2012MNRAS.424.1807R -
Mon. Not. R. Astron. Soc., 424, 1807-1816 (2012/August-2)
The VMC survey – V. First results for classical cepheids.
RIPEPI V., MORETTI M.I., MARCONI M., CLEMENTINI G., CIONI M.-R.L., MARQUETTE J.B., GIRARDI L., RUBELE S., GROENEWEGEN M.A.T., DE GRIJS R., GIBSON B.K., OLIVEIRA J.M., VAN LOON J.Th. and EMERSON J.P.
Abstract (from CDS):
The VISTA Magellanic Cloud (VMC; PI: M.-R. L. Cioni) survey is collecting deep
Ks-band time series photometry of the pulsating variable stars hosted by the system formed by the two Magellanic Clouds (MCs) and the bridge connecting them. In this paper, we present the first results for classical Cepheids, from the VMC observations of two fields in the Large Magellanic Cloud (LMC), centred on the South Ecliptic Pole and the 30 Doradus star-forming regions, respectively. The VMC
Ks-band light curves of the Cepheids are well sampled (12 epochs) and of excellent precision (typical errors of ∼ 0.01mag). We were able to measure for the first time the
Ksmagnitude of the faintest classical Cepheids in the LMC (
Ks ∼ 17.5mag), which are mostly pulsating in the first overtone (FO) mode, and to obtain FO period–luminosity (
PL), period–Wesenheit (
PW) and period–luminosity–colour (
PLC) relations, spanning the full period range from 0.25 to 6d. Since the longest period Cepheid in our data set has a variability period of 23d, we have complemented our sample with literature data for brighter F Cepheids. On this basis, we have built a
PL relation in the
Ks band that, for the first time, includes short-period – hence low-luminosity – pulsators, and spans the full range from 1.6 to 100 d in period.We also provide the first ever empirical
PW and
PLC relations using the (
V -
Ks) colour and time series
Ksphotometry. The very small dispersion ( ∼ 0.07mag) of these relations makes them very well suited to study the three-dimensional geometry of the Magellanic system. The use of `direct' (parallax- and Baade–Wesselink-based) distance measurements to both Galactic and LMC Cepheids allowed us to calibrate the zero-points of the
PL,
PW and
PLC relations obtained in this paper, and in turn to estimate an absolute distance modulus of (
m -
M)
0 the latest literature determinations based on classical Cepheids.
Research fellow at the Alexander von Humboldt Foundation.
Based on observations made with VISTA at ESO under programme ID 179.B-2003.
Abstract Copyright:
2012 The Authors Monthly Notices of the Royal Astronomical Society 2012 RAS
Journal keyword(s):
surveys - stars: variables: Cepheids - galaxies: distances and redshifts - Magellanic Clouds University of Hertfordshire Science Foundation of China Cambridge Astronomy Survey Unit Archive at Wide Field Astronomy Unit
VizieR on-line data:
<Available at CDS (J/MNRAS/424/1807): table2.dat table3.dat lc/*>
Nomenclature:
Tables 2-3: [RMM2012b] VMC JHHMMSS.ss+DDMMSS.s N=350+11.
Simbad objects:
357
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