;Bono et al 1997;Wallerstein 2002;Feast et al 2008;Matsunaga et al 2011;Soszyński et al 2008;Ripepi et al 2015) and are usually divided into three classes: BL Herculis (BL Her) with periods from 1 to 4 days, W Virginis (W Vir) with periods from 4 to 20 days, and RV Tauri (RV Tau) with periods from 20 to 150 days. The light curves of BL Her and W Vir stars can be almost sinusoidal or highly non-sinusoidal, those of RV Tauri have alternating minima.…”

Section: Type II Cepheidsmentioning

confidence: 99%

“…To de-redden the K s and J magnitudes we applied the extinction laws A J = 0.87E(B−V) and A K = 0.35E(B−V) from Cardelli et al (1989), adopting R V = 3.1. We also calculated the Wesenheit magnitude W(K s , J) = K s − 0.69(J − K s ) and fitted the PM K s , PM J , and PW(K s , J − K s ) relations, adopting the slopes derived by Ripepi et al (2015) for BL Her and W Wir stars in the LMC. For the Type II Cepheids we only have single-phase 2MASS J and K s magnitudes instead of magnitudes averaged over the whole pulsation cycle, which introduced additional uncertainty.…”

Section: Type II Cepheidsmentioning

confidence: 99%

“…PL relation in the K s band of the Type II Cepheids obtained i) via linear least-squares fits of the stars' absolute magnitudes inferred by direct transformation of the TGAS parallaxes (upper panel); ii) via non-linear least-squares fits and the ABL method (middle panel); and iii) using the Bayesian approach (bottom panel). The slope of the fit is adopted from Ripepi et al (2015). The bottom part of each panel shows the residuals from the best fit line.…”

Section: Type II Cepheidsmentioning

confidence: 99%

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Gaia Data Release 1

Clementini¹,

Eyer²,

Ripepi³

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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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