scholarly journals Radio continuum and molecular gas in the Galactic Center

2007 ◽  
pp. 185-192
Author(s):  
Yoshiaki Sofue
Keyword(s):  
Galactic Center ◽  
Radio Continuum ◽  
Molecular Gas

scholarly journals 4.1. Radio continuum and molecular gas in the Galactic center: large-scale structures

1998 ◽  
Vol 184 ◽  
pp. 161-168
Author(s):  
Yoshiaki Sofue
Keyword(s):  
Radio Emission ◽  
Linear Polarization ◽  
Large Scale ◽  
Galactic Center ◽  
Thermal Emission ◽  
Radio Continuum ◽  
Molecular Gas ◽  
Large Scale Structures ◽  
Almost Everywhere ◽  
Scale Structures

The radio emission from the Galactic Center is a mixture of thermal (free-free) and non-thermal (synchrotron) emissions (Fig. 1a). However, the spectral index in the central 3° region is flat almost everywhere (Sofue 1985), even in regions where strong linear polarization is detected. Therefore, a flat spectrum observed near the galactic center can no longer be taken as an indicator of thermal emission.

scholarly journals Large-Scale Ejection Structures in the Galactic Center

1989 ◽  
Vol 136 ◽  
pp. 213-231 ◽  
Author(s):  
Yoshiaki Sofue
Keyword(s):  
Magnetic Fields ◽  
Energy Release ◽  
Large Scale ◽  
Galactic Center ◽  
Galactic Plane ◽  
Radio Continuum ◽  
Molecular Gas ◽  
Unusual Manifestation ◽  
Continuum Structures ◽  
The Continuum

Radio continuum observations of the galactic center region have revealed a number of vertical structures running across the galactic plane, most of which are reasonably attributed either to vertical magnetic fields or to energy release out of the galactic plane. We review the observed radio structures and discuss their properties and origins with a particular attention to the unusual manifestation of energy release in the galactic center. The relation of the continuum structures to the expanding and/or contracting molecular gas rings is also discussed.

scholarly journals Low frequency (74 MHz) radio continuum observations of the inner 13° × 7° of the Galactic center

2013 ◽  
Vol 9 (S303) ◽  
pp. 464-466
Author(s):  
M. Rickert ◽  
F. Yusef-Zadeh ◽  
C. Brogan
Keyword(s):  
High Resolution ◽  
Molecular Cloud ◽  
Supernova Remnant ◽  
Galactic Center ◽  
Low Frequency ◽  
Radio Continuum ◽  
Large Array ◽  
Very Large Array ◽  
Image Displays ◽  
Western Side

AbstractWe analyze a high resolution (114″ × 60″) 74 MHz image of the Galactic center taken with the Very Large Array (VLA). We have identified several absorption and emission features in this region, and we discuss preliminary results of two Galactic center sources: the Sgr D complex (G1.1–0.1) and the Galactic center lobe (GCL).The 74 MHz image displays the thermal and nonthermal components of Sgr D and we argue the Sgr D supernova remnant (SNR) is consistent with an interaction with a nearby molecular cloud and the location of the Sgr D Hii region on the near side of the Galactic center. The image also suggests that the emission from the eastern side of the GCL contains a mixture of both thermal and nonthermal sources, whereas the western side is primarily thermal.

scholarly journals The TANGO Project: Thorough ANalysis of radio-Galaxies Observations

2009 ◽  
Vol 5 (S267) ◽  
pp. 127-127
Author(s):  
Breezy Ocaña Flaquer ◽  
Stephane Leon Tanne ◽  
Francoise Combes ◽  
Jeremy Lim
Keyword(s):  
Selection Criteria ◽  
Radio Galaxies ◽  
Elliptical Galaxies ◽  
Radio Continuum ◽  
Continuum Emission ◽  
Molecular Gas

AbstractWe present a sample of radio galaxies selected only on the basis of radio continuum emission and we confirm that these galaxies have lower molecular gas mass than other elliptical galaxies with different selection criteria.

The Warm Molecular Gas in the Galactic Center

2002 ◽  
pp. 331-332
Author(s):  
N. J. Rodríguez-Fernández ◽  
J. Martín-Pintado ◽  
P. De Vicente ◽  
A. Fuente
Keyword(s):  
Galactic Center ◽  
Molecular Gas

How maser observations unravel the gas motions in the Galactic Center

2017 ◽  
Vol 13 (S336) ◽  
pp. 176-179
Author(s):  
K. Immer ◽  
M. Reid ◽  
A. Brunthaler ◽  
K. Menten ◽  
Q. Zhang ◽  
...  
Keyword(s):  
Spectral Line ◽  
Proper Motion ◽  
Galactic Center ◽  
Galactic Plane ◽  
Orbital Dynamics ◽  
Line Of Sight ◽  
Molecular Gas ◽  
Kinematic Structure ◽  
3D Motion ◽  
Motion Measurements

AbstractThe Central Molecular Zone (CMZ), the inner 450 pc of our Galaxy, is an exceptional region where the volume and column densities, gas temperatures, velocity dispersions, etc. are much higher than in the Galactic plane. It has been suggested that the formation of stars and clusters in this area is related to the orbital dynamics of the gas. The complex kinematic structure of the molecular gas was revealed by spectral line observations. However, these results are limited to the line-of-sight-velocities. To fully understand the motions of the gas within the CMZ, we have to know its location in 6D space (3D location + 3D motion). Recent orbital models have tried to explain the inflow of gas towards and its kinematics within this region. With parallax and proper motion measurements of masers in the CMZ we can discriminate among these models and constrain how our Galactic Center is fed with gas.

scholarly journals Molecular and ionized gas kinematics in the GC Radio Arc

2016 ◽  
Vol 11 (S322) ◽  
pp. 133-136
Author(s):  
N. Butterfield ◽  
C.C. Lang ◽  
E. A. C. Mills ◽  
D. Ludovici ◽  
J. Ott ◽  
...  
Keyword(s):  
Star Formation ◽  
Molecular Cloud ◽  
Molecular Clouds ◽  
Radio Continuum ◽  
Molecular Gas ◽  
The South ◽  
Ionized Gas ◽  
Molecular Emission ◽  
Gas Kinematics

AbstractWe present NH3 and H64α+H63α VLA observations of the Radio Arc region, including the M0.20 – 0.033 and G0.10 – 0.08 molecular clouds. These observations suggest the two velocity components of M0.20 – 0.033 are physically connected in the south. Additional ATCA observations suggest this connection is due to an expanding shell in the molecular gas, with the centroid located near the Quintuplet cluster. The G0.10 – 0.08 molecular cloud has little radio continuum, strong molecular emission, and abundant CH3OH masers, similar to a nearby molecular cloud with no star formation: M0.25+0.01. These features detected in G0.10 – 0.08 suggest dense molecular gas with no signs of current star formation.

scholarly journals IRAS Observations of the Galactic Center

1989 ◽  
Vol 136 ◽  
pp. 121-128 ◽  
Author(s):  
P. Cox ◽  
R. Laureijs
Keyword(s):  
Near Infrared ◽  
Galactic Center ◽  
Galactic Disk ◽  
Radio Continuum ◽  
Star Formation History ◽  
Zodiacal Light ◽  
Heating Source ◽  
Formation History ◽  
Cool Stars ◽  
Center Area

IRAS observations of the Galactic Center are presented. The maps at 12, 25, 60 and 100 μm have a typical resolution of a few arcmin and cover an area 6×2 deg2 centered on SgrA. All data have been corrected for the zodiacal light contamination and for the diffuse emission associated with the galactic disk. The infrared radiation originating in the Galactic Center arises from well-defined sources which can be identified with known radio sources and from an extended emission which accounts for most of the infrared luminosity. The total infrared luminosity associated with the Galactic Center (area 3°×2°) amounts to 109L⊙. The sources contribute 10% to this luminosity. A comparison with surveys in the radio continuum and in the near infrared is presented. Results are analyzed in terms of star formation history. In particular, it is suggested that the dominant heating source for the dust is the population of cool stars - K and M giants - comprising the galactic nucleus.

scholarly journals Wide-Line Molecular Clouds and the Gamma-Ray Deficit Toward the Galactic Center

1989 ◽  
Vol 136 ◽  
pp. 157-158 ◽  
Author(s):  
J. G. Stacy ◽  
M. E. Bitran ◽  
T. M. Dame ◽  
P. Thaddeus
Keyword(s):  
Gravitational Field ◽  
Molecular Clouds ◽  
Stellar Population ◽  
Gamma Ray ◽  
Galactic Center ◽  
Molecular Gas ◽  
Show Evidence ◽  
Wide Line ◽  
Γ Ray ◽  
Co Emission

The discrepancy between observed and predicted γ-ray emission toward the Galactic Center is attributed to a unique population of wide-line molecular clouds. The most prominent objects of this class show evidence of rotation and a significant stellar population. The observed 12CO emission traces the gravitational field produced primarily by stars, not molecular gas.

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