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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 358 110 Source parameters sed/* 0 110 Individual SED pdf file for each source (AGALLLL.lll+BB.bbb_sed.pdf) imidir/* 0 110 Individual Mid-IR pdf images for each source (AGALLLL.lll+BB.bbbimagesmidIr.pdf) isubmm/* 0 110 Individual submm pdf images for each source (AGALLLL.lll+BB.bbbimagessubmm.pdf)
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
Bytes Format Units Label Explanations
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
Note (1): Source classification as follows: 70d = Weak at 70 micron 24d = Mid-infrared weak IRb = Mid-infrared bright HII = Compact HII region
Acknowledgements: Carsten Koenig, koenig(at) References: Giannetti et al., Paper I 2014A&A...570A..65G, Cat. J/A+A/570/A65 Csengeri et al., Paper II 2016A&A...586A.149C, Cat. J/A+A/586/A149
(End) Carsten Koenig [MPIfR, Germany], Patricia Vannier [CDS] 11-Jan-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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