Dynamical response of the interstellar medium to explosions at the galactic center

1976 ◽  
Vol 208 ◽  
pp. 52 ◽  
Author(s):  
R. J. Defouw
Keyword(s):  
Interstellar Medium ◽  
Galactic Center ◽  
Dynamical Response

Kinematical Structure of the Local Interstellar Medium: The Galactic Center Hemisphere

1997 ◽  
Vol 484 (2) ◽  
pp. 761-778 ◽  
Author(s):  
Ricardo Genova ◽  
John E. Beckman ◽  
Stuart Bowyer ◽  
Thomas Spicer
Keyword(s):  
Interstellar Medium ◽  
Galactic Center ◽  
Local Interstellar Medium

The Hot Interstellar Medium of the Galactic Center: Observations with Chandra

1997 ◽  
pp. 281-285 ◽  
Author(s):  
M. Morris ◽  
C. Howard ◽  
M. Muno ◽  
F. K. Baganoff ◽  
S. Park ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Galactic Center

scholarly journals ISO observations of the Galactic center interstellar medium

2005 ◽  
Vol 429 (3) ◽  
pp. 923-938 ◽  
Author(s):  
N. J. Rodríguez-Fernández ◽  
J. Martín-Pintado
Keyword(s):  
Interstellar Medium ◽  
Galactic Center

scholarly journals Kinematical Structure of the Local Interstellar Medium

1997 ◽  
Vol 166 ◽  
pp. 195-198
Author(s):  
R. Génova ◽  
J. E. Beckman ◽  
J. Rodríguez Álamo
Keyword(s):  
Interstellar Medium ◽  
Velocity Vector ◽  
Galactic Center ◽  
Galactic Plane ◽  
The Sun ◽  
Local Interstellar Medium

AbstractObservations of interstellar Na I in the spectra of 93 stars within 315 pc from the Sun show that it lies in a tunnel of gas moving away from Scorpio-Centaurus and is surrounded by gas moving toward the Galactic center.Gas approaches the Sun from Scorpio-Centaurus expanding from (r, l, b)=(160 pc, 313°7, +28°2) with LSR velocity 15.3 km s−1. The radius of this shell is 153 pc.We identify these clouds:D: velocity vector (υd, ld, bd)=(+7.2 km s−1, 305°1, −13°5), above and below the Galactic plane (GP) in the range of Galactic longitudes 357°–55°.C: velocity vector (υc, lc, bc)=(+11.5 km s−1, 349°0, −35°2), above and below the GP in the range 30°≤l≤110°.M: velocity vector (υm, lm, bm)=(+21.9 km s−1, 34°2, +1°5), above and below the GP in the range 100°≤l≤130°.P: velocity vector (υp, lp, bp)=(+13.8 km s−1, 244°9, +5°4), above and below the GP from l~120° to the limit of our data at l~210°.E: velocity vector (υe, le, be)=(+16.8 km s−1, 208°4, +6°2) in the range 160°≤l≤185° and −10°≤b≤–35°.A: velocity vector (υa, la, ba)=(+12.9 km s−1, 73°6, −5°6) towards the Galactic anti-center, below the GP.I: velocity vector (υi, li, bi)=(+37.7 km s−1, 132°8, −64°3) towards the Galactic anti-center, above the GP.

scholarly journals The Galactic center: not an active galactic nucleus

2013 ◽  
Vol 9 (S303) ◽  
pp. 54-58
Author(s):  
Deokkeun An ◽  
Solange V. Ramírez ◽  
Kris Sellgren
Keyword(s):  
Interstellar Medium ◽  
Emission Line ◽  
Active Galactic Nuclei ◽  
Active Galactic Nucleus ◽  
Galactic Center ◽  
Galactic Nuclei ◽  
Extensive Area ◽  
Star Forming ◽  
Nearby Galaxies

AbstractWe present 10 μm – 35μm Spitzer spectra of the interstellar medium in the central molecular zone (CMZ), the central 210 pc × 60 pc of the Galactic center (GC). We present maps of the CMZ in ionic and H2 emission, covering a more extensive area than earlier spectroscopic surveys in this region. We compare diagnostic line ratios measured in the Spitzer Infrared Nearby Galaxies Survey to our data. Previous work shows that forbidden line ratios can distinguish star-forming galaxies from low-ionization nuclear emission-line regions (LINERs) and active galactic nuclei (AGNs). Our GC line ratios agree with star-forming galaxies and not with LINERs or AGNs.

scholarly journals Dynamics and Interactions of High-Redshift Galaxies

1999 ◽  
Vol 186 ◽  
pp. 431-438
Author(s):  
M. Noguchi
Keyword(s):  
Galaxy Evolution ◽  
Galactic Center ◽  
Hubble Space Telescope ◽  
Gravitational Instability ◽  
High Redshift ◽  
Evolutionary Process ◽  
Dynamical Response ◽  
Massive Black Hole ◽  
High Redshift Galaxies ◽  
Redshift Galaxies

A large number of high redshift galaxies observed with the Hubble Space Telescope (HST) show anomalous morphology and photometric properties, which may be an indication of evolutionary process in young galaxies. We show here by means of numerical simulations that the copious interstellar gas existing in the disks of rapidly collapsing protogalaxies can bring about these peculiarities. Gravitational instability in a gas-rich disk leads to the formation of massive gas clumps with a typical mass of 109M⊙. These subgalactic clumps make disk galaxy evolution a dynamically energetic and chaotic process, and give a natural explanation for peculiar morphology of high redshift galaxies. Moreover, the present model provides a new picture on the causal relationship between the emergence of quasar activities and the dynamical evolution of host galaxies. The clump-driven evolution model is also capable of explaining the correlations observed among present-day galaxies. Namely, the relative bulge dominance, existence of a thick disk, and a mass of the super-massive black hole situated at the galactic center should all be correlated positively. In contrast to their vigorous evolution in isolated state, primeval disk galaxies do not show any dramatic enhancement of activity or remarkable dynamical response in interaction with another galaxies.

scholarly journals 7.4. The 3.4 micron absorption in the Galactic center sources

1998 ◽  
Vol 184 ◽  
pp. 299-300
Author(s):  
T. Nagata
Keyword(s):  
Interstellar Medium ◽  
Near Infrared ◽  
Galactic Center ◽  
Absorption Feature ◽  
Visual Extinction ◽  
Stretching Vibrations ◽  
Central Parsec ◽  
Infrared Sources

The 3.4μm absorption feature, first detected in the Galactic center source IRS7 (Soifer et al., 1976), has been observed in other Galactic center sources IRS3, IRS12 (McFadzean et al., 1989), and IRS6E (Pendleton et al., 1994). This feature is regarded as characteristic of dust in the diffuse interstellar medium, and attributed to C-H stretching vibrations. Several objects in the lines of sight other than the Galactic center is now known to have the feature (Sandford et al. 1995 and references therein; Imanishi et al. 1996). The absorption depths per unit visual extinction τ3.4/AV for these sources are compared with those for the Galactic center sources, and they are thought to increase near the Galactic center. However, the “Galactic center” sources are all in the central parsec cluster, and the features observed in them may be only representative of interstellar medium local to the central parsec, not the general diffuse interstellar medium of the inner Galaxy. In this paper, we report the 3.4μm absorption feature detected in near-infrared sources within 1° of the Galactic center.

scholarly journals The Mid‐Infrared Colors of the Interstellar Medium and Extended Sources at the Galactic Center

2008 ◽  
Vol 682 (1) ◽  
pp. 384-399 ◽  
Author(s):  
R. G. Arendt ◽  
S. R. Stolovy ◽  
S. V. Ramírez ◽  
K. Sellgren ◽  
A. S. Cotera ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Galactic Center ◽  
Mid Infrared ◽  
Extended Sources
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