J/MNRAS/424/1807 VISTA Magellanic Cloud Survey. V. Cepheids (Ripepi+, 2012)
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.T, Emerson J.P.
<Mon. Not. R. Astron. Soc., 424, 1807-1816 (2012)>
=2012MNRAS.424.1807R 2012MNRAS.424.1807R
ADC_Keywords: Surveys ; Magellanic Clouds ; Stars, variable ; Photometry
Keywords: surveys - stars: variables: Cepheids -
galaxies: distances and redshifts - Magellanic Clouds
Abstract:
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=18.46±0.03mag for the LMC. This result
is in agreement with most of the latest literature determinations
based on classical Cepheids.
Description:
In order to obtain well-sampled light curves, the VMC Ks-band time
series observations were scheduled into 12 separate epochs distributed
over ideally several consecutive months. The VMC data, processed
through the pipeline (Irwin et al., 2004, Proc. SPIE, 5493, 411) of
the VISTA Data Flow System (VDFS; Emerson et al. 2004, Proc. SPIE,
5493, 401), were retrieved from the VISTA Science Archive (VSA; Cross
et al., 2012A&A...548A.119C 2012A&A...548A.119C, http://horus.roe.ac.uk/versus/).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 97 323 Results for classical Cepheids in the 30 Dor field
table3.dat 91 11 Results for classical Cepheids in the South Eclitpic
Pole (SEP) field
lc/* . 334 Individual light curves
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See also:
J/A+A/531/A157 : LMC planetary nebulae (VMC Survey II) (Miszalski+, 2011)
J/A+A/537/A105 : Modelisation of AGB stars in the LMC (Gullieuszik+, 2012)
J/A+A/549/A29 : Quasars behind the Magellanic system (Cioni+, 2013)
J/A+A/554/A33 : VMC Survey. VII. 30 Doradus reddening map (Tatton+, 2013)
Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- --- [VMC]
5- 23 A19 --- VMC VMC name, JHHMMSS.ss+DDMMSS.s
25- 32 F8.5 deg RAdeg Right ascension (J2000)
34- 42 F9.5 deg DEdeg Declination (J2000)
44- 48 A5 --- M Pulsation mode (Fundamental or First Overtone)
50- 55 F6.3 mag <Imag> ? Average I magnitude (not for SEP field)
57- 62 F6.3 mag <Vmag> ?=99.999 Average V magnitude
64- 72 F9.6 d Per Period
74- 79 F6.3 mag <Ksmag> Average Ks magnitude
81- 84 F4.2 mag Kamp Amplitude in Ks band
86- 91 F6.4 mag e_<Ksmag> rms uncertainty on <Ksmag>
92- 95 F4.2 mag E(V-I) ? Colour excess (not for SEP field)
97 A1 --- n_VMC [a] a: star was not used to derive the
period-luminosity/Wesenheit/color relations
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Byte-by-byte Description of file: lc/*
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Bytes Format Units Label Explanations
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2- 12 F11.5 d MJD Modified Julian date
19- 24 F6.3 mag Ksmag Ks magnitude
32- 36 F5.3 mag e_Ksmag rms uncertainty on Ksmag
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History:
From electronic version of the journal
References:
Cioni et al. Paper I 2011A&A...527A.116C 2011A&A...527A.116C
Miszalski et al. Paper II 2011A&A...531A.157M 2011A&A...531A.157M Cat. J/A+A/531/A157
Gullieuszik et al. Paper III 2012A&A...537A.105G 2012A&A...537A.105G Cat. J/A+A/537/A105
Rubele et al. Paper IV 2012A&A...537A.106R 2012A&A...537A.106R
Cioni et al. PaPer VI 2013A&A...549A..29C 2013A&A...549A..29C Cat. J/A+A/549/A29
Tatton et al. Paper VII 2013A&A...554A..33T 2013A&A...554A..33T Cat. J/A+A/554/A33
Ripepi et al. Paper VIII 2014MNRAS.437.2307R 2014MNRAS.437.2307R Cat. J/MNRAS/437/2307
Cioni et al. Paper IX 2014A&A...562A..32C 2014A&A...562A..32C
Moretti et al. Paper X 2014MNRAS.437.2702M 2014MNRAS.437.2702M Cat. J/MNRAS/437/2702
Li et al. Paper XI 2014ApJ...790...35L 2014ApJ...790...35L
Piatti et al. Paper XII 2014A&A...570A..74P 2014A&A...570A..74P
Ripepi et al. Paper XIII 2015MNRAS.446.3034R 2015MNRAS.446.3034R Cat. J/MNRAS/446/3034
Rubele et al. Paper XIV 2015MNRAS.449..639R 2015MNRAS.449..639R Cat. J/MNRAS/449/639
Piatti et al. Paper XV 2015MNRAS.450..552P 2015MNRAS.450..552P
Piatti et al. Paper XVI 2015MNRAS.454..839P 2015MNRAS.454..839P
Cioni et al. Paper XVII 2016A&A...586A..77C 2016A&A...586A..77C
Zhang et al. Paper XVIII 2015ApJ...815...95Z 2015ApJ...815...95Z
Ripepi et al. Paper XIX 2016ApJS..224...21R 2016ApJS..224...21R Cat. J/ApJS/224/21
Moretti et al. Paper XX 2016MNRAS.459.1687M 2016MNRAS.459.1687M Cat. J/MNRAS/459/1687
Piatti et al. Paper XXI 2016MNRAS.460..383P 2016MNRAS.460..383P
Sun et al. Paper XXII 2017ApJ...835..171S 2017ApJ...835..171S
Marconi et al. Paper XXIII 2017MNRAS.466.3206M 2017MNRAS.466.3206M
Subramanian et al. Paper XXIV 2017MNRAS.467.2980S 2017MNRAS.467.2980S
Ripepi et al. Paper XXV 2017MNRAS.472..808R 2017MNRAS.472..808R
Sun et al. Paper XXVII 2017ApJ...849..149S 2017ApJ...849..149S Cat. J/ApJ/849/149
Niederhofer et al. Paper XXVIII 2018A&A...612A.115N 2018A&A...612A.115N
Sun et al. Paper XXIX 2018ApJ...858...31S 2018ApJ...858...31S Cat. J/ApJ/858/31
Niederhofer et al. Paper XXX 2018A&A...613L...8N 2018A&A...613L...8N
Rubele et al. Paper XXXI 2018MNRAS.478.5017R 2018MNRAS.478.5017R
Zivkov et al. Paper XXXII 2018A&A...620A.143Z 2018A&A...620A.143Z
Groenewegen et al. Paper XXXIII 2019A&A...622A..63G 2019A&A...622A..63G
Acknowledgements:
Please include the following acknowledgment in any published material
that makes use of this data products: Based on observations made with
ESO Telescopes at the La Silla or Paranal Observatories under
programme ID(s) 179.B-2003(G), 179.B-2003(F), 179.B-2003(D),
179.B-2003(C), 179.B-2003(H), 179.B-2003(B).
(End) Patricia Vannier [CDS] 06-Jan-2014