2017A&A...599A.136L


Query : 2017A&A...599A.136L

2017A&A...599A.136L - Astronomy and Astrophysics, volume 599A, 136-136 (2017/3-1)

Kinematics and properties of the central molecular zone as probed with [C II].

LANGER W.D., VELUSAMY T., MORRIS M.R., GOLDSMITH P.F. and PINEDA J.L.

Abstract (from CDS):

Context. The Galactic central molecular zone (CMZ) is a region containing massive and dense molecular clouds, with dynamics driven by a variety of energy sources including a massive black hole.It is thus the nearest template for understanding physical processes in extragalactic nuclei. The CMZ's neutral interstellar gas has been mapped spectrally in many neutral atomic and molecular gas tracers, but the ionized and CO-dark H2 regions are less well traced spectroscopically.
Aims. We identify features of the UV irradiated neutral gas, photon dominated regions (PDRs) and CO-dark H2, and highly ionized gas in the CMZ as traced by the fine structure line of C+ at 158µm, [CII], and characterize their properties.
Methods. We observed the [CII] 158µm fine structure line with high spectral resolution using Herschel HIFI with two perpendicular on-the-fly strip scans, along l=-0.8 to +0.8 and b=-0.8 to +0.8, both centered on (l, b)=(0°, 0°). We analyze the spatial-velocity distribution of the [CII] data, compare them to those of [CI] and CO, and to dust continuum maps, in order to determine the properties and distribution of the ionized and neutral gas and its dynamics within the CMZ.
Results. The longitude- and latitude-velocity maps of [CII] trace portions of the orbiting open gas streams of dense molecular clouds, the cloud G0.253+0.016, also known as the Brick, the arched filaments, the ionized gas within several pc of Sgr A and Sgr B2, and the warm dust bubble. We use the [CII] data to determine the physical and dynamical properties of these CMZ features.
Conclusions. The bright far-IR 158µm C+ line, [CII], when observed with high spatial and spectral resolution, traces a wide range of emission features in the CMZ. The [CII] emission arises primarily from dense PDRs and highly ionized gas, and is an important tracer of the kinematics and physical conditions of this gas.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: ISM - Galaxy: center - ISM: clouds - ISM: atoms - ISM: atoms

CDS comments: G0.217+0.0 and G0.250+0.0 not in SIMBAD.

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13449 0
2 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 4049 3
3 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 700 0
4 NAME the Brick MoC 17 46 09 -28 43.8           ~ 181 0
5 LBN 000.03+00.13 HII 17 46.2 -28 51           ~ 16 0
6 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 503 0
7 GCM +0.20 -0.03 MoC 17 46 14 -28 46.8           ~ 11 0
8 2E 3944 LXB 17 46 21.09 -28 43 42.3     12.50     ~ 119 0
9 NAME Sgr B MoC 17 47 02 -28 25.4           ~ 213 0
10 NAME Sgr B2 (North) Rad 17 47 20.2 -28 22 21           ~ 625 1
11 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 2150 1
12 NAME Sgr B2 Main Rad 17 47 20.5 -28 23 06           ~ 380 1
13 NAME Heeschen Cloud Cld ~ ~           ~ 12 0

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2023.02.02-19:33:45

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