2009A&A...499..233F


Query : 2009A&A...499..233F

2009A&A...499..233F - Astronomy and Astrophysics, volume 499, 233-247 (2009/5-3)

Linking pre- and proto-stellar objects in the intermediate-/high-mass star forming region IRAS 05345+3157.

FONTANI F., ZHANG Q., CASELLI P. and BOURKE T.L.

Abstract (from CDS):

To better understand the initial conditions of the high-mass star formation process, it is crucial to study at high angular resolution the morphology, the kinematics, and the interactions of the coldest condensations associated with intermediate-/high-mass star forming regions. This paper studies the cold condensations in the intermediate-/high-mass proto-cluster IRAS 05345+3157, focusing on the interaction with the other objects in the cluster. We performed millimeter high-angular resolution observations, both in the continuum and several molecular lines, with the PdBI and the SMA. In a recent paper, we published part of these data. The main finding of that work was the detection of two cold and dense gaseous condensations, called N and S (masses ∼2 and ∼ 9M), characterised by high values of deuterium fractionation (∼0.1 in both cores) obtained from the column density ratio N(N2D+)/N(N2H+). In this paper, we present a full report of the observations, and a complete analysis of the data obtained. The millimeter maps reveal the presence of 3 cores inside the interferometer primary beam, called C1-a, C1-b and C2. None of them are associated with cores N and S. C1-b is very likely associated with a newly formed early-B ZAMS star embedded inside a hot core, while C1-a is more likely associated with a class 0 intermediate-mass protostar. The nature of C2 is unclear. Both C1-a and C1-b are good candidates as driving sources of a powerful 12CO outflow, which strongly interacts with N, as demonstrated by the velocity gradient of the gas along this condensation. The N2H+ linewidths are between ∼1 and 2km/s in the region where the continuum cores are located, and smaller (∼0.5-1.5km/s) towards N and S, indicating that the gas in the deuterated condensations is more quiescent than that associated with the continuum sources. This is consistent with the fact that they are still in the pre-stellar phase and hence the star formation process has not yet taken place there. The study of the gas kinematics across the source indicates a tight interaction between deuterated condensations and the sources embedded in millimeter cores. For the nature of N and S, we propose two scenarios: they can be low-mass pre-stellar condensations or ``seeds'' of future high-mass star(s). However, from these data it is not possible to establish how the turbulence triggered by the neghbouring cluster of protostars can influence the evolution of the condensations.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/499/233): list.dat fits/*>

Nomenclature: Fig. 2, Table 3: [FCB2008] CN-a (Nos C1-a, C1-b).

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1363 0
2 3C 111 Sy1 04 18 21.2772425736 +38 01 35.801359968   19.75 18.05     ~ 949 1
3 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 862 0
4 NAME [BM89] L1544 cor 05 04 22.5 +25 11 36           ~ 437 1
5 QSO B0507+179 QSO 05 10 02.36912937 +18 00 41.5815635   20.0 19.0 19.09   ~ 432 1
6 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 205 2
7 QSO J0530+13 Bla 05 30 56.41674741 +13 31 55.1494688     20.00 19.35   ~ 958 1
8 NAME Ori Trapezium OpC 05 35 16.5 -05 23 14           ~ 1618 1
9 NGC 1985 RNe 05 37 47.8 +31 59 24           ~ 135 2
10 [FCB2008] C1-b cor 05 37 52.17 +32 00 04.0           ~ 3 0
11 [FCB2008] C1-a cor 05 37 52.27 +32 00 06.0           ~ 4 0
12 [FCB2008] C4 cor 05 37 52.5 +31 59 45           ~ 4 0
13 [LLK2011] Core 4 cor 05 37 52.5 +32 00 04           ~ 5 0
14 [FCB2008] C2 cor 05 37 53.0 +31 59 59           ~ 5 0
15 [LLK2011] Core 1 cor 05 37 53.03 +31 59 34.9           ~ 4 0
16 [FCB2008] S cor 05 37 53.2 +31 59 50           ~ 3 0
17 [FCB2008] N cor 05 37 53.3 +32 00 14           ~ 3 0
18 IRAS 05358+3543 Y*O 05 39 09.92 +35 45 17.2           ~ 163 0
19 7C 055201.39+394824.00 Bla 05 55 30.80561419 +39 48 49.1649683     18.30 17.5   ~ 504 2
20 3C 279 Bla 12 56 11.16657958 -05 47 21.5251510   18.01 17.75 15.87   ~ 3040 2
21 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3625 1
22 NAME Her B Sy1 16 42 58.80997043 +39 48 36.9939552   16.81 16.59 16.84   ~ 1723 2
23 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 797 0
24 IRAS 20343+4129 HII 20 36 07.1 +41 40 01           ~ 54 0
25 DR 21 (OH) cor 20 39 01.01 +42 22 50.2           ~ 409 0

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