2010A&A...519A..27D


Query : 2010A&A...519A..27D

2010A&A...519A..27D - Astronomy and Astrophysics, volume 519, A27-27 (2010/9-1)

The physical and dynamical structure of Serpens. Two very different sub-(proto)clusters.

DUARTE-CABRAL A., FULLER G.A., PERETTO N., HATCHELL J., LADD E.F., BUCKLE J., RICHER J. and GRAVES S.F.

Abstract (from CDS):

The Serpens North cluster is a nearby low mass star forming region which is part of the Gould belt. It contains a range of young stars thought to correspond to two different bursts of star formation and provides the opportunity to study different stages of cluster formation. This work aims to study the molecular gas in the Serpens North cluster to probe the origin of the most recent burst of star formation in Serpens. Transitions of the C17O and C18O observed with the IRAM 30m telescope and JCMT are used to study the mass and velocity structure of the region while the physical properties of the gas are derived using LTE and non-LTE analyses of the three lowest transitions of C18O. The molecular emission traces the two centres of star formation which are seen in submillimetre dust continuum emission. In the ∼40M NW sub-cluster the gas and dust emission trace the same structures although there is evidence of some depletion of the gas phase C18O. The gas has a very uniform temperature (∼10K) and velocity (∼8.5km/s) throughout the region. This is in marked contrast to the SE sub-cluster. In this region the dust and the gas trace different features, with the temperature peaking between the submillimetre continuum sources, reaching up to ∼14K. The gas in this region has double peaked line profiles which reveal the presence of a second cloud in the line of sight. The submillimetre dust continuum sources predominantly appear located in the interface region between the two clouds. Even though they are at a similar stage of evolution, the two Serpens sub-clusters have very different characteristics. We propose that these differences are linked to the initial trigger of the collapse in the regions and suggest that a cloud-cloud collision could explain the observed properties.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: kinematics and dynamics - ISM: molecules - ISM: clouds - ISM: structure

VizieR on-line data: <Available at CDS (J/A+A/519/A27): maps.dat fig/*>

Simbad objects: 13

goto Full paper

goto View the references in ADS

Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 SH 2-68 N Y*O 18 29 48.09 +01 16 45.0           ~ 116 1
2 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 992 2
3 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 252 2
4 V* V371 Ser Or* 18 29 51.21240 +01 16 39.4860           ~ 102 1
5 NAME Serpens SMM 10 IR Y*O 18 29 52.20 +01 15 47.6           ~ 44 1
6 NAME Serpens SVS 2 Cluster Cl* 18 29 56.8 +01 14 46           ~ 10 0
7 NAME Serpens SMM 4 cor 18 29 57.1 +01 13 15           ~ 131 0
8 IRAS 18274+0112 Y*O 18 29 57.73680 +01 14 05.6940           M4: 137 2
9 NAME SERPENS SMM 3 smm 18 29 59.7 +01 14 00           ~ 88 1
10 NAME Serpens SMM 11 smm 18 30 00.3 +01 11 42           ~ 23 0
11 JCMTSE J183000.2+011251 Y*O 18 30 00.4 +01 12 50           ~ 51 0
12 [CED93] 8 smm 18 30 01.8 +01 15 07           ~ 17 0
13 NAME Gould Belt PoG ~ ~           ~ 779 1

To bookmark this query, right click on this link: simbad:objects in 2010A&A...519A..27D and select 'bookmark this link' or equivalent in the popup menu


2021.12.07-15:50:22

© Université de Strasbourg/CNRS

    • Contact