2011A&A...532A..88V


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:45:54

2011A&A...532A..88V - Astronomy and Astrophysics, volume 532A, 88-88 (2011/8-1)

The JCMT spectral legacy survey: physical structure of the molecular envelope of the high-mass protostar AFGL 2591.

VAN DER WIEL M.H.D., VAN DER TAK F.F.S., SPAANS M., FULLER G.A., PLUME R., ROBERTS H. and WILLIAMS J.L.

Abstract (from CDS):

The understanding of the formation process of massive stars (γ8M) is limited by a combination of theoretical complications and observational challenges. The high UV luminosities of massive stars give rise to chemical complexity in their natal molecular clouds and affect the dynamical properties of their circumstellar envelopes. We investigate the physical structure of the large-scale (∼104-105AU) molecular envelope of the high-mass protostar AFGL2591. Observational constraints are provided by spectral imaging in the 330-373GHz regime from the JCMT Spectral Legacy Survey and its high-frequency extension. While the majority of the ∼160 spectral features from the survey cube are spatially unresolved, this paper uses the 35 that are significantly extended in the spatial directions. For these features we present integrated intensity maps and velocity maps. The observed spatial distributions of a selection of six species are compared with radiative transfer models based on (i) a static spherically symmetric structure; (ii) a dynamic spherical structure; and (iii) a static flattened structure. The maps of CO and its isotopic variations exhibit elongated geometries on scales of ∼100'', and smaller scale substructure is found in maps of N2H+, o-H2CO, CS, SO2, C2H, and various CH3OH lines. In addition, a line-of-sight velocity gradient is apparent in maps of all molecular lines presented here, except SO, SO2, and H2CO. We find two emission peaks in warm (Eup ∼200K) CH3OH separated by 12'' (12000AU), indicative of a secondary heating source in the envelope. The spherical models are able to explain the distribution of emission for the optically thin H13CO+ and C34S, but not for the optically thick HCN, HCO+, and CS or for the optically thin C17O. The introduction of velocity structure mitigates the optical depth effects, but does not fully explain the observations, especially in the spectral dimension. A static flattened envelope viewed at a small inclination angle does slightly better. Based on radiative transfer modeling, we conclude that a geometry of the envelope other than an isotropic static sphere is needed to circumvent line optical depth effects. We propose that this could be achieved in circumstellar envelope models with an outflow cavity and/or an inhomogeneous structure on scales λ104AU. The picture of inhomogeneity is supported by substructure observed in at least six different species.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: molecules - ISM: individual objects: AFGL2591 - techniques: imaging spectroscopy

Simbad objects: 9

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Number of rows : 9

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 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 596 1
2 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 465 0
3 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 553 0
4 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
5 W 49a SFR 19 10 15.7 +09 06 05           ~ 258 2
6 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 619 1
7 NAME AFGL 2591 N2 Y*O 20 29 24.52 +40 11 20.1           ~ 17 1
8 NAME AFGL 2591 N1 Y*O 20 29 24.59 +40 11 15.0           ~ 19 1
9 RAFGL 2591 Y*O 20 29 25.03656 +40 11 20.3316           ~ 570 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:45:54

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