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J/MNRAS/461/2288    Infall motions in massive star-forming regions  (He+, 2016)

Properties of massive star-forming clumps with infall motions. He Y., Zhou J., Esimbek J., Ji W., Wu G., Tang X., Komesh T., Yuan Y., Li D., Baan W.A. <Mon. Not. R. Astron. Soc., 461, 2288-2308 (2016)> =2016MNRAS.461.2288H (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs; Millimetric/submm sources; Spectroscopy; Radio lines Keywords: stars: formation - ISM: kinematics and dynamics - ISM: molecules - radio lines: ISM Abstract: In this work, we aim to characterize high-mass clumps with infall motions. We selected 327 clumps from the Millimetre Astronomy Legacy Team 90-GHz survey, and identified 100 infall candidates. Combined with the results of He et al. (2015, Cat. J/MNRAS/450/1926), we obtained a sample of 732 high-mass clumps, including 231 massive infall candidates and 501 clumps where infall is not detected. Objects in our sample were classified as pre-stellar, proto-stellar, HII or photodissociation region (PDR). The detection rates of the infall candidates in the pre-stellar, proto-stellar, HII and PDR stages are 41.2 per cent, 36.6 per cent, 30.6 per cent and 12.7 per cent, respectively. The infall candidates have a higher H2 column density and volume density compared with the clumps where infall is not detected at every stage. For the infall candidates, the median values of the infall rates at the pre-stellar, proto-stellar, HII and PDR stages are 2.6 x 10-3, 7.0x10-3, 6.5x10-3 and 5.5x10-3M/yr, respectively. These values indicate that infall candidates at later evolutionary stages are still accumulating material efficiently. It is interesting to find that both infall candidates and clumps where infall is not detected show a clear trend of increasing mass from the pre-stellar to proto-stellar, and to the HII stages. The power indices of the clump mass function are 2.04±0.16 and 2.17±0.31 for the infall candidates and clumps where infall is not detected, respectively, which agree well with the power index of the stellar initial mass function (2.35) and the cold Planck cores (2.0). Description: We selected high-mass clumps with N2H+(1-0), HNC(1-0), and HCO+(1-0) emission lines detected simultaneously from the MALT90 survey data, i.e. with an S/N>3, and searched for infall signatures using these three lines. To ensure the clumps in our sample are separated, and not contaminated by emission from an adjacent clump, each source with an angular separation of less than 36 arcsec (the Mopra beam size at 90GHz) from its nearest neighbour was excluded. HYX15 (He et al., 2015, Cat. J/MNRAS/450/1926) studied 405 high-mass clumps selected from the MALT90 survey (years 1 and 2) and identified 131 infall candidates; in this work, 327 high-mass clumps were selected from the remaining data from the MALT90 survey and an additional 100 infall candidates were identified. In total, we created a sample of 732 high-mass clumps, and identified 231 infall candidates. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 86 405 Derived clump parameters (list of He et al., 2015, Cat. J/MNRAS/450/1926) tablea2.dat 88 327 Derived clump parameters of the observed sources tablea3.dat 76 327 The derived line parameters and profiles of the observed sources
See also: J/MNRAS/450/1926 : Infall motions in massive star-forming regions (He+, 2015) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1 A1 --- n_Clump [*] * for infall candidates (G1) 2- 15 A14 --- Clump Clump name (GLLL.lll+B.bbb) (G2) 17- 21 F5.2 Jy/beam Fpeak Peak submillimetre emission 23- 28 F6.2 Jy Fint Integrated submillimetre emission 30- 33 F4.1 K Tdust Dust temperature 35- 39 F5.2 kpc Dist ?=- Heliocentric distance 41- 45 F5.2 pc Reff ?=- Effective physical radius 47- 50 F4.2 --- AR Aspect ratio 52- 56 F5.2 [cm-2] logNH2 H2 column density 58- 61 F4.2 [Msun] logMclump ?=- Clump mass derived from the integrated 870um emission 63- 66 F4.2 [Msun] logMVir ?=- Virial mass 68- 72 F5.2 10+4cm-3 VDens ?=- Volume density 74- 86 A13 --- Class Spitzer classification
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
1 A1 --- n_Clump [*] * for infall candidates (G1) 2- 15 A14 --- Clump Clump name (GLLL.lll+B.bbb) (G2) 17- 21 F5.2 Jy/beam Fpeak Peak submillimetre emission 23- 28 F6.2 Jy Fint Integrated submillimetre emission 30- 33 F4.1 K Tdust Dust temperature 35- 39 F5.2 kpc Dist ?=- Heliocentric distance 41- 42 I2 --- r_Dist ?=- Distance reference (3) 44- 47 F4.2 pc Reff ?=- Effective physical radius 49- 52 F4.2 --- AR Aspect ratio 54- 58 F5.2 [cm-2] logNH2 H2 column density 60- 63 F4.2 [Msun] logMclump ?=- Clump mass derived from the integrated 870um emission 65- 68 F4.2 [Msun] logMvirial ?=- Virial mass 70- 74 F5.2 10+4cm-3 VDens ?=- Volume density 76- 88 A13 --- Class Spitzer classification
Note (3): References as follows: 1 = Faundez et al. (2004, Cat. J/A+A/426/97) 2 = Hill et al. (2005, Cat. J/MNRAS/363/405) 3 = Urquhart et al. (2012, Cat. J/MNRAS/420/1656) 4 = Morales et al. (2013, Cat. J/A+A/560/A76) 5 = Chen et al. (2013, Cat. J/ApJS/206/9) 6 = Urquhart et al. (2013, Cat. J/MNRAS/431/1752) 7 = Ellsworth-Bowers et al. (2013, Cat. J/ApJ/770/39) 8 = Ragan, Henning & Beuther (2013A&A...559A..79R) 9 = Sanchez-Monge et al. (2013, Cat. J/A+A/550/A21) 10 = Lumsden et al. (2013, Cat. J/ApJS/208/11) 11 = Vasyunina et al. (2014, Cat. J/ApJ/780/85) 12 = Urquhart et al. (2014, Cat. J/MNRAS/437/1791) 13 = Urquhart et al. (2014, Cat. J/MNRAS/443/1555) 14 = Anderson et al. (2014, Cat. J/ApJS/212/1) 15 = Giannetti et al. (2014, Cat. J/A+A/570/A65) 16 = Traficante et al. (2015, Cat. J/MNRAS/451/3089) 17 = IRDC 18 = tangential point 19 = this paper
Byte-by-byte Description of file: tablea3.dat
Bytes Format Units Label Explanations
1 A1 --- n_Clump [*] * indicates infall candidates (G1) 2- 15 A14 --- Clump Clump name (G2) 17- 23 F7.2 km/s VHCO+ Peak velocity of HCO+(1-0) 25- 27 F3.2 km/s e_VHCO+ rms uncertainty on VHCO+ 29- 35 F7.2 km/s VHNC Peak velocity of HNC(1-0) 37- 39 F3.2 km/s e_VHNC rms uncertainty on VHNC 41- 47 F7.2 km/s VN2H+ Peak velocity of N2H+(1-0) 49- 51 F3.2 km/s e_VN2H+ rms uncertainty on VN2H 53- 56 F4.2 km/s DVN2H+ FWHM of N2H+(1-0) 58- 60 F3.2 km/s e_DVN2H+ rms uncertainty on DVN2H+ 62- 66 F5.2 --- dvHCO+ Asymmetry of HCO+(1-0) 68- 72 F5.2 --- dvHNC Asymmetry of HNC(1-0) 74 A1 --- PHCO+ [BRN] Profile of HCO+(1-0) (3) 75 A1 --- --- [,] 76 A1 --- PHNC [BRN] Profile of HNC(1-0) (3)
Note (3): Profile is judged from our HCO+(1-0) and HNC(1-0) as follows: B = blue profile R = red profile N = neither blue nor red
Global notes: Note (G1): An * indicates infall candidates. Note (G2): Sources are named by galactic coordinates of ATLASGAL sources.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Dec-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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