The Nature of the Strong 24 micron Spitzer Source J222557+601148: Not a Young Galactic Supernova Remnant

Details The Nature of the Strong 24 micron Spitzer Source J222557+601148: Not a Young Galactic Supernova Remnant The Nature of the Strong 24 micron Spitzer Source J222557+601148: Not a Young Galactic Supernova Remnant

2010-04-19

arxiv.org/abs/1004.3293v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

6 pages, 3 figures, accepted to The Astronomical Journal

Scientific paper

The nebula J222557+601148, tentatively identified by Morris et al. (2006) 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 a SNR remnant based on Halpha, [O III], [S II] images and low dispersion optical spectra. The object is seen in Halpha and [O III] 5007 images as a faint, roughly circular ring nebula with dimensions matching that seen in 24 micron Spitzer images. Low-dispersion optical spectra show it to have narrow Halpha and [N II] 6548, 6583 line emissions with no evidence of broad or high-velocity (v > 300 km/s) line emissions. The absence of any high-velocity optical features, the presence of relatively strong [N II] emissions, a 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 the nebula is unlikely to be a 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 of approximately 2 - 3 kpc with unusual but not extraordinary mid-IR colors and spectrum. We have identified a m_r' = 22.4 +/- 0.2 star as a PN central star candidate.

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