J/ApJ/927/89 NIR light curves of type II Cepheids (Wielgorski+, 2022)
An absolute calibration of the near-infrared period-luminosity relations of
type II Cepheids in the Milky Way and in the Large Magellanic Cloud.
Wielgorski P., Pietrzynski G., Pilecki B., Gieren W., Zgirski B.,
Gorski M., Hajdu G., Narloch W., Karczmarek P., Smolec R., Kervella P.,
Storm J., Gallenne A., Breuval L., Lewis M., Kaluszynski M., Graczyk D.,
Pych W., Suchomska K., Taormina M., Rojas Garcia G., Kotek A., Chini R.,
Pozo Nunez F., Noroozi S., Sobrino Figaredo C., Haas M., Hodapp K.,
Mikolajczyk P., Kotysz K., Mozdzierski D., Kolaczek-Szymanski P.
<Astrophys. J., 927, 89 (2022)>
=2022ApJ...927...89W 2022ApJ...927...89W
ADC_Keywords: Stars, variable; Photometry, infrared; Milky Way; Extinction;
Magellanic Clouds; Parallaxes, trigonometric; Abundances, [Fe/H]
Keywords: Type II Cepheid variable stars ; Pulsating variable stars ;
Large Magellanic Cloud ; Milky Way Galaxy ; Distance indicators ;
Galaxy distances ; Stellar distance ;
Population II Cepheid variable stars ; Population II stars
Abstract:
We present time-series photometry of 21 nearby type II Cepheids in the
near-infrared J, H, and Ks passbands. We use this photometry, together
with the Third Gaia Early Data Release parallaxes, to determine for
the first time period-luminosity relations (PLRs) for type II Cepheids
from field representatives of these old pulsating stars in the
near-infrared regime. We found PLRs to be very narrow for BL Herculis
stars, which makes them candidates for precision distance indicators.
We then use archival photometry and the most accurate distance
obtained from eclipsing binaries to recalibrate PLRs for type II
Cepheids in the Large Magellanic Cloud (LMC). Slopes of our PLRs in
the Milky Way and in the LMC differ by slightly more than 2σ and
are in a good agreement with previous studies of the LMC, Galactic
bulge, and Galactic globular cluster type II Cepheids samples. We use
PLRs of Milky Way type II Cepheids to measure the distance to the LMC,
and we obtain a distance modulus of
18.540±0.026(stat.)±0.034(syst.)mag in the WJK Wesenheit index.
We also investigate the metallicity effect within our Milky Way
sample, and we find a rather significant value of about -0.2mag/dex in
each band meaning that more metal-rich type II Cepheids are
intrinsically brighter than their more metal-poor counterparts, in
agreement with the value obtained from type II Cepheids in Galactic
globular clusters. The main source of systematic error on our Milky
Way PLRs calibration, and the LMC distance, is the current uncertainty
of the Gaia parallax zero-point.
Description:
Observations were handled between 2017 February and 2020 March using
the 0.81m InfraRed Imaging Survey (IRIS) telescope equipped with 1kx1k
HAWAII detector (resulting in 7'x7' field of view), located in
Observatorio Cerro Armazones (OCA) in Chile.
For 3 bright type II Cepheids (T2Ceps) --κ Pav, V553 Cen, and
SW Tau-- archival infrared photometry collected at the South African
Astronomical Observatory (SAAO) with the MkII photometer installed on
the 0.75m telescope is available (Feast+ 2008, J/MNRAS/386/2115). We
transform these photometric data to the 2MASS system using formulae
from Koen+ (2007MNRAS.380.1433K 2007MNRAS.380.1433K).
The most complete list of T2Ceps in the LMC is the OGLE catalog
(Soszynski+ 2018, J/AcA/68/89), so we adopt classification and periods
from this source. Infrared photometry from several sources is
available. We preferentially use mean magnitudes determined from
time-series photometry over the single-point measurement.
See Section 2.2.1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 44 1523 Near infrared photometry of Milky Way T2Ceps
table2.dat 116 21 Data of Milky Way T2Ceps
table3.dat 102 128 Data of T2Ceps in the LMC
table9.dat 57 21 Parallax zero point offset (ZPO) determined using
the procedure from Groenewegen (2021A&A...654A..20G 2021A&A...654A..20G)
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See also:
II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
II/288 : IRSF Magellanic Clouds Point Source Catalog (Kato+ 2007)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/AJ/123/789 : ARAUCARIA project: NGC 300 Cepheids (Pietrzynski+, 2002)
J/MNRAS/370/1979 : JHKs photometry of T2Cs in GCs (Matsunaga+, 2006)
J/MNRAS/386/2115 : Type II Cepheid and RR Lyrae variables (Feast+, 2008)
J/AcA/58/293 : Type-II and anomalous Cepheids in LMC (Soszynski+, 2008)
J/MNRAS/397/933 : LMC type II Cepheids JHKs magnitudes (Matsunaga+, 2009)
J/AJ/139/2300 : BVIc light curves of 3 type II Cepheids (Rabidoux+, 2010)
J/AJ/142/187 : HST obs. of 7 Pop.II variable stars (Benedict+, 2011)
J/A+A/526/A116 : W Virginis high-resolution spectra (Kovtyukh+, 2011)
J/MNRAS/413/223 : Magellanic clouds Cepheids JHKs phot. (Matsunaga+, 2011)
J/AcA/61/285 : VI LCs of Galactic Bulge Cepheids (Soszynski+, 2011)
J/MNRAS/446/3034 : LMC Type II Cepheids J and Ks light curves (Ripepi+, 2015)
J/AJ/153/154 : LMC NIR survey. IV. Type II Cepheids (Bhardwaj+, 2017)
J/A+A/605/A100 : VVV survey Galactic Bulge Pop. II Cepheids (Bhardwaj+, 2017)
J/A+A/603/A70 : Type II and anomalous Ce* luminosities (Groenewegen+, 2017)
J/AcA/67/297 : OGLE Galactic center Cepheids & RR Lyrae (Soszynski+, 2017)
J/A+A/619/A51 : Type II Cepheids in the Galactic bulge (Braga+, 2018)
J/A+A/620/A99 : SMC Cepheids K-band and RV curves (Gieren+, 2018)
J/ApJ/868/30 : OGLE LMC-T2CEP-211 EBs LCs and RVs (Pilecki+, 2018)
J/AcA/68/89 : VI light curves of SMC type II Cepheids (Soszynski+, 2018)
J/A+A/625/A14 : Reclassification of Cepheids in the Gaia DR2 (Ripepi+, 2019)
J/ApJ/913/38 : Compilation of Cepheids in the MW and MCs (Breuval+, 2021)
J/A+A/654/A20 : Plx zero-point offset from Gaia EDR3 (Groenewegen, 2021)
J/MNRAS/508/4047 : Classical Cepheids HARPSN@TNG spectroscopy (Ripepi+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
11- 12 A2 --- Filt Filter (J, H or Ks)
14- 26 F13.5 d HJD Heliocentric Julian date of observation
28- 33 F6.3 mag omag [2.7/11.5] Observed magnitude in Filt
35- 39 F5.3 mag e_omag [0.01/0.2] Uncertainty in omag
41- 44 A4 --- Source Source ("IRIS" or "SAAO")
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
13- 20 F8.5 d Per [1/20] Period (1)
22- 27 F6.4 mas plx [0.2/5.3] Gaia EDR3 parallax
29- 34 F6.4 mas e_plx [0.013/0.13] Uncertainty in plx
36- 42 F7.4 mas ZPO [-0.03/0.005] Parallax zero point offset
44- 47 F4.2 --- RUWE [0.89/2.3] Gaia EDR3 Renormalised Unit Weight
Error
49- 53 F5.2 --- GOF [-3.6/37.6] Gaia EDR3 Goodness Of Fit
55- 60 F6.3 mag mumag [6.4/13.4] Distance modulus
62- 66 F5.3 mag e_mumag [0.01/0.3] Uncertainty in mumag
68- 73 F6.3 mag Jmag [3.2/11.4] Mean J-band magnitude
75- 79 F5.3 mag e_Jmag [0.007/0.04] Uncertainty in Jmag
81- 86 F6.3 mag Hmag [2.88/11.1]? Mean H-band magnitude
88- 92 F5.3 mag e_Hmag [0.007/0.06]? Uncertainty in Hmag
94- 99 F6.3 mag Ksmag [2.78/11] Mean Ks-band magnitude
101-105 F5.3 mag e_Ksmag [0.008/0.05] Uncertainty in Ksmag
107-111 F5.3 mag E(B-V) [0.019/0.4] B-V color excess (2)
113-116 F4.1 [-] [Fe/H] [-1/0.5]? Metallicity
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Note (1): Periods available from AAVSO and modified to produce the smoothest
light curves.
Note (2): E(B-V) values from Schlafly & Finkbeiner (2011ApJ...737..103S 2011ApJ...737..103S) map
corrected per the process found in Suchomska et al. (2015MNRAS.451..651S 2015MNRAS.451..651S).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- OGLE OGLE identifier, OGLE-LMC-T2CEP-###
20- 29 F10.7 d Per [1/17.2] Period (1)
31- 37 F7.3 mag Jmag [15/18]?=-99.99 Mean J-band magnitude (2)
39- 45 F7.3 mag e_Jmag [0.003/0.1]?=-99.99 Uncertainty in Jmag (2)
47- 53 F7.3 mag Hmag1 [14.5/17]?=-99.99 Mean LMCSS H-band magnitude (3)
55- 61 F7.3 mag e_Hmag1 [0.027/0.2]?=-99.99 Uncertainty in Hmag1 (3)
63- 68 F6.3 mag Hmag2 [13.96/18.1]?=-99.99 Mean IRSF H-band
magnitude (4)
70- 73 F4.2 mag e_Hmag2 [0.01/0.2]?=-99.99 Uncertainty in Hmag2 (4)
75- 81 F7.3 mag Kmag [14.5/17.5]?=-99.99 Mean K-band magnitude (2)
83- 89 F7.3 mag e_Kmag [0.004/0.07]?=-99.99 Uncertainty in Kmag (2)
91- 95 F5.3 mag E(B-V) [0.089/0.3] B-V color excess (5)
97-102 F6.3 mag Corr [-0.04/0.05] Geometric correction
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Note (1): Periods from OGLE catalogue
Note (2): Mean magnitudes from Ripepi+ (2015, J/MNRAS/446/3034) transformed
to the 2MASS system
Note (3): Mean magnitudes from Bhardwaj+ (2017, J/AJ/153/154)
Note (4): Mean magnitudes from Matsunaga+ (2009, J/MNRAS/397/933) transformed
to the 2MASS system
Note (5): E(B-V) from maps in Gorski+ (2020ApJ...889..179G 2020ApJ...889..179G)
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Name (1)
13- 31 I19 --- GaiaEDR3 ? Gaia EDR3 identifier
33- 33 I1 --- Pix [0/2]? HEALPix level pixel value (3)
35- 40 F6.3 mas ZPO-TW [-0.04/-0.01] Parallax zero point offset
(mean=-0.026)
42- 42 A1 --- f_ZPO-TW a = spatial correction only
45- 49 F5.3 mas e_ZPO-TW [0.003/0.007]? Uncertainty in ZPO-TW
51- 57 F7.4 mas ZPO-L21 [-0.024/0.005] ZPO
from Lindegren+ 2021A&A...649A...4L 2021A&A...649A...4L
(mean=-0.013)
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Note (1): The last row contains the mean ZPO for this work and L21
(Lindegren+ 2021A&A...649A...4L 2021A&A...649A...4L)
Note (3): HEALPix level defines the resolution of the used ZPO map
(for details see Groenewegen (2021, J/A+A/654/A20).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Jan-2024