Erratum: "Hubble Space Telescope Observations of Oxygen-Rich Supernova Remnants in the Magellanic Clouds. I. Narrowband Imaging of N132D in the LMC" [A. J. 112,2,509(1996)]

1996 ◽  
Vol 112 ◽  
pp. 2350
Author(s):  
Jon A. Morse ◽  
William P. Blair ◽  
Michael A. Dopita ◽  
John P. Hughes ◽  
Robert P. Kirshner ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Hubble Space Telescope ◽  
Magellanic Clouds ◽  
Space Telescope ◽  
Narrowband Imaging

scholarly journals CSI in Supernova Remnants

2017 ◽  
Vol 12 (S331) ◽  
pp. 81-85
Author(s):  
You-Hua Chu
Keyword(s):  
Supernova Remnants ◽  
Hubble Space Telescope ◽  
Orbital Plane ◽  
Large Magellanic Cloud ◽  
Close Binary System ◽  
Close Binary ◽  
Binary Interaction ◽  
Space Telescope ◽  
Multi Wavelength ◽  
Mass Ejection

AbstractSupernovae (SNe) explode in environments that have been significantly modified by the SN progenitors. For core-collapse SNe, the massive progenitors ionize the ambient interstellar medium (ISM) via UV radiation and sweep the ambient ISM via fast stellar winds during the main sequence phase, replenish the surroundings with stellar material via slow winds during the luminous blue variable (LBV) or red supergiant (RSG) phase, and sweep up the circumstellar medium (CSM) via fast winds during the Wolf-Rayet (WR) phase. If a massive progenitor was in a close binary system, the binary interaction could have caused mass ejection in certain preferred directions, such as the orbital plane, and even bipolar outflow/jet. As a massive star finally explodes, the SN ejecta interacts first with the CSM that was ejected and shaped by the star itself. As the newly formed supernova remnant (SNR) expands further, it encounters interstellar structures that were shaped by the progenitor from earlier times. Therefore, the structure and evolution of a SNR is largely dependent on the initial mass and close binarity of the SN progenitor. The Large Magellanic Cloud (LMC) has an excellent sample of over 50 confirmed SNRs that are well resolved by Hubble Space Telescope, Chandra X-ray Observatory, and Spitzer Space Telescope. These multi-wavelength observations allow us to conduct stellar forensics in SNRs and understand the wide variety of morphologies and physical properties of SNRs observed.

Hubble Space Telescope Observations of Oxygen-Rich Supernova Remnants in the Magellanic Cloud. I. Narrow-Band Imaging of N132D in the LMC

1996 ◽  
Vol 112 ◽  
pp. 509 ◽  
Author(s):  
J. A. Morse ◽  
W. P. Blair ◽  
M. A. Dopita ◽  
J. P. Hughes ◽  
R. P. Kirshner ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Narrow Band ◽  
Hubble Space Telescope ◽  
Narrow Band Imaging ◽  
Magellanic Cloud ◽  
Space Telescope

scholarly journals The mid-infrared Leavitt law for classical Cepheids in the Magellanic Clouds

2020 ◽  
Vol 500 (1) ◽  
pp. 817-837
Author(s):  
Abigail H Chown ◽  
Victoria Scowcroft ◽  
Stijn Wuyts
Keyword(s):  
Hubble Space Telescope ◽  
Zero Point ◽  
Large Magellanic Cloud ◽  
Magellanic Clouds ◽  
Light Curves ◽  
Log P ◽  
Mid Infrared ◽  
Space Telescope ◽  
Classical Cepheids ◽  
Combining Data

ABSTRACT The Cepheid Leavitt Law (LL), also known as the Period–Luminosity relation, is a crucial tool for assembling the cosmic distance ladder. By combining data from the OGLE-IV catalogue with mid-infrared photometry from the Spitzer Space Telescope, we have determined the 3.6 and 4.5 $\mu$m LLs for the Magellanic Clouds using ∼5000 fundamental-mode classical Cepheids. Mean magnitudes were determined using a Monte Carlo Markov Chain (MCMC) template fitting procedure, with template light curves constructed from a subsample of these Cepheids with fully phased, well-sampled light curves. The dependence of the Large Magellanic Cloud LL coefficients on various period cuts was tested, in addition to the linearity of the relationship. The zero-point of the LL was calibrated using the parallaxes of Milky Way Cepheids from the Hubble Space Telescope and Gaia Data Release 2. Our final calibrated relations are M[3.6] = −3.246(±0.008)(log (P) − 1.0) − 5.784(±0.030) and M[4.5] = −3.162(±0.008)(log (P) − 1.0) − 5.751(±0.030).

Hubble Space Telescope Observations of Planetary Nebulae in the Magellanic Clouds

1997 ◽  
pp. 417-427 ◽  
Author(s):  
M. A. Dopita ◽  
P. R. Wood ◽  
S. J. Meatheringham ◽  
E. Vassiliadis ◽  
R. C. Bohlin ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Magellanic Clouds ◽  
Space Telescope

Hubble Space Telescope Spectroscopy of Massive Hot Stars in the Magellanic Clouds and M31

1994 ◽  
pp. 179-182
Author(s):  
S. M. Haser ◽  
D. J. Lennon ◽  
R.-P. Kudritzki ◽  
J. Puls ◽  
N. R. Walborn ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Magellanic Clouds ◽  
Hot Stars ◽  
Space Telescope

Hubble Space Telescope Observations of Planetary Nebulae in the Magellanic Clouds. I. The Extreme Type I SMP 83/WS 35

1993 ◽  
Vol 418 ◽  
pp. 804 ◽  
Author(s):  
Michael A. Dopita ◽  
Holland C. Ford ◽  
Ralph Bohlin ◽  
Ian N. Evans ◽  
Stephen J. Meatheringham
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Magellanic Clouds ◽  
Type I ◽  
Space Telescope ◽  
Extreme Type

Hubble Space Telescope Observations of Planetary Nebulae in the Magellanic Clouds. IV. [O iii] Images and Evolutionary Ages

1996 ◽  
Vol 460 ◽  
pp. 320 ◽  
Author(s):  
M. A. Dopita ◽  
E. Vassiliadis ◽  
S. J. Meatheringham ◽  
R. C. Bohlin ◽  
H. C. Ford ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Magellanic Clouds ◽  
Space Telescope
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