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

Marelli, M.; Pizzocaro, D.; Luca, A. De; Gastaldello, F.; Caraveo, P. A.; Parkinson, P. Saz

doi:10.3847/0004-637x/819/1/40

Cited by 19 publications

(32 citation statements)

References 49 publications

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“…Gotthelf & Bogdanov (2017) reported in Table 3. The best-fit parameters and non-thermal X-ray fluxes obtained in this work are consistent within the uncertainties (at a confidence level ≤ 2σ in all cases) with those reported in the literature using the same data sets (see Marelli et al 2011Marelli et al , 2013Marelli et al , 2014aMarelli et al , 2015Marelli et al , 2016Ransom et al 2011;Van Etten et al 2012;Lin et al 2013Lin et al , 2014Arumugasamy et al 2014;Guillot et al 2016). The spectra we derived here, together with the best-fitting models are shown in the left-hand panels of Figure A1 in the Appendix A.…”

Section: X-ray Spectral Modellingsupporting

confidence: 89%

Spectral characterization of the non-thermal X-ray emission of gamma-ray pulsars

Zelati

Torres

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report on a detailed spectral characterization of the non-thermal X-ray emission for a large sample of gamma-ray pulsars in the second Fermi LAT catalogue. We outline the criteria adopted for the selection of our sample, its completeness, and critically describe different approaches to estimate the spectral shape and flux of pulsars. We perform a systematic modelling of the pulsars' X-ray spectra using archival observations with XMM-Newton, Chandra and NuSTAR and extract the corresponding non-thermal X-ray spectral distributions. This set of data is made available online and is useful to confront with predictions of theoretical models.

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Section: X-ray Spectral Modellingsupporting

confidence: 89%

Spectral characterization of the non-thermal X-ray emission of gamma-ray pulsars

Zelati

Torres

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Two other examples are the outflows associated with PSR J1101-6101 (the Lighthouse Nebula; Pavan et al 2014) and PSR J2055 +2539 (Marelli et al 2015). The former shows a particularly remarkable structure.…”

Section: Large-scale Pwn Structurementioning

confidence: 99%

Chandra Observations of Outflows From PSR J1509–5850

Klingler

Kargaltsev

Rangelov

et al. 2016

ApJ

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PSR J1509-5850 is a middle-aged pulsar with a period of P≈89 ms and spin-down power oḟ =É 5.1 10 35 erg s −1 , at a distance of about 3.8 kpc. We report on deep Chandra X-ray Observatory observations of this pulsar and its pulsar wind nebula (PWN). In addition to the previously detected tail extending up to 7′ southwest from the pulsar (the southern outflow), the deep images reveal similarly long, faint, diffuse emission stretched toward the north (the northern outflow) and the fine structure of the compact nebula (CN) in the pulsar vicinity. The CN is resolved into two lateral tails and one axial tail pointing southwest (a morphology remarkably similar to that of the Geminga PWN), which supports the assumption that the pulsar moves toward the northeast. The luminosities of the southern and northern outflows are about1 10 33 and 4 10 32 erg s −1 , respectively. The spectra extracted from four regions of the southern outflow do not show any softening with increasing distance from the pulsar. The lack of synchrotron cooling suggests a high flow speed or in situ acceleration of particles. The spectra extracted from two regions of the northern outflow show a hint of softening with distance from the pulsar, which may indicate slower particle propagation. We speculate that the northern outflow is associated with particle leakage from the bow-shock apex into the ISM, while the southern outflow represents the tail of the shocked pulsar wind behind the moving pulsar. We estimate the physical parameters of the observed outflows and compare the J1509-5850 PWN with PWNe of other supersonically moving pulsars.

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“…In the case of a classical X-ray synchrotron emission, a variation of the mean interstellar density would cause the formation of such lobes, although this would imply a variation of a factor ∼10 on a ∼0.01 pc scale (for a 0.38 kpc distance). Alternatively, a spatial-dependent particle re-acceleration mechanism could be at work, as already invoked for other peculiar PWNe around, e.g., PSR J2055+2539 (Marelli et al 2016) and PSR J1509−5850 (Klingler et al 2016), or a different emission mechanism could be responsible for powering the X-ray PWN, like, e.g., in PSR J0357+3205 (Marelli et al 2013). …”

Section: Discussionmentioning

confidence: 99%

A CANDIDATE OPTICAL COUNTERPART TO THE MIDDLE AGED Γ-Ray PULSAR PSR J1741–2054*

Mignani

Testa

Marelli

et al. 2016

ApJ

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We carried out deep optical observations of the middle aged γ-ray pulsar PSR J1741−2054 with the Very Large Telescope (VLT). We identified two objects, of magnitudes m v = 23.10 ± 0.05 and m v = 25.32 ± 0.08, at positions consistent with the very accurate Chandra coordinates of the pulsar, the faintest of which is more likely to be its counterpart. From the VLT images we also detected the known bow-shock nebula around PSR J1741 −2054. The nebula is displaced by ∼0 9 (at the 3σ confidence level) with respect to its position measured in archival data, showing that the shock propagates in the interstellar medium consistently with the pulsar proper motion. Finally, we could not find evidence of large-scale extended optical emission associated with the pulsar wind nebula detected by Chandra, down to a surface brightness limit of ∼28.1 mag arcsec −2 . Future observations are needed to confirm the optical identification of PSR J1741−2054 and characterize the spectrum of its counterpart.

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

Cited by 19 publications

References 49 publications

Spectral characterization of the non-thermal X-ray emission of gamma-ray pulsars

Spectral characterization of the non-thermal X-ray emission of gamma-ray pulsars

Chandra Observations of Outflows From PSR J1509–5850

A CANDIDATE OPTICAL COUNTERPART TO THE MIDDLE AGED Γ-Ray PULSAR PSR J1741–2054*

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