J/AJ/155/17 Infrared photometric study of Wolf-Rayet galaxies (Chen+, 2018)
Infrared photometric study of Wolf-Rayet galaxies.
Chen P.S., Yang X.H., Liu J.Y., Shan H.G.
<Astron. J., 155, 17 (2018)>
=2018AJ....155...17C 2018AJ....155...17C (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, infrared ; Redshifts ;
Extinction ; Photometry, millimetric/submm
Keywords: galaxies: photometry - infrared: galaxies
Abstract:
We collected observational data on 781 Wolf-Rayet (WR) galaxies from
the literature to photometrically study their infrared properties measured
by the 2MASS, WISE, IRAS, AKARI, and Herschel missions. It is found
that in the 1-5 µm range the radiations of WR galaxies are dominated
by the free-free emissions from the stellar winds and the circumstellar
dust from the late-type stars in the host galaxy. In the 5-22 µm range,
the radiation of WR galaxies is dominated by the free-free emissions
and the synchrotron radiation from the central active galactic nucleus
(AGN; but not always present). In the 22-140 µm range, the radiations
of WR galaxies are dominated by the free-free emissions and the star
formation/starburst activities. In the 250-500 µm range, the radiation
of WR galaxies is dominated by the free-free emissions. In addition,
the comparison with the non-WR galaxies is made. It is shown that some
star formation WR galaxies have redder near-infrared colors than non-WR
star-forming galaxies probably due to the gas emission in the
near-infrared. In the 2-5 µm region WR galaxies have redder colors
due to the thermal emission from circumstellar dust of late-type stars
and the enhanced gas emission. In the 5-22 µm region, both WR galaxies
and non-WR galaxies have similar behavior, indicative of having similar
free-free emission as the dominant radiation. In the 25-140 µm region,
both types of galaxies also have similar behavior, indicative of having
free-free emission from the stellar winds or the thermal radiation
from the starburst/star formation as the dominant radiation.
Description:
In this paper, by using 2MASS, WISE, IRAS, AKARI FIS, and Herschel
(APCS and SPIRE) data, we can systematically investigate WR galaxies
photometrically from 1 to 500 µm to outline their properties and
radiation mechanisms in the infrared and submillimeter regions.
We have collected almost all WR galaxies from the literature up to date
in order to construct our sample. The main resources of WR galaxies are
from Conti (1991ApJ...377..115C 1991ApJ...377..115C), Schaerer et al. (1999A&A...341..399S 1999A&A...341..399S),
Kniazev et al. (2004, J/ApJS/153/429), Zhang et al. (2007, J/ApJ/655/851),
Brinchmann et al. (2008, J/A+A/485/657), and Shirazi & Brinchmann (2012,
J/MNRAS/421/1043). Other WR galaxies are from what we listed in the
Table 1. Finally, 781 WR galaxies are found, which are listed in Table 1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 184 781 Infrared photometric observation of Wolf-Rayet
galaxies
table2.dat 47 140 IRAS observation of WR galaxies
table3.dat 38 41 AKARI observation of WR galaxies
table4.dat 49 13 Herschel PACS and SPIRE observations of
WR galaxies
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
II/298 : AKARI/FIS All-Sky Survey Point Source Catalogues (ISAS/JAXA, 2010)
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
VIII/103 : Herschel Multi-tiered Extragalactic Survey (Oliver+, 2012)
J/A+AS/136/35 : WR galaxies and HII regions catalog (Schaerer+ 1999)
J/A+A/426/399 : HST photometry of brightest stars of NGC 588 (Jamet+, 2004)
J/ApJS/153/429 : SDSS strong emission line HII galaxies (Kniazev+, 2004)
J/ApJ/655/851 : Wolf-Rayet galaxies in the SDSS (Zhang+, 2007)
J/A+A/485/657 : Physical parameters of Wolf-Rayet galaxies
(Brinchmann+, 2008)
J/MNRAS/421/1043 : Emission-line galaxies from SDSS DR7 (Shirazi+, 2012)
J/MNRAS/428/1880 : Far-IR properties of VCC galaxies (Auld+, 2013)
J/A+A/574/A126 : HeViCS. XVIII. Star-forming dwarf galaxies (Grossi+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Num [1/781] Galaxy index number
5- 28 A24 --- Name Galaxy identifier
30- 31 I2 h RAh Hour of Right Ascension (J2000)
33- 34 I2 min RAm Minute of Right Ascension (J2000)
36- 40 F5.2 s RAs Second of Right Ascension (J2000)
42 A1 --- DE- Sign of the Declination (J2000)
43- 44 I2 deg DEd Degree of Declination (J2000)
46- 47 I2 arcmin DEm Arcminute of Declination (J2000)
49- 52 F4.1 arcsec DEs Arcsecond of Declination (J2000)
54- 61 F8.5 --- z [-0.00146/0.2809]? Spectroscopic redshift
63- 66 A4 --- BPT BPT type (G1)
68- 73 F6.3 mag W1mag [5.715/17.236] WISE 3.4 micron band magnitude
75- 79 F5.3 mag e_W1mag [0.019/0.366] Uncertainty in W1mag
81 A1 --- l_W2mag [<] Limit flag on W2mag
82- 87 F6.3 mag W2mag [5.194/16.901] WISE 4.6 micron band magnitude (1)
89- 93 F5.3 mag e_W2mag [0.018/0.472]? Uncertainty in W2mag
95 A1 --- l_W3mag [<] Limit flag on W3mag
96-101 F6.3 mag W3mag [2.598/12.803] WISE 12 micron band magnitude (1)
103-107 F5.3 mag e_W3mag [0.009/0.429]? Uncertainty in W3mag
109 A1 --- l_W4mag [<] Limit flag on W4mag
110-115 F6.3 mag W4mag [-0.722/9.476] WISE 22 micron band magnitude (1)
117-121 F5.3 mag e_W4mag [0.01/0.543]? Uncertainty in W4mag
123 A1 --- l_Jmag [<] Limit flag on Jmag
124-129 F6.3 mag Jmag [0.0/17.129]? 2MASS J band magnitude (1)
131-135 F5.3 mag e_Jmag [0.029/0.245]? Uncertainty in Jmag
137 A1 --- l_Hmag [<] Limit flag on Hmag
138-143 F6.3 mag Hmag [9.665/17.023]? 2MASS H band magnitude (1)
145-149 F5.3 mag e_Hmag [0.027/0.465]? Uncertainty in Hmag
151 A1 --- l_Ksmag [<] Limit flag on Ksmag
152-157 F6.3 mag Ksmag [8.847/16.427]? 2MASS Ks band magnitude (1)
159-163 F5.3 mag e_Ksmag [0.025/0.32]? Uncertainty in Ksmag
165-169 F5.3 mag AV [0.01/2.547]? The V band extinction
171-181 A11 --- IRAS IRAS PSC/FSC name (Cat. II/125, II/156)
183-184 I2 --- Ref [1/15] Reference number for the origin of
the WR galaxy (2)
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Note (1): The upper limit value and the related magnitude is not used for any
analyses.
Note (2): Reference as follows:
1 = Schaerer et al. (1999A&A...341..399S 1999A&A...341..399S);
2 = Zhang et al. (2007, J/ApJ/655/851);
3 = Brinchmann et al. (2008, J/A+A/485/657);
4 = Stevens & Strickland (1998MNRAS.301..215S 1998MNRAS.301..215S);
5 = Mendez & Esteban (2000A&A...359..493M 2000A&A...359..493M);
6 = Guseva et al. (2000ApJ...531..776G 2000ApJ...531..776G);
7 = Lopez-Sanchez & Esteban (2008A&A...491..131L 2008A&A...491..131L);
8 = Shirazi & Brinchmann (2012, J/MNRAS/421/1043);
9 = Kniazev et al. (2004, J/ApJS/153/429);
10 = Popescu & Hopp (2000A&AS..142..247P 2000A&AS..142..247P);
11 = Gonzalez-Delgado et al. (2001ApJ...546..845G 2001ApJ...546..845G);
12 = Pindao et al. (2002A&A...394..443P 2002A&A...394..443P);
13 = Fernandes et al. (2004MNRAS.355..728F 2004MNRAS.355..728F);
14 = Jamet et al. (2004, J/A+A/426/399);
15 = Miralles-Caballero et al. (2016A&A...592A.105M 2016A&A...592A.105M).
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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- 3 I3 --- Num [21/773] Galaxy index number (1)
5- 8 A4 --- BPT BPT type (G1)
10- 20 A11 --- IRAS IRAS PSC/FSC name (Cat. II/125, II/156)
22- 29 E8.3 Jy F25 [0.072/21.5] IRAS 25µm flux density
31- 38 E8.3 Jy F60 [0.198/172] IRAS 60µm flux density
40- 47 E8.3 Jy F100 [0.48/338] IRAS 100µm flux density
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Note (1): Only objects with good data in three IRAS bands are shown.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Num [39/772] Galaxy index number (1)
5- 8 A4 --- BPT BPT type (G1)
10- 18 E9.4 Jy F65 [2.313/135.8] AKARI 65µm flux density
20- 28 E9.4 Jy F90 [2.921/88.83] AKARI 90µm flux density
30- 38 E9.4 Jy F140 [3.44/63.81] AKARI 140µm flux density
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Note (1): Only objects with good data in three AKARI bands are shown.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Num [223/739] Galaxy index number (1)
5- 8 A4 --- BPT BPT type (G1)
10- 15 F6.3 Jy F250 [0.105/69.484] Herschel/SPIRE 250µm flux
density
17- 21 F5.3 Jy e_F250 [0.003/4.879] Uncertainty in F250
23- 28 F6.3 Jy F350 [0.039/28.853] Herschel/SPIRE 350µm flux
density
30- 34 F5.3 Jy e_F350 [0.003/2.044] Uncertainty in F350
36- 41 F6.3 Jy F500 [0.025/10.144] Herschel/SPIRE 500µm flux
density
43- 47 F5.3 Jy e_F500 [0.004/0.733] Uncertainty in F500
49 I1 --- Ref [1/3] Reference (2)
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Note (1): Only objects with good data in three Herschel bands (250, 350, and
500 micron) are shown.
Note (2): Reference as follows:
1 = Oliver et al. (2012MNRAS.424.1614O 2012MNRAS.424.1614O);
2 = Auld et al. (2013, J/MNRAS/428/1880);
3 = Grossi et al. (2015, J/A+A/574/A126).
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Global notes:
Note (G1): From Brinchmann et al. (2008, J/A+A/485/657), Shirazi & Brinchmann
(2012, J/MNRAS/421/1043) or the Simbad database.
The BPT class is determined on the basis of the Baldwin, Phillips & Terlevich
(1981PASP...93....5B 1981PASP...93....5B) excitation diagram, as follows:
SF = Star-Forming galaxies;
Comp = Composite galaxies, intermediate between the SF and AG classes;
AGN = Active Galaxy Nuclei class;
Uncl = Unclassified.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 12-Sep-2018