2017A&A...606A.123H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST02:40:10

2017A&A...606A.123H - Astronomy and Astrophysics, volume 606A, 123-123 (2017/10-1)

Fibers in the NGC 1333 proto-cluster.

HACAR A., TAFALLA M. and ALVES J.

Abstract (from CDS):

Are the initial conditions for clustered star formation the same as for non-clustered star formation? To investigate the initial gas properties in young proto-clusters we carried out a comprehensive and high-sensitivity study of the internal structure, density, temperature, and kinematics of the dense gas content of the NGC 1333 region in Perseus, one of the nearest and best studied embedded clusters. The analysis of the gas velocities in the position-position-velocity space reveals an intricate underlying gas organization both in space and velocity. We identified a total of 14 velocity-coherent, (tran-)sonic structures within NGC 1333, with similar physical and kinematic properties than those quiescent, star-forming (aka fertile) fibers previously identified in low-mass star-forming clouds. These fibers are arranged in a complex spatial network, build-up the observed total column density, and contain the dense cores and protostars in this cloud. Our results demonstrate that the presence of fibers is not restricted to low-mass clouds but can be extended to regions of increasing mass and complexity. We propose that the observational dichotomy between clustered and non-clustered star-forming regions might be naturally explained by the distinct spatial density of fertile fibers in these environments.

Abstract Copyright: © ESO, 2017

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

VizieR on-line data: <Available at CDS (J/A+A/606/A123): list.dat fits/* class/*>

Nomenclature: Table 2: [HTA2017] NN (Nos 1-50).

Status at CDS:   All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 29

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Number of rows : 29

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 V* VX Cas Ae* 00 31 30.6816836826 +61 58 50.982831889 11.83 11.59 10.50 11.19 10.94 A0Vep 126 0
2 * alf UMi cC* 02 31 49.09456 +89 15 50.7923 3.00 2.62 2.02 1.53 1.22 F8Ib 609 2
3 LDN 1448 DNe 03 22.5 +30 35           ~ 466 0
4 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 169 1
5 IRAS 03255+3103 Y*O 03 28 37.068 +31 13 31.00           ~ 78 1
6 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 158 1
7 SSTYSV J032901.53+312020.6 cor 03 29 01.165 +31 20 24.41           ~ 70 1
8 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 332 0
9 LZK 12 Y*O 03 29 10.4138336046 +31 21 59.070333199   16.06 14.25     B5:V+F2: 127 0
10 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 465 0
11 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1219 1
12 BD+30 549 Y*O 03 29 19.7770675177 +31 24 57.044403187 10.81 10.95 10.47 10.587   B8:p 93 1
13 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 257 0
14 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1061 0
15 IC 348 OpC 03 44 34 +32 09.8           ~ 1227 1
16 LDN 1495 DNe 04 18.1 +27 37           ~ 289 1
17 Barnard 213 DNe 04 20 51 +27 16.3           ~ 153 0
18 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 768 1
19 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
20 LDN 1517 DNe 04 55 45 +30 33.0           ~ 97 0
21 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1
22 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1015 2
23 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
24 LDN 1746 DNe 17 11.3 -27 22           ~ 108 0
25 NAME Oph Cluster ClG 17 12 24.7 -23 21 01           ~ 240 0
26 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 333 1
27 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 912 2
28 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 944 0
29 IC 5146 OpC 21 53 24 +47 16.0           ~ 385 2

    Equat.    Gal    SGal    Ecl

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2020.07.08-02:40:11

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