2014A&A...568L...5C


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST08:44:39

2014A&A...568L...5C - Astronomy and Astrophysics, volume 568, L5-5 (2014/8-1)

The ALMA view of the protostellar system HH 212. The wind, the cavity, and the disk.

CODELLA C., CABRIT S., GUETH F., PODIO L., LEURINI S., BACHILLER R., GUSDORF A., LEFLOCH B., NISINI B., TAFALLA M. and YVART W.

Abstract (from CDS):

Because it is viewed simply edge-on, the HH212 protostellar system is an ideal laboratory for studying the interplay of infall, outflow, and rotation in the earliest stages of low-mass star formation. We wish to exploit the unmatched combination of high angular resolution, high sensitivity, high-imaging fidelity, and spectral coverage provided by ALMA to shed light on the complex kinematics of the innermost central regions of HH212. We mapped the inner 10" (4500AU) of the HH212 system at ≃0.5" resolution in several molecular tracers and in the 850 µm dust continuum using the ALMA interferometer in band 7 in the extended configuration of the Early Science Cycle 0 operations. Within a single ALMA spectral set-up, we simultaneously identify all the crucial ingredients known to be involved in the star formation recipe: (i) the fast, collimated bipolar SiO jet driven by the protostar; (ii) the large-scale swept-up CO outflow; (iii) the flattened rotating and infalling envelope, with bipolar cavities carved by the outflow (in C17O(3-2)); and (iv) a rotating wide-angle flow that fills the cavities and surrounds the axial jet (in C34S(7-6)). In addition, the compact high-velocity C17O emission (±1.9-3.5km/s from systemic) shows a velocity gradient along the equatorial plane consistent with a rotating disk of ≃0.2"=90AU around a≃0.3 ±0.1M source. The rotating disk is possibly Keplerian. HH212 is the third Class 0 protostar with possible signatures of a Keplerian disk of radius ≥30AU. The warped geometry in our CS data suggests that this large Keplerian disk might result from misaligned magnetic and rotation axes during the collapse phase. The wide-angle CS flow suggests that disk winds may be present in this source.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: jets and outflows - ISM: molecules - ISM: individual objects: HH212

VizieR on-line data: <Available at CDS (J/A+A/568/L5): list.dat fits/*>

Simbad objects: 7

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Number of rows : 7

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 V* DG Tau TT* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 900 1
2 LDN 1527 DNe 04 39 53 +25 45.0           ~ 467 0
3 QSO B0537-441 BLL 05 38 50.36155219 -44 05 08.9389165   15.77 16.48 16   ~ 764 2
4 [CCG2007] MM1 smm 05 43 51.4100 -01 02 53.160           ~ 13 1
5 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 256 1
6 QSO B0605-0834 QSO 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 381 1
7 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 365 0

    Equat.    Gal    SGal    Ecl

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2019.10.17-08:44:39

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