2014A&A...571A..52B


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET12:13:10

2014A&A...571A..52B - Astronomy and Astrophysics, volume 571A, 52-52 (2014/11-1)

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA.

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

Abstract (from CDS):

Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion. To test the theoretical predictions on the formation of massive stars, we wish to make a thorough study at high-angular resolution of the structure and kinematics of the dust and gas emission toward the high-mass star-forming region G35.03+0.35, which harbors a disk candidate around a B-type (proto)star. We carried out ALMA Cycle 0 observations at 870µm of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of <0.5". Complementary Subaru COMICS 25µm observations were carried out to trace the mid-infrared emission toward this star-forming region. The submillimeter continuum emission has revealed a filamentary structure fragmented into six cores, called A-F. The filament could be in quasi-equilibrium taking into account that the mass per unit length of the filament, 200-375M/pc, is similar to the critical mass of a thermally and turbulently supported infinite cylinder, ∼335M/pc. The cores, which are on average separated by ∼0.02 pc, have deconvolved sizes of 1300-3400AU, temperatures of 35-240K, H2 densities >107cm–3, and masses in the range 1-5M, and they are subcritical. Core A, which is associated with a hypercompact HII region and could be the driving source of the molecular outflow observed in the region, is the most chemically rich source in G35.03+0.35 with strong emission of typical hot core tracers such as CH3CN. Tracers of high density and excitation show a clear velocity gradient along the major axis of the core, which is consistent with a disk rotating about the axis of the associated outflow. The PV plots along the SE-NW direction of the velocity gradient show clear signatures of Keplerian rotation, although infall could also be present, and they are consistent with the pattern of an edge-on Keplerian disk rotating about a star with a mass in the range 5-13M. The high tff/trot ratio for core A suggests that the structure rotates fast and that the accreting material has time to settle into a centrifugally supported disk. G35.03+0.35 is one of the most convincing examples of Keplerian disks rotating about high-mass (proto)stars. This supports theoretical scenarios according to which high-mass stars, at least B-type stars, would form through disk-mediated accretion.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: G35.03+0.35 - ISM: molecules - stars: formation - stars: kinematics and dynamics - regions HII

Nomenclature: Table 3: [BSC2014] A (Nos A-F).

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 - 2021
#notes
1 RAFGL 490 Y*O 03 27 38.7928323987 +58 47 00.017662871           ~ 341 0
2 * del Oph PM* 16 14 20.73853 -03 41 39.5612 6.30 4.34 2.75 1.46 0.43 M0.5III 346 0
3 * bet Oph PM* 17 43 28.3526482 +04 34 02.295484 5.150 3.930 2.750 1.96 1.38 K2IIICN0.5 456 0
4 4C 09.57 BLL 17 51 32.81857318 +09 39 00.7284829   17.46 16.78 15.57   ~ 833 1
5 NAME HH 80-81 HH 18 19 06 -20 51.4           ~ 198 0
6 NAME HH 80-81 IRS HII 18 19 11.8 -20 47 35           ~ 135 0
7 GAL 029.96-00.02 Y*O 18 46 03.7 -02 39 21           ~ 336 1
8 [CBH2011c] EGO G35.03+0.35 -CM5 Rad 18 54 00.45 +02 01 21.2           ~ 5 0
9 [BSC2014] E cor 18 54 00.453 +02 01 17.54           ~ 2 0
10 [BSC2014] F cor 18 54 00.479 +02 01 17.06           ~ 2 0
11 [BSC2014] D cor 18 54 00.479 +02 01 18.90           ~ 2 0
12 [BSC2014] C cor 18 54 00.490 +02 01 20.26           ~ 2 0
13 [CBH2011c] EGO G35.03+0.35 -CM1 Rad 18 54 00.49098 +02 01 18.2920           ~ 9 0
14 EGO G035.03+0.35 of? 18 54 00.5 +02 01 18           ~ 24 0
15 [CBH2011c] EGO G35.03+0.35 -CM4 Rad 18 54 00.523 +02 01 15.60           ~ 6 0
16 [BSC2014] B cor 18 54 00.586 +02 01 19.78           ~ 2 0
17 [BSC2014] A cor 18 54 00.645 +02 01 19.23           ~ 5 0
18 [CBH2011c] EGO G35.03+0.35 -CM2 Rad 18 54 00.6498 +02 01 19.320           ~ 10 0
19 [CBH2011c] EGO G35.03+0.35 -CM3 Rad 18 54 00.766 +02 01 22.82           ~ 7 0
20 GAL 035.03+00.35 HII 18 54 01.0 +02 01 32           ~ 41 0
21 [CPA2006] N65 bub 18 54 02.0 +01 59 30           ~ 14 0
22 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 97 0
23 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 403 0
24 NAME AFGL 2591 N3 Y*O 20 29 24.88 +40 11 19.5           ~ 35 1
25 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 573 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-12:13:10

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