Document Type
Article
Publication Date
5-10-2010
Publication Title
The Astronomical Journal
Department
Department of Physics and Astronomy
Abstract
The nebula J222557+601148, tentatively identified by Morris et al. as a young Galactic supernova remnant (SNR) from Spitzer Galactic First Look Survey images and a follow-up mid-infrared spectrum, is unlikely to be an SNR remnant based on Hα, [O III], [S II] images, and low-dispersion optical spectra. The object is seen in Hα and [O III] λ5007 images as a faint, roughly circular ring nebula with dimensions matching that seen in 24 μm Spitzer images. Low-dispersion optical spectra show it to have narrow Hα and [N II] λλ6548,6583 line emissions with no evidence of broad or high-velocity (v ≥ 300 km s–1) line emissions. The absence of any high-velocity optical features, the presence of relatively strong [N II] emissions, the lack of detected [S II] emission which would indicate the presence of shock-heated gas, plus no coincident X-ray or nonthermal radio emissions indicate that the nebula is unlikely to be an SNR, young or old. Instead, it is likely a faint, high-excitation planetary nebula (PN) as its elliptical morphology would suggest, lying at a distance ~2-3 kpc with unusual but not extraordinary mid-IR colors and spectra. We have identified an m r' = 22.4 ± 0.2 star as a PN central star candidate.
DOI
10.1088/0004-6256/139/6/2595
Original Citation
Robert A. Fesen and Dan Milisavljevic 2010 AJ 139 2595
Dartmouth Digital Commons Citation
Fesen, Robert A. and Milisavljevic, Dan, "The Nature of the Strong 24 Μmspitzersource J222557+601148: Not a Young Galactic Supernova Remnant" (2010). Dartmouth Scholarship. 3435.
https://digitalcommons.dartmouth.edu/facoa/3435
