NASA/IPAC EXTRAGALACTIC DATABASE
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For refcode 1994AJ....107..651Y:
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1994AJ....107..651Y A KINEMATIC SEARCH FOR SUPERNOVA REMNANT'S IN GIANT EXTRAGALACTIC H II REGIONS HUI YANG AND EVAN D. SKILLMAN Astronomy Department, University of Minnesota, 116 Church St. SE Minneapolis, Minnesota 55455 Electronic mail: yangh@sonne.spa.umn.edu, slcilima@wn.spumn.edu RICHARD A. SRAMEK National Radio Astronomy Observatory, P.O. Box O, Socorro, New Mexico 87801 Electronic mail: dsramek@aoc.nrao.edu Received 1992 November 9: revised 1993 October 14 ABSTRACT We have obtained velocity fields of the Giant H II complexes NGC 5471 in M101, NGC 2363 in NGC 2366, and the largest H II region in NGC 2403 from H{alpha} observations using the TAURUS imaging Fabry-Perot interferometer. We have detected five H{alpha} sources with velocity profiles which are broad when compared with the surrounding H II region. Region B in NGC 5471 has been previously determined to contain a supernova remnant by the presence of nonthermal radio continuum radiation and enhanced [O I] and [S II] emission (Skillman 1985) and broad H{alpha} emission (Chu & Kennicutt 1986). Two broad H{alpha} sources in NGC 2363 coincide with regions where strong splitting has been found in the [O III] line (Roy et al. 1991). Two more broad H{alpha} sources have been identified in the largest H II region in NGC 2403. VLA radio continuum observations with a resolution of 2" at {lambda}6 and {lambda}20 cm of all 3 H II complexes are presented. In addition, high resolution (subarcsecond) VLA images of NGC 5471 were made at {lambda}2 and {lambda}6 cm. The presence of a nonthermal source in region NGC 5471 B was confirmed while region NGC 5471 A appears to be dominated by thermal emission. The nonthermal spectral index in NGC 2363 A indicates the existence of one or more supernova remnants at the position of a large velocity width source detected in H{alpha} emission. No similar nonthermal sources were detected in NGC 2403 #1. Supernovae explosions and stellar winds are considered as causes for these large velocity width sources (LVWS). If the emission from the LVWSs is attributed to single supernova remnants, they are unusually luminous in both nonthermal radio continuum and H{alpha} emission. The very large H{alpha} luminosities could be a result of high velocity gas being ionized by the neighboring stellar cluster. ========================================================================== 1994AJ....107..651Y A KINEMATIC SEARCH FOR SUPERNOVA REMNANT'S IN GIANT EXTRAGALACTIC H II REGIONS HUI YANG AND EVAN D. SKILLMAN Astronomy Department, University of Minnesota, 116 Church St. SE Minneapolis, Minnesota 55455 Electronic mail: yangh@sonne.spa.umn.edu, slcilima@wn.spumn.edu RICHARD A. SRAMEK National Radio Astronomy Observatory, P.O. Box O, Socorro, New Mexico 87801 Electronic mail: dsramek@aoc.nrao.edu Received 1992 November 9: revised 1993 October 14 ABSTRACT We have obtained velocity fields of the Giant H II complexes NGC 5471 in M101, NGC 2363 in NGC 2366, and the largest H II region in NGC 2403 from H{alpha} observations using the TAURUS imaging Fabry-Perot interferometer. We have detected five H{alpha} sources with velocity profiles which are broad when compared with the surrounding H II region. Region B in NGC 5471 has been previously determined to contain a supernova remnant by the presence of nonthermal radio continuum radiation and enhanced [O I] and [S II] emission (Skillman 1985) and broad H{alpha} emission (Chu & Kennicutt 1986). Two broad H{alpha} sources in NGC 2363 coincide with regions where strong splitting has been found in the [O III] line (Roy et al. 1991). Two more broad H{alpha} sources have been identified in the largest H II region in NGC 2403. VLA radio continuum observations with a resolution of 2" at {lambda}6 and {lambda}20 cm of all 3 H II complexes are presented. In addition, high resolution (subarcsecond) VLA images of NGC 5471 were made at {lambda}2 and {lambda}6 cm. The presence of a nonthermal source in region NGC 5471 B was confirmed while region NGC 5471 A appears to be dominated by thermal emission. The nonthermal spectral index in NGC 2363 A indicates the existence of one or more supernova remnants at the position of a large velocity width source detected in H{alpha} emission. No similar nonthermal sources were detected in NGC 2403 #1. Supernovae explosions and stellar winds are considered as causes for these large velocity width sources (LVWS). If the emission from the LVWSs is attributed to single supernova remnants, they are unusually luminous in both nonthermal radio continuum and H{alpha} emission. The very large H{alpha} luminosities could be a result of high velocity gas being ionized by the neighboring stellar cluster.
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