J/ApJS/257/23 Multiwavelength obs. of Miras in the LMC (Iwanek+, 2021)
Multiwavelength properties of Miras.
Iwanek P., Kozlowski S., Gromadzki M., Soszynski I., Wrona M.,
Skowron J., Ratajczak M., Udalski A., Szymanski M.K., Pietrukowicz P.,
Ulaczyk K., Poleski R., Mroz P., Skowron D.M., Rybicki K.
<Astrophys. J. Suppl. Ser., 257, 23 (2021)>
=2021ApJS..257...23I 2021ApJS..257...23I
ADC_Keywords: Stars, variable; Photometry, UBVRI; Photometry, infrared;
Magellanic Clouds
Keywords: Asteroseismology ; Stellar astronomy ; Mira variable stars ;
Late-type giant stars ; Long period variable stars ;
Pulsating variable stars ; Asymptotic giant branch stars ;
Stellar distance ; Infrared astronomy ; Near infrared astronomy ;
Large Magellanic Cloud ; Magellanic Clouds
Abstract:
We comprehensively study the variability of Miras in the Large
Magellanic Cloud by simultaneously analyzing light curves in 14 bands
in the range of 0.5-24µm. We model over 20yr long, high-cadence
I-band light curves collected by the Optical Gravitational Lensing
Experiment (OGLE) and fit them to light curves collected in the
remaining optical/near-infrared/mid-infrared bands to derive both the
variability amplitude ratio and phase lag as a function of wavelength.
We show that the variability amplitude ratio declines with increasing
wavelength for both oxygen-rich (O-rich) and carbon-rich (C-rich)
Miras, while the variability phase lag increases slightly with
increasing wavelength. In a significant number of Miras, mostly the
C-rich ones, the spectral energy distributions (SEDs) require the
presence of a cool component (dust) in order to match the mid-IR data.
Based on SED fits for a golden sample of 140 Miras, we calculated
synthetic period-luminosity relations (PLRs) in 42 bands for the
existing and future sky surveys that include OGLE, the VISTA
Near-Infrared YJKs Survey of the Magellanic Clouds System, Legacy
Survey of Space and Time, Gaia, Spitzer, the Wide-field Infrared
Survey Explorer, the James Webb Space Telescope, the Nancy Grace Roman
Space Telescope (formerly WFIRST), and the Hubble Space Telescope. We
show that the synthetic PLR slope decreases with increasing wavelength
for both the O-rich and C-rich Miras in the range of 0.1-40µm.
Finally, we show the location and motions of Miras on the
color-magnitude and color-color diagrams.
Description:
In this study, we used the sample of 1663 Miras discovered in the LMC
by the OGLE during the third phase of the project (OGLE-III
Udalski 2003AcA....53..291U 2003AcA....53..291U ; Soszynski+ 2005AcA....55..331S 2005AcA....55..331S and
2009, J/AcA/59/239). The authors discovered almost 100000 LPVs and
provided two-band light curves (I and V bands from the Johnson-Cousins
photometric system) spanning ∼13yr since 1996.
The OGLE-III phase ended in 2009. In 2010, the Warsaw telescope,
located at the Las Campanas Observatory, Chile, was equipped with a
32-chip CCD camera, which began the fourth phase of the Optical
Gravitational Lensing Experiment project (OGLE-IV;
Udalski+ 2015AcA....65....1U 2015AcA....65....1U). The monitoring of the southern sky
lasted until 2020 March 17.
In this paper, we revised the pulsation periods of Miras using the
full, two-decade-long light curves.
In our study, we also used measurements taken in the near-infrared Y
band (λeff=1.02um), J band (λeff=1.22um), and KS
band (λeff=2.19um) by the Near-Infrared YJKs Survey of the
Magellanic Clouds System (VMC; Cioni+ 2011, II/351).
We cross-matched the sample of LMC Miras with the Wide Field Infrared
Survey Explorer (WISE, see II/311). See Section 2.4.1.
Additionally, we retrieved data from Spitzer in the Surveying the
Agents of Galaxy's Evolution (SAGE; Meixner+ 2006, J/AJ/132/2268) IRAC
and MIPS. See Section 2.4.2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 28 400 Variability amplitude ratio R as a function of
wavelength for the O- and C-rich Miras
table2.dat 38 400 Phase-lag φ as a function of wavelength for
the O- and C-rich Miras
table3.dat 55 140 Bolometric luminosities of Miras from the
golden sample
table4.dat 32 400 Synthetic PLR slope a1 derived from the SED
analysis, as a function of wavelength, for
the O- and C-rich Miras
table5.dat 79 42 Parameters of synthetic PLRs for the O-rich Miras
table6.dat 79 42 Parameters of synthetic PLRs for the C-rich Miras
table7.dat 355 140 *Basic parameters of the golden sample Miras
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Note on table7.dat: We create 42 synthetic Period-Luminosity Relations (PLRs)
in frequently used filters in major present/future surveys. They
include V, I from OGLE; Y, J, and Ks from VMC (Cioni+ 2011, II/351);
G, Gbp , and Grp from Gaia; u, g, r, i, z, and y from the Legacy
Survey of Space and Time (LSST); F110W, F140W, and F160W from the
Hubble Space Telescope (HST); J129, H158, and F184 from the Nancy
Grace Roman Space Telescope (formerly WFIRST); F200W, F277W, F356W,
F444W, F560, F770W, F1000, F1130W, F1280, F1500W, F1800W, F2100W, and
F2550W from the James Webb Space Telescope (JWST); W1, W2, W3, and W4
(3.4, 4.6, 12, 22um) from WISE; and I1, I2, I3, I4, and M1 (3.6, 4.5,
5.8, 8.0, and 24um) from IRAC/MIPS Spitzer. The transmission curves
for all mentioned bands are presented in Figure 8. See Section 5.3
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
II/195 : Namelists of variable stars Nos.67-73 (Khopolov+, 1985-97)
II/305 : SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)
II/351 : VISTA Magellanic Survey (VMC) catalog (Cioni+, 2011)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
J/AcA/50/421 : OGLE-II DIA BUL_SC1 field (Wozniak, 2000)
J/AJ/132/2268 : SAGE calibration stars (Meixner+, 2006)
J/AJ/131/612 : Infrared-optical phase lags in AGB stars (Smith+, 2006)
J/MNRAS/369/751 : Near-infrared photometry of carbon stars (Whitelock+, 2006)
J/AcA/59/239 : VI LCs of LMC long-period variables (Soszynski+, 2009)
J/ApJ/723/1195 : SAGE AGB candidates (Riebel+, 2010)
J/AcA/61/217 : VI LCs of SMC long-period variables (Soszynski+, 2011)
J/ApJ/758/11 : Bayesian distances to M31 satellites (Conn+, 2012)
J/MNRAS/428/2216 : JHKs photometry of AGB stars in NGC 6822 (Whitelock+, 2013)
J/ApJ/792/30 : NEOWISE magnitudes for near-Earth objects (Mainzer+, 2014)
J/MNRAS/452/910 : IC 1613 asymptotic giant branch variables (Menzies+, 2015)
J/A+A/586/A49 : r- and s- process elements in MW disk (Battistini+, 2016)
J/AJ/152/164 : I-band light curves of OGLE LMC Miras (He+, 2016)
J/AJ/153/170 : The M33 Synoptic Stellar Survey. II. Miras (Yuan+, 2017)
J/ApJ/857/67 : HST obs. of Mira candidates in NGC 4258 (Huang+, 2018)
J/AJ/156/112 : NIR Mira period-luminosity relations in M33 (Yuan+, 2018)
J/ApJ/884/20 : OGLE-III Miras in Magellanic Clouds (Bhardwaj+, 2019)
J/ApJ/887/82 : Galactic carbon stars infrared spectroscopy (Kraemer+, 2019)
J/ApJS/247/44 : Mira-like variables from the KELT survey (Arnold+, 2020)
J/A+A/636/A48 : VMC Survey. XXXVII. MC AGB stars (Groenewegen+, 2020)
J/ApJ/889/5 : HST obs. of Miras in SNIa host NGC1559 (Huang+, 2020)
J/ApJS/252/23 : E(V-I) reddening map of MCs from OGLE-IV (Skowron+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 um lambda [0.1/40] Wavelength
6- 10 F5.3 --- RO [0.29/6.87] O-rich Miras mean variability
amplitude ratio (1)
12- 16 F5.3 --- e_RO [0/0.4] Boundary of calculated models
for O-rich Miras
18- 22 F5.3 --- RC [0.37/5.8] C-rich Miras mean variability
amplitude ratio (1)
24- 28 F5.3 --- e_RC [0/1.5] Boundary of calculated models
for C-rich Miras
--------------------------------------------------------------------------------
Note (1): The variability amplitude ratio R is defined as ratio between the
amplitude at wavelength lambda and the amplitude in I-band. Values
presented here represent the mean value of the variability amplitude
ratios obtained from the synthetic light curves (marked by solid
lines in Figure 2), while the band reflects the spread of calculated
models.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 um lambda [0.1/40] Wavelength
6- 13 F8.5 --- PhiO [-0.04/0.15] O-rich Miras mean phase-lag (1)
15- 21 F7.5 --- e_PhiO [0/0.091] Boundary of calculated models
for O-rich Miras
23- 30 F8.5 --- PhiC [-0.0062/0.018] C-rich Miras mean phase-lag (1)
32- 38 F7.5 --- e_PhiC [0/0.22] Boundary of calculated models
for C-rich Miras
--------------------------------------------------------------------------------
Note (1): The phase-lag phi is defined as a shift between a light curve at
wavelength lambda and the I-band light curve. Values presented here
represent the mean value of phase-lags obtained from the synthetic
light curves (marked by solid lines in Figure 3), while the band
reflects the spread of calculated models.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- ID OGLE-III Star ID (1)
20 A1 --- Type Surface chemistry type of Miras
(O=29 occurrences; C=111 occurrences) (1)
22- 26 I5 Lsun Lbol [796/50377] Total bolometric luminosity of Miras
28- 31 I4 Lsun e_Lbol [20/4046] Uncertainty in Lbol
33- 37 I5 Lsun Lbol* [59/46593] Bolometric luminosity of star
39- 43 I5 Lsun Lbold [0/42136] Bolometric luminosity of dust
45- 49 F5.3 --- fStar [0.018/1] Fraction of bolometric luminosity of
star to total bolometric luminosity (2)
51- 55 F5.3 --- fDust [0/0.99] Fraction of bolometric luminosity of
dust to total bolometric luminosity (2)
--------------------------------------------------------------------------------
Note (1): From the catalog of Soszynski+ 2009, J/AcA/59/239
Note (2): fStar+fDust=1.
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 F4.1 um lambda [0.1/40] Wavelength
6- 11 F6.3 mag a1O [-4.8/42.9] O-rich Miras slope of the synthetic
PLRs (1)
13- 18 F6.3 mag e_a1O [0.38/14] Uncertainty in a1O
20- 25 F6.3 mag a1C [-9.7/47.4] C-rich Miras slope of the synthetic
PLRs (1)
27- 32 F6.3 mag e_a1C [0.28/11.2] Uncertainty in a1C
--------------------------------------------------------------------------------
Note (1): The Period-Luminosity Relation (PLR) slope a1 from the
linear fit in a form m=a0+a1*(logP-2.3).
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Byte-by-byte Description of file: table[56].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 28 A28 --- Names Survey and filter names
30- 34 F5.2 um lambda [0.37/25.5] Wavelength
36- 41 F6.3 mag a0obs [10.5/21.7] Observational zero-point (1)
43- 47 F5.3 mag e_a0obs [0.03/0.8] Uncertainty in a0abs
49- 54 F6.3 mag a0abs [-7.9/3.2] Absolute zero-point (1)
56- 60 F5.3 mag e_a0abs [0.04/0.8] Uncertainty in a0abs (1)
62- 68 F7.3 mag a1 [-10.4/7.2] Slope (1)
70- 74 F5.3 mag e_a1 [0.3/3.4] Uncertainty in a1
76- 79 F4.2 mag RMS [0.19/3] Root mean square
--------------------------------------------------------------------------------
Note (1): The Period-Luminosity Relation (PLR) slope a1 from the
linear fit in a form m=a0+a1*(logP-2.3). We provide observational
(a0obs) and absolute (a0abs) zero-points calculated with the distance
modulus of 18.477mag (Pietrzynski+ 2009Natur.567..200P 2009Natur.567..200P).
The uncertainties of a0abs are a square root of a sum in quadrature
of the a0obs uncertainty, the statistical (0.09kpc), and
systematical (0.54kpc) LMC distance uncertainties.
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- ID OGLE-III Star ID (1)
20- 21 I2 h RAh [4/5] Hour of Right Ascension (J2000) (1)
23- 24 I2 min RAm Minute of Right Ascension (J2000) (1)
26- 30 F5.2 s RAs Second of Right Ascension (J2000) (1)
32 A1 --- DE- [-] Sign of the Declination (J2000) (1)
33- 34 I2 deg DEd [66/71] Degree of Declination (J2000) (1)
36- 37 I2 arcmin DEm Arcminute of Declination (J2000) (1)
39- 42 F4.1 arcsec DEs Arcsecond of Declination (J2000) (1)
44 A1 --- Type Surface chemistry type of Miras
(O=29 occurrences; C=111 occurrences) (1)
46- 51 F6.2 d Per [107.9/569.6] Pulsation period
53- 56 I4 K Tstar [1395/4462] Star's effective temperature
58- 61 I4 K Tdust [0/1729] Dust effective temperature (2)
63- 68 F6.3 mag umag [15.77/40.78] Synthetic LSST u (AB)
magnitude
70- 75 F6.3 mag gmag [13.25/31.44] Synthetic LSST g (AB)
magnitude
77- 82 F6.3 mag BPmag [12.28/27.63] Synthetic Gaia Gbp (Vega)
magnitude
84- 89 F6.3 mag Vmag [12.7/29.67] Synthetic OGLE V (Vega)
magnitude
91- 96 F6.3 mag rmag [11.89/26.3] Synthetic LSST r (AB)
magnitude
98- 103 F6.3 mag Gmag [10.98/22.04] Synthetic Gaia G (Vega)
magnitude
105- 110 F6.3 mag imag [11.13/23.11] Synthetic LSST i (AB)
magnitude
112- 117 F6.3 mag RPmag [10.47/21.02] Synthetic Gaia Grp (Vega)
magnitude
119- 124 F6.3 mag Imag [10.51/21.75] Synthetic OGLE I (Vega)
magnitude
126- 131 F6.3 mag zmag [10.69/21.07] Synthetic LSST z (AB)
magnitude
133- 138 F6.3 mag ymag [10.43/19.6] Synthetic LSST y (AB)
magnitude
140- 145 F6.3 mag Ymag [9.68/17.26] Synthetic VMC Y (Vega)
magnitude
147- 152 F6.3 mag F110Wmag [9.3/16.55] Synthetic HST WFC3IR F110W
(Vega) magnitude
154- 159 F6.3 mag Jmag [9.15/16] Synthetic VMC J (Vega) magnitude
161- 166 F6.3 mag J129mag [9.03/15.85] Synthetic WFIRST WFI J129
(Vega) magnitude
168- 173 F6.3 mag F140Wmag [8.84/15.57] Synthetic HST WFC3IR F140W
(Vega) magnitude
175- 180 F6.3 mag F160Wmag [8.63/15.27] Synthetic HST WFC3IR F160W
(Vega) magnitude
182- 187 F6.3 mag H158mag [8.59/15.2] Synthetic WFIRST WFI H158
(Vega) magnitude
189- 194 F6.3 mag F184mag [8.33/14.81] Synthetic WFIRST WFI F184
(Vega) magnitude
196- 201 F6.3 mag F200Wmag [8.21/14.65] Synthetic JWST NIRCam F200W
(Vega) magnitude
203- 208 F6.3 mag Ksmag [8.1/14.51] Synthetic VMC Ks (Vega)
magnitude
210- 215 F6.3 mag F277Wmag [7.38/13.71] Synthetic JWST NIRCam F277W
(Vega) magnitude
217- 222 F6.3 mag W1mag [7.69/13.96] Synthetic WISE W1 (3.4um)
(Vega) magnitude
224- 229 F6.3 mag F356Wmag [7.59/13.86] Synthetic JWST NIRCam F356W
(Vega) magnitude
231- 236 F6.3 mag 3.6mag [7.62/13.9] Synthetic Spitzer IRAC
I1 (3.6um) (Vega) magnitude
238- 243 F6.3 mag F444Wmag [7.41/13.65] Synthetic JWST NIRCam F444W
(Vega) magnitude
245- 250 F6.3 mag 4.5mag [7.43/13.67] Synthetic Spitzer IRAC
I2 (4.5um) (Vega) magnitude
252- 257 F6.3 mag W2mag [7.36/13.66] Synthetic WISE W2 (4.6um)
(Vega) magnitude
259- 264 F6.3 mag F560Wmag [6.89/13.53] Synthetic JWST MIRI F560W
(Vega) magnitude
266- 271 F6.3 mag 5.8mag [6.88/13.54] Synthetic Spitzer IRAC
I3 (5.8um) (Vega) magnitude
273- 278 F6.3 mag F770Wmag [6.17/13.36] Synthetic JWST MIRI F770W
(Vega) magnitude
280- 285 F6.3 mag 8.0mag [6.14/13.36] Synthetic Spitzer IRAC
I4 (8.0um) (Vega) magnitude
287- 292 F6.3 mag F1000Wmag [4.52/13.3] Synthetic JWST MIRI F1000W
(Vega) magnitude
294- 299 F6.3 mag F1130Wmag [3.73/13.3] Synthetic JWST MIRI F1130W
(Vega) magnitude
301- 306 F6.3 mag W3mag [3.36/13.31] Synthetic WISE W3 (12um)
(Vega) magnitude
308- 313 F6.3 mag F1280Wmag [3/13.23] Synthetic JWST MIRI F1280W
(Vega) magnitude
315- 320 F6.3 mag F1500Wmag [2.26/13.2] Synthetic JWST MIRI F1500W
(Vega) magnitude
322- 327 F6.3 mag F1800Wmag [1.59/13.15] Synthetic JWST MIRI F1800W
(Vega) magnitude
329- 334 F6.3 mag F2100Wmag [1.12/13.06] Synthetic JWST MIRI F2100W
(Vega) magnitude
336- 341 F6.3 mag W4mag [0.96/13.05] Synthetic WISE W4 (22um)
(Vega) magnitude
343- 348 F6.3 mag 24mag [0.76/13] Synthetic Spitzer MIPS
M1 (24um) (Vega) magnitude
350- 355 F6.3 mag F2550Wmag [0.6/12.91] Synthetic JWST MIRI F2550W
(Vega) magnitude
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Note (1): From the catalog of Soszynski+ 2009, J/AcA/59/239
( in Simbad).
Note (2): The Tdust for O-rich Miras are reported as 0 in the table, as SEDs
for these stars required only hotter components (for more details
see Section 5).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 18-Feb-2022