X‐Ray Observations of Parsec‐scale Tails behind Two Middle‐Aged Pulsars

Kargaltsev, Oleg; Misanovic, Zdenka; Pavlov, G. G.; Wong, Jian-Syuan; Garmire, Gordon

doi:10.1086/589145

Cited by 64 publications

(56 citation statements)

References 39 publications

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“…The model of Gaensler & Slane (2006) predicts a low-scale termination shock of ∼0 6 fo J2055 (at 600 pc), thus not resolved by XMM-Newton, even in the case of typical ambient densities (0.01 atoms cm −3 ) and pulsar velocities (some hundreds ofkilometers per second). In that case, part of the flux we assign to the pulsar comes instead from the termination shock (Kargaltsev & Pavlov 2008a). Along their main axis, the brightness profiles of both nebulae are consistent with an almost flat behavior, with a sudden decrease at the end.…”

Section: The Nebulaementioning

confidence: 57%

“…If the pulsar moves supersonically, shocked pulsar wind is expected to flow in an elongated region downstream of the termination shock (basically, the cavity in the interstellar medium (ISM)created by the moving neutron star and its wind), confined by ram pressure. X-ray emission is due to synchrotron emission from the wind particles accelerated at the termination shock, which is typically seen (if angular resolution permits) as the brightest portion of the extended structure (see, e.g., Kargaltsev & Pavlov 2008a), as predicted by MHD simulations (Bucciantini 2002; Van der Swaluw 2003;Bucciantini et al 2005). In order to produce a population of high-energy particles, a highly energetic pulsar is required (Ė greater than ∼10 34 ; see, e.g., Kargaltsev & Pavlov 2008b).…”

Section: Introductionmentioning

confidence: 99%

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The Tale of the Two Tails of the Oldish PSR J2055+2539

Marelli

Pizzocaro

Luca

et al. 2016

ApJ

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We analyzed a deep XMM-Newton observation of the radio-quiet γ-ray PSR J2055+2539. The spectrum of the X-ray counterpart is nonthermal, with a photon index of Γ=2.36±0.14 (1σ confidence). We detected X-ray pulsations with a pulsed fraction of 25% ± 3% and a sinusoidal shape. Taking into account considerations on the γ-ray efficiency of the pulsar and on its X-ray spectrum, we can infer a pulsar distance ranging from 450 to 750 pc. We found two different nebular features associated withPSR J2055+2539 and protruding from it. The angle between the two nebular main axes is ∼162°.8±0°.7. The main, brighter feature is 12′ long and <20″ thick, characterized by an asymmetry with respect to the main axis that evolves with the distance from the pulsar, possibly forming a helical pattern. The secondary feature is 250″×30″. Both nebulae present an almost flat brightness profile with a sudden decrease at the end. The nebulae can be fitted byeithera power-law model or a thermal bremsstrahlung model. A plausible interpretation of the brighter nebula is in terms of a collimated ballistic jet. The secondary nebula is most likely a classical synchrotron-emitting tail.

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Section: The Nebulaementioning

confidence: 57%

Section: Introductionmentioning

confidence: 99%

The Tale of the Two Tails of the Oldish PSR J2055+2539

Marelli

Pizzocaro

Luca

et al. 2016

ApJ

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“…Note that this argument is independent of the possible X-ray "tail" of PSR J1740+1000 (Kargaltsev et al 2008), whose orientation could be interpreted as indicating motion parallel to the Galactic plane. In any case, the tail may not be real, because the 64 ks Chandra image of PSR J1740+1000 from 2010 does not clearly show it.…”

Section: Comparison With Psr J1740+1000mentioning

confidence: 82%

X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

Halpern

Bogdanov

Gotthelf

2013

ApJ

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We measure spin-down of the 59 ms X-ray pulsar Calvera by comparing the XMM-Newton discovery data from 2009 with new Chandra timing observations taken in 2013. Its period derivative isṖ = (3.19 ± 0.08) × 10 −15 , which corresponds to spin-down luminosityĖ = 6.1 × 10 35 erg s −1 , characteristic age τ c ≡ P /2Ṗ = 2.9 × 10 5 yr, and surface dipole magnetic field strength B s = 4.4 × 10 11 G. These values rule out a mildly recycled pulsar, but Calvera could be an orphaned central compact object (anti-magnetar), with a magnetic field that was initially buried by supernova debris and is now reemerging and approaching normal strength. We also performed unsuccessful searches for high-energy γ -rays from Calvera in both imaging and timing of >100 MeV Fermi photons. Even though the distance to Calvera is uncertain by an order of magnitude, an upper limit of d < 2 kpc inferred from X-ray spectra implies a γ -ray luminosity limit of <3.3 × 10 32 erg s −1 , which is less than that of any pulsar of comparableĖ. Calvera shares some properties with PSR J1740+1000, a young radio pulsar that we show by virtue of its lack of proper motion was born outside of the Galactic disk. As an energetic, high-Galactic-latitude pulsar, Calvera is unique in being undetected in both radio and γ -rays to faint limits, which should place interesting constraints on models for particle acceleration and beam patterns in pulsar magnetospheres.

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“…The pulsar's position is from D' Amico et al (2001). PSR J1509−5850 (see Figure 2): The pulsar is located inside an X-ray (Kargaltsev et al 2008) and radio (Hui & Becker 2007) wind nebula. Weltevrede et al (2009) report the gamma-ray detection of the pulsar.…”

Section: Results: Fermi Pulsarsmentioning

confidence: 99%

Pulsar Timing with the Parkes Radio Telescope for the Fermi Mission

Weltevrede

Johnston

Manchester

et al. 2010

Publ. – Astron. Soc. Aust

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Abstract:We report here on two years of timing of 168 pulsars using the Parkes radio telescope. The vast majority of these pulsars have spin-down luminosities in excess of 10 34 erg s −1 and are prime target candidates to be detected in gamma-rays by the Fermi Gamma-Ray Space Telescope. We provide the ephemerides for the ten pulsars being timed at Parkes which have been detected by Fermi in its first year of operation. These ephemerides, in conjunction with the publicly available photon list, can be used to generate gamma-ray profiles from the Fermi archive. We will make the ephemerides of any pulsars of interest available to the community upon request. In addition to the timing ephemerides, we present the parameters for 14 glitches which have occurred in 13 pulsars, seven of which have no previously known glitch history. The Parkes timing programme, in conjunction with Fermi observations, is expected to continue for at least the next four years.

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X‐Ray Observations of Parsec‐scale Tails behind Two Middle‐Aged Pulsars

Cited by 64 publications

References 39 publications

The Tale of the Two Tails of the Oldish PSR J2055+2539

The Tale of the Two Tails of the Oldish PSR J2055+2539

X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

Pulsar Timing with the Parkes Radio Telescope for the Fermi Mission

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