2006ApJ...651..301V


Query : 2006ApJ...651..301V

2006ApJ...651..301V - Astrophys. J., 651, 301-320 (2006/November-1)

Dense cores with multiple protostars: the velocity fields of L1448 IRS 3, NGC 1333 IRAS 2, and NGC 1333 IRAS 4.

VOLGENAU N.H., MUNDY L.G., LOONEY L.W. and WELCH W.J.

Abstract (from CDS):

The embedded cores L1448 IRS 3, NGC 1333 IRAS 2, and NGC 1333 IRAS 4 are mapped in emission from the C18O, H13CO+, and N2H+ J=1⟶0 transitions. The maps are created by combining BIMA and FCRAO observations and are tuned to resolutions of ∼50", 10", 5", and 3". The higher resolution maps reveal emission structures that are considerably smaller than the characteristic core radius (∼0.1 pc) identified in earlier single-dish studies. We focus our study on the kinematics of the envelope material traced by the emission lines. We find that although the FCRAO data show relatively smooth velocity gradients across the cores, the velocity fields seen with higher resolution are more random, with central velocities varying over a range of ∼1 km/s. In general, the distribution of velocities, as well as the complexity of the fields, increases with resolution. To analyze variations in the widths of the emission lines, we employ a method of gridding the datacubes that was initially developed to quantify properties of turbulent cloud models. The cores exhibit a broad range of line widths even at the smallest measurable scales. Pure thermal broadening at the prevailing envelope temperatures (T~20 K) is insufficient to produce the measured line widths; the narrowest lines must have a turbulent component at least as great as the thermal component, and for nearly all lines, the turbulent component makes the dominant contribution. Our results suggest that turbulent motions persist down to subcore scales of at least 2400 AU.

Abstract Copyright:

Journal keyword(s): Stars: Circumstellar Matter - ISM: Kinematics and Dynamics - Radio Lines: Stars - Stars: Formation - stars: individual (L1448 IRS 3) - stars: individual (NGC 1333 IRAS 2) - stars: individual (NGC 1333 IRAS 4) - Turbulence

Simbad objects: 27

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Number of rows : 27
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 W 3 OH HII 02 27 04.1 +61 52 22           ~ 968 2
2 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3680 3
3 LDN 1448 DNe 03 22.5 +30 35           ~ 490 0
4 LDN 1448NW Y*O 03 25 35.66 +30 45 34.2           ~ 65 0
5 JCMTSE J032536.1+304514 Y*O 03 25 36.22 +30 45 15.7           ~ 109 0
6 SSTc2d J032536.4+304522 Y*O 03 25 36.49 +30 45 22.2           ~ 190 1
7 LDN 1448NA smm 03 25 36.49 +30 45 22.2           ~ 178 1
8 IRAS 03225+3034 IR 03 25 36.49 +30 45 22.2           ~ 154 1
9 NAME [BM89] L1450D DNe 03 28 36.8 +31 15 20           ~ 51 0
10 [JCC87] IRAS 2C IR 03 28 53.90 +31 14 53.5           ~ 14 0
11 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 160 1
12 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 420 3
13 BD+30 547 Y*O 03 28 57.2107612240 +31 14 19.076624755   10.73 9.98 9.1   G4V 99 1
14 NAME HH 7-11 FIR 03 29 03.9 +31 16 06           ~ 339 0
15 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 638 1
16 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 473 0
17 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1279 1
18 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 573 0
19 [JCC87] IRAS 4C Y*O 03 29 13.54 +31 13 58.2           ~ 91 1
20 LDN 1450 DNe 03 29.6 +31 20           ~ 59 0
21 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 284 0
22 4C 32.14 QSO 03 36 30.10760600 +32 18 29.3422210     17.50 16.6   ~ 596 1
23 V* IK Tau Mi* 03 53 28.8884898148 +11 24 21.865959095 16.99 17.03 13.39 7.29 3.20 M7-11 591 0
24 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 879 1
25 Barnard 220 DNe 04 41 38.8 +26 00 42           ~ 125 0
26 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5467 1
27 LDN 1251A DNe 22 30 31.8 +75 14 17           ~ 73 2

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2021.09.20-22:31:37

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