2018A&A...616A..31M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST19:15:00

2018A&A...616A..31M - Astronomy and Astrophysics, volume 616A, 31-31 (2018/8-1)

C+ distribution around S 1 in ρ Ophiuchi.

MOOKERJEA B., SANDELL G., VACCA W., CHAMBERS E. and GUSTEN R.

Abstract (from CDS):

We analyze a [CII] 158µm map obtained with the L2 GREAT receiver on SOFIA of the reflection nebula illuminated by the early B star S 1 in the ρ Oph A cloud core. This data set has been complemented with maps of CO(3-2), 13CO(3-2), and C18O(3-2), observed as a part of the James Clerk Maxwell Telescope (JCMT) Gould Belt Survey, with archival HCO+(4-3) JCMT data, as well as with [OI] 63 and 145 µm imaging with Herschel/PACS. The [CII] emission is completely dominated by the strong emission from the photon dominated region (PDR) in the nebula surrounding S 1 expanding into the dense Oph A molecular cloud west and south of S 1. The [CII] emission is significantly blueshifted relative to the CO spectra and also relative to the systemic velocity, particularly in the northwestern part of the nebula. The [CII] lines are broader toward the center of the S 1 nebula and narrower toward the PDR shell. The [CII] lines are strongly self-absorbed over an extended region in the S 1 PDR. Based on the strength of the [13CII] F=2-1 hyperfine component, [CII] is significantly optically thick over most of the nebula. CO and 13CO(3-2) spectra are strongly self-absorbed, while C18O(3-2) is single peaked and centered in the middle of the self-absorption. We have used a simple two-layer LTE model to characterize the background and foreground cloud contributing to the [CII] emission. From this analysis we estimated the extinction due to the foreground cloud to be ∼9.9mag, which is slightly less than the reddening estimated toward S 1. Since some of the hot gas in the PDR is not traced by low-J CO emission, this result appears quite plausible. Using a plane parallel PDR model with the observed [OI](145)/[CII] brightness ratio and an estimated FUV intensity of 3100-5000G0 suggests that the density of the [CII] emitting gas is ∼3-4x103cm–3.

Abstract Copyright: © ESO 2018

Journal keyword(s): HII regions - ISM: molecules - ISM: clouds - submillimeter: ISM - submillimeter: diffuse background

Simbad objects: 12

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Number of rows : 12

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 HD 17889 * 02 58 56.7253089187 +77 04 48.261449380   7.73 6.87     G0 9 0
2 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 570 1
3 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1071 1
4 HD 147889 pr* 16 25 24.3162969787 -24 27 56.570239619 8.56 8.73 7.90     B2III/IV 433 1
5 EM* SR 3 Y*O 16 26 09.3231207767 -24 34 12.176811236   10.9 9.88   9.01 A0 106 0
6 GSS 30 Y*O 16 26 21.38160 -24 23 04.0524           ~ 200 1
7 NAME rho Oph A Cloud MoC 16 26 26.4 -24 22 33           ~ 238 1
8 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 373 0
9 GSS 35 TT* 16 26 34.1750440278 -24 23 28.331873112     16.53 14.75 12.51 B3 214 1
10 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
11 NAME Oph Cloud Complex DNe 16 30 -24.3           ~ 63 1
12 LDN 1689N DNe 16 32 31 -24 28.6           ~ 108 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-19:15:00

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