New Galactic supernova remnants discovered with IPHAS

被引:59
作者
Sabin, L. [1 ,2 ]
Parker, Q. A. [3 ,4 ,5 ]
Contreras, M. E. [1 ]
Olguin, L. [6 ]
Frew, D. J. [3 ,4 ]
Stupar, M. [3 ,4 ,5 ]
Vazquez, R. [1 ]
Wright, N. J. [7 ]
Corradi, R. L. M. [8 ,9 ]
Morris, R. A. H. [10 ]
机构
[1] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico
[2] Univ Guadalajara, CUCEI, Dept Fis, Inst Aston & Meteorol, Guadalajara 44130, Jalisco, Mexico
[3] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia
[4] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia
[5] Australian Astron Observ, Epping, NSW 1710, Australia
[6] Univ Sonora, Dept Invest Fis, Hermosillo 83190, Sonora, Mexico
[7] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[8] Inst Astrofis Canarias, E-38200 Tenerife, Spain
[9] Univ La Laguna, Dept Astrofis, E-38200 Tenerife, Spain
[10] Univ Bristol, Dept Phys, Astrophys Grp, Bristol BS8 1TL, Avon, England
基金
美国国家航空航天局;
关键词
ISM: supernova remnants; H-ALPHA SURVEY; LARGE-MAGELLANIC-CLOUD; CANDIDATE PLANETARY-NEBULAE; EMISSION-LINE PROPERTIES; DIFFUSE IONIZED-GAS; WOLF-RAYET STARS; GHZ SKY SURVEY; NOVA REMNANT; CRAB-NEBULA; INTERSTELLAR-MEDIUM;
D O I
10.1093/mnras/stt160
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
As part of a systematic search programme of a 10 degrees wide strip of the northern Galactic plane, we present preliminary evidence for the discovery of four (and possibly five) new supernova remnants (SNRs). The pilot search area covered the 19-20 h right ascension zone sampling from +20 degrees to +55 degrees in declination using binned mosaic images from the Isaac Newton Telescope Photometric H alpha Survey (IPHAS). The optical identification of the candidate SNRs was based mainly on their filamentary and arc-like emission morphologies, their apparently coherent, even if fractured, structure and clear disconnection from any diffuse neighbouring H II region type nebulosity. Follow-up optical spectroscopy was undertaken, sampling carefully across prominent features of these faint sources. The resulting spectra revealed typical emission-line ratios for shock-excited nebulae which are characteristic of SNRs, which, along with the latest diagnostic diagrams, strongly support the likely SNR nature of these sources: G038.7-1.3 (IPHASX J190640.5+042819), G067.6+0.9 (IPHASX J195744.9+305306), G066.0-0.0 (IPHASX J195749.2+290259) and G065.8-0.5 (IPHASX J195920.4+283740). A fifth possible younger, higher density nebula SNR candidate, G067.8+0.5 (IPHASX J200002.4+305035), was discovered similar to 5 arcmin to the west of IPHASX J195744.9+305306, and it warrants further study. A multiwavelength cross-check from available archived data in the regions of these candidates was also performed with a focus on possible radio counterparts. A close positional match between previously unrecognized radio structures at several frequencies and across various components of the H alpha optical image data was found for all SNR candidates. This lends further direct support for the SNR nature of these objects. Evolved SNRs may have very weak and/or highly fragmented radio emission which could explain why they had not been previously recognized, but the association becomes clear in combination with the optical emission.
引用
收藏
页码:279 / 291
页数:13
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