Proper motion, spectra, and timing of PSR J1813–1749 using Chandra and NICER
| Autor: | C. Malacaria, P. M. Saz Parkinson, Sebastien Guillot, Cristobal M. Espinoza, Wynn C. G. Ho, Brynmor Haskell, Gaurava K. Jaisawal, B. Limyansky, Micha l. Bejger, Chi-Yung Ng |
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| Přispěvatelé: | Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS) |
| Jazyk: | angličtina |
| Rok vydání: | 2020 |
| Předmět: |
Brightness
Proper motion Photon ISM: individual: G12.82–0.02 FOS: Physical sciences X-rays: stars Astrophysics 01 natural sciences Pulsar wind nebula Article Spectral line Luminosity HESS J1813–178 PSR J1813–1749 Pulsar pulsars: general 0103 physical sciences 010306 general physics 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) pulsars: individual: CXOU J181335.16–174957.4 ISM: supernova remnants High Energy Astrophysical Phenomena (astro-ph.HE) Physics Astronomy and Astrophysics Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science Glitch (astronomy) Astrophysics - High Energy Astrophysical Phenomena [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] |
| Zdroj: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 2020, 498 (3), pp.4396-4403. ⟨10.1093/mnras/staa2653⟩ Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P-Oxford Open Option A, 2020, 498 (3), pp.4396-4403. ⟨10.1093/mnras/staa2653⟩ Mon Not R Astron Soc Ho, W C G, Guillot, S, Parkinson, P M S, Limyansky, B, Ng, C-Y, Bejger, M, Espinoza, C M, Haskell, B, Jaisawal, G K & Malacaria, C 2020, ' Proper motion, spectra, and timing of PSR J1813−1749 using Chandra and NICER ', Monthly Notices of the Royal Astronomical Society, vol. 498, pp. 4396–4403 . https://doi.org/10.1093/mnras/staa2653 |
| ISSN: | 0035-8711 1365-2966 |
| DOI: | 10.1093/mnras/staa2653⟩ |
| Popis: | PSR J1813-1749 is one of the most energetic rotation-powered pulsars known, producing a pulsar wind nebula (PWN) and gamma-ray and TeV emission, but whose spin period is only measurable in X-ray. We present analysis of two Chandra datasets that are separated by more than ten years and recent NICER data. The long baseline of the Chandra data allows us to derive a pulsar proper motion mu_R.A.=-(0.067"+/-0.010") yr^-1 and mu_decl.=-(0.014"+/-0.007") yr^-1 and velocity v_perp~900-1600 km/s (assuming a distance d=3-5 kpc), although we cannot exclude a contribution to the change in measured pulsar position due to a change in brightness structure of the PWN very near the pulsar. We model the PWN and pulsar spectra using an absorbed power law and obtain best-fit absorption NH=(13.1+/-0.9)x10^22 cm^-2, photon index Gamma=1.5+/-0.1, and 0.3-10 keV luminosity Lx~5.4x10^34 erg/s (d/5 kpc)^2 for the PWN and Gamma=1.2+/-0.1 and Lx~9.3x10^33 erg/s (d/5 kpc)^2 for PSR J1813-1749. These values do not change between the 2006 and 2016 observations. We use NICER observations from 2019 to obtain a timing model of PSR J1813-1749, with spin frequency nu=22.35 Hz and spin frequency time derivative nudot=(-6.428+/-0.003)x10^-11 Hz/s. We also fit nu measurements from 2009-2012 and our 2019 value and find a long-term spin-down rate nudot=(-6.3445+/-0.0004)x10^-11 Hz/s. We speculate that the difference in spin-down rates is due to glitch activity or emission mode switching. 9 pages, 5 figures; accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
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