A young pulsar with a long radio trail emerging from SNR G F. Camilo, C.-Y. NG et al. arxiv : v1
Page 2 目录 IntroductionDiscussionObservations and results
Page 3 Introduction Frying pan SNR G contour and 20mJy Shell ~13' Jet like tail ~8' no IR counterpart Mills 1981
Page 4 Whiteoak&Green 1996
Page 5 Observations and results Image from ATCA 2.4 GHz ATNF Parkes 2008 June with 288MHz BW
Page 6 Identified pulsar PSR J P~61ms DM=549pc cm -3 D~8kpc(from Cordes&Lazio NE2001 electron density model) ~50% linearly polarized throughout the pulse profile
Page 7
Page 8 9.6ks Swift observation on 2008 July 5 only one photon within 5" of the pulsar position N H =1.6 × cm −2 photon index Γ ＝ 1.5 assume 5 photons as the limit f X < 4.5 × 10 −14 erg cm −2 s −1 L X < 3.5 × d 8 ^2 erg s −1 L X / E dot < 2.5 × 10 −4 d 8 ^2
Page 9 Discussion Suggesting PSR association with the SNR NE2001 model uncertainty for the system~25% d 8 = 1 ± 0.25 τ c = 114 kyr τ 114 = τ/τ c V t = 300 d 8 /τ 114 km s −1 R SNR = 17 d 8 pc the SNR shell radius is small for such the age 114 kyr
Page 10 Sedov solution constraints on age τ≈ 22 d 8 5/2 (n 0 /E 51 ) 1/2 kyr hydrogen ambient medium density n 0 cm -3 SN explosion kinetic energy E 51
Page 11 Other constraints on age the trail ~ R SNR = 17 d 8 pc τ c = 114 kyr The pulsar wind trail collimated for about 50kyr. Detailed study of PWN will find if it's resonable.(under way using ATCA) If τ 114 = τ/τ c <<1, e.g. τ 114 ∽ 0.2, V t ≈ 1500 km s −1 The proper motion is µ = 8/τ 114 mas yr −1, this could be measurable with the ATCA.
Page 12 PSR J1437–5959 has a very small flux density luminosity L 1.4 ≡ S 1.4 d 2 ≈5d 8 ^2 mJy kpc 2 now unremarkable following numerous young pulsar discoveries in recent years Parkes multibeam survey 1997(Manchester et al. 2001)
Page 13 the faint tail of the population remains out of reach in a significant Galactic volume
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