Astronomy and Astrophysics – Astronomy
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.8506v&link_type=abstract
American Astronomical Society, 194th AAS Meeting, #85.06; Bulletin of the American Astronomical Society, Vol. 31, p.973
Astronomy and Astrophysics
Astronomy
Scientific paper
The observation of a skin of [OIII] lambda 5007 Angstroms emission around the edge of the visible Crab supernova remnant has been explained as a cooling region behind a radiative shock, driven by synchrotron pressure and sweeping up freely expanding ejecta from the original supernova explosion (Sankrit & Hester 1997). Higher ioization species such as [NeV] lambda 3426 Angstroms provide an opportunity for tracing shocks with velocities in excess of about 170 km/s. With recent observations of [NeV] in the southern portion of the remnant (Van Tassell et.al. 1998), little doubt is left about the existence of a shock, and the production of high ionization line emission in the cooling region behind it. Shock parameters such as the shock velocity are constrained by observations covering a wide range of ionizations and excitations. We are presenting images of the entire remnant in emission from [NeV] lambda 3426 Angstroms , and compare these with observations in [OIII] lambda 5007 Angstroms , [SII] lambda 6717 Angstroms & lambda 6734 Angstroms , and Hα , and with spectra of select locations. Images of the Crab in narrowband filters were taken this winter at the Steward 2.3 meter telescope on Kitt Peak. The images show [NeV] emission spatially exterior to the [OIII] emission, and relatively stronger at the boundary of the nebula than in the filaments. Spectra for the Crab were taken throughout December and January of 1998 and 1999 using the B&C Spectrograph at the Steward 2.3 meter telescope on Kitt Peak. Preliminary analysis of these data are presented, and their implications as to shock properties are discussed. Partial funding for this project was provided by a NASA Space Grant, and by NASA support of the WFPC2 IDT.
Hester Jeff J.
Sankrit Ravi
Szentgyorgyi Andrew
van Tassell Heidi A.
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