Stellar populations in the edge-on spiral galaxy NGC 4565. I - Surface brightness and color distributions

1982 ◽  
Vol 50 ◽  
pp. 421 ◽  
Author(s):  
E. B. Jensen ◽  
T. X. Thuan
Keyword(s):  
Spiral Galaxy ◽  
Surface Brightness ◽  
Stellar Populations

scholarly journals Stellar Populations of the Most Massive Galaxies

2009 ◽  
Vol 5 (S267) ◽  
pp. 459-459
Author(s):  
Alexander Fritz ◽  
Michael D. Hoenig ◽  
Ricardo P. Schiavon
Keyword(s):  
High Velocity ◽  
Surface Brightness ◽  
Stellar Populations ◽  
Spectroscopic Properties ◽  
Low Density ◽  
Early Type ◽  
Small Surface ◽  
Fundamental Plane ◽  
Massive Galaxies ◽  
Bona Fide

Within the hierarchical CDM framework, gas-poor mergers contribute substantially to the building of the most massive galaxies (Faber et al. 2007). We want to test this scenario by studying the fundamental plane (FP) and the stellar populations of the most massive galaxies. We investigate a well-defined sample of massive early-type galaxies at 0.1<z<0.4, identified from the SDSS database. Out of 42,000 possible targets in the SDSS database, we extracted 23 luminous early-type galaxies with bona fide high velocity dispersions of σ>350 km s−1. These systems are located either in high or low-density environments and show a variety of small surface-brightness structure. Using archival HST/ACS images and Gemini/GMOS spectroscopy, we will explore the photometric and spectroscopic properties of these galaxies.

scholarly journals 5.18. Molecular gas in the poststarburst galaxy NGC7331

1998 ◽  
Vol 184 ◽  
pp. 247-248
Author(s):  
T. Tosaki ◽  
Y. Shioya
Keyword(s):  
High Resolution ◽  
Spiral Galaxy ◽  
Stellar Populations ◽  
Optical Spectra ◽  
Molecular Gas ◽  
Early Type ◽  
Origin And Evolution ◽  
Co Observations

To understand the origin and evolution of starburst activity, we must study the full evolution of starburst; i.e., pre-, on-going, and post-starburst phases. It seems reasonable to suppose the numerous A-type stars indicate past starburst and they show strong Balmer absorption. NGC7331, nearby early-type spiral galaxy, is one of the poststarburst galaxies which show strong Balmer absorption. The optical spectra of NGC7331 were dominated by component of intermediate-age (5 × 109 years) stellar populations (Ohyama & Taniguchi 1996). We present the result of the high resolution CO observations of NGC7331 using Nobeyama Milimeter Array.

scholarly journals Surface Photometry of Spiral Galaxy NGC 5005 and Elliptical Galaxy NGC 4278

2018 ◽  
Vol 15 (3) ◽  
pp. 314-323
Author(s):  
Baghdad Science Journal
Keyword(s):  
Spiral Galaxy ◽  
Surface Brightness ◽  
Elliptical Galaxy ◽  
Position Angle ◽  
Sloan Digital Sky Survey ◽  
Surface Photometry ◽  
Contour Maps ◽  
Sky Survey ◽  
Flat Field ◽  
The Galaxy

Two galaxies have been chosen, spiral galaxy NGC 5005 and elliptical galaxy NGC 4278 to study their photometric properties by using surface photometric techniques with griz-Filters. Observations are obtained from the Sloan Digital Sky Survey (SDSS). The data reduction of all images have done, like bias and flat field, by SDSS pipeline. The overall structure of the two galaxies (a bulge, a disk), together with isophotal contour maps, surface brightness profiles and a bulge/disk decomposition of the galaxy images were performed, although the disk position angle, ellipticity and inclination of the galaxies have been estimated.

A Wide Field CCD Survey for Low Surface Brightness Galaxies.II.Color Distributions, Stellar Populations, and Missing Baryons

1997 ◽  
Vol 114 ◽  
pp. 2448 ◽  
Author(s):  
Karen O'Neil ◽  
G. D. Bothun ◽  
J. Schombert ◽  
Mark E. Cornell ◽  
C. D. Impey
Keyword(s):  
Surface Brightness ◽  
Stellar Populations ◽  
Wide Field ◽  
Low Surface Brightness

scholarly journals Dating the formation of the counter-rotating stellar disc in the spiral galaxy NGC 5719 by disentangling its stellar populations★

2011 ◽  
Vol 412 (1) ◽  
pp. L113-L117 ◽  
Author(s):  
L. Coccato ◽  
L. Morelli ◽  
E. M. Corsini ◽  
L. Buson ◽  
A. Pizzella ◽  
...  
Keyword(s):  
Spiral Galaxy ◽  
Stellar Populations ◽  
Stellar Disc

scholarly journals Stellar Populations and Hubble Type

1983 ◽  
Vol 6 ◽  
pp. 187-190
Author(s):  
Sidney van den Bergh
Keyword(s):  
Strong Correlation ◽  
Globular Clusters ◽  
Surface Brightness ◽  
Stellar Populations ◽  
Elliptical Galaxies ◽  
Young Stars ◽  
Stellar Content ◽  
Clear Cut ◽  
Spiral Arm ◽  
Galaxy Morphology

Men are more apt to be mistaken in their generalization than in their particular observations. MachiavelliIt was already realized by Hubble (1936) that galaxy morphology and stellar content were correlated. He pointed out that resolution into stars increases along the classification sequence Sa-Sb-Sc. Simultaneously the colours of spirals become bluer and their integrated spectral types become earlier as one proceeds from Sa to Sc. Baade (1944) speculated that the red stars in ellipticals and in the nuclear bulges of spirals were identical to those in globular clusters. He suggested that stars in galaxies belong to two distinct populations: young metal-rich stars of Population I which inhabit the disc and spiral arm regions of spirals, and old metal-poor stars of Population II which dominate the light of elliptical galaxies and the nuclear bulges of spirals. Subsequently Baade (1950) emphasized the strong correlation between the occurrence of gas and dust and the presence of young stars. As Baade put it so succinctly “No dust, no Population I”. Belief in a clear cut dichotomy between Population I and Population II was strengthened by the differences in their radial luminosity distributions. The surface brightness of Population I in spirals is well represented by an exponential disc, whereas the surface brightness of Population II stars in ellipticals and the bulges of spirals may be described by an r1/4 law (de Vaucouleurs 1959).

scholarly journals Stellar Populations of Dwarf Galaxies

1995 ◽  
Vol 164 ◽  
pp. 430-431
Author(s):  
Elchanan Almoznino ◽  
Noah Brosch
Keyword(s):  
Surface Brightness ◽  
Dwarf Galaxies ◽  
High Surface ◽  
Stellar Populations ◽  
Virgo Cluster ◽  
Original Sample ◽  
High Surface Brightness ◽  
Brightness Level ◽  
Low Surface Brightness ◽  
Low Surface Brightness Galaxies

We selected a sample of dwarf galaxies in the Virgo cluster from the original catalog of Bingelli, Sandage and Tamman (1985), which have been measured at 21 cm by Hoffman et al. (1987). The original sample was selected to have both high surface brightness objects (classified as BCD or anything/BCD), and low surface brightness galaxies (classified as ImIII, ImIV or ImV). An additional selection was done on the total amount of HI, as given in Hoffman et al. We selected from each surface brightness group objects with high HI content (flux integral larger than a set threshold), and others with low HI content. We thus defined four samples differing in surface brightness level and total HI content.

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