Star Count

2018 ◽  
Vol 2018 (90) ◽  
pp. 10-10
Author(s):  
John Sibley Williams
Keyword(s):  
Star Count

scholarly journals Estimation of Galactic model parameters in high latitudes with the SDSS and SCUSS

2013 ◽  
Vol 9 (S298) ◽  
pp. 404-404
Author(s):  
Cuihua Du ◽  
Yunpeng Jia ◽  
Xiyan Peng
Keyword(s):  
Model Parameters ◽  
High Latitudes ◽  
The South ◽  
Statistical Errors ◽  
Count Method ◽  
Sky Survey ◽  
Star Count ◽  
The Galaxy ◽  
Galactic Model

AbstractBased on the South Galactic Cap U-band Sky Survey (SCUSS) and SDSS observation, we adopted the star-count method to analyze the stellar distribution in different directions of the Galaxy. We find that these model parameters may be variable with observed direction, which cannot simply be attributed to statistical errors.

Wide Field Star Count Mapping of Large Scale Areas of Star Formation in the Large Magellanic Cloud

1994 ◽  
pp. 516-517
Author(s):  
E. Kontizas ◽  
S. E. Maravelias ◽  
A. Dapergolas ◽  
Y. Bellas-Velidis ◽  
M. Kontizas
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Wide Field ◽  
Field Star ◽  
Star Count

UBV star-count data in the region of the North Galactic Pole

1987 ◽  
Vol 93 ◽  
pp. 624 ◽  
Author(s):  
R. S. Stobie ◽  
K. Ishida
Keyword(s):  
Count Data ◽  
The North ◽  
Star Count ◽  
North Galactic

scholarly journals Star Counts

1984 ◽  
Vol 78 ◽  
pp. 315-324
Author(s):  
Richard G. Kron
Keyword(s):  
Spatial Distribution ◽  
Density Function ◽  
Luminosity Function ◽  
Stellar Populations ◽  
Line Of Sight ◽  
Luminosity Functions ◽  
Star Count

The number of stars counted along a particular line of sight depends on the spatial distribution of stars, the luminosity function, and the absorption. Thus star count programs are designed to constrain or determine one or more of these functions. Early efforts to understand the structure of our Galaxy, including the fundamentals of stellar statistics, were largely based on work that involved star counts. Since then a growing appreciation has developed for the variety of forms the density function D(r) and the luminosity function Φ(M) can take, especially the recognition of different stellar populations, each with different density and luminosity functions. In the simplest formulation two distinct populations are considered: disk and halo. This suggests two distinct formation histories, but uncertainty in the picture remains (Eggen, Lynden-Bell and Sandage 1962; Ostriker and Thuan 1975; Saio and Yoshii 1979; Jones and Wyse 1983).

scholarly journals Galactic structure studies with SCUSS and SDSS surveys

2012 ◽  
Vol 8 (S295) ◽  
pp. 309-310
Author(s):  
Cuihua Du ◽  
Xiyan Peng
Keyword(s):  
Galactic Halo ◽  
Galactic Structure ◽  
Scale Height ◽  
Thick Disk ◽  
Axis Ratio ◽  
Statistical Errors ◽  
Count Method ◽  
Sky Survey ◽  
Star Count ◽  
The Galaxy

AbstractBased on the South Galactic Cap U-band Sky Survey (SCUSS) and SDSS observations, we adopted the star-count method to analyze the stellar distribution in different directions of the Galaxy. We find that the scale height of the disk may be variable with the observed direction, which cannot simply be attributed to statistical errors. The main reason can be possibly attributed to the disk (mainly the thick disk) being flared, with a scale height increasing with radius. The axis ratio of the Galactic halo is in the range 0.4-0.6. This finding supports Galactic models with a flattened inner halo, partly formed through a merger early in the Galaxy's history.

scholarly journals Atlas and Catalog of Dark Clouds Based on Digitized Sky Survey I

2005 ◽  
Vol 57 (sp1) ◽  
pp. S1-S386 ◽  
Author(s):  
Kazuhito Dobashi ◽  
Hayato Uehara ◽  
Ryo Kandori ◽  
Tohko Sakurai ◽  
Masahiro Kaiden ◽  
...  
Keyword(s):  
Physical Parameters ◽  
Galactic Latitude ◽  
Entire Region ◽  
Optical Extinction ◽  
Dark Clouds ◽  
Latitude Range ◽  
Cloud Parameters ◽  
Sky Survey ◽  
Star Count

Abstract We present a quantitative atlas and catalog of dark clouds derived by using the optical database “Digitized Sky Survey I”. Applying a traditional star-count technique to 1043 plates contained in the database, we produced an $A_V$ map covering the entire region in the galactic latitude range $\vert b\vert \le 40^\circ$. The map was drawn at two different angular resolutions of $6'$ and $18'$, and is shown in detail in a series of figures in this paper. Based on the $A_V$ map, we identified 2448 dark clouds and 2841 clumps located inside them. Some physical parameters, such as the position, extent, and optical extinction, were measured for each of the clouds and clumps. We also searched for counterparts among already known dark clouds in the literature. The catalog of dark clouds presented in this paper lists the cloud parameters as well as the counterparts.

scholarly journals INFORMATION ON THE MILKY WAY FROM THE 2MASS ALL SKY STAR COUNT: BIMODAL COLOR DISTRIBUTIONS

2012 ◽  
Vol 759 (2) ◽  
pp. 94 ◽  
Author(s):  
Chan-Kao Chang ◽  
Shao-Yu Lai ◽  
Chung-Ming Ko ◽  
Ting-Hung Peng
Keyword(s):  
Milky Way ◽  
Star Count

scholarly journals Wide Field Star Count Mapping of Large Scale Areas of Star Formation in the Large Magellanic Cloud

1994 ◽  
Vol 161 ◽  
pp. 516-517 ◽  
Author(s):  
E. Kontizas ◽  
S.E. Maravelias ◽  
A. Dapergolas ◽  
Y. Bellas-Velidis ◽  
M. Kontizas
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Large Magellanic Cloud ◽  
Wide Field ◽  
Dark Clouds ◽  
Star Count ◽  
Astrophysical Problem ◽  
Star Formation In Galaxies ◽  
The Individual ◽  
Parent Galaxy

Star formation in galaxies is a major astrophysical problem which can be investigated in several ways. The distribution and loci of all kinds of young objects, including OB associations, young clusters, HII regions, GMCs, Bok globules, dark clouds, dust lanes, protostars, as well as YSOs detected in NIR and FIR surveys constitute the principal signposts for this investigation. The individual nature of all these objects has been and is still continously studied. However it is also extremely interesting to associate the coexistence of these objects, and their relation to the structure of the parent galaxy. Such studies have been carried out by several investigators and are frequently summarized when star formation processes are examined.

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