J/ApJS/252/21 Multiwavelength survey of WR stars in LMC (Hung+, 2021)
A multiwavelength survey of Wolf-Rayet nebulae in the Large Magellanic Cloud.
Hung C.S., Ou P.-S., Chu Y.-H., Gruendl R.A., Li C.-J.
<Astrophys. J. Suppl. Ser., 252, 21 (2021)>
=2021ApJS..252...21H 2021ApJS..252...21H
ADC_Keywords: Stars, Wolf-Rayet; Interstellar medium; Magellanic Clouds;
Cross identifications; H I data
Keywords: Wolf-Rayet stars ; Stellar wind bubbles ; Interstellar medium ;
Large Magellanic Cloud
Abstract:
Surveys of Wolf-Rayet (WR) stars in the Large Magellanic Cloud (LMC)
have yielded a fairly complete catalog of 154 known stars. We have
conducted a comprehensive, multiwavelength study of the
interstellar/circumstellar environments of WR stars, using the
Magellanic Cloud Emission Line Survey images in the Hα, [OIII],
and [SII] lines; Spitzer Space Telescope 8 and 24µm images; Blanco
4m Telescope Hα CCD images; and Australian Telescope Compact
Array + Parkes Telescope HI data cube of the LMC. We have also
examined whether the WR stars are in OB associations, classified the
HII environments of WR stars, and used this information to
qualitatively assess the WR stars' evolutionary stages. The 30 Dor
giant HII region has active star formation and hosts young massive
clusters, thus we have made statistical analyses for 30 Dor and the
rest of the LMC both separately and altogether. Due to the presence of
massive young clusters, the WR population in 30 Dor is quite different
from that from elsewhere in the LMC. We find small bubbles (<50pc
diameter) around ∼12% of WR stars in the LMC, most of which are WN
stars and not in OB associations. The scarcity of small WR bubbles is
discussed. Spectroscopic analyses of abundances are needed to
determine whether the small WR bubbles contain interstellar medium or
circumstellar medium. Implications of the statistics of interstellar
environments and OB associations around WR stars are discussed.
Multiwavelength images of each LMC WR star are presented.
Description:
We have used multiwavelength images to examine the ionized and neutral
gaseous environments of the LMC Wolf-Rayet (WR) stars.
The UM/CTIO Magellanic Cloud Emission-line Survey (MCELS) is an
emission-line survey of the Magellanic Clouds (Smith & MCELS Team
1999IAUS..190...28S 1999IAUS..190...28S). The survey used the Curtis Schmidt Telescope at
Cerro Tololo Inter-American Observatory (CTIO) and a CCD camera to
take images in the Hα, [OIII]5007, and [SII]6716,6731 bands, as
well as two continuum bands centered at λ6850 and λ5130.
In this paper, we only used the emission-line images without continuum
subtraction.
A higher-resolution Hα survey of the Magellanic Clouds has been
conducted with the MOSAIC II camera on the Blanco 4m Telescope at
CTIO; this survey has been called MCELS2 (PI: You-Hua Chu).
In celebration of the 30yr anniversary of the Hubble Space Telescope
(HST), a public release of an HST Hα image of NGC 2020 became
available, and this image is used for WR 71.
The HI 21cm data cube was constructed by Kim+ (2003ApJS..148..473K 2003ApJS..148..473K)
using the ATCA survey data in conjunction with single-dish observations
from the Parkes Telescope.
The Spitzer Space Telescope Infrared Array Camera (IRAC) 8um images
are used to identify polycyclic aromatic hydrocarbons associated with
partially dissociated regions, and the Multiband Imaging Photometer
for Spitzer (MIPS) 24um images to reveal emission from heated dust.
The Spitzer images of the LMC were from the Legacy Program Surveying
the Agents of a Galaxy's Evolution (SAGE; Meixner+ 2006, J/AJ/132/2268).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 117 154 LMC Wolf-Rayet (WR) stars and their stellar and
interstellar environments
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
VII/232 : Nebulae in the Magellanic Clouds (Davies+ 1976)
J/ApJ/448/179 : HST photometry in R136 (Hunter+ 1995)
J/AJ/132/2268 : SAGE calibration stars (Meixner+, 2006)
J/AJ/138/1003 : IR photometry of massive LMC stars (Bonanos+, 2009)
J/A+A/565/A27 : Wolf-Rayet stars in Large Magellanic Cloud (Hainich+, 2014)
J/A+A/585/A162 : X-ray supernova remnants in LMC (Maggi+, 2016)
J/ApJ/863/181 : The fifth catalog of LMC Wolf-Rayet stars (Neugent+, 2018)
J/AJ/158/192 : He II emission from WR stars in MW & LMC (Leitherer+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/154] Running sequence number of the WR star
in Neugent+ 2018, J/ApJ/863/181
5- 6 I2 h RAh Hour of right ascension (J2000)
8- 9 I2 min RAm Minute of right ascension (J2000)
11- 15 F5.2 s RAs Second of right ascension (J2000)
17 A1 --- DE- Sign of declination (J2000)
18- 19 I2 deg DEd Degree of declination (J2000)
21- 22 I2 arcmin DEm Arcminute of declination (J2000)
24- 27 F4.1 arcsec DEs Arcsecond of declination (J2000)
29- 31 A3 --- BAT99 ID from Breysacher+ (1999A&AS..137..117B 1999A&AS..137..117B)
33- 35 A3 --- Brey ID from Breysacher (1981A&AS...43..203B 1981A&AS...43..203B)
37- 53 A17 --- SpT Spectral type from Neugent+ 2018, J/ApJ/863/181
55- 65 A11 --- LH Host OB association from
Lucke & Hodge (1970AJ.....75..171L 1970AJ.....75..171L) (1)
67- 70 A4 --- LHA Associated HII regions from
Henize (1956ApJS....2..315H 1956ApJS....2..315H ;
in Simbad)
72- 75 A4 --- DEML Associated HII regions from
Davies+ (1976MmRAS..81...89D 1976MmRAS..81...89D)
77- 81 A5 --- Morph HII morphology classification
82 A1 --- u_Morph Uncertainty flag on Morph
84- 90 A7 arcmin Buble Dimensions of any bubble associated
with the WR star
91 A1 --- u_Buble Uncertainty flag on Buble
93- 101 A9 arcmin SBuble Dimensions of any superbubble associated
with the WR star
102 A1 --- u_SBuble Uncertainty flag on Buble
104- 107 A4 --- LMC HII supergiant shells from
Meaburn (1980MNRAS.192..365M 1980MNRAS.192..365M ;
<LMC-SGS N> in Simbad)
109- 117 A9 --- [KDS99] HI giant and supergiant shells from
Kim+ (1999AJ....118.2797K 1999AJ....118.2797K ; GS= giant shell,
SGS = supergiant shell)
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Note (1): Single parentheses mark WR stars not in the OB association but are
within 50pc and double parentheses denote WR stars beyond 50pc but
within 100pc to the center.
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History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 22-Apr-2021