Discovery of a Highly Energetic Pulsar Associated With Igr J14003–6326 in the Young Uncataloged Galactic Supernova Remnant G310.6–1.6

Abstract

We report the discovery of 31.18 ms pulsations from the INTEGRAL source IGR J14003−6326 using the Rossi Xray Timing Explorer (RXTE). This pulsar is most likely associated with the bright Chandra X-ray point source lying at the center of G310.6−1.6, a previously unrecognized Galactic composite supernova remnant (SNR) with a bright central non-thermal radio and X-ray nebula, taken to be the pulsar wind nebula (PWN). PSR J1400−6325 is amongst the most energetic rotation-powered pulsars in the Galaxy, with a spin-down luminosity ofĖ = 5.1 × 10 37 erg s −1 . In the rotating dipole model, the surface dipole magnetic field strength is B s = 1.1 × 10 12 G and the characteristic age τ c ≡ P /2Ṗ = 12.7 kyr. The high spin-down power is consistent with the hard spectral indices of the pulsar and the nebula of 1.22 ± 0.15 and 1.83 ± 0.08, respectively, and a 2-10 keV flux ratio F PWN /F PSR ∼ 8. Followup Parkes observations resulted in the detection of radio emission at 10 and 20 cm from PSR J1400−6325 at a dispersion measure of ∼560 cm −3 pc, which implies a relatively large distance of 10 ± 3 kpc. However, the resulting location off the Galactic plane of ∼280 pc would be much larger than the typical thickness of the molecular disk, and we argue that G310.6−1.6 lies at a distance of ∼7 kpc. There is no gamma-ray counterpart to the nebula or pulsar in the Fermi data published so far. A multi-wavelength study of this new composite SNR, from radio to very high-energy gamma rays, suggests a young ( 10 3 yr) system formed by a sub-energetic ( 10 50 erg), low ejecta mass (M ej ∼ 3 M ) supernova explosion that occurred in a low-density environment (n 0 ∼ 0.01 cm −3 ).

First narrow-band search for continuous gravitational waves from known pulsars in advanced detector data

“…J1400-6326: First discovered as an INTEGRAL source and then identified as a pulsar by the Rossi X-ray Timing Explorer (RXTE). This NS is located in the galactic supernova remnant G310.6-1.6 and it is supposed to be quite young; the distance and its uncertainty correspond to the 1σ confidence level [15].…”

Multiband nonthermal radiative properties of pulsar wind nebulae

“…With T age = 1500 yr, which is less than the age of <1900 yr found in Renaud et al (2010), R pwn = 1.32 pc Table 2. and B pwn ≈ 13 µG are obtained here. We note that gave R pwn = 1.3 pc and B pwn = 17 µG with T age = 600 yr, and Martin et al (2014) obtained R pwn = 1.3 pc and B pwn = 8.2 µG with T age = 1100 yr.…”

A search for near infrared counterparts of three pulsar wind nebulae

“…On the other hand, the detection of a proposed counterpart to IGR J18490−0000 at K s ∼ 17 is significantly brighter than any other optical identification of an isolated neutron star, except for the Crab; it should also be noted that the proposed counterpart is significantly brighter than a simple power-law extrapolation of the X-ray spectra (Gotthelf et al 2011) which implies a magnitude of K s ∼ 23 (uncorrected for Galactic extinction). While the power-law extrapolation of the X-ray spectra of HESS J1632−478 (Balbo et al 2010) is not constraining, that of IGR J14003−6326 (Renaud et al 2010) implies that a counterpart should be much dimmer than the observed optical limit, at approximately K s ∼ 22. The extrapolations should however be treated with caution as the extracted X-ray spectra themselves may suffer from contamination from the surrounding PWN and thus inaccurate spectral slopes and fluxes.…”

“…Based on Chandra spectra, Tomsick et al (2009) confirm that IGR J14003−6326 (Keek et al 2006) is an SNR with a PWN, while Renaud et al (2010) discovered a 31.18 ms X-ray/radio pulsar at its centre. Tomsick et al do not find any higher energy (TeV, GeV) counterparts to the source but Renaud et al obtain radio observations which reveal counterparts to both the point source and the PWN.…”