The VMC survey – V. First results for classical Cepheids

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dc.creator Ripepi, V.
dc.creator Moretti, M. I.
dc.creator Marconi, M.
dc.creator Clementini, G.
dc.creator Cioni, M.-R. L.
dc.creator Marquette, J. B.
dc.creator Girardi, L.
dc.creator Rubele, S.
dc.creator Groenewegen, M. A. T.
dc.creator de Grijs, R.
dc.creator Gibson, Brad K.
dc.date.accessioned 2018-04-19T16:31:08Z
dc.date.available 2018-04-19T16:31:08Z
dc.date.issued 2012-08
dc.identifier.issn 0035-8711
dc.identifier.uri http://library2.smu.ca/handle/01/27434
dc.description Publisher's Version/PDF
dc.description.abstract The VISTA Magellanic Cloud (VMC; PI: M.-R. L. Cioni) survey is collecting deep K<sub>s</sub>-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 K<sub>s</sub>-band light curves of the Cepheids are well sampled (12 epochs) and of excellent precision (typical errors of &sim;0.01 mag). We were able to measure for the first time the K<sub>s</sub> magnitude of the faintest classical Cepheids in the LMC (K<sub>s</sub> &sim; 17.5 mag), which are mostly pulsating in the first overtone (FO) mode, and to obtain FO period&ndash;luminosity (PL), period&ndash;Wesenheit (PW) and period&ndash;luminosity&ndash;colour (PLC) relations, spanning the full period range from 0.25 to 6 d. Since the longest period Cepheid in our data set has a variability period of 23 d, we have complemented our sample with literature data for brighter F Cepheids. On this basis, we have built a PL relation in the K<sub>s</sub> band that, for the first time, includes short-period &ndash; hence low-luminosity &ndash; 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 &minus; K<sub>s</sub>) colour and time series K<sub>s</sub> photometry. The very small dispersion (&sim;0.07 mag) of these relations makes them very well suited to study the three-dimensional geometry of the Magellanic system. The use of &lsquo;direct&rsquo; (parallax- and Baade&ndash;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 &minus; M)<sub>0</sub> = 18.46 &plusmn; 0.03 mag for the LMC. This result is in agreement with most of the latest literature determinations based on classical Cepheids.&nbsp; en_CA
dc.language.iso en en_CA
dc.publisher Oxford University Press en_CA
dc.relation.uri https://dx.doi.org/10.1111/j.1365-2966.2012.21274.x
dc.rights This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.subject.lcsh Cepheids
dc.subject.lcsh Magellanic Clouds
dc.subject.lcsh Astronomy -- Observations
dc.subject.lcsh Galaxies
dc.title The VMC survey – V. First results for classical Cepheids en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Monthly Notices of the Royal Astronomical Society 424(3), 1807-1816. (2012) en_CA


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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
 
Published Version: https://dx.doi.org/10.1111/j.1365-2966.2012.21274.x
 
 

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