Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0508309)
· On-line Data
· References in the article
· Citations to the Article (11) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (12)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Exploring the Kinematics of the Oxygen-rich Supernova Remnant G292.0+1.8: Ejecta Shells, Fast-moving Knots, and Shocked Circumstellar Material
Authors:
Ghavamian, Parviz; Hughes, John P.; Williams, T. B.
Affiliation:
AA(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686 .), AB(Department of Physics and Astronomy, Rutgers University, Piscataway, NJ 08854-8019 , .; Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory. CTIO is operated by AURA, Inc., under contract to the National Science Foundation.), AC(Department of Physics and Astronomy, Rutgers University, Piscataway, NJ 08854-8019 , .; Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory. CTIO is operated by AURA, Inc., under contract to the National Science Foundation.)
Publication:
The Astrophysical Journal, Volume 635, Issue 1, pp. 365-380. (ApJ Homepage)
Publication Date:
12/2005
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: G292.0+1.8, ISM: Supernova Remnants
DOI:
10.1086/497283
Bibliographic Code:
2005ApJ...635..365G

Abstract

We present the results of an in-depth optical study of the core-collapse supernova remnant G292.0+1.8 using the Rutgers Fabry-Perot (RFP) imaging spectrometer. Our observations provide a detailed picture of the supernova remnant in the emission lines of [O III] λ5007, Hα, and [N II] λ6548. The [O III] Fabry-Perot scans reveal a bright crescent-shaped spur of previously known high-velocity (Vradial~1500 km s-1) O-rich ejecta located on the eastern side of the remnant. The spur consists of a semicoherent structure of mostly redshifted material, along with several clumps that have apparently broken out of the more orderly shell-like expansion. The high-velocity (>~600 km s-1) component of the spur also displays a scalloped morphology characteristic of Rayleigh-Taylor instabilities. We also find a large number of fast-moving knots (FMKs) of O-rich ejecta undetected in prior photographic plate images and similar to features seen in Cas A. The FMKs are distributed sparsely in the interior of G292.0+1.8 and are seen mostly in blueshifted emission out to Vradial~-1700 km s-1. The position-velocity distribution of the FMKs can be kinematically described as a shell 3.4 arcmin in radius expanding at a velocity of 1700 km s-1. Another feature apparent in the [O III] scans is an equatorial belt consisting of both a barlike structure at zero radial velocity and a clumpy, high-velocity ejecta component seen in projection along the line of sight. Portions of the zero-velocity bar are spatially well correlated with a similar structure seen in the Chandra X-ray image of G292.0+1.8. The bar is also detected in our Hα RFP images at zero radial velocity, providing further evidence that this structure is of circumstellar origin. We find that the optical and X-ray properties of the bar are consistent with incomplete (partially radiative) shocks in material of moderate densities. There are also a number of faint, elongated structures seen in Hα at zero radial velocity across the interior of G292.0+1.8 that lack [O III] and X-ray counterparts. These filaments may be low-density H I clouds photoionized by hard radiation from the interior of the remnant. Overall, these results suggest that G292.0+1.8 is currently interacting with a low-density environment. We find no evidence for high-velocity Hα or [N II] emission over the dynamical range sampled by the RFP. Assuming a distance of 6 kpc for G292.0+1.8, we estimate a kinematic age of (3000-3400)d6 yr for this remnant.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints