J/A+A/599/A139 ATLASGAL massive clumps dust characterization (Koenig+, 2017)
ATLASGAL-selected massive clumps in the inner Galaxy.
III. Dust continuum characterization of an evolutionary sample.
Koenig C., Urquhart J.S., Csengeri T., Leurini S., Wyrowski F.,
Giannetti A., Wienen M., Pillai T., Kauffmann J., Menten K.M., Schuller F.
<Astron. Astrophys. 599, A139 (2017)>
=2017A&A...599A.139K 2017A&A...599A.139K (SIMBAD/NED BibCode)
ADC_Keywords: Millimetric/submm sources; Molecular clouds; Interstellar medium
Keywords: stars: formation - stars: evolution - stars: massive -
radiative transfer - surveys
Abstract:
The ATLASGAL survey provides an ideal basis for detailed studies of
large numbers of massive star forming clumps covering the whole range
of evolutionary stages. The ATLASGAL Top100 is a sample of clumps
selected from their infrared and radio properties to be representative
for the whole range of evolutionary stages. The ATLASGAL Top100
sources are the focus of a number of detailed follow-up studies that
will be presented in a series of papers. In the present work we use
the dust continuum emission to constrain the physical properties of
this sample and identify trends as a function of source evolution. We
determine flux densities from mid-infrared to submm wavelength
(8-870micron) images and use these values to fit their spectral energy
distributions (SEDs) and determine their dust temperature and flux.
Combining these with recent distances from the literature including
maser parallax measurements we determine clump masses, luminosities
and column densities. We find trends for increasing temperature,
luminosity and column density with the proposed evolution sequence,
confirming that this sample is representative of different
evolutionary stages of massive star formation. We show that most of
the sample has the ability to form massive stars (including the most
massive O-type stars) and that the majority is gravitationally
unstable and hence likely to be collapsing. The highest column density
ATLASGAL sources presented cover the whole range of evolutionary
stages from the youngest to the most evolved high-mass star forming
clumps. Their study provides a unique starting point for more in-depth
research on massive star formation in four distinct evolutionary
stages whose well defined physical parameters afford more detailed
studies. As most of the sample is closer than 5kpc, these sources are
also ideal for follow-up observations with high spatial resolution.
Description:
Parameters for 110 selected ATLASGAL clumps in 4 distinct evolutionary
stages.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 358 110 Source parameters
sed/* . 110 Individual SED pdf file for each source
(AGALLLL.lll+BB.bbb_sed.pdf)
imidir/* . 110 Individual Mid-IR pdf images for each source
(AGALLLL.lll+BB.bbbimagesmidIr.pdf)
isubmm/* . 110 Individual submm pdf images for each source
(AGALLLL.lll+BB.bbbimagessubmm.pdf)
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See also:
J/A+A/570/A65 : ATLASGAL massive clumps CO depletion (Giannetti+, 2014)
J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [AGAL]
5- 18 A14 --- AGAL AGAL source name (LLL.lll+BB.bbb)
20- 23 F4.1 kpc Dist ? Distance
25- 30 F6.1 km/s RV ? Radial velocity
32- 40 F9.4 deg GLON Galactic longitude of peak
42- 50 F9.4 deg GLAT Galactic latitude of peak
52- 56 F5.1 arcsec Diam Aperture diameter
58- 60 A3 --- Class Source classification (1)
62- 65 F4.1 K Tdust Dust temperature
67- 69 F3.1 K e_Tdust Error of Tdust
71- 77 E7.1 Lsun Lbol ? Bolometric luminosity
79- 85 E7.1 Lsun e_Lbol ? Error of Lbol
87- 93 E7.1 Msun Mass ? Clump mass
95-101 E7.1 Msun e_Mass ? Error of Mass
103-106 F4.2 --- avir ? Virial parameter
108-114 E7.1 Jy F70 ? Flux at 70um (PACS)
116-122 E7.1 Jy e_F70 ? Error of F70
124 I1 --- sat70 ? Pixel saturated at 70um
126-132 E7.1 Jy F160 ? Flux at 160um (PACS)
134-140 E7.1 Jy e_F160 ? Error of F160
142 I1 --- sat160 ? Pixel saturated at 160um
144-150 E7.1 Jy F250 ? Flux at 250um (SPIRE)
152-158 E7.1 Jy e_F250 ? Error of F250
160 I1 --- sat250 ? Pixel saturated at 250um
162-168 E7.1 Jy F350 ? Flux at 350um (SPIRE)
170-176 E7.1 Jy e_F350 ? Error of F350
178 I1 --- sat350 ? Pixel saturated at 350um
180-186 E7.1 Jy F500 ? Flux at 500um (SPIRE)
188-194 E7.1 Jy e_F500 ? Error of F500
196 I1 --- sat500 ? Pixel saturated at 500um
198-204 E7.1 Jy F870 ? Flux at 870um (ATLASGAL)
206-212 E7.1 Jy e_F870 ? Error of F870
214 I1 --- sat870 ? Pixel saturated at 870um
216-222 E7.1 Jy F8 ? Flux at 8um (MSX)
224-230 E7.1 Jy e_F8 ? Error of F8
232 I1 --- sat8 ? Pixel saturated at 8um
234-240 E7.1 Jy F12 ? Flux at 12um (MSX)
242-248 E7.1 Jy e_F12 ? Error of F12
250 I1 --- sat12 ? Pixel saturated at 12um
252-258 E7.1 Jy F14 ? Flux at 14um (MSX)
260-266 E7.1 Jy e_F14 ? Error of F14
268 I1 --- sat14 ? Pixel saturated at 14um
270-276 E7.1 Jy F21 ? Flux at 21um (MSX)
278-284 E7.1 Jy e_F21 ? Error of F21
286 I1 --- sat21 ? Pixel saturated at 21um
288-294 E7.1 Jy FW1 ? Flux at 3.4um (WISE)
296-302 E7.1 Jy e_FW1 ? Error of FW1
304 I1 --- satW1 ? Pixel saturated at 3.4um
306-312 E7.1 Jy FW2 ? Flux at 4.6um (WISE)
314-320 E7.1 Jy e_FW2 ? Error of FW2
322 I1 --- satW2 ? Pixel saturated at 4.6um
324-330 E7.1 Jy FW3 ? Flux at 12um (WISE)
332-338 E7.1 Jy e_FW3 ? Error of FW3
340 I1 --- satW3 ? Pixel saturated at 12um
342-348 E7.1 Jy FW4 ? Flux at 22um (WISE)
350-356 E7.1 Jy e_FW4 ? Error of FW4
358 I1 --- satW4 ? Pixel saturated at 22um
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Note (1): Source classification as follows:
70d = Weak at 70 micron
24d = Mid-infrared weak
IRb = Mid-infrared bright
HII = Compact HII region
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Acknowledgements:
Carsten Koenig, koenig(at)mpifr-bonn.mpg.de
References:
Giannetti et al., Paper I 2014A&A...570A..65G 2014A&A...570A..65G, Cat. J/A+A/570/A65
Csengeri et al., Paper II 2016A&A...586A.149C 2016A&A...586A.149C, Cat. J/A+A/586/A149
(End) Carsten Koenig [MPIfR, Germany], Patricia Vannier [CDS] 11-Jan-2017