2010A&A...512A..40M


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.19CEST06:04:37

2010A&A...512A..40M - Astronomy and Astrophysics, volume 512, A40-40 (2010/3-1)

Toward understanding the formation of multiple systems. A pilot IRAM-PdBI survey of class 0 objects.

MAURY A.J., ANDRE P., HENNEBELLE P., MOTTE F., STAMATELLOS D., BATE M., BELLOCHE A., DUCHENE G. and WHITWORTH A.

Abstract (from CDS):

The formation process of binary stars and multiple systems is poorly understood. The multiplicity rate of Class II pre-main-sequence stars and Class I protostars is well documented and known to be high (∼30% to 50% between ∼100 and 4000 AU). However, optical/ near-infrared observations of Class I/Class II YSOs barely constrain the pristine properties of multiple systems, since dynamical evolution can quickly alter these properties during the protostellar phase. Here, we seek to determine the typical outcome of protostellar collapse and to constrain models of binary formation by core fragmentation during collapse, using high-resolution millimeter continuum imaging of very young (Class 0) protostars observed at the beginning of the main accretion phase. We carried out a pilot high-resolution study of 5 Class 0 objects, including 3 Taurus sources and 2 Perseus sources, using the most extended (A) configuration of the IRAM Plateau de Bure Interferometer (PdBI) at 1.3 mm. Our PdBI observations have a typical HPBW resolution ∼0.3''-0.5'' and rms continuum sensitivity ∼0.1-1mJy/beam, which allow us to probe the multiplicity of Class 0 protostars down to separations a ∼50AU and circumstellar mass ratios q∼0.07. We detected all 5 primary Class 0 sources in the 1.3mm dust continuum. A single component associated with the primary Class 0 object was detected in the case of the three Taurus sources, while robust evidence of secondary components was found toward the two Perseus sources: L1448-C and NGC1333-IR2A. We show that the secondary 1.3mm continuum component detected ∼600AU south-east of L1448-C, at a position angle close to that of the CO(2-1) jet axis traced by our data, is an outflow feature directly associated with the powerful jet driven by L1448-C. The secondary 1.3mm continuum component detected ∼1900AU south-east of NGC1333-IR2A may either be a genuine protostellar companion or trace the edge of an outflow cavity. Therefore, our PdBI observations revealed only wide (>1500AU) protobinary systems and/or outflow-generated features. When combined with previous millimeter interferometric observations of Class 0 protostars, our pilot PdBI study tentatively suggests that the binary fraction in the ∼75-1000AU range increases from the Class 0 to the Class I stage. It also seems to argue against purely hydrodynamic models of binary star formation. We briefly discuss possible alternative scenarios to reconcile the low multiplicity rate of Class 0 protostars on small scales with the higher binary fraction observed at later (e.g. Class I) evolutionary stages.

Abstract Copyright:

Journal keyword(s): stars: formation - binaries: general - ISM: clouds - ISM: jets and outflows

Simbad objects: 31

goto Full paper

goto View the reference in ADS

Number of rows : 31

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 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3567 3
2 LDN 1448 DNe 03 22.5 +30 35           ~ 467 0
3 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 303 0
4 [SDA2014] West4 Y*O 03 25 38.83 +30 44 06.2           ~ 242 1
5 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 159 1
6 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 397 3
7 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 84 1
8 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 604 1
9 [JCC87] IRAS 4A1 Y*O 03 29 10.510 +31 13 31.01           ~ 77 1
10 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 466 0
11 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1228 1
12 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 558 0
13 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1081 0
14 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 860 1
15 IRAS 04191+1523 Y*O 04 22 00.43944 +15 30 21.2148           ~ 185 0
16 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 186 1
17 Bad 16 Y*O 04 30 50.2775823865 +23 00 08.771252817       14.95   F1 132 0
18 RAFGL 5123 FU* 04 31 34.07736 +18 08 04.9020           K3V/M3III 815 0
19 LDN 1527 DNe 04 39 53 +25 45.0           ~ 503 0
20 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3531 0
21 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 884 1
22 HH 2 HH 05 36.4 -06 47           ~ 335 1
23 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5336 1
24 CRBR 2316.0-1626 Y*? 16 26 17.46816 -24 23 12.9552           ~ 21 0
25 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 375 0
26 [SSG2006] MMS002 smm 16 26 26.50 -24 24 30.9           ~ 241 0
27 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3055 0
28 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 186 0
29 NAME IRAS 16293-2422A Y*O 16 32 22.869 -24 28 36.11           ~ 111 0
30 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 709 0
31 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2515 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2010A&A...512A..40M and select 'bookmark this link' or equivalent in the popup menu


2020.09.19-06:04:37

© Université de Strasbourg/CNRS

    • Contact