2018A&A...617A..89C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:13:17

2018A&A...617A..89C - Astronomy and Astrophysics, volume 617A, 89-89 (2018/9-1)

Search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS). I. Indication for a centrifugal barrier in the environment of a single high-mass envelope.

CSENGERI T., BONTEMPS S., WYROWSKI F., BELLOCHE A., MENTEN K.M., LEURINI S., BEUTHER H., BRONFMAN L., COMMERCON B., CHAPILLON E., LONGMORE S., PALAU A., TAN J.C. and URQUHART J.S.

Abstract (from CDS):

The conditions leading to the formation of the most massive O-type stars are still an enigma in modern astrophysics. To assess the physical conditions of high-mass protostars in their main accretion phase, here we present a case study of a young massive clump selected from the ATLASGAL survey, G328.2551-0.5321. The source exhibits a bolometric luminosity of 1.3x104L, which allows us to estimate that its current protostellar mass lies between ∼11 and 16M. We show high angular resolution observations with ALMA that reach a physical scale of ∼400au. To reveal the structure of this high-mass protostellar envelope in detail at a ∼0.17'' resolution, we used the thermal dust continuum emission and spectroscopic information, amongst others from the CO (J=3-2) line, which is sensitive to the high-velocity molecular outflow of the source. We also used the SiO (J=8-7) and SO2 (J=82,6-71,7) lines, which trace shocks along the outflow, as well as several CH3OH and HC3N lines that probe the gas of the inner envelope in the closest vicinity of the protostar. Our observations of the dust continuum emission reveal a single high-mass protostellar envelope, down to our resolution limit. We find evidence for a compact, marginally resolved continuum source that is surrounded by azimuthal elongations that could be consistent with a spiral pattern. We also report on the detection of a rotational line of CH3OH within its vt=1 torsionally excited state. This shows two bright emission peaks that are spatially offset from the dust continuum peak and exhibit a distinct velocity component ±4.5km/s offset from the systemic velocity of the source. Rotational diagram analysis and models based on local thermodynamic equilibrium assumption require high CH3OH column densities that reach N(CH3OH)=1.2-2x1019cm–2, and kinetic temperatures of the order of 160-200 K at the position of these peaks. A comparison of their morphology and kinematics with those of the outflow component of the CO line and the SO2 line suggests that the high-excitation CH3OH spots are associated with the innermost regions of the envelope. While the HC3N v7=0 (J=37-36) line is also detected in the outflow, the HC3N v7=1e (J=38-37) rotational transition within the first vibrationally excited state of the molecule shows a compact morphology. We find that the velocity shifts at the position of the observed high-excitation CH3 OH spots correspond well to the expected Keplerian velocity around a central object with 15M consistent with the mass estimate based on the bolometric luminosity of the source. We propose a picture where the CH3 OH emission peaks trace the accretion shocks around the centrifugal barrier, pinpointing the interaction region between the collapsing envelope and an accretion disc. The physical properties of the accretion disc inferred from these observations suggest a specific angular momentum several times higher than typically observed towards low-mass protostars. This is consistent with a scenario of global collapse setting on at larger scales that could carry a more significant amount of kinetic energy compared to the core-collapse models of low-mass star formation. Furthermore, our results suggest that vibrationally excited HC3 N emission could be a new tracer for compact accretion discs around high-mass protostars.

Abstract Copyright: © ESO 2018

Journal keyword(s): accretion, accretion disks - stars: massive - stars: formation - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/A+A/617/A89): list.dat fits/*>

Simbad objects: 17

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Number of rows : 17

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 LDN 1527 DNe 04 39 53 +25 45.0           ~ 495 0
2 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1359 0
3 RAFGL 4176 IR 13 43 01.704 -62 08 51.23           ~ 87 0
4 MSXDC G328.25-0.51 a cor 15 57 55 -53 57.4           ~ 3 0
5 IRAS 15541-5349 HII 15 57 59.75 -53 58 00.4           ~ 51 0
6 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 373 0
7 GSS 39 Y*O 16 26 45.0321556934 -24 23 07.808781522           M0 141 1
8 IRAS 16562-3959 SFR 16 59 42.257 -40 03 45.17           ~ 47 0
9 LDN 1746 DNe 17 11.3 -27 22           ~ 108 0
10 2MASS J17112317-2724315 ** 17 11 23.18 -27 24 31.5           ~ 43 0
11 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1
12 MSX5C G023.0126-00.4177 IR 18 34 42.2 -09 00 41           ~ 45 0
13 [DLW84] G35.2N HII 18 58 13.036 +01 40 36.00           ~ 91 0
14 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 396 0
15 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 570 0
16 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 484 0
17 [MBS2007c] CygX-N63 mm 20 40 05.2 +41 32 13           ~ 14 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:13:17

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