scholarly journals Physically Motivated Fit to Mass Surface Density Profiles Observed in Galaxies

2021 ◽  
Vol 921 (2) ◽  
pp. 125
Author(s):  
Jorge Sánchez Almeida ◽  
Ignacio Trujillo ◽  
Angel R. Plastino
Keyword(s):  
Surface Density ◽  
Density Profiles

scholarly journals Dynamical Evolution of Globular Clusters After Core Collapse

1985 ◽  
Vol 113 ◽  
pp. 139-160 ◽  
Author(s):  
Douglas C. Heggie
Keyword(s):  
Surface Density ◽  
Globular Clusters ◽  
Stellar System ◽  
Dynamical Evolution ◽  
Theoretical Models ◽  
Numerical Calculations ◽  
Core Collapse ◽  
Density Profiles ◽  
The Core ◽  
Fokker Planck

This review describes work on the evolution of a stellar system during the phase which starts at the end of core collapse. It begins with an account of the models of Hénon, Goodman, and Inagaki and Lynden-Bell, as well as evaporative models, and modifications to these models which are needed in the core. Next, these models are related to more detailed numerical calculations of gaseous models, Fokker-Planck models, N-body calculations, etc., and some problems for further work in these directions are outlined. The review concludes with a discussion of the relation between theoretical models and observations of the surface density profiles and statistics of actual globular clusters.

Radial stability of critical-surface density profiles

1979 ◽  
Vol 19 (5) ◽  
pp. 659-664 ◽  
Author(s):  
Linda V. Powers ◽  
G.R. Montry ◽  
R.L. Berger
Keyword(s):  
Surface Density ◽  
Critical Surface ◽  
Density Profiles

scholarly journals THE STELLAR MASS STRUCTURE OF MASSIVE GALAXIES FROMz= 0 TOz= 2.5: SURFACE DENSITY PROFILES AND HALF-MASS RADII

2013 ◽  
Vol 763 (2) ◽  
pp. 73 ◽  
Author(s):  
Daniel Szomoru ◽  
Marijn Franx ◽  
Pieter G. van Dokkum ◽  
Michele Trenti ◽  
Garth D. Illingworth ◽  
...  
Keyword(s):  
Surface Density ◽  
Stellar Mass ◽  
Density Profiles ◽  
Massive Galaxies

Dark matter distribution in superthin galaxies

2020 ◽  
Vol 495 (4) ◽  
pp. 3722-3726
Author(s):  
Ilia Kalashnikov
Keyword(s):  
Dark Matter ◽  
Surface Density ◽  
Distribution Density ◽  
Spherically Symmetric ◽  
Matter Distribution ◽  
Galactic Disc ◽  
Density Profiles ◽  
Visible Matter ◽  
Simple Physical Model ◽  
Dark Matter Distribution

ABSTRACT This paper presents a new method of calculating dark matter density profiles for superthin axial symmetric galaxies without a bulge. This method is based on a simple physical model, which includes an infinitely thin galactic disc immersed in a spherically symmetric halo of dark matter. To obtain the desired distribution density, it suffices to know a distribution of visible matter surface density in a galaxy and a dependence of angular velocity on the radius. As a byproduct, the well-known expression, which reproduces surface density of a superthin galaxy expressed through a rotation law, was obtained.

Population gradients in dwarf spheroidal galaxies KKs 3 and ESO 269-66

2018 ◽  
Vol 14 (S344) ◽  
pp. 420-421
Author(s):  
M. E. Sharina ◽  
L. N. Makarova ◽  
D. I. Makarov
Keyword(s):  
Surface Density ◽  
Globular Clusters ◽  
Stellar Populations ◽  
Density Profiles ◽  
Dwarf Spheroidal Galaxies ◽  
Star Forming ◽  
Central Regions ◽  
Low Metallicity ◽  
High Metallicity ◽  
Spheroidal Galaxies

AbstractWe compare the properties of stellar populations for globular clusters (GCs) and field stars in two dwarf spheroidal galaxies (dSphs): ESO269-66, a close neighbour of NGC5128, and KKs3, one of the few isolated dSphs within 10 Mpc. We analyse the surface density profiles of low and high metallicity (blue and red) stars in two galaxies using the Sersic law. We argue that 1) the density profiles of red stars are steeper than those of blue stars, which evidences in favour of the metallicity and age gradients in dSphs; 2) globular clusters in KKs3 and ESO 269-66 contain 4 and 40 percent of all stars with [Fe / H] ~ 1.6 dex and the age of 12 Gyr, correspondingly. Therefore, GCs are relics of the first powerful star-forming bursts in the central regions of the galaxies. KKs 3 has lost a smaller percentage of old low-metallicity stars than ESO269-66, probably, thanks to its isolation.

scholarly journals Radial Surface Density Profiles of Gas and Dust in the Debris Disk around 49 Ceti

2017 ◽  
Vol 839 (2) ◽  
pp. 86 ◽  
Author(s):  
A. Meredith Hughes ◽  
Jesse Lieman-Sifry ◽  
Kevin M. Flaherty ◽  
Cail M. Daley ◽  
Aki Roberge ◽  
...  
Keyword(s):  
Surface Density ◽  
Density Profiles ◽  
Debris Disk

scholarly journals The Surface Density Profiles and Lensing Characteristics of Hickson Compact Groups of Galaxies

1996 ◽  
Vol 473 (2) ◽  
pp. L83-L86 ◽  
Author(s):  
M. L. Montoya ◽  
R. Domínguez-Tenreiro ◽  
G. González-Casado ◽  
G. A. Mamon ◽  
E. Salvador-Solé
Keyword(s):  
Surface Density ◽  
Compact Groups ◽  
Density Profiles ◽  
Groups Of Galaxies ◽  
Hickson Compact Groups

scholarly journals Radial Distributions of Dark and Luminous Matter in Bright Spiral Galaxies

2004 ◽  
Vol 220 ◽  
pp. 307-308
Author(s):  
Susan A. Kassin ◽  
Roelof S. De Jong ◽  
Richard W. Pogge
Keyword(s):  
Surface Density ◽  
Spiral Galaxies ◽  
Ohio State University ◽  
State University ◽  
Rotation Curves ◽  
Density Profiles ◽  
Multiband Imaging ◽  
Stellar Component ◽  
Luminous Matter ◽  
The Ohio State University

We present a work in progress investigating the radial distributions of dark and luminous matter in local bright spiral galaxies spanning a range of Hubble types. the distributions are derived from multiband imaging (BVRJHK) predominately from the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS) and rotation curves from the literature. We use stellar colour-MIL relationships from Bell & de Jong (2001, ApJ, 550, 212) to create radial stellar mass surface density profiles for each of our galaxies. These profiles are used to create rotation curves for the stellar component; gas masses are derived from HI when available. the resulting stellar and gas mass rotation curves are compared to observed (total mass) rotation curves, and the rotation due to dark matter is determined for each galaxy. Fits to Navarro, Frenk, & White (1996, ApJ, 462, 563; NFW) halo profiles are shown. We present this analysis for 2 example galaxies from our sample of nearly 50. We will use this data to investigate correlations between these mass components and physical properties of galaxies.

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