J/ApJ/815/130 High-mass molecular clumps from MALT90 (Guzman+, 2015)
Far-infrared dust temperatures and column densities of the MALT90 molecular
clump sample.
Guzman A.E., Sanhueza P., Contreras Y., Smith H.A., Jackson J.M., Hoq S.,
Rathborne J.M.
<Astrophys. J., 815, 130 (2015)>
=2015ApJ...815..130G 2015ApJ...815..130G (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; H II regions ; Surveys ;
Millimetric/submm sources
Keywords: ISM: clouds; stars: formation; stars: massive; surveys
Abstract:
We present dust column densities and dust temperatures for ∼3000
young, high-mass molecular clumps from the Millimeter Astronomy Legacy
Team 90GHz survey, derived from adjusting single-temperature dust
emission models to the far-infrared intensity maps measured between
160 and 870µm from the Herschel/Herschel Infrared Galactic Plane
Survey (Hi-Gal) and APEX/APEX Telescope Large Area Survey of the
Galaxy (ATLASGAL) surveys. We discuss the methodology employed in
analyzing the data, calculating physical parameters, and estimating
their uncertainties. The population average dust temperature of the
clumps are 16.8±0.2K for the clumps that do not exhibit mid-infrared
signatures of star formation (quiescent clumps), 18.6±0.2K for the
clumps that display mid-infrared signatures of ongoing star formation
but have not yet developed an HII region (protostellar clumps), and
23.7±0.2 and 28.1±0.3K for clumps associated with HII and
photo-dissociation regions, respectively. These four groups exhibit
large overlaps in their temperature distributions, with dispersions
ranging between 4 and 6K. The median of the peak column densities of
the protostellar clump population is 0.20±0.02g/cm2, which is about
50% higher compared to the median of the peak column densities
associated with clumps in the other evolutionary stages. We compare
the dust temperatures and column densities measured toward the center
of the clumps with the mean values of each clump. We find that in the
quiescent clumps, the dust temperature increases toward the outer
regions and that these clumps are associated with the shallowest
column density profiles. In contrast, molecular clumps in the
protostellar or HII region phase have dust temperature gradients more
consistent with internal heating and are associated with steeper
column density profiles compared with the quiescent clumps.
Description:
We use public Herschel Space Observatory (HSO) data from Hi-GAL
(Molinari et al. 2010PASP..122..314M 2010PASP..122..314M) observed between 2010 January
and 2012 November and obtained from the Herschel Science Archive.
In addition to Hi-GAL data, we used data from three observations made
using the SPIRE bright mode by the HOBYS key project (Herschel Imaging
Survey of OB YSOs, Motte et al. 2010A&A...518L..77M 2010A&A...518L..77M) in 2012 March.
Data at 870um were taken between 2007 and 2010 using the bolometer
LABOCA installed on the APEX telescope located in Chajnantor valley,
Chile, as part of the ATLASGAL key project (Schuller et al.
2009A&A...504..415S 2009A&A...504..415S).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 109 3218 Temperature and dust column density of MALT90 sources
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See also:
J/MNRAS/443/1555 : ATLASGAL massive star forming clump sample (Urquhart+, 2014)
J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)
J/A+A/565/A75 : ATLASGAL dust condensation in Galactic plane (Csengeri+, 2014)
J/ApJ/777/157 : 90GHz obs. of high-mass star-forming regions (Hoq+, 2013)
J/MNRAS/435/400 : ATLASGAL Properties of compact HII regions (Urquhart+, 2013)
J/ApJS/208/11 : The Red MSX Source Survey: massive protostars (Lumsden+, 2013)
J/MNRAS/431/1752 : ATLASGAL 6.7GHz methanol masers (Urquhart+, 2013)
J/A+A/553/A115 : Millimetric and far-IR maps of IRDC 18310-4 (Beuther+, 2013)
J/A+A/552/A40 : MSX high-contrast IRDCs with NH3 (Chira+, 2013)
J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)
J/ApJ/756/60 : A 3mm line survey in 37 IR dark clouds (Sanhueza+, 2012)
J/A+A/544/A146 : ATLASGAL cold high-mass clumps with NH3 (Wienen+, 2012)
J/MNRAS/418/1689 : Red MSX water maser and ammonia emissions (Urquhart+, 2011)
J/ApJS/197/25 : MALT90 pilot survey (Foster+, 2011)
J/ApJ/741/110 : The BGPS. VII. Massive star-forming regions (Dunham+, 2011)
J/ApJ/723/1019 : Galactic SFR and gas surface densities (Heiderman+, 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/A+A/501/539 : RMS survey. 6cm observations of YSOs (Urquhart+, 2009)
J/A+A/487/993 : MAMBO Mapping of c2d Clouds and Cores (Kauffmann+, 2008)
J/A+A/481/345 : SED evolution in MYSOs (Molinari+, 2008)
J/A+A/461/11 : Radio observations of MYSO candidates (Urquhart+, 2007)
J/A+A/426/97 : SIMBA survey. 1.2-mm/IRAS sources (Faundez+, 2004)
J/ApJ/566/945 : Massive star forming regions at 1.2mm (Beuther+, 2002)
J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)
http://malt90.bu.edu/ : MALT90 home page
http://www.cosmos.esa.int/web/herschel/home : Herschel home page
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [AGAL]
5- 18 A14 --- AGAL Source identifier (LLL.lll+BB.bbb;
in Simbad)
20 A1 --- f_AGAL [m] Flag on AGAL (1)
22- 26 F5.1 arcsec Rad [11/145] Effective radius
28- 32 F5.2 K <Td> [9.9/51] Average dust temperature
34- 37 F4.2 K e_<Td> Lower 1σ uncertainty in <Td>
39- 42 F4.2 K E_<Td> Upper 1σ uncertainty in <Td>
44- 47 F4.1 K Tdpk [5/51] Dust temperature at peak column
density position
49- 52 F4.1 K e_Tdpk Lower 1σ uncertainty in Tdpk
54- 57 F4.1 K E_Tdpk Upper 1σ uncertainty in Tdpk
59- 63 F5.3 g/cm2 <Ng> [0.008/5.8] Average column density
65- 70 F6.3 [g/cm2] <logNg> [-2.1/0.8] Average log column density (2)
72- 76 F5.3 [g/cm2] e_<logNg> The 1σ uncertainty in <logNg>
78- 83 F6.3 g/cm2 Ngpk [0.02/25.2] Peak column density
85- 89 F5.2 [g/cm2] logNgpk [-1.7/1.4] Log peak column density
91- 94 F4.2 [g/cm2] e_logNgpk The 1σ uncertainty in logNgpk
96-108 A13 --- Class Mid-IR classification (PDR=photodissociation
region)
109 A1 --- f_Class [CD] Flag on Class (3)
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Note (1):
m = In the direction of this ATLASGAL clump there are multiple MALT90
sources (Rathborne et al. in preparation).
Note (2): The logarithm of the mass column density is related to the logarithm
of the number column density of molecules and H2 through:
log(Ng)=-23.4146+log(Np)=-23.3291+log(NH2).
Note (3): No flag means that we do not detect either of these morphological
features at 70 micron (see Section 3.6). Class as follows:
C = Quiescent clumps with a 70 micron compact emission source.
D = far-infrared dark clump (far-IRDC).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Mar-2016