scholarly journals Mid‐Infrared High Spatial Resolution Observations of NGC 1569: Detection of Embedded Embryos of Star Formation

2006 ◽  
Vol 648 (1) ◽  
pp. 355-365 ◽  
Author(s):  
D. Tokura ◽  
T. Onaka ◽  
H. Takahashi ◽  
T. Miyata ◽  
S. Sako ◽  
...  
1999 ◽  
Vol 193 ◽  
pp. 517-522
Author(s):  
Kelsey E. Johnson

In an effort to better understand how the properties of star formation in starburst galaxies depend on various environmental parameters, I present a comparison between two well-known WR galaxies: the interacting galaxy system NGC 1741 in the Hickson Compact Group 31, and the dwarf galaxy He2-10. The high spatial resolution of HST has allowed identification of a large number of starburst knots, or ‘super star clusters’ in these WR galaxies. Broad-band photometry and the latest stellar synthesis models are used to estimate the ages and masses of the super star clusters. The properties of the clusters are then used to compare and contrast the overall star-formation histories in the two WR galaxies.


2003 ◽  
Vol 126 (1) ◽  
pp. 143-152 ◽  
Author(s):  
B. T. Soifer ◽  
J. J. Bock ◽  
K. Marsh ◽  
G. Neugebauer ◽  
K. Matthews ◽  
...  

2014 ◽  
Vol 441 (1) ◽  
pp. 630-639 ◽  
Author(s):  
Dinalva A. Sales ◽  
D. Ruschel-Dutra ◽  
M. G. Pastoriza ◽  
R. Riffel ◽  
Cláudia Winge

1999 ◽  
Vol 192 ◽  
pp. 108-111
Author(s):  
P. Linde ◽  
A. Ardeberg ◽  
B. Gustafsson

The history of star formation and chemical evolution are studied in the LMC Bar centre with the HST PC and WFC and uvby photometry. Using dedicated image processing, we secured high spatial resolution and photometric quality. We present colour magnitude diagrams (CMDs) from PC and WFC y and b data. The PC provides a CMD close to complete to V = 23.5, the WFC contributes favourable statistics on brighter stars. We find a population of stars seemingly around or younger than 0.2 Gyr comprising around 30% of the total amount of stars. Star formation seems to have decreased 3-0.2 Gyr ago. Older populations are aged 3–9 Gyr. Stars older than 10 Gyr seem rare if not absent. Our CMD morphology and, especially, our uvby metallicity index give [Me/H] close to −0.4, with older stars more and younger stars less metal poor.


2006 ◽  
Vol 636 (2) ◽  
pp. 932-951 ◽  
Author(s):  
C. McCabe ◽  
A. M. Ghez ◽  
L. Prato ◽  
G. Duchene ◽  
R. S. Fisher ◽  
...  

2004 ◽  
Vol 116 (820) ◽  
pp. 493-496 ◽  
Author(s):  
B. T. Soifer ◽  
G. Neugebauer ◽  
K. Matthews ◽  
E. Egami ◽  
L. Armus

2000 ◽  
Vol 120 (6) ◽  
pp. 2904-2919 ◽  
Author(s):  
J. J. Bock ◽  
G. Neugebauer ◽  
K. Matthews ◽  
B. T. Soifer ◽  
E. E. Becklin ◽  
...  

2006 ◽  
Vol 652 (2) ◽  
pp. L83-L87 ◽  
Author(s):  
Almudena Alonso-Herrero ◽  
Luis Colina ◽  
Christopher Packham ◽  
Tanio Díaz-Santos ◽  
George H. Rieke ◽  
...  

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