Distance Determination to the Crab-like PWN G54.1+0.3 and Search for its Supernova Remnant Shell

Abstract

We discover a large-scale shell G53.9+0.2 around the Crab-like pulsar wind nebula (PWN) G54.1+0.3 with 1420 MHz continuum VLA observations. This is confirmed by a new infrared image at 8 μm from the GLIMPSE Legacy Project, which reveals an intriguing infrared shell just surrounding the large radio shell. We analyze the 21 cm HI absorption spectra and 13CO emission spectra towards PWN G54.1+0.3 and bright sources on both radio and IR shells. Continuous HI absorption up to the tangent point and absence of negative HI absorption features imply that PWN G54.1+0.3 has a distance beyond the tangent point but within the Solar circle, i.e. 4.5 to 9 kpc. G54.1+0.3 is likely at distance of \simeq 6.2 kpc due to the morphological association between the PWN and a CO molecular cloud at velocity of \simeq 53 km/s, as revealed by high-resolution 13CO images. Based on the HI absorption spectrum and recombination line velocity (\simeq 40 km/s) of the bright HII region G54.09-0.06, which is on the IR shell, the IR shell is likely located at a distance of \simeq 7.3 kpc, which is also the distance of the associated large-scale radio shell. At this distance, the radio shell has a radius of ~ 30 pc. The radio shell may be thermal and lack IR emission due to dust destruction, or it may be nonthermal and part of a newly found old SNR. In either case it is located at a different distance than PWN G54.1+0.3.

11 page, 3 figures, accepted by AJ

References in corpus (7)

• The Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey
• The VLA Galactic Plane Survey
• Discovery of the radio and X-ray counterpart of TeV Gamma-ray source HESS J1731-347
• The Milky Way Rotation Curve and its Vertical Derivatives Inside the Solar Circle
• The Distances of SNR W41 and overlapping HII regions
• Radio and X-ray images of SNR G18.8+0.3 interacting with molecular clouds
• Arecibo HI Absorption Measurements of Pulsars and the Electron Density at Intermediate Longitudes in the First Galactic Quadrant

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