J/ApJS/241/35 Period-luminosity relations of RSGs in M33 & M31 (Ren+, 2019)
The period-luminosity relations of red supergiants in M33 and M31.
Ren Y., Jiang B.-W., Yang M., Gao J.
<Astrophys. J. Suppl. Ser., 241, 35-35 (2019)>
=2019ApJS..241...35R 2019ApJS..241...35R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, supergiant; Stars, late-type; Photometry, infrared;
Optical
Keywords: stars: late-type; stars: oscillations including pulsations
supergiants
Abstract:
Based on previously selected preliminary samples of red supergiants
(RSGs) in M33 and M31, the foreground stars and luminous asymptotic
giant branch stars are further excluded, which leads to the samples of
717 RSGs in M33 and 420 RSGs in M31. With the time-series data from
the Intermediate Palomar Transient Factory survey spanning nearly 2000
days, the period and amplitude of RSGs are analyzed. According to the
light-curve characteristics, they are classified into four categories
in which 84 and 56 objects in M33 and M31, respectively, are
semi-regular variables. For these semi-regular variables, the
pulsation mode is identified by comparing with the theoretical model,
which yielded 19 (7) sources in the first overtone mode in M33 (M31),
and the other 65 (49) RSGs in M33 (M31) in the fundamental mode. The
period-luminosity (P-L) relation is analyzed for the RSGs in the
fundamental mode. The P-L relation is found to be tight in the
infrared, i.e., the Two Mircon All-Sky Survey (2MASS) JHKS bands and
the short-wavelength bands of Spitzer. Meanwhile, the inhomogeneous
extinction causes the P-L relation scattering in the V band, and the
dust emission causes the less tight P-L relation in the Spitzer/[8.0]
and [24] bands. The derived P-L relations in the 2MASS/KS band are
in agreement with those of RSGs in the Small Magellanic Cloud, the
Large Magellanic Cloud, and the Milky Way within the uncertainty
range. It is found that the number ratio of RSGs pulsating in the
fundamental mode to the first overtone mode increases with
metallicity.
Description:
The time-series data is taken from the Intermediate Palomar Transient
Factory (iPTF) survey, a wide-field survey for an exploration of
optical transients using the 1.2m Samuel Oschin Telescope at Palomar
Observatory. This survey uses a large field camera covering 7.8deg2
with 11 2048x4096 charge-coupled devices (CCDs) at a resolution of
1.01arcsec/pixel. In the iPTF survey, 2 and 6 frames covered the M33
and M31 sky area, respectively, from 2009 August to 2015 January
(about 2000 days in total) with a typical seeing of 2".
We choose the R-band iPTF data to analyze the variation of the red
supergiants (RSGs) in M33 and M31.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 147 717 Parameters of red supergiants (RSGs) in M33
table5.dat 147 420 Parameters of red supergiants (RSGs) in M31
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See also:
I/250 : The Tycho Reference Catalogue (Hog+ 1998)
II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/96/1884 : BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)
J/AJ/99/784 : IR photometry of LMC long-period variables (Hughes+ 1990)
J/ApJS/89/85 : Blue and red supergiants in M33 (Ivanov+ 1993)
J/A+A/333/231 : O-M stars model atmospheres (Bessell+ 1998)
J/ApJ/501/153 : VRB photometry of red supergiants (Massey 1998)
J/A+A/357/225 : Mass loss of M supergiants (Josselin+, 2000)
J/AJ/126/2867 : Red supergiants in Magellanic Clouds (Massey+, 2003)
J/AJ/131/2478 : M31 and M33 UBVRI photometry (Massey+, 2006)
J/AJ/133/2393 : UBVRI phot. in 7 Local Group dwarfs galaxies (Massey+, 2007)
J/ApJ/703/420 : Red supergiants in M31 (Massey+, 2009)
J/MNRAS/395/1409 : Type II-P SN progenitor constraints (Smartt+, 2009)
J/A+A/507/1375 : HST/ACS VI data of M31 globular clusters (Perina+, 2009)
J/ApJ/727/53 : Red supergiant stars in the LMC. I. (Yang+, 2011)
J/A+A/537/A146 : Stellar models with rotation; 0.8<M<120 (Ekstrom+, 2012)
J/ApJ/750/97 : The yellow and red supergiants of M33 (Drout+, 2012)
J/ApJ/754/35 : Red supergiant stars in the SMC. II. (Yang+, 2012)
J/ApJ/825/50 : Variable stars in M31 & M33. III. YSGs & RSGs (Gordon+, 2016)
J/ApJ/826/224 : RSG and foreground candidates in M31 (Massey+, 2016)
J/AJ/152/62 : Revised LGGS UBVRI phot. of M31 and M33 stars (Massey+, 2016)
J/A+A/616/A175 : Red supergiant stars in the LMC. II. (Yang+, 2018)
J/ApJ/859/73 : Variability of RSGs in M31 from iPTF (Soraisam+, 2018)
J/ApJ/889/44 : UKIRT obs. of red supergiants in M31 (Neugent+, 2020)
J/ApJ/898/24 : Granulations in RSGs from ASAS-SN & iPTF (Ren+, 2020)
J/AJ/161/79 : Red supergiant stars in M31 and M33 (Massey+, 2021)
Byte-by-byte Description of file: table[45].dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/717] Internal index number
5- 24 A20 --- LGGS Local Group Galaxies Survey identifier
(JHHMMSS.ss+DDMMSS.s)
26- 31 F6.3 mag Jmag [12.7/17.3]? 2MASS J band magnitude
33- 38 F6.3 mag Hmag [12.1/16.7]? 2MASS H band magnitude
40- 45 F6.3 mag Ksmag [11.9/17]? 2MASS Ks band magnitude
47- 54 F8.3 d GLS [10/3487]? 1st period from Generalized
Lomb-Scargle periodogram
(Zechmeister & Kurster 2009A&A...496..577Z 2009A&A...496..577Z)
algorithm
56- 63 F8.3 d DFT [10/2612]? 1st period from Discrete Fourier
Transform method
65- 70 F6.1 d PDM [10/3493]? 1st period from Phase Dispersion
Minimization (Stellingwerf 1978ApJ...224..953S 1978ApJ...224..953S)
algorithm
72- 79 F8.3 d WWZ [15/3500]? 1st period from Weighted Wavelet
Z-transform (Foster 1996AJ....112.1709F 1996AJ....112.1709F)
algorithm (1)
81- 88 F8.3 d Per [10/3500]? Adopted period
90- 97 F8.3 d GLS2 [10/3491]? 2nd period from Generalized
Lomb-Scargle
99- 106 F8.3 d DFT2 [10/2613]? 2nd period from Discrete Fourier
Transform
108- 113 F6.1 d PDM2 [10/3469]? 2nd period from Phase Dispersion
Minimization
115- 122 F8.3 d WWZ2 [12/3500]? 2nd period from Weighted Wavelet
Z-transform (1)
124- 131 F8.3 d Per2 [10/3500]? 2nd adopted period
133- 138 F6.3 mag Amp [0.011/32]? Amplitude
140 A1 --- Type Type code (2)
142- 147 F6.4 --- RMS [0/0.3]? Root-mean-square of the light curve fit
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Note (1): Object number 428, in Table 4, has WWZ and WWZ2 infinite values.
Note (2): Type code as follows:
S = Semi-regular variable;
L = Long secondary period (LSP) variable;
I = Irregular variable;
U = Undefined class;
N = No significant variation.
See section 4 for full details.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 05-Nov-2021