2012A&A...542L..18S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST15:47:25

2012A&A...542L..18S - Astronomy and Astrophysics, volume 542, L18-18 (2012/6-1)

Globules and pillars seen in the [CII] 158 µm line with SOFIA.

SCHNEIDER N., GUESTEN R., TREMBLIN P., HENNEMANN M., MINIER V., HILL T., COMERON F., REQUENA-TORRES M.A., KRAEMER K.E., SIMON R., ROELLIG M., STUTZKI J., DJUPVIK A.A., ZINNECKER H., MARSTON A., CSENGERI T., CORMIER D., LEBOUTEILLER V., AUDIT E., MOTTE F., BONTEMPS S., SANDELL G., ALLEN L., MEGEATH T. and GUTERMUTH R.A.

Abstract (from CDS):

Molecular globules and pillars are spectacular features, found only in the interface region between a molecular cloud and an HII-region. Impacting far-ultraviolet (FUV) radiation creates photon-dominated regions (PDRs) on their surfaces that can be traced by typical cooling lines. With the GREAT receiver onboard SOFIA we mapped and spectrally resolved the [CII] 158µm atomic fine-structure line and the highly excited 12CO J=11-10 molecular line from three objects in Cygnus X (a pillar, a globule, and a strong IRAS source). We focus here on the globule and compare our data with existing Spitzer data and recent Herschel open-time PACS data. Extended [CII] emission and more compact CO-emission was found in the globule. We ascribe this emission mainly to an internal PDR, created by a possibly embedded star-cluster with at least one early B-star. However, external PDR emission caused by the excitation by the Cyg OB2 association cannot be fully excluded. The velocity-resolved [CII] emission traces the emission of PDR surfaces, possible rotation of the globule, and high-velocity outflowing gas. The globule shows a velocity shift of ∼2km/s with respect to the expanding HII-region, which can be understood as the residual turbulence of the molecular cloud from which the globule arose. This scenario is compatible with recent numerical simulations that emphazise the effect of turbulence. It is remarkable that an isolated globule shows these strong dynamical features traced by the [CII]-line, but it demands more observational studies to verify if there is indeed an embedded cluster of B-stars.

Abstract Copyright:

Journal keyword(s): ISM: clouds - ISM: individual objects: Cygnus - ISM: molecules - ISM: kinematics and dynamics - radio lines: ISM

Simbad objects: 8

goto Full paper

goto View the reference in ADS

Number of rows : 8

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 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 445 0
2 * alf Vir bC* 13 25 11.57937 -11 09 40.7501 -0.20 0.74 0.97 1.06 1.30 B1V 816 2
3 * bet Cen bC* 14 03 49.40535 -60 22 22.9266   0.38 0.60     B1III 338 0
4 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 935 2
5 SH 2-106 HII 20 27 26.8 +37 22 49           ~ 409 2
6 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 619 1
7 [BNM96] 079.296+0.284 HII 20 32 27.9386824590 +40 16 07.618081278           ~ 30 0
8 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 790 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2012A&A...542L..18S and select 'bookmark this link' or equivalent in the popup menu


2020.07.08-15:47:25

© Université de Strasbourg/CNRS

    • Contact