2016A&A...595A..51K


Query : 2016A&A...595A..51K

2016A&A...595A..51K - Astronomy and Astrophysics, volume 595A, 51-51 (2016/11-1)

Evolutionary status of dense cores in the NGC 1333 IRAS 4 star-forming region.

KOUMPIA E., VAN DER TAK F.F.S., KWON W., TOBIN J.J., FULLER G.A. and PLUME R.

Abstract (from CDS):

Context. Protostellar evolution after the formation of the protostar is becoming reasonably well characterized, but the evolution from a prestellar core to a protostar is not well known, although the first hydrostatic core (FHSC) must be a pivotal step.
Aims. NGC 1333 - IRAS 4C is a potentially very young object that we can directly compare with the nearby Class 0 objects IRAS 4A and IRAS 4B. Observational constraints are provided by spectral imaging from the JCMT Spectral Legacy Survey (330-373 GHz). We present integrated intensity and velocity maps of several species, including CO, H2CO and CH3OH. CARMA observations provide additional information with which we can distinguish IRAS 4C from other evolutionary stages.
Methods. We present the observational signatures of the velocity of an observed outflow, the degree of CO depletion, the deuterium fractionation of [DCO+]/[HCO+], and gas kinetic temperatures.
Results. We report differences between the three sources in four aspects: a) the kinetic temperature as probed using the H2CO lines is much lower toward IRAS 4C than the other two sources; b) the line profiles of the detected species show strong outflow activity toward IRAS 4A and IRAS 4B, but not toward IRAS 4C; c) the HCN/HNC is <1 toward IRAS 4C, which confirms the cold nature of the source; d) the degree of CO depletion and the deuteration are lowest toward the warmest of the sources, IRAS 4B.
Conclusions. IRAS 4C seems to be in a different evolutionary state than the sources IRAS 4A and IRAS 4B. We can probably exclude the FHSC stage becaues of the relatively low Lsmm/Lbol (∼6%), and we investigate the earliest accretion phase of Class 0 stage and the transition between Class 0 to Class I. Our results do not show a consistent scenario for either case; the main problem is the absence of outflow activity and the cold nature of IRAS 4C. The number of FHSC candidates in Perseus is ∼10 times higher than current models predict, which suggests that the lifespan of these objects is ≥103yrs, which might be due to an accretion rate lower than 4x10–5M/yr.

Abstract Copyright: © ESO, 2016

Journal keyword(s): ISM: abundances - ISM: kinematics and dynamics - ISM: molecules - stars: formation - stars: low-mass - stars: protostars

Simbad objects: 19

goto Full paper

goto View the references in ADS

Number of rows : 19
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 NAME LDN 1451-mm cor 03 25 09.5 +30 23 51           ~ 45 0
2 JCMTSE J032525.9+304502 Y*O 03 25 25.9 +30 45 03           ~ 51 0
3 JCMTSE J032906.9+311725 cor 03 29 07.06 +31 17 25.6           ~ 34 0
4 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 675 1
5 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 473 0
6 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1338 1
7 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 585 0
8 [JCC87] IRAS 4C Y*O 03 29 13.54 +31 13 58.2           ~ 97 1
9 [KJT2007] SMM J032942+31282 cor 03 29 25.5 +31 28 18           ~ 58 0
10 [HRF2005] 3 PoC 03 33 21.3 +31 07 27           ~ 70 0
11 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 95 0
12 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1229 0
13 Ass Per OB 2 As* 03 42.2 +33 26           ~ 322 0
14 IRAS 04191+1523 Y*O 04 22 00.43944 +15 30 21.2148           ~ 195 0
15 WISE J042838.78+265134.6 Y*O 04 28 38.78544 +26 51 34.6824           ~ 47 0
16 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 193 1
17 IRAS 04368+2557 Y*O 04 39 53.97816 +26 03 09.6804           ~ 255 0
18 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 788 0
19 NAME LDN 1014 IRS Y*O 21 24 07.58 +49 59 08.9           ~ 77 0

To bookmark this query, right click on this link: simbad:objects in 2016A&A...595A..51K and select 'bookmark this link' or equivalent in the popup menu


2022.08.18-03:57:54

© Université de Strasbourg/CNRS

    • Contact