A ring nebula surrounding evolved massive stars in the post-starburst galaxy NGC 1569

1994 ◽  
Vol 106 ◽  
pp. 974 ◽  
Author(s):  
Laurent Drissen ◽  
Jean-Rene Roy
Keyword(s):  
Massive Stars ◽  
Starburst Galaxy ◽  
Ring Nebula ◽  
Ngc 1569

FISICA observations of the starburst galaxy, NGC 1569

2006 ◽  
Vol 50 (4-5) ◽  
pp. 433-435
Author(s):  
D.M. Clark ◽  
S.S. Eikenberry ◽  
S.N. Raines ◽  
N. Gruel ◽  
R. Elston ◽  
...  
Keyword(s):  
Starburst Galaxy ◽  
Ngc 1569

scholarly journals Massive stars and their interstellar environment in the Magellanic Clouds

1999 ◽  
Vol 193 ◽  
pp. 441-448
Author(s):  
Michael A. Dopita ◽  
Sungeun Kim ◽  
M. Sally Oey ◽  
Tatyana M. Lozinskaya
Keyword(s):  
Star Formation Rate ◽  
Massive Stars ◽  
Formation Rate ◽  
Large Magellanic Cloud ◽  
Magellanic Clouds ◽  
Disk Galaxies ◽  
Ring Nebula ◽  
Halo Gas ◽  
The Vertical Distribution ◽  
Insight Into

The winds of massive stars play a major role in setting up and controlling both the phase structure of the interstellar medium in galaxies and the vertical distribution of gas in galactic disks. In turn, these processes provide feedback into control of the star formation rate. Thanks to their proximity, these processes can be studied in detail in the Magellanic Clouds. Here we describe the results of a deep emission-line image survey of the ring nebula population, and a global high-resolution H I and H II survey of the Large Magellanic Cloud. These data provide a new insight into the process of feedback between the disk and the halo gas in disk galaxies in general, and the LMC in particular.

scholarly journals The Life and Death of Massive Stars in the Starburst Galaxy I Zw 18

2015 ◽  
Vol 11 (A29B) ◽  
pp. 215-216
Author(s):  
Dorottya Szécsi ◽  
Norbert Langer
Keyword(s):  
Stellar Evolution ◽  
Gamma Ray ◽  
Massive Stars ◽  
Gamma Ray Bursts ◽  
Starburst Galaxy ◽  
Life And Death ◽  
Long Duration ◽  
Low Metallicity ◽  
The Universe ◽  
Evolution Proceeds

AbstractMassive stars at low metallicity are strong candidates for two of the most energetic explosions in the Universe: long duration gamma-ray bursts and superluminous supernovae. But what is the reason these explosions prefer low metallicity environments? To answer this question, we investigate how massive stellar evolution proceeds in low metallicity environments.

The Environment of X-Ray Binaries in the Dwarf Starburst Galaxy NGC 1569

2008 ◽  
Author(s):  
David M. Clark ◽  
Stephen S. Eikenberry ◽  
Steven N. Raines ◽  
Reba M. Bandyopadhyay ◽  
Stefanie Wachter ◽  
...  
Keyword(s):  
Starburst Galaxy ◽  
X Ray ◽  
X Ray Binaries ◽  
Ngc 1569

scholarly journals 3.19. ROSAT HRI observations of the young starburst galaxy NGC 5253

1998 ◽  
Vol 184 ◽  
pp. 127-128
Author(s):  
D. K. Strickland ◽  
I. R. Stevens
Keyword(s):  
Dwarf Galaxy ◽  
Massive Stars ◽  
Young Star ◽  
Starburst Galaxy ◽  
X Ray ◽  
Ideal Object ◽  
Enhanced Resolution ◽  
Large Numbers ◽  
The Individual ◽  
Young Star Clusters

Large numbers of Wolf-Rayet stars in the nearby (4.1 Mpc) star-bursting dwarf galaxy NGC 5253 indicate the starburst is only ~ 5 million years old (Schaerer et al. 1997). This makes NGC 5253 an ideal object for studying the early phases of starburst activity, in particular superbubbles blown by supernovae and winds from massive stars.Previous low resolution observations suggested the observed X-ray emission was due to a superbubble. We use the enhanced resolution available with a long ROSAT High Resolution Imager (HRI) observation and find that the X-ray emission arises from several unresolved sources associated with the young star clusters seen in the optical. We discuss the possible origins of the point-like emission, and find that they could be small superbubbles blown by the individual clusters of massive stars.

scholarly journals The chaotic ISM of the post(?)-starburst galaxy NGC 1569

2003 ◽  
Vol 212 ◽  
pp. 549-550
Author(s):  
Reginald J. Dufour ◽  
Brent A. Buckalew ◽  
Patrick L. Shopbell ◽  
Donald K. Walter
Keyword(s):  
Supernova Remnants ◽  
Large Scale ◽  
Wide Band ◽  
Primary Data ◽  
Starburst Galaxy ◽  
Main Body ◽  
Ionized Gas ◽  
Super Star Clusters ◽  
Dust Distribution ◽  
Ngc 1569

We present the results and analysis of HST-wfpc2 imagery of the starburst galaxy NGC 1569 (d = 2.2 Mpc), which permit unprecedented resolution (~ 1pc) of the ionized gas and stellar population. The primary data in our analysis consists of images taken through narrow-band filters isolating Hβ, Hα, [O iii]λ5007, and [S ii]λλ6717+30, as part of go Program 8133. A variety of color-coded and grey-scaled maps of the morphology, ionization structure, and dust distribution are presented. Unsharp masks of the Hα images show a very chaotic structure for the ionized gas, with numerous filaments and arc-like bright rim features across the entire galaxy, but without significant large-scale ionization variations. Variations in the ionization and line-of-sight reddening occur on smaller scales (~ 10 – 50 pc), with numerous low-ionization semi-stellar knots seen throughout the main body of the galaxy, even within the ‘hole’ in the ionized gas distribution around the central super star clusters previously noted from H i maps. Several of these features have strong [S ii] emission indicative of being supernova remnants. We combine these data with archival wide-band HST-wfpc2 imagery to quantitatively evaluate the source(s) of the (largely photo-) ionized gas.

scholarly journals Star cluster formation and evolution in the dwarf starburst galaxy NGC 1569

2004 ◽  
Vol 347 (1) ◽  
pp. 17-28 ◽  
Author(s):  
P. Anders ◽  
R. de Grijs ◽  
U. Fritze-v. Alvensleben ◽  
N. Bissantz
Keyword(s):  
Cluster Formation ◽  
Star Cluster ◽  
Starburst Galaxy ◽  
Formation And Evolution ◽  
Ngc 1569

scholarly journals Ring Nebulae Around PN Nuclei and Massive Stars

1993 ◽  
Vol 155 ◽  
pp. 139-145 ◽  
Author(s):  
You-Hua Chu
Keyword(s):  
Massive Star ◽  
Massive Stars ◽  
Planetary Nebulae ◽  
Central Star ◽  
Ring Nebula ◽  
Fast Wind ◽  
Ring Nebulae

Planetary nebulae (PNe) and ring nebulae around massive stars are not just superficially similar in morphologies. For massive stars that evolve through red supergiant phase, the final fast wind would sweep up the slow red supergiant wind and form a bubble of stellar material, reminiscing the two-wind formation of a PN. Sometimes it can be really difficult to determine whether the central star of a ring nebula is a PN nucleus or a Pop I massive star. Parallel studies of PNe and ring nebulae around massive stars can greatly benefit each other.

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