J/ApJS/218/1 BGPS. XI. SHARC-II 350um observations (Merello+, 2015)
The Bolocam Galactic Plane Survey.
XI. Temperatures and substructure of Galactic clumps based on 350µm
observations.
Merello M., Evans II N.J., Shirley Y.L., Rosolowsky E., Ginsburg A.,
Bally J., Battersby C., Dunham M.M.
<Astrophys. J. Suppl. Ser., 218, 1 (2015)>
=2015ApJS..218....1M 2015ApJS..218....1M
ADC_Keywords: Surveys ; Millimetric/submm sources
Keywords: catalogs; dust, extinction; Galaxy: structure; stars: formation;
submillimeter: ISM; surveys
Abstract:
We present 107 maps of continuum emission at 350µm from Galactic
molecular clumps. Observed sources were mainly selected from the
Bolocam Galactic Plane Survey (BGPS) catalog, with three additional
maps covering star-forming regions in the outer Galaxy. The higher
resolution of the SHARC-II images (8.5" beam) compared with the 1.1mm
images from BGPS (33" beam) allowed us to identify a large population
of smaller substructures within the clumps. A catalog is presented for
the 1386 sources extracted from the 350µm maps. The color
temperature distribution of clumps based on the two wavelengths has a
median of 13.3K and mean of 16.3±0.4K, assuming an opacity law index
of 1.7. For the structures with good determination of color
temperatures, the mean ratio of gas temperature, determined from NH3
observations, to dust color temperature is 0.88 and the median ratio
is 0.76. About half the clumps have more than 2 substructures and 22
clumps have more than 10. The fraction of the mass in dense
substructures seen at 350µm compared to the mass of their parental
clump is ∼0.19, and the surface densities of these substructures are,
on average, 2.2 times those seen in the clumps identified at 1.1mm.
For a well-characterized sample, 88 structures (31%) exceed a surface
density of 0.2g/cm2, and 18 (6%) exceed 1.0g/cm2, thresholds for
massive star formation suggested by theorists.
Description:
Observations were taken in several runs between 2006 June and 2012
September at the Caltech Submillimeter Observatory (CSO) with SHARC-II
camera at 350um.
We found a total of 619 V2.1 sources in our sample of SHARC-II maps,
with an average and median flux density of 0.79Jy and 0.29Jy.
File Summary:
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FileName Lrecl Records Explanations
-------------------------------------------------------------------------------
ReadMe 80 . This file
table3.dat 125 1386 Properties of sources recovered in the 350um maps
table5.dat 120 619 BGPS V2.1 sources fluxes and fitted dust temperature
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See also:
J/ApJ/799/29 : BGPS. XII. DR2 distance catalog (Ellsworth-Bowers+, 2015)
J/ApJS/209/2 : The BGPS. X. Dense molecular gas (Shirley+, 2013)
J/A+A/559/A79 : IRDC APEX/SABOCA observations (Ragan+, 2013)
J/ApJ/772/45 : Hi-GAL obs.: third quadrant star formation (Elia+, 2013)
J/ApJ/770/39 : BGPS. VIII. MIR kinematic distances (Ellsworth-Bowers+, 2013)
J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)
J/A+A/544/A146 : ATLASGAL cold high-mass clumps with NH3 (Wienen+, 2012)
J/ApJ/741/110 : The BGPS. VII. Massive star-forming regions (Dunham+, 2011)
J/ApJS/195/14 : Bolocam Galactic Plane Survey (BGPS). V. (Schlingman+, 2011)
J/ApJ/721/137 : The Bolocam Galactic Plane Survey (BGPS) (Bally+, 2010)
J/ApJS/188/123 : The Bolocam Galactic Plane Survey. II. (Rosolowsky+, 2010)
J/ApJ/715/310 : Early stages of star formation in IRDCs (Rathborne+, 2010)
J/AJ/138/1380 : Dust clumps in the Galactic Plane (Matthews+, 2009)
J/AJ/133/1560 : Spitzer c2d small clouds and cores (Wu+, 2007)
J/ApJ/641/389 : Millimetric observations of IRDC cores (Rathborne+, 2006)
J/ApJ/639/227 : MSX IRDC candidate catalog (Simon+, 2006)
J/ApJS/161/361 : Millimeter continuum survey for protoclusters (Klein+, 2005)
J/A+A/426/97 : SIMBA survey. 1.2-mm/IRAS sources (Faundez+, 2004)
J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)
http://irsa.ipac.caltech.edu/data/BOLOCAM_GPS/ : NASA/IRSA Bolocam GPS archive
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- Seq [1/1386] Running sequence number
6- 11 A6 --- --- [SHARC_]
12- 28 A17 --- SHARC Source identifier (GLLL.llll+BB.bbbb) (1)
30- 37 F8.4 deg GLON Galactic longitude of peak intensity
39- 46 F8.4 deg GLAT Galactic latitude of peak intensity
48- 55 F8.4 deg GLONc Galactic longitude of emission centroid
57- 64 F8.4 deg GLATc Galactic latitude of emission centroid
66- 67 I2 arcsec amaj [3/28] Major axis 1/e width of source
69- 70 I2 arcsec amin [2/17] Minor axis 1/e width of source
72- 74 I3 deg PA [0/180] Position angle
76- 78 I3 arcsec theta [2/46]? Deconvolved angular size θ
80- 86 F7.2 Jy S20 [0.8/1429] 350um flux densities derived for
20" aperture
88- 93 F6.2 Jy e_S20 ? Error in S20
95-101 F7.2 Jy S40 [-11/2336] 350um flux densities derived for
40" aperture
103-108 F6.2 Jy e_S40 ? Error in S40
110-116 F7.2 Jy S [0.5/4331] Integrated 350um flux density
118-123 F6.2 Jy e_S ? Error in S
125 A1 --- Type Type of substructure (C=compact or F=faint) (2)
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Note (1): Derived from Galactic coordinates of the maximum
intensity in the object.
Note (2): As defined in section 4.5:
sources with amplitude Pamp (=2σ(l,b); see section 4.2)
above 10σrms ("compact substructure") are more related with
possible dense core-like structures in the interior of millimeter
clumps, and sources below this limit ("faint substructure") trace a
more diffuse medium in addition to weak sources.
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [BGPSv2_]
8- 22 A15 --- BGPS BGPS source identifier (GLLL.lll+BB.bbb) in
the V2.1 catalog
24- 28 F5.2 Jy F1.1 [0.02/25] The 1.1mm flux in 40" aperture from
BGPS V1.0 catalog
30- 33 F4.2 Jy e_F1.1 Error in F1.1
35- 41 F7.2 Jy F350 [-5.8/2446] Convolved 350um flux in
40" aperture (1)
43- 48 F6.2 Jy e_F350 Error F350
50 A1 --- l_T1.0 [>] Limit flag on T1.0
51- 56 F6.1 K T1.0 [4.1/1000]? The β=1.0 dust temperature (2)
58 A1 --- l_T1.0M [>] Limit flag on T1.0M
59- 64 F6.1 K T1.0M [3/1000]? Upper limit on T1.0
66 A1 --- l_T1.0m [>] Limit flag on T1.0m
67- 72 F6.1 K T1.0m [3/1000]? Lower limit on T1.0
74 A1 --- l_T1.7 [>] Limit flag on T1.7
75- 80 F6.1 K T1.7 [3.7/1000]? The β=1.7 dust temperature (2)
82 A1 --- l_T1.7M [>] Limit flag on T1.7M
83- 88 F6.1 K T1.7M [2/1000]? Upper limit on T1.7
90 A1 --- l_T1.7m [>] Limit flag on T1.7m
91- 96 F6.1 K T1.7m [2/1000]? Lower limit on T1.7
98 A1 --- l_T2.0 [>] Limit flag on T2.0
99-104 F6.1 K T2.0 [3.5/1000]? The β=2.0 dust temperature (2)
106 A1 --- l_T2.0M [>] Limit flag on T2.0M
107-112 F6.1 K T2.0M [2/1000]? Upper limit on T2.0
114 A1 --- l_T2.0m [>] Limit flag on T2.0m
115-120 F6.1 K T2.0m [2/1000]? Lower limit on T2.0
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Note (1): Fluxes were obtained from SHARC-II maps convolved to
match a 33 micron beam size (see Section 4.6).
Note (2): β is the parameter of the variation of the optical depth
with frequency: τ∝νβ
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History:
From electronic version of the journal
References:
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(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 06-Jul-2015