2014A&A...567A..10L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:51:29

2014A&A...567A..10L - Astronomy and Astrophysics, volume 567A, 10-10 (2014/7-1)

Filament L1482 in the California molecular cloud.

LI D.L., ESIMBEK J., ZHOU J.J., LOU Y.-Q., WU G., TANG X.D. and HE Y.X.

Abstract (from CDS):

The process of gravitational fragmentation in the L1482 molecular filament of the California molecular cloud is studied by combining several complementary observations and physical estimates. We investigate the kinematic and dynamical states of this molecular filament and physical properties of several dozens of dense molecular clumps embedded therein. We present and compare molecular line emission observations of the J=2-1 and J=3-2 transitions of 12CO in this molecular complex, using the Koelner Observatorium fuer Sub-Millimeter Astronomie (KOSMA) 3-m telescope. These observations are complemented with archival data observations and analyses of the 13CO J=1-0 emission obtained at the Purple Mountain Observatory (PMO) 13.7-m radio telescope at Delingha Station in QingHai Province of west China, as well as infrared emission maps from the Herschel Space Telescope online archive, obtained with the SPIRE and PACS cameras. Comparison of these complementary datasets allows for a comprehensive multiwavelength analysis of the L1482 molecular filament. We have identified 23 clumps along the molecular filament L1482 in the California molecular cloud. For these molecular clumps, we were able to estimate column and number densities, masses, and radii. The masses of these clumps range from ∼6.8 to 62.8M with an average value of 24.7–16.2+31.1M. Eleven of the identified molecular clumps appear to be associated with protostars and are thus referred to as protostellar clumps. Protostellar clumps and the remaining starless clumps of our sample appear to have similar temperatures and linewidths, yet on average, the protostellar clumps appear to be slightly more massive than the latter. All these molecular clumps show supersonic nonthermal gas motions. While surprisingly similar in mass and size to the much better known Orion molecular cloud, the formation rate of high-mass stars appears to be suppressed in the California molecular cloud compared with that in the Orion molecular cloud based on the mass-radius threshold derived from the static Bonnor-Ebert sphere. The largely uniform 12CO J=2-1 line-of-sight velocities along the L1482 molecular cloud shows that it is a generally coherent filamentary structure. Since the NGC1579 stellar cluster is at the junction of two molecular filaments, the origin of the NGC1579 stellar cluster might be merging molecular filaments fed by converging inflows. Our analysis suggests that these molecular filaments are thermally supercritical and molecular clumps may form by gravitational fragmentation along the filament. Instead of being static, these molecular clumps are most likely in processes of dynamic evolution.

Abstract Copyright:

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

Nomenclature: Table 1: [LEZ2014] NN (Nos 1-23).

Simbad objects: 35

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Number of rows : 35

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME California Molecular Cloud MoC 04 10.0 +39 00           ~ 96 1
2 LDN 1482 DNe 04 28.3 +35 37           ~ 18 0
3 [LEZ2014] 11 MoC 04 29 53.900 +35 15 41.51           ~ 1 0
4 [LEZ2014] 12 MoC 04 30 02.670 +35 14 15.14           ~ 1 0
5 NGC 1579 HII 04 30 11 +35 16.7           ~ 72 1
6 [LEZ2014] 17 MoC 04 30 13.940 +35 07 46.97           ~ 1 0
7 [LEZ2014] 13 MoC 04 30 14.800 +35 12 07.16           ~ 1 0
8 [LEZ2014] 10 MoC 04 30 16.150 +35 17 06.51           ~ 1 0
9 [LEZ2014] 8 MoC 04 30 16.920 +35 23 02.94           ~ 1 0
10 [LEZ2014] 15 MoC 04 30 20.060 +35 09 38.44           ~ 1 0
11 [LEZ2014] 9 MoC 04 30 22.370 +35 19 59.27           ~ 1 0
12 [LEZ2014] 14 MoC 04 30 26.600 +35 10 44.14           ~ 1 0
13 [LEZ2014] 18 MoC 04 30 27.830 +35 05 16.42           ~ 1 0
14 [LEZ2014] 16 MoC 04 30 29.880 +35 08 54.14           ~ 1 0
15 [LEZ2014] 5 MoC 04 30 34.510 +35 34 57.04           ~ 1 0
16 [LEZ2014] 19 MoC 04 30 38.950 +35 02 12.12           ~ 1 0
17 [LEZ2014] 6 MoC 04 30 40.470 +35 29 25.00           ~ 1 0
18 [LEZ2014] 4 MoC 04 30 47.050 +35 37 27.99           ~ 1 0
19 [LEZ2014] 20 MoC 04 30 47.540 +34 58 48.27           ~ 1 0
20 [LEZ2014] 21 MoC 04 30 53.980 +34 55 41.59           ~ 1 0
21 [LEZ2014] 7 MoC 04 30 55.740 +35 29 16.76           ~ 1 0
22 [LEZ2014] 22 MoC 04 30 56.400 +34 54 11.01           ~ 1 0
23 [LEZ2014] 2 MoC 04 30 56.900 +35 39 45.37           ~ 1 0
24 [LEZ2014] 1 MoC 04 31 03.590 +35 42 16.93           ~ 1 0
25 [LEZ2014] 23 MoC 04 31 24.800 +34 50 43.96           ~ 1 0
26 [LEZ2014] 3 MoC 04 31 25.080 +35 39 22.76           ~ 1 0
27 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
28 M 42 HII 05 35 17.3 -05 23 28           ~ 3724 0
29 NAME Ori A MoC 05 38 -07.1           ~ 2675 0
30 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 848 1
31 NAME ROSETTE MOL CLOUD MoC 06 34.7 +04 02           ~ 227 0
32 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 162 1
33 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
34 NAME Aql Rift DNe 18 32 -01.0           ~ 234 1
35 NAME Gould Belt PoG ~ ~           ~ 711 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:51:29

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