2014A&A...569A..11S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST04:18:27

2014A&A...569A..11S - Astronomy and Astrophysics, volume 569A, 11-11 (2014/9-2)

A necklace of dense cores in the high-mass star forming region G35.20-0.74N: ALMA observations.

SANCHEZ-MONGE A., BELTRAN M.T., CESARONI R., ETOKA S., GALLI D., KUMAR M.S.N., MOSCADELLI L., STANKE T., VAN DER TAK F.F.S., VIG S., WALMSLEY C.M., WANG K.-S., ZINNECKER H., ELIA D., MOLINARI S. and SCHISANO E.

Abstract (from CDS):

The formation process of high-mass stars (with masses >8 M) is still poorly understood, and represents a challenge from both the theoretical and observational points of view. The advent of the Atacama Large Millimeter Array (ALMA) is expected to provide observational evidence to better constrain the theoretical scenarios. The present study aims at characterizing the high-mass star forming region G35.20-0.74N, which is found associated with at least one massive outflow and contains multiple dense cores, one of them recently found associated with a Keplerian rotating disk. We used the radio-interferometer ALMA to observe the G35.20-0.74N region in the submillimeter continuum and line emission at 350 GHz. The observed frequency range covers tracers of dense gas (e.g., H13CO+, C17O), molecular outflows (e.g., SiO), and hot cores (e.g., CH3CN, CH3OH). These observations were complemented with infrared and centimeter data. The ALMA 870 µm continuum emission map reveals an elongated dust structure (∼0.15 pc long and ∼0.013 pc wide; full width at half maximum) perpendicular to the large-scale molecular outflow detected in the region, and fragmented into a number of cores with masses ∼1-10 M and sizes ∼1600 AU (spatial resolution ∼960 AU). The cores appear regularly spaced with a separation of ∼0.023 pc. The emission of dense gas tracers such as H13CO+ or C17O is extended and coincident with the dust elongated structure. The three strongest dust cores show emission of complex organic molecules characteristic of hot cores, with temperatures around 200 K, and relative abundances 0.2-2x10–8 for CH3CN and 0.6-5x10–6 for CH3OH. The two cores with highest mass (cores A and B) show coherent velocity fields, with gradients almost aligned with the dust elongated structure. Those velocity gradients are consistent with Keplerian disks rotating about central masses of 4-18 M. Perpendicular to the velocity gradients we have identified a large-scale precessing jet/outflow associated with core B, and hints of an east-west jet/outflow associated with core A. The elongated dust structure in G35.20-0.74N is fragmented into a number of dense cores that may form high-mass stars. Based on the velocity field of the dense gas, the orientation of the magnetic field, and the regularly spaced fragmentation, we interpret this elongated structure as the densest part of a 1D filament fragmenting and forming high-mass stars.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: massive - ISM: individual objects: G35.20-0.74 N - ISM: molecules - jets ISM:, outflows

VizieR on-line data: <Available at CDS (J/A+A/569/A11): maps.dat fits/*>

Simbad objects: 11

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Number of rows : 11

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 NAME W3 IRS 5 Y*O 02 25 40.54 +62 05 51.4           B1 322 0
2 SDC G335.579-0.292 DNe 16 30 58.00 -48 44 16.3           ~ 22 0
3 4C 09.57 BLL 17 51 32.81857318 +09 39 00.7284829   17.46 16.78 15.57   ~ 784 1
4 [CCE98b] 011.11-0.12 Cld 18 10.5 -19 23           ~ 82 1
5 NAME Dragon Nebula DNe 18 42 50.6 -04 03 30           ~ 98 0
6 GAL 035.03+00.35 HII 18 54 01.0 +02 01 32           ~ 34 0
7 [QZM2013] MM1 cor 18 58 12.98 +01 40 36.8           ~ 2 0
8 GAL 035.2-00.74 MoC 18 58 13 +01 40.6           ~ 151 0
9 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 89 0
10 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 132 0
11 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 388 0

    Equat.    Gal    SGal    Ecl

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2019.10.20-04:18:27

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