J/MNRAS/472/808 YJKs light curves of SMC Classical Cepheids (Ripepi+, 2017)
The VMC survey.
XXV. The 3D structure of the Small Magellanic Cloud from Classical Cepheids.
Ripepi V., Cioni M.-R.L., Moretti M.I., Marconi M., Bekki K.,
Clementini G., De Grijs R., Emerson J., Groenewegen M.A.T., Ivanov V.D.,
Molinaro R., Muraveva T., Oliveira J.M., Piatti A.E., Subramanian S.,
Van Loon J.T.
<Mon. Not. R. Astron. Soc., 472, 808-827 (2017)>
=2017MNRAS.472..808R 2017MNRAS.472..808R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Photometry, infrared
Keywords: stars: oscillations - stars: variables: Cepheids -
stars: variables: RR Lyrae - Magellanic Clouds - galaxies: structure
Abstract:
The VISTA near-infrared YJKs survey of the Magellanic System (VMC)
is collecting deep Ks-band time-series photometry of pulsating stars
hosted by the two Magellanic Clouds and their connecting bridge. Here,
we present Y, J, Ks light curves for a sample of 717 Small
Magellanic Cloud (SMC) Classical Cepheids (CCs). These data,
complemented with our previous results and V magnitude from
literature, allowed us to construct a variety of period-luminosity and
period-Wesenheit relationships, valid for Fundamental, First and
Second Overtone pulsators. These relations provide accurate individual
distances to CCs in the SMC over an area of more than 40 deg2.
Adopting literature relations, we estimated ages and metallicities for
the majority of the investigated pulsators, finding that (i) the age
distribution is bimodal, with two peaks at 120±10 and 220±10Myr;
(i) the more metal-rich CCs appear to be located closer to the centre
of the galaxy. Our results show that the three-dimensional
distribution of the CCs in the SMC is not planar but heavily elongated
for more than 25-30kpc approximately in the east/north-east towards
south-west direction. The young and old CCs in the SMC show a
different geometric distribution. Our data support the current
theoretical scenario predicting a close encounter or a direct
collision between the Clouds some 200Myr ago and confirm the presence
of a Counter-Bridge predicted by some models. The high-precision
three-dimensional distribution of young stars presented in this paper
provides a new test bed for future models exploring the formation and
evolution of the Magellanic System.
Description:
The list of classical Cepheids in the SMC used as reference was taken
from the OGLE IV survey (Soszynski et al., 2015, Cat J/AcA/65/297,
2015AcA....65..329S 2015AcA....65..329S; Udalski et al., 2015AcA....65..341U 2015AcA....65..341U).
We present results for the classical Cepheids included in 31 tiles
completely or nearly completely observed, processed and catalogued by
the VMC survey as of 2016 August 22 (including observations until 2016
March 31).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 131 4793 Photometric results for all the 4793 classical
Cepheids analysed in this paper
listlc.dat 17 757 List of Cepheids with light curves
lc/* . 2271 Individual Y, J and Ks light curves
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See also:
J/AcA/65/297 : OGLE4 LMC and SMC Cepheids (Soszynski+, 2015)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name OGLE name, OGLE-SMC-CEP-NNNN, from Soszynski
et al., 2010, Cat J/AcA/60/17
19- 26 A8 --- Mode Mode(s) of pulsation (1)
28- 34 A7 --- VMCTile VMC tile, SMCNN, in which the object
is found
36- 46 F11.7 d Per Period
48- 49 I2 --- NY Number of epochs in Y
51- 56 F6.3 mag <Ymag> Intensity-averaged Y magnitude
58- 62 F5.3 mag e_<Ymag> rms uncertainty in <Ymag>
64- 67 F4.2 mag A(Y) Peak-to-peak amplitude in Y
69- 72 F4.2 mag e_A(Y) rms uncertainty on A(Y)
74- 75 I2 --- NJ Number of epochs in J
77- 82 F6.3 mag <Jmag> Intensity-averaged J magnitude
84- 88 F5.3 mag e_<Jmag> rms uncertainty in <Jmag>
90- 93 F4.2 mag A(J) Peak-to-peak amplitude in J
95- 98 F4.2 mag e_A(J) rms uncertainty on A(J)
100-101 I2 --- NKs Number of epochs in Ks
103-108 F6.3 mag <Ksmag> Intensity-averaged Ks magnitude
110-114 F5.3 mag e_<Ksmag> rms uncertainty in <Ksmag>
116-120 F5.3 mag A(Ks) Peak-to-peak amplitude in Ks
122-126 F5.3 mag e_A(Ks) rms uncertainty on A(Ks)
128-131 F4.2 mag E(V-I) Adoped E(V-I) value in this work
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Note (1): Modes as follows:
F = Fundamental
1O = First Overtone
2O = Second Overtone
3O = Third Overtone
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Byte-by-byte Description of file: listlc.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name OGLE name, OGLE-SMC-CEP-NNNN, from Soszynski
et al., 2010, Cat J/AcA/60/17
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Byte-by-byte Description of file: lc/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
4- 14 F11.5 d HJD Heliocentric Julian date (JHD-2400000)
19- 24 F6.3 mag mag Magnitude (J, Y or Ks)
30- 34 F5.3 mag e_mag rms uncertainty on mag
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Jun-2020