2005A&A...435..113M


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.27CET12:09:02

2005A&A...435..113M - Astronomy and Astrophysics, volume 435, 113-124 (2005/5-3)

Evidence for transient clumps and gas chemical evolution in the CS core of L673.

MORATA O., GIRART J.M. and ESTALELLA R.

Abstract (from CDS):

We present FCRAO maps as well as combined BIMA and FCRAO maps of the high density molecular emission towards the CS core in the L673 region. With the FCRAO telescope we mapped the emission in the CS (2->1), C34S (2->1), HCO+ (1->0), and H13CO+ (1->0) lines. The high-density molecular emission, which arises from a filamentary structure oriented in the NW-SE direction, shows clear morphological differences for each molecule. We find that HCO+ has an extremely high optical depth, and that the H13CO+ emission is well correlated with submm sources. The BIMA and FCRAO combined maps recover emission from structure previously undetected or marginally detected, and show an overall aspect of a filamentary structure connecting several intense clumps. We found a total 15 clumps in our combined data cube, all of them resolved at our angular resolution, with diameters in the 0.03-0.09pc range. Their estimated masses range between 0.02 and 0.2M, except for the largest clump, which has a mass of ∼1.2M. We find a clear segregation between the northern and southern region of the map: the northern section shows the less chemically evolved gas and less massive but more numerous clumps, while the southern region is dominated by the largest and most massive clump, and contains the more evolved gas, as traced by emission of late-time molecules. We find that the derived clump masses are below the virial mass, and that the clump masses become closer to the virial mass when they get bigger and more massive. This supports the idea that these clumps must be transient, and that only the more massive ones are able to condense into stars. The clumps we detect are probably in an earlier evolutionary stage than the ``starless cores'' reported recently in the literature. Only the most massive one has properties similar to a ``starless core''.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: L673 - ISM: abundances - ISM: clouds - ISM: molecules - radio lines: ISM - stars: formation

CDS comments: Fig. 1: IRAS from the SSC (catalog II/126/): IRAS 19182+1112 is a misprint for 19181+1112 = IRAS S19181+112 in SIMBAD. IRAS 19183+1109 is a misprint for 19182+1109 = IRAS S19182+111 in SIMBAD. IRAS 19186+1106 = IRAS S19 186+111 in SIMBAD. IRAS 19187+1107 is not in the Serendipitous Survey Catalog, authors say 'associated with [VRC2001] L6 73 SMM 8'.

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3114 1
2 IRAS 19180+1116 IR 19 20 22.5 +11 22 07           ~ 17 0
3 IRAS 19181+1112 Y*? 19 20 30.8690348503 +11 17 54.607114491           ~ 6 0
4 IRAS S19182+1109 mul 19 20 38.8 +11 14 51           ~ 1 0
5 JCMTSF J192047.9+111414 smm 19 20 47.9 +11 14 12           ~ 5 0
6 [VRC2001] L673 SMM 6 smm 19 20 48.1 +11 16 00           ~ 4 0
7 JCMTSF J192051.5+111344 smm 19 20 51.6 +11 13 44           ~ 5 0
8 LDN 673 DNe 19 20 54.4 +11 13 12           ~ 68 0
9 IRAS S19186+1106 FIR 19 21 01.7 +11 11 50           ~ 1 0
10 [VRC2001] L673 SMM 8 smm 19 21 02.5 +11 11 46           ~ 4 0

    Equat.    Gal    SGal    Ecl

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2021.01.27-12:09:02

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