scholarly journals Ionization of the Galactic Center Arched Filaments

1989 ◽  
Vol 120 ◽  
pp. 132-133
Author(s):  
R. Rubin ◽  
M. Morris ◽  
E.F. Erickson ◽  
S. Colgan ◽  
J. Simpson
Keyword(s):  
Fine Structure ◽  
Radio Emission ◽  
Galactic Center ◽  
Galactic Plane ◽  
Line Emission ◽  
Far Infrared ◽  
Thin Filaments ◽  
Ob Stars ◽  
Structure Line ◽  
Photoionization Model

The remarkable filament system seen in radio observations in the vicinity of the galactic center includes two thin filaments which arch away from the galactic plane (E.G. Yusef-Zadem et al 1984). The brightest part of each of these thermal structures is located at GO.10+0.02 and GO.07+0.04. Morris and Yusef-Zadem (1989) reason that photoionization by OB stars is unlikely on geometrical and morphological grounds. They suggest a magnetohydrodynamic mechanism to account for the radio emission and ionization. Erickson et al. (1968) were able to explain most of their observations of the far infrared (FIR) fine structure line emission from these locations in terms of a photoionization model.

The Orion Molecular Clouds OMC‐1 and OMC‐2 Mapped in the Far‐Infrared Fine‐Structure Line Emission of C+and O0

1997 ◽  
Vol 481 (1) ◽  
pp. 343-354 ◽  
Author(s):  
F. Herrmann ◽  
S. C. Madden ◽  
T. Nikola ◽  
A. Poglitsch ◽  
R. Timmermann ◽  
...  
Keyword(s):  
Fine Structure ◽  
Molecular Clouds ◽  
Line Emission ◽  
Far Infrared ◽  
Structure Line

scholarly journals Diffuse [CII] Emission in the Galaxy

1996 ◽  
Vol 169 ◽  
pp. 497-498
Author(s):  
H. Okuda ◽  
T. Nakagawa ◽  
H. Shibai ◽  
Y. Doi ◽  
K. Mochizuki ◽  
...  
Keyword(s):  
Intensity Distribution ◽  
Emission Intensity ◽  
Galactic Center ◽  
Galactic Plane ◽  
Line Emission ◽  
Far Infrared ◽  
Extensive Survey ◽  
The Galaxy ◽  
Infrared Continuum ◽  
Tangential Directions

An extensive survey of [C II] line emission at 158 microns using the balloon borne telescope (BICE) has provided a complete map of the emission intensity distribution in the first and the fourth quadrants of the galactic plane (280° < l < 80°, −5° < b < 5°: Okuda et al. 1993). The emission is very extended throughout the galactic plane in which three intensity maxima are seen towards the tangential directions of the Scutum and the Norma arms as well as in the Galactic center region. However the Galactic center maximum is much less prominent compared with the two other distributions, unlike the case of far infrared continuum and CO emissions.

scholarly journals A 158μm [CII] Map of NGC 6946: Detection in Extragalactic Atomic and Ionized Gas

1992 ◽  
Vol 150 ◽  
pp. 117-119
Author(s):  
S. C. Madden ◽  
N. Geis ◽  
R. Genzel ◽  
F. Herrmann ◽  
A. Poglitsch ◽  
...  
Keyword(s):  
Infrared Imaging ◽  
Line Emission ◽  
Far Infrared ◽  
Max Planck ◽  
Ionized Gas ◽  
Ob Stars ◽  
Ngc 6946 ◽  
Total Luminosity ◽  
Fabry Perot ◽  
External Galaxies

The first observations of the [CII] line toward the nuclei of gas-rich external galaxies, showed that the far-infrared line emission contributes up to 1% of the total luminosity and most likely originates from dense photon-dominated regions (PDRs) associated with the surfaces of molecular clouds exposed to FUV from external or embedded OB stars (Crawford et al. 1985, Lugten et al. 1986, Stacey et al. 1991). We have mapped the [CII] emission toward NGC 6946 over an 8' × 6' (23 × 17 kpc) (Madden et al. 1991) using the Max-Planck Instutute/U.C.Berkeley Far-Infrared Imaging Fabry-Perot Interferometer (FIFI) on the Kuiper Airborne Observatory (KAO).

Far-infrared forbidden O III line emission from the galactic center

1980 ◽  
Vol 241 ◽  
pp. L43 ◽  
Author(s):  
D. M. Watson ◽  
J. W. V. Storey ◽  
C. H. Townes ◽  
E. E. Haller
Keyword(s):  
Galactic Center ◽  
Line Emission ◽  
Far Infrared

Surprisingly weak fine-structure line emission from S 140

2015 ◽  
Vol 75-76 ◽  
pp. 199-200
Author(s):  
V. Ossenkopf ◽  
E. Koumpia ◽  
Y. Okada ◽  
B. Mookerjea ◽  
F.F.S. van der Tak
Keyword(s):  
Fine Structure ◽  
Line Emission ◽  
Structure Line

scholarly journals The ‘Red Radio Ring’: ionized and molecular gas in a starburst/active galactic nucleus at z ∼ 2.55

2019 ◽  
Vol 488 (2) ◽  
pp. 1489-1500 ◽  
Author(s):  
Kevin C Harrington ◽  
A Vishwas ◽  
A Weiß ◽  
B Magnelli ◽  
L Grassitelli ◽  
...  
Keyword(s):  
Fine Structure ◽  
Spectral Energy Distribution ◽  
Formation Rate ◽  
Line Emission ◽  
Far Infrared ◽  
Spectral Energy ◽  
Molecular Gas ◽  
H Ii Regions ◽  
Galaxy Assembly ◽  
Dust Attenuation

ABSTRACT We report the detection of the far-infrared (FIR) fine-structure line of singly ionized nitrogen, [N ii] 205 $\mu$m , within the peak epoch of galaxy assembly, from a strongly lensed galaxy, hereafter ‘The Red Radio Ring’; the RRR, at z = 2.55. We combine new observations of the ground-state and mid-J transitions of CO (Jup = 1, 5, 8), and the FIR spectral energy distribution (SED), to explore the multiphase interstellar medium (ISM) properties of the RRR. All line profiles suggest that the H ii regions, traced by [N ii] 205 $\mu$m , and the (diffuse and dense) molecular gas, traced by CO, are cospatial when averaged over kpc-sized regions. Using its mid-IR-to-millimetre (mm) SED, we derive a non-negligible dust attenuation of the [N ii] 205 $\mu$m line emission. Assuming a uniform dust screen approximation results a mean molecular gas column density &gt;1024 cm−2, with a molecular gas-to-dust mass ratio of 100. It is clear that dust attenuation corrections should be accounted for when studying FIR fine-structure lines in such systems. The attenuation corrected ratio of $L_{\rm N\,{\small II}205} / L_{\rm IR(8\!-\!1000\, \mu m)} = 2.7 \times 10^{-4}$ is consistent with the dispersion of local and z &gt; 4 SFGs. We find that the lower limit, [N ii] 205 $\mu$m -based star formation rate (SFR) is less than the IR-derived SFR by a factor of 4. Finally, the dust SED, CO line SED, and $L_{\rm N\,{\small II}205}$ line-to-IR luminosity ratio of the RRR is consistent with a starburst-powered ISM.

scholarly journals Transfer of continuum UV radiation inside fragmented clouds

1991 ◽  
Vol 147 ◽  
pp. 394-395
Author(s):  
P. Boisse
Keyword(s):  
Magnetic Field ◽  
Fine Structure ◽  
Energy Balance ◽  
Line Emission ◽  
Photoelectric Effect ◽  
Interstellar Clouds ◽  
Governing Factor ◽  
Structure Line ◽  
Fractional Ionization ◽  
The Magnetic Field

The penetration of visible and UV continuum radiation is a governing factor for many processes inside interstellar clouds. It determines for instance: 1) the overall chemical equilibrium (formation/destruction of molecules and neutral or ionized species, fractional ionization of the gas which is directly related to the coupling with the magnetic field); 2) the overall energy balance (heating of the dust, heating of the gas through collisions with electrons extracted from grains by the photoelectric effect or with grains; 3) cooling of the gas due to fine structure line emission (OI,CI,CII).

scholarly journals Neon Fine‐Structure Line Emission by X‐Ray Irradiated Protoplanetary Disks

2007 ◽  
Vol 656 (1) ◽  
pp. 515-523 ◽  
Author(s):  
Alfred E. Glassgold ◽  
Joan R. Najita ◽  
Javier Igea
Keyword(s):  
Fine Structure ◽  
Line Emission ◽  
Protoplanetary Disks ◽  
X Ray ◽  
Structure Line

scholarly journals Radio Stars of the SKA

Universe ◽  
2021 ◽  
Vol 7 (5) ◽  
pp. 119
Author(s):  
Bin Yu ◽  
Albert Zijlstra ◽  
Biwei Jiang
Keyword(s):  
Radio Emission ◽  
Milky Way ◽  
Galactic Plane ◽  
High Sensitivity ◽  
Hii Regions ◽  
Be Stars ◽  
M Dwarfs ◽  
Ob Stars ◽  
5 Ghz ◽  
Radio Stars

Radio emission from stars can be used, for example, to study ionized winds or stellar flares. The radio emission is faint and studies have been limited to few objects. The Square Kilometer Array (SKA) brings a survey ability to the topic of radio stars. In this paper we investigate what the SKA can detect, and what sensitivity will be required for deep surveys of the stellar Milky Way. We focus on the radio emission from OB stars, Be stars, flares from M dwarfs, and Ultra Compact HII regions. The stellar distribution in the Milky Way is simulated using the Besançon model, and various relations are used to predict their radio flux. We find that the full SKA will easily detect all UltraCompact HII regions. At the limit of 10 nJy at 5 GHz, the SKA can detect 1500 Be stars and 50 OB stars per square degree, out to several kpc. It can also detect flares from 4500 M dwarfs per square degree. At 100 nJy, the numbers become about 8 times smaller. SKA surveys of the Galactic plane should be designed for high sensitivity. Deep imaging should consider the significant number of faint flares in the field, even outside the plane of the Milky Way.

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