2004A&A...415.1021J


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.24CEST12:51:24

2004A&A...415.1021J - Astronomy and Astrophysics, volume 415, 1021-1037 (2004/3-1)

The impact of shocks on the chemistry of molecular clouds. High resolution images of chemical differentiation along the NGC 1333-IRAS 2A outflow.

JORGENSEN J.K., HOGERHEIJDE M.R., BLAKE G.A., VAN DISHOECK E.F., MUNDY L.G. and SCHOEIER F.L.

Abstract (from CDS):

This paper presents a detailed study of the chemistry in the outflow associated with the low-mass protostar NGC 1333-IRAS 2A down to 3'' (650AU) scales. Millimeter-wavelength aperture-synthesis observations from the Owens Valley and Berkeley-Illinois-Maryland-Association interferometers and (sub)millimeter single-dish observations from the Onsala Space Observatory 20m telescope and Caltech Submillimeter Observatory are presented. The interaction of the highly collimated protostellar outflow with a molecular condensation ∼15000AU from the central protostar is clearly traced by molecular species such as HCN, SiO, SO, CS, and CH3OH. Especially SiO traces a narrow high velocity component at the interface between the outflow and the molecular condensation. Multi-transition single-dish observations are used to distinguish the chemistry of the shock from that of the molecular condensation and to address the physical conditions therein. Statistical equilibrium calculations reveal temperatures of 20 and 70K for the quiescent and shocked components, respectively, and densities near 106/cm3. The line-profiles of low- and high-excitation lines are remarkably similar, indicating that the physical properties are quite homogeneous within each component. Significant abundance enhancements of two to four orders of magnitude are found in the shocked region for molecules such as CH3OH, SiO and the sulfur-bearing molecules. HCO+ is seen only in the aftermath of the shock consistent with models where it is destroyed through release of H2O from grain mantles in the shock. N2H+ shows narrow lines, not affected by the outflow but rather probing the ambient cloud. The overall molecular inventory is compared to other outflow regions and protostellar environments. Differences in abundances of HCN, H2CO and CS are seen between different outflow regions and are suggested to be related to differences in the atomic carbon abundance. Compared to the warm inner parts of protostellar envelopes, higher abundances of in particular CH3OH and SiO are found in the outflows, which may be related to density differences between the regions.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: NGC 1333-IRAS 2 - stars: formation - ISM: jets and outflows - ISM: abundances

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 4C 28.07 QSO 02 37 52.40567732 +28 48 08.9900231     18.5 16.99   ~ 483 1
2 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3447 3
3 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1176 1
4 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 155 1
5 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 368 3
6 HH 2 HH 05 36.4 -06 47           ~ 335 1
7 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 111 0
8 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 672 1
9 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 983 1
10 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 457 0

    Equat.    Gal    SGal    Ecl

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2019.08.24-12:51:24

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