Three-dimensional Kinematics Of The Oxygen-rich Supernova Remnant G292.0+1.8

Details Three-dimensional Kinematics Of The Oxygen-rich Supernova Remnant G292.0+1.8 Three-dimensional Kinematics Of The Oxygen-rich Supernova Remnant G292.0+1.8

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21442602p&link_type=abstract

American Astronomical Society, AAS Meeting #214, #426.02; Bulletin of the American Astronomical Society, Vol. 41, p.695

Astronomy and Astrophysics

Astronomy

Scientific paper

We continue a study of kinematics of fast filaments in the young, oxygen-rich supernova remnant (SNR) G292.0+1.8, one of only three such SNRs identified in the Galaxy. Winkler et al. (2009 Ap.J.) used a series of [OIII] 5007 Å emission-line images taken from CTIO at epochs 1986 - 2008 to measure proper motions for 67 discrete oxygen-rich filaments. This analysis showed that the transverse velocities of the filaments are linearly proportional to their distances from a common expansion center, and thus these O-rich filaments must be ejecta fragments that have been traveling with very little deceleration since the initial supernova (SN) event. The rate of expansion implies the SN explosion occurred 3000 years ago.
If we assume the ejecta knots are expanding freely, then measuring the radial velocities of ejecta knots is equivalent to finding their positions within the SNR along the line of sight. We use data obtained from CTIO with the RC Spectrograph on the 1.5m telescope and with the Hydra Multi-Object Spectrograph on the Blanco 4m telescope to measure radial velocities for dozens of ejecta knots in G292.0+1.8. From the combination of radial velocity and proper motion measurements, we are mapping the three-dimensional structure and kinematics of the SNR. We will discuss the implications of the SNR's present geometry for core-collapse SNe.
This work has been sponsored in part by the NSF through grant AST-0307613.

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