X-ray ejecta kinematics of the Galactic core-collapse supernova remnant G292.0+1.8

Abstract

We report on the results from the analysis of our 114 ks Chandra HETGS observation of the Galactic core-collapse supernova remnant G292.0+1.8. To probe the 3D 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 <~ v_r <~ 1400 km s^-1. The distribution of ejecta knots in velocity vs. 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 10^51 erg, we estimate the total ejecta mass to be <~ 8 M_sun, and we propose an upper limit of <~ 35 M_sun on the progenitor's mass.

5 figures, accepted by ApJ

References in corpus (4)

• A Half-Megasecond Chandra Observation of the Oxygen-Rich Supernova Remnant G292.0+1.8
• The Kinematic and Plasma Properties of X-ray Knots in Cassiopeia A from the Chandra HETGS
• Chandra HETG Spectra of SN 1987A at 20 years
• The Outer Shock of the Oxygen-Rich Supernova Remnant G292.0+1.8: Evidence for the Interaction with the Stellar Winds from its Massive Progenitor

Cited by in corpus (3)

• Comparing Neutron Star Kicks to Supernova Remnant Asymmetries
• Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-Collapse Supernova Remnant G292.0+1.8
• The Cold Dust Content of the Oxygen-Rich Supernova Remnant G292.0+1.8