TY  - JOUR
A1  - Ripepi, V.
A1  - Marconi, M.
A1  - Moretti, M. I.
A1  - Clementini, Gisella
A1  - Cioni, Maria-Rosa L.
A1  - de Grijs, R.
A1  - Emerson, J. P.
A1  - Groenewegen, M. A. T.
A1  - Ivanov, V. D.
A1  - Piatti, A. E.
T1  - THE VMC SURVEY. XIX. CLASSICAL CEPHEIDS IN THE SMALL MAGELLANIC CLOUD
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Supplement series
N2  - The "VISTA near-infrared YJK(s) survey of the Magellanic Clouds System" (VMC) is collecting deep K-s-band time-series photometry of pulsating variable stars hosted by the two Magellanic Clouds and their connecting Bridge. In this paper, we present Y, J, K-s light curves for a sample of 4172 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with literature V values, allowed us to construct a variety of period-luminosity (PL), period-luminosity-color (PLC), and period-Wesenheit (PW) relationships, which are valid for Fundamental (F), First Overtone (FO), and Second Overtone (SO) pulsators. The relations involving the V, J, K-s bands are in agreement with their counterparts in the literature. As for the Y band, to our knowledge, we present the first CC PL, PW, and PLC relations ever derived using this filter. We also present the first near-infrared PL, PW, and PLC relations for SO pulsators to date. We used PW(V, K-s) to estimate the relative SMC-LMC distance and, in turn, the absolute distance to the SMC. For the former quantity, we find a value of Delta mu = 0.55. +/- 0.04 mag, which is in rather good agreement with other evaluations based on CCs, but significantly larger than the results obtained from older population II distance indicators. This discrepancy might be due to the different geometric distributions of young and old tracers in both Clouds. As for the absolute distance to the SMC, our best estimates are mu(SMC) = 19.01 +/- 0.05 mag and mu(SMC) = 19.04 +/- 0.06 mag, based on two distance measurements to the LMC which rely on accurate CC and eclipsing Cepheid binary data, respectively.
KW  - distance scale
KW  - Magellanic Clouds
KW  - stars: oscillations
KW  - stars: variables: Cepheids
Y1  - 2016
U6  - https://doi.org/10.3847/0067-0049/224/2/21
SN  - 0067-0049
SN  - 1538-4365
VL  - 224
SP  - 199
EP  - 229
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  - 
TY  - JOUR
A1  - Muraveva, Tatiana
A1  - Palmer, Max
A1  - Clementini, Gisella
A1  - Luri, Xavier
A1  - Cioni, Maria-Rosa L.
A1  - Moretti, Maria Ida
A1  - Marconi, Marcella
A1  - Ripepi, Vincenzo
A1  - Rubele, Stefano
T1  - New near-infrared period-luminosity-metallicity relations for RR lyrae stars and the outlock for GAIA
JF  - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2  - We present results of the analysis of 70 RR Lyrae stars located in the bar of the Large Magellanic Cloud (LMC). Combining the spectroscopically determined metallicity of these stars from the literature with precise periods from the OGLE III catalog and multi-epoch K-s photometry from the VISTA survey of the Magellanic Clouds system, we derive a new near-infrared period-luminosity-metallicity (PLKsZ) relation for RR Lyrae variables. In order to fit the relation we use a fitting method developed specifically for this study. The zero-point of the relation is estimated two different ways: by assuming the value of the distance to the LMC and by using Hubble Space Telescope parallaxes of five RR Lyrae stars in the Milky Way (MW). The difference in distance moduli derived by applying these two approaches is similar to 0.2 mag. To investigate this point further we derive the PL(Ks)Z relation based on 23 MW RR Lyrae stars that had been analyzed in Baade-Wesselink studies. We compared the derived PL(Ks)Z relations for RR Lyrae stars in the MW and LMC. Slopes and zero-points are different, but still consistent within the errors. The shallow slope of the metallicity term is confirmed by both LMC and MW variables. The astrometric space mission Gaia is expected to provide a huge contribution to the determination of the RR Lyrae PL(Ks)Z relation; however, calculating an absolute magnitude from the trigonometric parallax of each star and fitting a PL(Ks)Z relation directly to period and absolute magnitude leads to biased results. We present a tool to achieve an unbiased solution by modeling the data and inferring the slope and zero-point of the relation via statistical methods.
KW  - astrometry
KW  - distance scale
KW  - Magellanic Clouds
KW  - methods: data analysis
KW  - stars: statistics
KW  - stars: variables: RR Lyrae
Y1  - 2015
U6  - https://doi.org/10.1088/0004-637X/807/2/127
SN  - 0004-637X
SN  - 1538-4357
VL  - 807
IS  - 2
PB  - IOP Publ. Ltd.
CY  - Bristol
ER  -