2015A&A...576A...1L


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.27CET01:44:25

2015A&A...576A...1L - Astronomy and Astrophysics, volume 576A, 1-1 (2015/4-1)

Ionized gas at the edge of the central molecular zone.

LANGER W.D., GOLDSMITH P.F., PINEDA J.L., VELUSAMY T., REQUENA-TORRES M.A. and WIESEMEYER H.

Abstract (from CDS):

The edge of the central molecular zone (CMZ) is the location where massive dense molecular clouds with large internal velocity dispersions transition to the surrounding more quiescent and lower CO emissivity region of the Galaxy. Little is known about the ionized gas surrounding the molecular clouds and in the transition region. We determine the properties of the ionized gas at the edge of the CMZ near Sgr E using observations of N+ and C+. We observed a small portion of the edge of the CMZ near Sgr E with spectrally resolved [CII]158µm and [NII]205µm fine structure lines at six positions with the GREAT instrument on SOFIA and in [CII] using Herschel HIFI on-the-fly strip maps. We use the [NII] spectra along with a radiative transfer model to calculate the electron density of the gas and the [CII] maps to illuminate the morphology of the ionized gas and model the column density of CO-dark H2. We detect two [CII] and [NII] velocity components, one along the line of sight to a CO molecular cloud at -207km/s associated with Sgr E and the other at -174km/s outside the edge of another CO cloud. From the [NII] emission we find that the average electron density is in the range of ∼5 to 21cm–3 for these features. This electron density is much higher than that of the disk's warm ionized medium, but is consistent with densities determined for bright diffuse HII nebula. The column density of the CO-dark H2 layer in the -207km/s cloud is ∼1-2x1021cm–2 in agreement with theoretical models. The CMZ extends further out in Galactic radius by ∼7 to 14pc in ionized gas than it does in molecular gas traced by CO. The edge of the CMZ likely contains dense hot ionized gas surrounding the neutral molecular material. The high fractional abundance of N+ and high electron density require an intense EUV field with a photon flux of order 106 to 107 photons/cm2/s, and/or efficient proton charge exchange with nitrogen, at temperatures of order 104K, and/or a large flux of X-rays. Sgr E is a region of massive star formation as indicated by the presence of numerous compact Hiiregions. The massive stars are potential sources of the EUV radiation that ionizes and heat the gas. In addition, X-ray sources and the diffuse X-ray emission in the CMZ are candidates for ionizing nitrogen.

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Journal keyword(s): ISM: clouds - HII regions - Galaxy: center

Simbad objects: 5

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Number of rows : 5

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 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 877 2
2 NAME Sgr E Rad 17 42 38 -29 48.2           ~ 42 0
3 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 635 1
4 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11257 0
5 [FYF2006] loop 1 MoC 23 48 +01.0           ~ 6 0

    Equat.    Gal    SGal    Ecl

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2020.02.27-01:44:25

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