AHubble Space TelescopeCensus of Nuclear Star Clusters in Late-Type Spiral Galaxies. II. Cluster Sizes and Structural Parameter Correlations

2004 ◽  
Vol 127 (1) ◽  
pp. 105-118 ◽  
Author(s):  
Torsten Bker ◽  
Marc Sarzi ◽  
Dean E. McLaughlin ◽  
Roeland P. van der Marel ◽  
Hans-Walter Rix ◽  
...  
Keyword(s):  
Spiral Galaxies ◽  
Star Clusters ◽  
Structural Parameter ◽  
Late Type

A [ITAL]Hubble Space Telescope[/ITAL] Census of Nuclear Star Clusters in Late-Type Spiral Galaxies. I. Observations and Image Analysis

2002 ◽  
Vol 123 (3) ◽  
pp. 1389-1410 ◽  
Author(s):  
Torsten Böker ◽  
Seppo Laine ◽  
Roeland P. van der Marel ◽  
Marc Sarzi ◽  
Hans-Walter Rix ◽  
...  
Keyword(s):  
Image Analysis ◽  
Spiral Galaxies ◽  
Hubble Space Telescope ◽  
Star Clusters ◽  
Late Type ◽  
Space Telescope

scholarly journals THE STRUCTURE OF NUCLEAR STAR CLUSTERS IN NEARBY LATE-TYPE SPIRAL GALAXIES FROMHUBBLE SPACE TELESCOPEWIDE FIELD CAMERA 3 IMAGING

2015 ◽  
Vol 149 (5) ◽  
pp. 170 ◽  
Author(s):  
Daniel J. Carson ◽  
Aaron J. Barth ◽  
Anil C. Seth ◽  
Mark den Brok ◽  
Michele Cappellari ◽  
...  
Keyword(s):  
Spiral Galaxies ◽  
Star Clusters ◽  
Late Type

Erratum: “The Structure of Nuclear Star Clusters in Nearby Late-type Spiral Galaxies from Hubble Space Telescope Wide Field Camera 3 Imaging” (2015, AJ, 149 170)

2019 ◽  
Vol 158 (6) ◽  
pp. 260
Author(s):  
Daniel J. Carson ◽  
Aaron J. Barth ◽  
Anil C. Seth ◽  
Mark den Brok ◽  
Michele Cappellari ◽  
...  
Keyword(s):  
Spiral Galaxies ◽  
Hubble Space Telescope ◽  
Star Clusters ◽  
Wide Field ◽  
Late Type ◽  
Space Telescope

scholarly journals The HST Census of Nuclear Star Clusters in Late-type Spirals

2002 ◽  
Vol 207 ◽  
pp. 706-707
Author(s):  
Torsten Böker
Keyword(s):  
Structural Properties ◽  
Formation Mechanism ◽  
Spiral Galaxies ◽  
Morphological Evolution ◽  
Star Clusters ◽  
Star Cluster ◽  
Host Galaxy ◽  
Late Type ◽  
Preliminary Results

I describe preliminary results from an I-band snapshot survey with HST/WFPC2 of nuclear star clusters in late-type spiral galaxies. The goal of the program is to derive the fraction of galaxies that harbor a nuclear star cluster, and to analyse their photometric and structural properties. Together with follow-up spectroscopy, the survey will illuminate the formation mechanism of nuclear star clusters and the implications for the dynamical and morphological evolution of the host galaxy.

scholarly journals The inner mass distribution of late-type spiral galaxies fromSAURONstellar kinematic maps

2016 ◽  
Vol 464 (2) ◽  
pp. 1903-1922 ◽  
Author(s):  
Veselina Kalinova ◽  
Glenn van de Ven ◽  
Mariya Lyubenova ◽  
Jesús Falcón-Barroso ◽  
Dario Colombo ◽  
...  
Keyword(s):  
Mass Distribution ◽  
Spiral Galaxies ◽  
Late Type

scholarly journals Hubble Sequence as a Temporal Evolution Sequence

1999 ◽  
Vol 186 ◽  
pp. 491-491
Author(s):  
Xiaolei Zhang
Keyword(s):  
Spiral Galaxies ◽  
Temporal Evolution ◽  
Natural Question ◽  
Late Type ◽  
Present Epoch ◽  
Hubble Sequence ◽  
Deep Survey ◽  
Deep Fields ◽  
The Universe ◽  
Evolution Sequence

The results from Hubble Space Telescope's Medium Deep Survey and Deep Fields indicate that there exists far more blue spiral galaxies at the intermediate and high redshifts than at the present epoch. A natural question therefore is: what have become of these excess late type galaxies as the Universe aged?

scholarly journals A preliminary color-magnitude diagram for late-type stars in the solar neighborhood

1959 ◽  
Vol 10 ◽  
pp. 39-40
Author(s):  
O. C. Wilson
Keyword(s):  
Main Sequence ◽  
Star Clusters ◽  
Solar Neighborhood ◽  
Late Type ◽  
Main Sequence Stars ◽  
Individual Values ◽  
Magnitude Diagram ◽  
Trigonometric Parallaxes ◽  
Nearby Stars ◽  
The Mean

Modern photoelectric techniques yield magnitudes and colors of stars with accuracies of the order of a few thousandths and a few hundredths of a magnitude respectively. Hence for star clusters it is possible to derive highly accurate color-magnitude arrays since all of the members of a cluster may be considered to be at the same distance from the observer. It is much more difficult to do this for the nearby stars where all of the objects concerned are at different, and often poorly determined, distances. If one depends upon trigonometric parallaxes, the bulk of the reliable individual values will refer to main sequence stars, and while the mean luminosities of brighter stars are given reasonably well by this method, the scatter introduced into a color-magnitude array by using individual trigonometrically determined luminosities could obscure important features. Somewhat similar objections could be raised against the use of the usual spectroscopic parallaxes which also should be quite good for the main sequence but undoubtedly exhibit appreciable scatter for some, at least, of the brighter stars.

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