A spectroscopic method for determining the luminosities of spiral galaxies and estimating their stellar population

1982 ◽  
Vol 263 ◽  
pp. 1 ◽  
Author(s):  
A. P. Cowley ◽  
D. Crampton ◽  
R. D. McClure
Keyword(s):  
Stellar Population ◽  
Spiral Galaxies ◽  
Spectroscopic Method

scholarly journals IR imaging of spiral galaxy bulges

1993 ◽  
Vol 153 ◽  
pp. 441-442
Author(s):  
Dennis Zaritsky ◽  
Marcia Rieke ◽  
Hans-Walter Rix
Keyword(s):  
Spiral Galaxy ◽  
Stellar Population ◽  
Spiral Galaxies ◽  
Spiral Arms ◽  
Ir Imaging ◽  
The Impact

Imaging in the infrared (2.2μ) minimizes the impact of dust obscuration and allows reliable mapping of the mass-tracing stellar population in spiral galaxies. We find dramatic differences compared to photometry at shorter wavelengths (e.g. 0.8μ). As an example, the observations of the mini-bar and inner spiral arms of M 51 are discussed.

scholarly journals Stellar population in bulge of spiral galaxies

2006 ◽  
Vol 2 (S241) ◽  
Author(s):  
L. Morelli ◽  
E. Pompei ◽  
A. Pizzella ◽  
L. Coccato ◽  
E.M. Corsini ◽  
...  
Keyword(s):  
Stellar Population ◽  
Spiral Galaxies

scholarly journals Spectroscopic study of formation, evolution and interaction of M31 and M33 with star clusters

2014 ◽  
Vol 10 (S312) ◽  
pp. 201-202 ◽  
Author(s):  
Zhou Fan ◽  
Yanbin Yang
Keyword(s):  
Globular Clusters ◽  
Stellar Population ◽  
Local Group ◽  
Spiral Galaxies ◽  
Star Clusters ◽  
Star Cluster ◽  
Physical Parameters ◽  
Cluster Systems ◽  
Nearby Galaxies ◽  
Formation And Evolution

AbstractThe recent studies show that the formation and evolution process of the nearby galaxies are still unclear. By using the Canada France Hawaii Telescope (CFHT) 3.6m telescope, the PanDAS shows complicated substructures (dwarf satellite galaxies, halo globular clusters, extended clusters, star streams, etc.) in the halo of M31 to ~150 kpc from the center of galaxy and M31-M33 interaction has been studied. In our work, we would like to investigate formation, evolution and interaction of M31 and M33, which are the nearest two spiral galaxies in Local Group. The star cluster systems of the two galaxies are good tracers to study the dynamics of the substructures and the interaction. Since 2010, the Xinglong 2.16m, Lijiang 2.4m and MMT 6.5m telescopes have been used for our spectroscopic observations. The radial velocities and Lick absorption-line indices can thus be measured with the spectroscopy and then ages, metallicities and masses of the star clusters can be fitted with the simple stellar population models. These parameters could be used as the input physical parameters for numerical simulations of M31-M33 interaction.

scholarly journals The effect of ram-pressure stripping on dwarf galaxies

2020 ◽  
Vol 494 (1) ◽  
pp. 1114-1127 ◽  
Author(s):  
P Steyrleithner ◽  
G Hensler ◽  
A Boselli
Keyword(s):  
Galaxy Clusters ◽  
Stellar Population ◽  
Velocity Dispersion ◽  
Spiral Galaxies ◽  
Dwarf Galaxies ◽  
Gas Content ◽  
Gas Reservoirs ◽  
Interstellar Gas ◽  
Internal Structures ◽  
Ram Pressure

ABSTRACT Ram-pressure stripping (RPS) is a well observed phenomenon of massive spiral galaxies passing through the hot intracluster medium (ICM) of galaxy clusters. For dwarf galaxies (DGs) within a cluster, the transformation from gaseous to gas-poor systems by RPS is not easily observed and must happen in the outskirts of clusters. In a few objects in close by galaxy clusters and the field, RPS has been observed. Since cluster early-type DGs also show a large variety of internal structures (unexpected central gas reservoirs, blue stellar cores, composite radial stellar profiles), we aim in this study to investigate how ram pressure (RP) affects the interstellar gas content and therefore the star formation (SF) activity. Using a series of numerical simulations, we quantify the dependence of the stripped-off gas on the velocity of the infalling DGs and on the ambient ICM density. We demonstrated that SF can be either suppressed or triggered by RP depending on the ICM density and the DGs mass. Under some conditions, RP can compress the gas, so that it is unexpectedly retained in the central DG region and forms stars. When gas clouds are still bound against stripping but lifted from a thin disc and fall back, their new stars form an ellipsoidal (young) stellar population already with a larger velocity dispersion without the necessity of harassment. Most spectacularly, star clusters can form downstream in stripped-off massive gas clouds in the case of strong RP. We compare our results to observations.

scholarly journals Stellar Population Synthesis of Star-forming Clumps in Galaxy Pairs and Non-interacting Spiral Galaxies

2018 ◽  
Vol 234 (2) ◽  
pp. 35 ◽  
Author(s):  
Javier Zaragoza-Cardiel ◽  
Beverly J. Smith ◽  
Margarita Rosado ◽  
John E. Beckman ◽  
Theodoros Bitsakis ◽  
...  
Keyword(s):  
Stellar Population ◽  
Spiral Galaxies ◽  
Population Synthesis ◽  
Star Forming ◽  
Stellar Population Synthesis

The stellar population in the nuclei of spiral galaxies

1980 ◽  
Vol 236 ◽  
pp. 112 ◽  
Author(s):  
R. D. McClure ◽  
A. P. Cowley ◽  
D. Crampton
Keyword(s):  
Stellar Population ◽  
Spiral Galaxies

Far‐Ultraviolet and Hα Imaging of Nearby Spiral Galaxies: The OB Stellar Population in the Diffuse Ionized Gas

2001 ◽  
Vol 559 (2) ◽  
pp. 878-891 ◽  
Author(s):  
Charles G. Hoopes ◽  
Rene A. M. Walterbos ◽  
Gregory D. Bothun
Keyword(s):  
Stellar Population ◽  
Spiral Galaxies ◽  
Ionized Gas ◽  
Diffuse Ionized Gas ◽  
Far Ultraviolet

scholarly journals The Stellar Content of the Nuclei of Spiral Galaxies

1983 ◽  
Vol 6 ◽  
pp. 157-163
Author(s):  
D. Crampton ◽  
R.D. McClure ◽  
A.P. Cowley
Keyword(s):  
Spectral Type ◽  
Stellar Population ◽  
Main Sequence ◽  
Spiral Galaxies ◽  
Elliptical Galaxies ◽  
Solar Neighbourhood ◽  
Stellar Content ◽  
Late Type ◽  
Metal Abundances ◽  
Hydrogen Lines

Numerous studies have been attempted to determine the stellar content of the nuclei of galaxies. In the case of elliptical galaxies observations show that there is a change in spectral type from later to earlier types correlated with a variation from high to low luminosity (e.g. Faber 1977). This has been interpreted for the most part as being due to differences in metal abundances in an old stellar population, although some recent studies suggest a variation in stellar age may be important as well (e.g. O’Connell 1980, Heckman 1980). The nuclear bulges of spiral galaxies also display a change from late to early spectral type along a sequence from high to low luminosity bulges. In this case, however, the assumption has almost universally been made that these differences are due to differences in age of the stellar population. In particular, most stellar models for the nuclear bulges of spiral galaxies have used solar neighbourhood metal- rich stars, and assumed that the strong hydrogen lines and weak metal lines in late-type spiral nuclei are due to the predominance of a very young main-sequence population rather than old metal-poor stars.

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