J/ApJ/723/915 BLAST view of Aquila star-forming region (Rivera-Ingraham+, 2010)
The BLAST view of the star-forming region in Aquila (l = 45°, b = 0°).
Rivera-Ingraham A., Ade P.A.R., Bock J.J., Chapin E.L., Devlin M.J.,
Dicker S.R., Griffin M., Gundersen J.O., Halpern M., Hargrave P.C.,
Hughes D.H., Klein J., Marsden G., Martin P.G., Mauskopf P.,
Netterfield C.B., Olmi L., Patanchon G., Rex M., Scott D., Semisch C.,
Truch M.D.P., Tucker C., Tucker G.S., Viero M.P., Wiebe D.V.
<Astrophys. J., 723, 915-934 (2010)>
=2010ApJ...723..915R 2010ApJ...723..915R
ADC_Keywords: Molecular clouds ; Infrared sources
Keywords: balloons - ISM: clouds - stars: formation - submillimeter: ISM
Abstract:
We have carried out the first general submillimeter analysis of the
field toward GRSMC 45.46+0.05, a massive star-forming region in
Aquila. The deconvolved 6°2 (3°x2°) maps provided by
BLAST in 2005 at 250, 350, and 500um were used to perform a
preliminary characterization of the clump population previously
investigated in the infrared, radio, and molecular maps.
Interferometric CORNISH data at 4.8GHz have also been used to
characterize the Ultracompact HII regions (UCHIIRs) within the main
clumps. By means of the BLAST maps, we have produced an initial census
of the submillimeter structures that will be observed by Herschel,
several of which are known Infrared Dark Clouds.
Description:
BLAST observed Aquila during its first science flight in 2005 June,
mapping a total of 6deg2 (3°x2°) at 250, 350, and 500um
toward GRSMC 45.60+0.30.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 94 131 Submillimeter Clumps in the BLAST Aquila Map
table2.dat 40 91 *Coordinates of CORNISH sources in the BLAST
Aquila field at 4.8GHz
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Note on table2.dat: CORNISH = Co-Ordinated Radio "N" Infrared Survey
for High-mass star formation (see Purcell et al. 2008ASPC..387..389P 2008ASPC..387..389P)
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See also:
J/MNRAS/421/3257 : MHO catalogue for Serpens and Aquila (Ioannidis+, 2012)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- Source Source name ANNa <[RAB2010] ANNa> in Simbad
6 A1 --- f_Source [*h] low S/N or non-standard fit (1)
9- 22 A14 --- BLAST Name name (JHHMMSS+DDMMSS) (2)
24- 29 F6.3 deg GLON Galactic longitude
31- 36 F6.3 deg GLAT Galactic latitude
38- 47 A10 --- IRAS IRAS Name (HHMMm+DDMM) (3)
48 A1 --- f_IRAS [i] beyond 30" of IRAS position (1)
50- 54 A5 --- IRDC IR Dark Cloud name (PNNNN) (4)
56- 68 A13 --- Cloud Cloud name (GLLL.ll+BB.bb) (5)
72- 86 A15 --- Clump Clump name(s) (6)
88- 92 F5.2 kpc Dist ? Heliocentric distance from Roman-Duval
et al. 2009, Cat. J/ApJ/699/1153
94 A1 --- Assoc [Y?] Cloud association flag (7)
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Note (1): Notes as follows:
* = Detection S/N <3
h = Source designations ending in "a" refer to additional Gaussians
required during the fit of the main clump
i = Position beyond 30", but visually within the IRAS emission
Note (2): Source names include the prefix "BLAST" as part of the standard
BLAST nomenclature.
Note (3): Closest IRAS match within 30" in the Point Source Catalog (PSC).
Note (4): Closest IRDC match within 30" in the catalog from
Peretto & Fuller (2009, Cat. J/A+A/505/405).
Note (5): GRS name of the extended clouds from Rathborne et al. (2009,
Cat. J/ApJS/182/131) which contain the molecular clump counterpart(s) to the
BLAST source. A blank implies the absence of a clump counterpart in the
catalog.
Note (6): Clump(s) from Rathborne et al. (2009, Cat. J/ApJS/182/131)
containing the BLAST peak within its/their l and b FWHM.
Note (7): Cloud association flag as follows:
Y = BLAST clump is associated with the cloud. Cloud has a molecular clump
whose velocity FWHM contains the strongest molecular peak of spectrum,
measured at the peak of the submillimeter emission. Molecular clump
also has peak velocity closest to that measured for the BLAST source.
? = Cloud membership unclear. The main molecular emission in the BLAST
spectrum is within the velocity FWHM of this molecular cloud/clump,
but there is still another cloud with a clump with peak velocity
closer to that of the strongest line in the BLAST spectrum.
Contributions from different clouds are possible. A blank implies that
the velocity of main BLAST molecular emission is not compatible with
that assigned to the cloud/clump, despite the spatial agreement and
apparent location of the submillimeter peak within the spatial FWHM of
clump(s) associated with that cloud.
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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- 4 A4 --- Source Source name <[RAB2010] ANNa> in Simbad
6- 12 A7 --- Name CORNISH source name, ANNa-CNN,
<[RAB2010] ANNa-CNN> in Simbad
13 A1 --- n_Name [*] low S/N<3 detection
15- 16 I2 h RAh Right ascension (J2000)
18- 19 I2 min RAm Right ascension (J2000)
21- 26 F6.3 s RAs Right ascension (J2000)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination (J2000)
32- 33 I2 arcmin DEm Declination (J2000)
35- 40 F6.3 arcsec DEs Declination (J2000)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 12-Jan-2013