The spatial distribution of 10 micron luminosity in spiral galaxies

1987 ◽  
Vol 323 ◽  
pp. 91 ◽  
Author(s):  
Nicholas Devereux
Keyword(s):  
Spatial Distribution ◽  
Spiral Galaxies

scholarly journals Spatial distribution of different subtypes of core-collapse and thermonuclear supernovae in the galaxies

2017 ◽  
Vol 12 (S331) ◽  
pp. 75-80
Author(s):  
Dmitry Yu. Tsvetkov ◽  
Nickolay N. Pavlyuk
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Spiral Galaxies ◽  
Galactic Plane ◽  
Scale Height ◽  
Core Collapse ◽  
Strong Concentration ◽  
Different Types ◽  
Central Regions ◽  
Thermonuclear Supernovae

AbstractThe distributions of supernovae of different types and subtypes along the radius and in z coordinate of galaxies have been studied. We show that among SNe Ia in spiral galaxies, SNe Iax and Ia-norm have, respectively, the largest and smallest concentration to the center; the distributions of SNe Ia-91bg and Ia-91T are similar. A strong concentration of SNe Ibc to the central regions has been confirmed. In spiral galaxies, the supernovae of all types strongly concentrate to the galactic plane; the slight differences in scale height correlate with the extent to which the classes of supernovae are associated with star formation.

scholarly journals Kinematics and the Galactic Potential

1998 ◽  
Vol 179 ◽  
pp. 209-216
Author(s):  
O. Bienaymé
Keyword(s):  
Spatial Distribution ◽  
Mass Distribution ◽  
Spiral Galaxies ◽  
Stellar Kinematics ◽  
Dynamical Mass ◽  
Poisson Equations ◽  
Galactic Potential ◽  
The Galaxy ◽  
Gas Cloud ◽  
Cloud Density

The analysis of stellar kinematics and the Galactic potential is linked to the study of the spatial distribution of stars in the Galaxy since they are related through the Boltzmann and Poisson equations. Measuring all the visible density and mass distribution from general star counts and the gas cloud density gives only a small fraction of the total amount of the dynamical mass that is deduced from the kinematics of the galactic constituents. As in many spiral galaxies, most of the Galactic mass is unseen and unknown.

scholarly journals Theoretical Considerations on the Dynamics of Normal Galactic Nuclei

1980 ◽  
Vol 5 ◽  
pp. 197-204
Author(s):  
Robert H. Sanders
Keyword(s):  
Spatial Distribution ◽  
Gravitational Field ◽  
Mass Distribution ◽  
Rotation Curve ◽  
Spiral Galaxies ◽  
Neutral Hydrogen ◽  
Galactic Nuclei ◽  
The Galaxy ◽  
Theoretical Considerations ◽  
Normal Spiral

I want to discuss the origin of non-circular gas motions observed in the nuclei of normal spiral galaxies and the possibility that recurring violent activity in normal nuclei excites such motion. But first, let us review several basic aspects of the nearest normal galactic nucleus — the nucleus of our own Galaxy.The rotation curve as observed in the 21-cm line of neutral hydrogen gives some indication of the form of the gravitational field in the central region of the Galaxy. Figure 1 is a smooth fit to the rotation curve in the inner few kiloparsecs (solid line) taken essentially from the data of Rougoor and Oort (1960) and Simonson and Mader (1973). This rotation curve, within 1 kpc of the centre, is completely accounted for by the mass distribution implied by the extended 2.2-μ emission (Becklin and Neugebauer 1968, Oort 1971). Moreover, there is little doubt that this centrally condensed mass distribution should be identified with the bulge or spheroidal component of the Galaxy, because the spatial distribution of the 2.2-μ intensity is practically identical to the distribution of visible starlight in the bulge of M31 (Sandage, Becklin, and Neugebauer 1969). The conclusion is that the bulge overwhelmingly dominates the gravitational field inside of 1 kpc.

scholarly journals X-ray Properties of Spiral Galaxies

2003 ◽  
Vol 214 ◽  
pp. 59-69
Author(s):  
Roberto Soria
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Supernova Remnants ◽  
Spiral Galaxies ◽  
Star Formation History ◽  
High Mass ◽  
X Ray ◽  
Formation History ◽  
Statistical Studies ◽  
X Ray Binaries

X-ray studies of nearby spiral galaxies with star formation allow us to investigate temperature and spatial distribution of the hot diffuse plasma, and to carry out individual and statistical studies of different classes of discrete sources (low- and high-mass X-ray binaries, Supernova remnants, supersoft and ultra-luminous sources). In particular, we briefly review the different models proposed to explain the ultra-luminous sources. We can then use the X-ray properties of a galaxy to probe its star formation history. We choose the starburst spiral M83 to illustrate some of these issues.

scholarly journals Supernovae and Molecular Clouds in Spiral Galaxies

2001 ◽  
Vol 205 ◽  
pp. 392-393
Author(s):  
Guo-Xuan Song
Keyword(s):  
Spatial Distribution ◽  
Molecular Clouds ◽  
Supernova Remnants ◽  
Spiral Galaxies ◽  
Inelastic Collisions ◽  
Spiral Arms ◽  
The Galaxy ◽  
Random Distributions

We report N-body simulations of the birthrate and distribution of supernovae in spiral galaxies. The simulations assume that stars form in GMCs with mass greater than 105M⊙ and that a Miller-Scalo IMF results. We assume that the resulting supernovae disrupt the GMC into smaller clouds; these clouds aggregrate to form new GMCs via inelastic collisions. Imposing a spiral potential, we find that supernovae form throughout the disk, but concentrated in the spiral arms. Using conditions appropriate for the Galaxy, a set of simulations with different initial random distributions of molecular clouds predicts 755τ5 supernova remnants (SNR) should exist in the Galaxy (where τ5 is the ratio of the lifetimes of SNRs to 105 yr). The predicted number of remnants and their spatial distribution can be compared to observations.

scholarly journals When the Largest Spiral is Formed

2012 ◽  
Vol 8 (S292) ◽  
pp. 328-328
Author(s):  
Rafael T. Eufrasio ◽  
Duília F. de Mello ◽  
Fernanda Urrutia-Viscarra ◽  
Claudia Mendes de Oliveira ◽  
Eli Dwek
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Spatial Correlation ◽  
Spiral Galaxy ◽  
Stellar Population ◽  
Spiral Galaxies ◽  
Dwarf Galaxy ◽  
Archival Data ◽  
Physical Size ◽  
The Galaxy

AbstractWe used UV-to-IR archival data to investigate the nature of the giant spiral galaxy, NGC 6872, 65 Mpc away. It belongs to the southern Pavo group and is interacting with a small lenticular galaxy, IC4970. GALEX UV images show a very large part of the galaxy not seen before, making it one of the largest spiral galaxies known, with a physical size greater than 150 kpc. The SED of 17 regions (10 kpc of diameter) across the two arms show a remarkable spatial distribution, as if they were mirror images with respect to their stellar population. However, the last 40 kpc of the northeastern arm are much bluer than any other region of the southwestern one. There is a strong spatial correlation between the NUV luminosity and the distance to the nucleus. The UV data supports the scenario of an interaction at 130 Myr which triggered star formation all over the disk of NGC 6872. The tip of the northeastern arm resembles a tidal dwarf galaxy in the process of formation.

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