J/MNRAS/512/563 NIR light curves study of DCEPs in the LMC (Ripepi+, 2022)
The VMC survey - XLVIII. Classical cepheids unveil the 3D geometry of the LMC.
Ripepi V., Chemin L., Molinaro R., Cioni M.-R.L., Bekki K., Clementini G.,
De Grijs R., De Somma G., El Youssoufi D., Girardi L., Groenewegen M.A.T.,
Ivanov V., Marconi M., Mcmillan P.J., Van Loon J.T.
<Mon. Not. R. Astron. Soc. 512, 563-582 (2022)>
=2022MNRAS.512..563R 2022MNRAS.512..563R (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, standard ; Stars, variable ;
Photometry ; Optical ; Infrared ; Positional data ; Reddening
Keywords: stars: distances - stars: variables: Cepheids - Magellanic Clouds -
galaxies: photometry - galaxies: stellar content - galaxies: structure
Abstract:
We employed the VISTA near-infrared YJKs survey of the Magellanic
System (VMC) to analyse the Y, J, Ks light curves of δ Cepheid
stars (DCEPs) in the Large Magellanic Cloud (LMC). Our sample consists
of 4408 objects accounting for 97 per cent of the combined list of
OGLE IV and Gaia DR2 DCEPs. We determined a variety of
period-luminosity (PL) and period-Wesenheit PW relationships for
Fundamental (F) and First Overtone (1O) pulsators. We discovered for
the first time a break in these relationships for 1O DCEPs at P= 0.58
d. We derived relative individual distances for DCEPs in the LMC with
a precision of ∼1 kpc, calculating the position angle of the line of
nodes and inclination of the galaxy: θ = 145.6 ± 1.0 deg and
i = 25.7 ± 0.4 deg. The bar and the disc are seen under different
viewing angles. We calculated the ages of the pulsators, finding two
main episodes of DCEP formation lasting ∼40 Myr which happened 93 and
159 Myr ago. Likely as a result of its past interactions with the SMC,
the LMC shows a non-planar distribution, with considerable
structuring: the bar is divided into two distinct portions, the
eastern and the western displaced by more than 1 kpc from each other.
Similar behaviour is shown by the spiral arms. The LMC disc appears
'flared' and thick, with a disc scale height of h ∼ 0.97 kpc. This
feature can be explained by strong tidal interactions with the Milky
Way and/or the Small Magellanic Cloud or past merging events with now
disrupted LMC satellites.
Description:
The young stellar tracers are basically the δ Cepheid variables
(DCEPs hereafter) for which precise distances can be derived by means
of the PL and PW relations that hold for these objects. Due to their
unique properties, the DCEPs have been extensively used to study the
LMC disc in the literature. In this work, we take advantage of the
time-series photometry in the Y, J, Ks bands provided by the VISTA
survey of the Magellanic Clouds (VMC Cioni et al. 2011A&A...527A.116C 2011A&A...527A.116C,
Cat. II/351 and Cat. II/375) for the 97 per cent of known DCEPs
present in the LMC, (i.e see Introduction section).
As explained in the section 2, the list of LMC DCEPs used as reference
was taken from the OGLE IV survey (Optical Gravitational Lensing
Experiment IV; Soszynski et al. 2017AcA....67..103S 2017AcA....67..103S), as updated in
2019 July on the OGLE website. Additional stars were taken from Gaia
Data Release DR2. We cross-matched these samples with the VMC sources
with 1 arcsec tolerance, retaining only objects having at least four
epochs of observations in all the bands. In this way, we ended up with
4495 and five useful light curves from the OGLE and Gaia samples,
respectively. We measured the Y, J, and Ks intensity-averaged
magnitudes and the peak-to-peak amplitudes for the 4408 DCEPs
considered in this work using a technique similar to that of our
previous papers, time-series photometry curves are available in lcs/Y,
lcs/Ks and lcs/J folders. The 4410 LMC DCEPs analysed in this paper
are provided in table.dat, along with the respective errors. For
completeness, table2.dat also reports the data for the 90 sources
whose photometry was taken from Persson et al. (2004AJ....128.2239P 2004AJ....128.2239P,
Cat. J/AJ/128/2239), (i.e see section 3 for data analysis).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 168 4500 Photometric parameters for our LMC DCEPs sample
lcs/*Y.dat . 4408 The individual LMC DCEPs time-series photometry
in Y band (with file names Name_Y.dat)
lcs/*Ks.dat . 4408 The individual LMC DCEPs time-series photometry
in Ks band (with file names Name_Ks.dat)
lcs/*J.dat . 4408 The individual LMC DCEPs time-series photometry
in J band (with file names Name_J.dat)
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See also:
J/ApJ/832/176 : Classical Cepheids in MCs. I. LMC disk (Inno+, 2016)
J/AJ/128/2239 : JHKs photometry of 92 LMC Cepheids (Persson+, 2004)
II/351 : VISTA Magellanic Survey (VMC) catalog (Cioni+, 2011)
II/375 : VISTA Magellanic Survey (VMC) catalog (YJKs) DR6
(Cioni+, 2011)
J/MNRAS/472/808 : YJKs light curves of SMC Classical Cepheids (Ripepi+, 2017)
J/ApJS/224/21 : The VMC survey. XIX. Classical Cepheids in SMC
(Ripepi+, 2016)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
J/MNRAS/459/1687 : Ks light curve of 299 SMC new Cepheids (Moretti+, 2016)
J/MNRAS/437/2702 : MC Cepheids, RR Lyrae stars and binaries (Moretti+, 2014)
J/MNRAS/446/3034 : LMC Type II Cepheids J and Ks light curves (Ripepi+, 2015)
J/MNRAS/437/2307 : LMC anomalous Cepheid Ks light curves (Ripepi+, 2014)
J/A+A/625/A14 : Reclassification of Cepheids in the Gaia DR2 (Ripepi+, 2019)
J/A+A/622/A60 : Gaia DR2 misclassified RR Lyrae list (Clementini+, 2019)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 --- Name Identification name (SOURCEID) (1)
21- 28 A8 --- Mode Pulsation mode (MODE) (2)
30- 37 F8.5 deg RAdeg Right ascension (J2000) (RAdeg)
39- 47 F9.5 deg DEdeg Declination (J2000) (DECdeg)
49- 54 F6.3 mag Vmag ?=99.999 V-band magnitude (V)
56- 64 F9.5 d Per Pulsation period (P)
66- 71 F6.3 mag Ymag ?=99.999 Intensity-averaged magnitude in
Y band (Y)
73- 79 F7.4 mag e_Ymag Mean relative uncertainty σ<Y> of
Ymag (errY)
81- 86 F6.3 mag AmpYmag ?=99.999 Peak-to-peak intensity-averaged
amplitude A(Y) in Y band (ampY)
88- 94 F7.4 mag e_AmpYmag ?=99.999 Mean relative uncertainty
σA(Y) of AmpYmag (err_ampY)
96- 101 F6.3 mag Jmag Intensity-averaged magnitude in J band (J)
103- 108 E6.4 mag e_Jmag Mean relative uncertainty σ<J> of
Jmag(errJ)
110- 115 F6.3 mag AmpJmag ?=99.999 Peak-to-peak intensity-averaged
amplitude A(J) in J band (ampJ)
117- 122 F6.3 mag e_AmpJmag ?=99.999 Mean relative uncertainty
σA(J) of AmpJmag (err_ampJ)
124- 129 F6.3 mag Ksmag Intensity-averaged magnitude <Ks> in Ks band
(K)
131- 136 E6.4 --- e_Ksmag Mean relative uncertainty σ<Ks> of
Ksmag (errK)
138- 143 F6.3 --- AmpKsmag ?=99.999 Peak-to-peak intensity-averaged
amplitude A(Ks) in Ks band (ampK)
145- 150 F6.3 --- e_AmpKsmag ?=99.999 Mean relative uncertainty
σA(Ks) of AmpKsmag (err_ampK)
152- 156 F5.3 --- E(V-I) Calibrated reddening E (V-I) (evi)
158 I1 --- Flag1 [0/1] Flag indicating whether or not the star
was used in the derivation of PL(Y0)
relation, 4366 yes and 134 no (fl_PLY)
160 I1 --- Flag2 [0/1] Flag indicating whether or not the star
was used in the derivation of PL(J0)
relation, 4408 yes and 92 no (fl_PLJ)
162 I1 --- Flag3 [0/1] Flag indicating whether or not the star
was used in the derivation of PL(Ks0)
relation, 4385 yes and 115 no (fl_PLK)
164 I1 --- Flag4 [0/1] Flag indicating whether or not the star
was used in the derivation of PW(Y,Ks)
relation, 4307 yes and 193 no (fl_PWYK)
166 I1 --- Flag5 [0/1] Flag indicating whether or not the star
was used in the derivation of PW(J,Ks)
relation, 4360 yes and 140 no (fl_PWJK)
168 I1 --- Flag6 [0/1] Flag indicating whether or not the star
was used in the derivation of PW(V,Ks)
relation, 4134 yes and 366 no (fl_PWVK)
--------------------------------------------------------------------------------
Note (1): Name are taken from OGLE IV Soszynski et al. 2017AcA....67..103S 2017AcA....67..103S
for 4405 LMC DCEPs, from Persson et al. 2004AJ....128.2239P 2004AJ....128.2239P,
Cat. J/AJ/128/2239 for 90 LMC cepheids and from Gaia Collaboration
2016A&A...595A...1G 2016A&A...595A...1G, Cat. I/337 and 2018A&A...616A...1G 2018A&A...616A...1G, Cat. I/345
for 5 LMC cepheids.
Note (2): Pulsation mode are defined as follows:
F = Fundamental, 2483 objects in our sample
1O = First Overtone, 2110 objects in our sample
2O = Second Overtone, 312 objects in our sample
3O = Third Overtone, 8 objects in our sample
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Byte-by-byte Description of file: lcs/*Y.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d JD The Heliocentric Julian date time of the
recorded amplitude (HJD-2400000) (time)
13- 18 F6.3 mag Ymag Apparent magnitude in Y band (Y)
20- 24 F5.3 mag e_Ymag Mean uncertainty σY of Ymag
(σY)
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Byte-by-byte Description of file: lcs/*Ks.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d JD The Heliocentric Julian date time of
the recorded amplitude (HJD-2400000) (time)
13- 18 F6.3 mag Ksmag Apparent magnitude in Ks band (Ks)
20- 24 F5.3 mag e_Ksmag Mean uncertainty σKs of Ksmag
(σKs)
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Byte-by-byte Description of file: lcs/*J.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d JD The Heliocentric Julian date time of the
recorded amplitude (HJD-2400000) (time)
13- 18 F6.3 mag Jmag Apparent magnitude in J band (J)
20- 24 F5.3 mag e_Jmag Mean uncertainty σJ of Jmag
(σJ)
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History:
From electronic version of the journal
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(End) Luc Trabelsi [CDS] 06-Mar-2025