A young pulsar with a long radio trail emergA young pulsar with a long radio trail emerging from SNR G315.9-0.0ing from SNR G315.9-0.0

F. Camilo, C.-Y. NG et al.

arxiv :0908.2421v1

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目录

Introduction

Discussion

Observations and results

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Introduction

Frying pan SNR G315.9-0.0

contour 2.5 5 7.5

10 15 and 20mJy

Shell ~13'

Jet like tail ~8' no IR

counterpart

Mills 1981 MOST@843MHz

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MOST @843MHzWhiteoak&Green 1996

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Observations and results

Image fromATCA 2.4 GHz

ATNF Parkes2008 June 17 6.1 hr @1374MHzwith 288MHz BW

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Identified pulsar PSR J1437-595

9

P~61ms

DM=549pc cm-3

D~8kpc(from Cordes&Lazio NE2

001 electron density model)

~50% linearly polarized througho

ut the pulse profile

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9.6ks Swift observation on 2008 July 5

only one photon within 5" of the pulsar position

NH =1.6 × 1022 cm−2

photon index Γ ＝ 1.5

assume 5 photons as the limit

fX < 4.5 × 10−14 erg cm−2 s−1

LX < 3.5 × 1032 d8^2 erg s−1

LX / Edot < 2.5 × 10−4 d8^2

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Discussion

Suggesting PSR association with the SNR NE2001 model uncertainty for the system~25%

d8 = 1 ± 0.25 τc = 114 kyr

τ114 = τ/τc

Vt = 300 d8/τ114 km s−1

RSNR = 17 d8 pc the SNR shell radius is small for such the age 114 kyr

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Sedov solution constraints on age τ≈ 22 d8

5/2(n0/E51)1/2 kyr

hydrogen ambient medium density n0cm-3

SN explosion kinetic energy 1051E51

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Other constraints on age

the trail ~RSNR = 17 d8 pc τc = 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 τ114 = τ/τc<<1, e.g. τ114∽0.2, Vt≈ 1500 km s−1

The proper motion is µ = 8/τ114 mas yr−1 , this could be measurable with the ATCA.

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PSR J1437–5959 has a very small flux density

luminosity L1.4 ≡ S1.4d2≈5d8^2 mJy kpc2

now unremarkable following numerous young pulsar disc

overies in recent years

Parkes multibeam survey 1997(Manchester et al. 2001)

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the faint tail of the population remains out of reach in a significant Galactic volume

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