J/PASJ/71/6 Galactic infrared bubbles (Hanaoka+, 2019)
A systematic study of Galactic infrared bubbles along the Galactic plane with
AKARI and Herschel.
Hanaoka M., Kaneda H., Suzuki T., Kokusho T., Oyabu S., Ishihara D.,
Kohno M., Furuta T., Tsuchikawa T., Saito F.
<Publ. Astron. Soc. Jap., 71, 6 (2019)>
=2019PASJ...71....6H 2019PASJ...71....6H (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Galactic plane ; Photometry, infrared
Keywords: infrared: ISM - stars: formation - stars: massive - ISM: bubbles
Abstract:
Galactic infrared (IR) bubbles, which have shell-like structures in
the mid-IR wavelengths, are known to contain massive stars near their
centers. Infrared bubbles in inner Galactic regions (|l|≤65°,
|b|≤1°) have so far been studied well to understand the massive
star formation mechanisms. In this study, we expand the research area
to the whole Galactic plane (0°≤l<360°, |b|≤5°), using
the AKARI all-sky survey data. We limit our study to large bubbles
with angular radii of >1' to reliably identify and characterize
them. For the 247 IR bubbles in total, we derived the radii and the
covering fractions of the shells, based on the method developed by Y.
Hattori et al. (2016PASJ...68...37H 2016PASJ...68...37H). We also created their spectral
energy distributions, using the AKARI and Herschel photometric data,
and decomposed them with a dust model to obtain the total IR
luminosity and the luminosity of each dust component, i.e., polycyclic
aromatic hydrocarbons (PAHs), warm dust, and cold dust. As a result,
we find that there are systematic differences in the IR properties of
the bubbles between the inner and outer Galactic regions. The total IR
luminosities are lower in outer Galactic regions, while there is no
systematic difference in the range of the shell radii between inner
and outer Galactic regions. More IR bubbles tend to be observed as
broken bubbles rather than closed ones and the fractional luminosities
of the PAH emission are significantly higher in outer Galactic
regions. We discuss the implications of these results for the massive
stars and the interstellar environments associated with the Galactic
IR bubbles.
Description:
We searched for new IR bubbles in outer Galactic regions (|l|>65°,
|b|≤5°) and high-latitude inner Galactic regions (|l|≤65°
1°<|b|≤ 5°) using the AKARI all-sky survey data in the mid-IR
wavelengths (central wavelengths 9um and 18um)
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 70 319 Summary of the central positions, radii, distances,
and covering fractions of the IR bubbles
table3.dat 173 319 *Summary of the aperture-corrected flux densities of
the IR bubbles obtained by aperture photometry
table4.dat 48 288 Summary of the luminosities of the IR bubbles
obtained by the SED fitting
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Note on table3.dat: We considered random and systematic errors as flux
uncertainties (see text for details).
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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- 5 A5 --- Name Name
6- 12 F7.3 deg GLON Galactic longitude
14- 19 F6.3 deg GLAT Galactic latitude
21- 25 F5.2 arcmin Rad Radius
27- 30 F4.1 kpc Dist ?=- Distance
32- 34 F3.1 kpc e_Dist ? rms uncertainty in Dist
35 A1 --- n_Dist [+] + when the nearer kinematic distance
is adopted
37- 49 A13 --- r_Dist Distance reference (1)
52- 55 F4.1 kpc DGal ?=- Galactocentric distance
57- 59 F3.1 kpc e_DGal ? rms uncertainty on galactocentric distance
61- 65 F5.2 pc R ?=- Linear radius
67- 70 F4.2 --- CF Covering fraction
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Note (1): References as follows:
Beaumont+10 = Beaumont and Williams (2010ApJ...709..791B 2010ApJ...709..791B)
Churchwell+06 = Churchwell et al. (2006, Cat. J/ApJ/649/759)
Churchwell+07 = Churchwell et al. (2007, Cat. J/ApJ/670/428)
Deharveng+09 = Deharveng et al. (2009, Cat. J/A+A/496/177)
Deharveng+10 = Deharveng et al. (2010A&A...523A...6D 2010A&A...523A...6D)
Dewangan+15 = Dewangan et al. (2015MNRAS.446.2640D 2015MNRAS.446.2640D)
Gennaro+12 = Gennaro et al. (2012A&A...542A..74G 2012A&A...542A..74G)
Hou&Gao+14 = Hou and Gao (2014, Cat. J/MNRAS/438/426)
Hou&Han+14 = Hou and Han (2014, Cat. J/A+A/569/A125)
Pavel+12 = Pavel and Clemens (2012ApJ...760..150P 2012ApJ...760..150P)
Rahman+10 = Rahman and Murray (2010, Cat. J/ApJ/719/1104)
Rodriguez+12 = Rodriguez-Esnard, Trinidad, and Migenes (2012ApJ...761..158R 2012ApJ...761..158R)
Watson+09 = Watson et al. (2009, Cat. J/ApJ/694/546)
Watson+10 = Watson, Hanspal, and Mengistu (2010ApJ...716.1478W 2010ApJ...716.1478W)
Zhang+13 = Zhang, Wang, and Xu (2013A&A...550A.117Z 2013A&A...550A.117Z)
For Orion, Perseus, and Sagittarius, the distance is estimated by
assuming the IR bubble is located on each Galactic spiral arm.
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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- 5 A5 --- Name Name
7- 13 E7.3 Jy F9um AKARI IRC flux at 9um
15- 20 E6.3 Jy e_F9um AKARI IRC flux at 9um error
22- 28 E7.3 Jy F18um AKARI IRC flux at 18um
30- 35 E6.3 Jy e_F18um AKARI IRC flux at 18um error
37- 43 E7.3 Jy F65um AKARI FIS flux at 65um
45- 50 E6.3 Jy e_F65um AKARI FIS flux at 65um error
52- 58 E7.3 Jy F90um AKARI FIS flux at 90um
60- 65 E6.3 Jy e_F90um AKARI FIS flux at 90um error
67- 73 E7.3 Jy F140um AKARI FIS flux at 140um
75- 80 E6.3 Jy e_F140um AKARI FIS flux at 140um error
82- 88 E7.3 Jy F160umA AKARI FIS flux at 160um
90- 95 E6.3 Jy e_F160umA AKARI FIS flux at 160um error
97-103 E7.3 Jy F70um ?=- Herschel PACS flux at 70um
105-110 E6.3 Jy e_F70um ?=- Herschel PACS flux at 70um error
112-118 E7.3 Jy F160umH ?=- Herschel PACS flux at 160um
120-125 E6.3 Jy e_F160umH ?=- Herschel PACS flux at 160um error
127-133 E7.3 Jy F250um ?=- Herschel SPIRE flux at 250um
135-140 E6.3 Jy e_F250um ?=- Herschel SPIRE flux at 250um error
142-148 E7.3 Jy F350um ?=- Herschel SPIRE flux at 350um
150-155 E6.3 Jy e_F350um ?=- Herschel SPIRE flux at 350um error
157-163 E7.3 Jy F500um ?=- Herschel SPIRE flux at 5000um
165-170 E6.3 Jy e_F500um ?=- Herschel SPIRE flux at 5000um error
172-173 A2 --- Note Note (1)
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Note (1): sc = Targets with source contamination in their background regions,
where areas larger than 10% suffer source contamination.
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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- 5 A5 --- Name Name
7- 10 F4.2 [Lsun] logLTIR ?=- TIR luminosity
12- 15 F4.2 [Lsun] e_logLTIR ? TIR luminosity error
17- 21 F5.2 [-] log(LPAH/LTIR) PAH-to-TIR luminosity ratio
23- 26 F4.2 [-] e_log(LPAH/LTIR) PAH-to-TIR luminosity ratio error
28- 32 F5.2 [-] log(Lwarm/LTIR) Warm-to-TIR luminosity ratio
34- 37 F4.2 [-] e_log(Lwarm/LTIR) Warm-to-TIR luminosity ratio error
39- 43 F5.2 [-] log(Lcold/LTIR) Cold-to-TIR luminosity ratio
45- 48 F4.2 [-] e_log(Lcold/LTIR) Cold-to-TIR luminosity ratio error
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Mar-2020