X-RAY EJECTA KINEMATICS OF THE GALACTIC CORE-COLLAPSE SUPERNOVA REMNANT G292.0+1.8
Name
Bhalerao-2015-X-RAY EJECTA KINEMAT.pdf
Size
1.99 MB
Format
Adobe PDF
Checksum (MD5)
3a44db066634c8fb0732997dfcd82966
Author(s)
Bhalerao, Jayant
Park, Sangwook
Dewey, Dan
Hughes, John P.
Mori, Koji
Lee, Jae-Joon
Date Issued
February 2015
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Bhalerao, Jayant, Sangwook Park, Daniel Dewey, John P. Hughes, Koji Mori, and Jae-Joon Lee. “X-RAY EJECTA KINEMATICS OF THE GALACTIC CORE-COLLAPSE SUPERNOVA REMNANT G292.0+1.8.” The Astrophysical Journal 800, no. 1 (February 10, 2015): 65. © 2015 The American Astronomical Society
Version
Final published version
Abstract
We report on the results from the analysis of our 114 ks Chandra High Energy Transmision Grating Spectrometer observation of the Galactic core-collapse supernova remnant G292.0+1.8. To probe the three-dimensional structure of the clumpy X-ray emitting ejecta material in this remnant, we measured Doppler shifts in emission lines from metal-rich ejecta knots projected at different radial distances from the expansion center. We estimate radial velocities of ejecta knots in the range of –2300 [< over ~] v[subscript r] [< over ~] 1400 km s[superscript –1]. The distribution of ejecta knots in velocity versus projected-radius space suggests an expanding ejecta shell with a projected angular thickness of ~90'' (corresponding to ~3 pc at d = 6 kpc). Based on this geometrical distribution of the ejecta knots, we estimate the location of the reverse shock approximately at the distance of ~4 pc from the center of the supernova remnant, putting it in close proximity to the outer boundary of the radio pulsar wind nebula. Based on our observed remnant dynamics and the standard explosion energy of 10[superscript 51] erg, we estimate the total ejecta mass to be [< over ~]8 M [subscript ☉], and we propose an upper limit of [< over ~]35 M [subscript ☉] on the progenitor's mass.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
Terms of Use
Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1088/0004-637x/800/1/65
