scholarly journals A NEW METHOD FOR MEASURING METALLICITIES OF YOUNG SUPER STAR CLUSTERS

2014 ◽  
Vol 787 (2) ◽  
pp. 142 ◽  
Author(s):  
J. Zachary Gazak ◽  
Ben Davies ◽  
Nate Bastian ◽  
Rolf Kudritzki ◽  
Maria Bergemann ◽  
...  
2007 ◽  
Vol 662 (1) ◽  
pp. 250-258
Author(s):  
Yan‐Ning Fu ◽  
Wen‐Hao Liu ◽  
Jie‐Hao Huang ◽  
Zu‐Gan Deng

2020 ◽  
Vol 897 (2) ◽  
pp. 176 ◽  
Author(s):  
Nico Krieger ◽  
Alberto D. Bolatto ◽  
Adam K. Leroy ◽  
Rebecca C. Levy ◽  
Elisabeth A. C. Mills ◽  
...  

1999 ◽  
Vol 193 ◽  
pp. 587-587
Author(s):  
Sara C. Beck ◽  
Orly Kovo ◽  
Jean L. Turner

We have observed nine Wolf-Rayet galaxies at 20,6, 3.6 and 2 cm from the VLA and at Hα from the Wise Observatory, and have mapped the radio spectral index in each galaxy on sub-arcsec scales. We find that more than half the WR sample has distinct regions where the radio spectrum rises between 6 and 2 cm. We believe that this is the radio signature of the youngest super-star-clusters which are otherwise invisible, and which require NLyc ≳ 1052, or equivalent to 750 stars of the 07 subtype. We call these sources radio super-star-clusters.


2018 ◽  
Vol 869 (2) ◽  
pp. 126 ◽  
Author(s):  
Adam K. Leroy ◽  
Alberto D. Bolatto ◽  
Eve C. Ostriker ◽  
Fabian Walter ◽  
Mark Gorski ◽  
...  

2017 ◽  
Vol 842 (1) ◽  
pp. 47 ◽  
Author(s):  
E. Vanzella ◽  
M. Castellano ◽  
M. Meneghetti ◽  
A. Mercurio ◽  
G. B. Caminha ◽  
...  

1994 ◽  
Vol 433 ◽  
pp. 65 ◽  
Author(s):  
Robert W. O'Connell ◽  
John S., III Gallagher ◽  
Deidre A. Hunter

2002 ◽  
Vol 207 ◽  
pp. 149-151
Author(s):  
Benjamin F. Williams ◽  
Paul W. Hodge

We present a new method for finding associations of young stars in M31 using broadband WFPC2 data from the HST data archive. Applying our identification method to 13 WFPC2 fields, covering an area of ∼60 arcmin2, has revealed 80 new candidate young star clusters in these portions of the M31 disk. Most of these clusters are small (≳5 pc) young (∼10–200 Myr) star groups located within large OB associations. We have estimated the reddening values and the ages of each candidate individually by fitting isochrones to the stellar photometry. We provide a catalogue of the candidates including rough approximations of their reddenings and ages.


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