J/A+A/647/A154 NGC6357 686 molecular cores physical properties (Brand+, 2021)
A possible far-ultraviolet flux-dependent core mass function in NGC 6357.
Brand J., Giannetti A., Massi F., Wouterloot J.G.A., Verdirame C.
<Astron. Astrophys. 647, A154 (2021)>
=2021A&A...647A.154B 2021A&A...647A.154B (SIMBAD/NED BibCode)
ADC_Keywords: Photometry, millimetric/submm ; Interstellar medium ;
Molecular clouds; H II regions
Keywords: ISM: clouds - HII regions - ISM: structure - stars: formation -
submillimeter: ISM - ISM: individual objects: NGC 6357
Abstract:
We mapped the NGC6357 star forming region at 450 and 850 micron with
SCUBA-2 and in the CO(3-2) line with HARP at the JCMT. We also
retrieved Herschel Hi-GAL data at 70 and 160 micron. The submm
continuum emission was decomposed into cores with the algorithm
Gaussclumps (Stutzki & Guesten, 1990ApJ...356..513S 1990ApJ...356..513S). By fitting
greybodies to the core 4-point SEDs we derived their temperature and
mass. Core mass functions were derived in the region more exposed to
the FUV flux from massive stars (associated with the HII regions
G353.2+0.9, G353.1+0.6, and G353.2+0.7) and in the region less
exposed. Table 2 lists the physical properties of the cores in
NGC6357.
Description:
Table 2 lists core position, peak flux density at 70, 160, 450 and 850
micron, total flux density at 850 micron and its formal (photometric)
error, size (not deconvolved for beam size), mass and mass formal
error both derived from the total flux density at 850 micron, dust
temperature along with its formal error and chi-square value from the
greybody fits. All maps were first convolved to the resolution at 850
micron, and the extended emission was subtracted. Emission at 850
micron was further corrected for CO(3-2) emission.
The cores were retrieved from the emission at 850 micron, by using the
algorithm Gaussclumps. Gaussclumps fits 2-D Gaussians to the emission,
providing flux densities projected on elliptical spatial distributions
for each retrieved core. The sizes listed in Table 2 are the
geometrical means of the ellipse axes (sqrt[major-axis x minor-axis])
at 850 micron.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 107 686 Physical properties of the dense cores
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See also:
J/A+A/573/A95 : Photometry of the young open cluster Pismis 24 (Massi+, 2015)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/686] Source identification code
5- 12 F8.4 deg RAdeg Right ascension (J2000.0)
14- 21 F8.4 deg DEdeg Declination (J2000.0)
23- 30 F8.0 mJy/beam F70 ?=-10000 Peak flux density
at 70 micron (1)
32- 39 F8.0 mJy/beam F160 ?=-10000 Peak flux density
at 160 micron (1)
41- 48 F8.1 mJy/beam F450 ?=-10000 Peak flux density
at 450 micron (1)
50- 57 F8.1 mJy/beam F850 Peak flux density at 850 micron,
in 10-24erg/cm2/s/Hz) (2)
59- 65 F7.2 10-27W/m2/s/Hz IF850 Total flux density at 850 micron,
in 10-24erg/cm2/s/Hz) (2)
67- 73 F7.2 10-27W/m2/s/Hz e_IF850 Error total flux density,
in 10-24erg/cm2/s/Hz) (2)
75- 78 F4.1 arcsec SZ Geometrical mean of ellipse FWHMs (3)
80- 85 F6.2 Msun Mg Gas mass
87- 92 F6.2 Msun e_Mg Error gas mass
94- 97 F4.1 K Td Dust temperature from greybody fit
99-102 F4.1 K e_Td Error dust temperature
104-107 F4.1 --- CHI Chi-square greybody fit
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Note (1): After convolution to the resolution at 850 micron and removal of
extended emission.
Note (2): After correction for CO(3-2) emission and removal of extended
emission.
Note (3): Not deconvolved for beam size.
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Acknowledgements:
Jan Brand (brand(at)ira.inaf.it)
Fabrizio Massi (fmassi(at)arcetri.astro.it)
References:
Stutzki J., & Guesten, R., 1990ApJ...356..513S 1990ApJ...356..513S,
High spatial resolution isotopic CO and CS observations of M 17 SW:
the clumpy structure of the molecular cloud core
Giannetti et al., 2012A&A...538A..41G 2012A&A...538A..41G,
Molecular clouds under the influence of massive stars in the
Galactic HII region G353.2+0.9
(End) Jan Brand [INAF-IRA, Bologna, Italy], Patricia Vannier [CDS] 22-Mar-2021