J/A+A/625/A134 NGC 6357 massive dense cores (Russeil+, 2019)
Herschel-HOBYS study of the earliest phases of high-mass star formation in
NGC 6357.
Russeil D., Figueira M., Zavagno A., Motte F., Schneider N.,
Men'shchikov A., Bontemps S., Andre P., Anderson L.D., Benedettini M.,
Didelon P., Di Francesco J., Elia D., Koenyves V., Nguyen Luong Q., Nony T.,
Pezzuto S., Rygl K.L.J., Schisano E., Spinoglio L., Tige J., White G.J.
<Astron. Astrophys. 625, A134 (2019)>
=2019A&A...625A.134R 2019A&A...625A.134R (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Infrared sources; Interstellar medium
Keywords: stars: massive - stars: formation
Abstract:
To constrain models of high-mass star formation it is important to
identify the massive dense cores (MDCs) able to form high-mass
star(s).
It is one of purposes of the Herschel/HOBYS key program. Here, we make
the census and characterisation of the properties of the MDCs
population of the NGC 6357 HII region. Our study is based on the
Herschel PACS and SPIRE 70-500 microns images of NGC 6357 complemented
with (sub)millimetre and mid-infrared data. We followed the procedure,
established by the Herschel/HOBYS consortium, to extract ∼0.1pc
massive dense cores using the getsources software. We estimated their
physical parameters (temperatures, masses, luminosities) from spectral
energy distribution (SED) fitting.
We have obtained a complete census of 23 massive dense cores, amongs
which one is found to be IR-quiet and twelve are starless,
representing very early stages of the star-formation process.
Focussing on the starless MDCs, we consider their evolutionary status,
and suggest that only five are likely to form a high-mass star.
We find that, contrarily to the case in NGC 6334, the NGC 6357 region
does not exhibit any ridge/hub features that are believed to be
crucial to the massive star formation process.
This study adds support for an empirical model in which massive dense
cores and protostars simultaneously accrete mass from the surrounding
filaments. In addition, the massive star formation in NGC 6357 seems
to have stopped and the hottest stars in Pismis 24 have disrupted the
filaments.
Description:
Fluxes and information for the 23 massive dense cores (MDCs) found in
NGC 6357. Information for 155 reliable sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 78 155 Information of the 155 reliable sources
tabc2-4.dat 386 23 Information and fluxes of the 23 massive
dense cores (MDCs)
list.dat 99 6 List of fits maps
fits/* . 6 Individual fits maps
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See also:
J/ApJS/168/100 : X-ray study of star-forming region NGC 6357 (Wang+, 2007)
J/A+A/538/A142 : OB stars in NGC 6334 and NGC 6357 (Russeil+, 2012)
J/A+A/587/A135 : Halpha images of NGC 6334 and NGC 6357 (Russeil+, 2016)
J/A+A/607/A86 : NGC 6334 and NGC 6357 OB stars spectra (Russeil+, 2017)
J/A+A/602/A77 : HOBYS: 46 MDCs found in NGC 6334 (Tige+, 2017)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Number [1/155] Source number
5- 8 F4.2 pc FWHM Deconvolved size
10- 13 F4.1 K T Temperature
15- 18 F4.1 K e_T Temperature uncertainty
20- 24 F5.1 Msun Mass Mass
26- 29 F4.1 Msun e_Mass Mass uncertainty
31- 35 I5 Lsun Ldata Luminosity from data
37- 40 I4 Lsun Lfit Luminosity from fit
42- 46 F5.2 10+6cm-3 nH2 Density
48- 50 F3.1 10+6cm-3 e_nH2 Density uncertainty
52- 53 I2 h RAh Right ascension (J2000.0)
55- 56 I2 min RAm Right ascension (J2000.0)
58- 62 F5.2 s RAs Right ascension (J2000.0)
64 A1 --- DE- Declination sign (J2000.0)
65- 66 I2 deg DEd Declination (J2000.0)
68- 69 I2 arcmin DEm Declination (J2000.0)
71- 75 F5.2 arcsec DEs Declination (J2000.0)
77- 78 I2 --- MDC ? MDC number
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Byte-by-byte Description of file: tabc2-4.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- MDC [1/23] MDC identification number
4- 5 I2 h RAh Right ascension (J2000.0)
7- 8 I2 min RAm Right ascension (J2000.0)
10- 15 F6.3 s RAs Right ascension (J2000.0)
17 A1 --- DE- Declination sign (J2000.0)
18- 19 I2 deg DEd Declination (J2000.0)
21- 22 I2 arcmin DEm Declination (J2000.0)
24- 28 F5.2 arcsec DEs Declination (J2000.0)
30- 36 F7.3 Jy/beam Sp70 ?=- Peak intensity at 70um
38- 43 F6.3 Jy/beam e_Sp70 ?=- Peak intensity at 70um uncertainty
45- 51 F7.2 Jy Si70 ?=- Integrated flux at 70um
53- 57 F5.2 Jy e_Si70 ?=- Integrated flux at 70um uncertainty
59- 62 F4.1 arcsec AMAJ70 ?=- FWHM major axis at 70um
64- 67 F4.1 arcsec AMIN70 ?=- FWHM minor axis at 70um
69- 73 F5.1 deg PA70 ?=- Position angle at 70um
75- 80 F6.2 Jy/beam Sp160 Peak intensity at 160um
82- 86 F5.2 Jy/beam e_Sp160 Peak intensity at 160um uncertainty
88- 94 F7.2 Jy Si160 Integrated flux at 160um
96-100 F5.2 Jy e_Si160 Integrated flux at 160um uncertainty
102-105 F4.1 arcsec AMAJ160 FWHM major axis at 160um
107-110 F4.1 arcsec AMIN160 FWHM minor axis at 160um
112-116 F5.1 deg PA160 Position angle at 160um
118-123 F6.2 Jy/beam Sp250 Peak intensity at 250um
125-129 F5.2 Jy/beam e_Sp250 Peak intensity at 250um uncertainty
131-136 F6.2 Jy Si250 Integrated flux at 250um
138-143 F6.3 Jy e_Si250 Integrated flux at 250um uncertainty
145-148 F4.1 arcsec AMAJ250 FWHM major axis at 250um
150-153 F4.1 arcsec AMIN250 FWHM minor axis at 250um
155-159 F5.1 deg PA250 Position angle at 250um
161-166 F6.2 Jy/beam Sp350 Peak intensity at 350um
168-172 F5.2 Jy/beam e_Sp350 Peak intensity at 350um uncertainty
174-179 F6.2 Jy Si350 Integrated flux at 350um
181-185 F5.2 Jy e_Si350 Integrated flux at 350um uncertainty
187-190 F4.1 arcsec AMAJ350 FWHM major axis at 350um
192-195 F4.1 arcsec AMIN350 FWHM minor axis at 350um
197-201 F5.1 deg PA350 Position angle at 350um
203-207 F5.2 Jy/beam Sp500 Peak intensity at 500um
209-212 F4.2 Jy/beam e_Sp500 Peak intensity at 500um uncertainty
214-218 F5.2 Jy Si500 Integrated flux at 500um
220-223 F4.2 Jy e_Si500 Integrated flux at 500um uncertainty
225-228 F4.1 arcsec AMAJ500 FWHM major axis at 500um
230-233 F4.1 arcsec AMIN500 FWHM minor axis at 500um
235-239 F5.1 deg PA500 Position angle at 500um
241-244 F4.2 Jy/beam Sp870 Peak intensity at 870um
246-249 F4.2 Jy/beam e_Sp870 Peak intensity at 870um uncertainty
251-255 F5.2 Jy Si870 Integrated flux at 870um
257-260 F4.2 Jy e_Si870 Integrated flux at 870um uncertainty
262-265 F4.1 arcsec AMAJ870 FWHM major axis at 870um
267-270 F4.1 arcsec AMIN870 FWHM minor axis at 870um
272-276 F5.1 deg PA870 Position angle at 870um
278-281 F4.2 Jy/beam Sp1200 ? Peak intensity at 1200um
283-286 F4.2 Jy/beam e_Sp1200 ? Peak intensity at 1200um uncertainty
288-291 F4.2 Jy Si1200 ? Integrated flux at 1200um
293-298 F6.4 Jy e_Si1200 ? Integrated flux at 1200um uncertainty
300-303 F4.1 arcsec AMAJ1200 ? FWHM major axis at 1200um
305-308 F4.1 arcsec AMIN1200 ? FWHM minor axis at 1200um
310-314 F5.1 deg PA1200 ? Position angle at 1200um
316-320 F5.2 Jy Si3.6 ? Integrated flux at 3.6um
322-325 F4.2 Jy e_Si3.6 ? 3.6um flux .6um uncertainty
327-331 F5.2 Jy Si4.5 ? Integrated flux at 4.5um
333-336 F4.2 Jy e_Si4.5 ? 4.5um flux .5um uncertainty
338-343 F6.2 Jy Si5.8 ? Integrated flux at 5.8um
345-348 F4.2 Jy e_Si5.8 ? 5.8um flux uncertainty
350-355 F6.2 Jy Si8.0 ? Integrated flux at 8.0um
357-360 F4.2 Jy e_Si8.0 ? 8.0um flux uncertainty
362-386 A25 --- GName GLIMPSE identification
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 34 I5 Kibyte size Size of FITS file
36- 72 A37 --- FileName Name of FITS file, in subdirectory fits
74- 99 A26 --- Title Title of the FITS file
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History:
From Delphine Russeil, delphine.russeil(at)lam.fr
Acknowledgements:
We are grateful to Alexander Men'shchikov for his help and
discussions on getsources. SPIRE has been developed by a consortium of
institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge
(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);
IAC (Spain); Stockholm Observatory (Sweden); Imperial College London,
RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ.
Colorado (USA). This development has been supported by national
funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK);
and NASA (USA). PACS has been developed by a consortium of institutes
led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL,
IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/
OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has
been supported by the funding agencies BMVIT (Austria), ESA-PRODEX
(Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and
CICYT/MCYT (Spain). This research has made use of the SIMBAD database,
operated at CDS, Strasbourg, France. Part of this work was supported
by the ANR (Agence Nationale pour la Recherche) project PROBeS, number
ANR-08-BLAN-0241. We acknowledge financial support from "Programme
National de Physique Stellaire (PNPS) and program 'Physique et Chime
du Milieu Interstellaire' (PCMI) of CNRS/INSU, France. GJW gratefully
acknowledges the receipt of a Leverhulme Emeritus Professorial
Fellowship.
References:
Motte et al., 2010A&A...518L..77M 2010A&A...518L..77M
(End) Patricia Vannier [CDS] 09-Apr-2019