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Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER

Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER
Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER
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.
ISM: individual: G12.82-0.02, HESS J1813-178, ISM: supernova remnants, X-rays: stars, pulsars: general, pulsars: individual: CXOU J181335.16-174957.4, PSR J1813-1749
0035-8711
4396-4403
Ho, Wynn C. G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Guillot, Sebastien
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Saz Parkinson, P.M.
e4b078fb-34ff-4709-b3f7-64dfb330f147
Limyansky, B.
386957c8-f8da-438a-b083-804a5be3f228
Ng, C.-Y.
76622418-7d39-49bd-832e-54363ee26ddf
Bejger, Michal
1699003c-05ed-4f4e-8879-ba7073e2f007
Espinoza, Cristobal M.
505d9674-e6db-4fa6-bcb3-5365b2d8121c
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Jaisawal, Gaurava K.
4d5dcd39-0881-426d-8ad7-f378238405ae
Malacaria, Christian
309a8f91-28a7-4365-b0a3-633171fc2e51
Ho, Wynn C. G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Guillot, Sebastien
26b90302-d8b3-4b06-9254-d3327cac3ccc
Saz Parkinson, P.M.
e4b078fb-34ff-4709-b3f7-64dfb330f147
Limyansky, B.
386957c8-f8da-438a-b083-804a5be3f228
Ng, C.-Y.
76622418-7d39-49bd-832e-54363ee26ddf
Bejger, Michal
1699003c-05ed-4f4e-8879-ba7073e2f007
Espinoza, Cristobal M.
505d9674-e6db-4fa6-bcb3-5365b2d8121c
Haskell, B.
a3c09067-6932-45cc-902d-3b7117ec848d
Jaisawal, Gaurava K.
4d5dcd39-0881-426d-8ad7-f378238405ae
Malacaria, Christian
309a8f91-28a7-4365-b0a3-633171fc2e51

Ho, Wynn C. G., Guillot, Sebastien, Saz Parkinson, P.M., Limyansky, B., Ng, C.-Y., Bejger, Michal, Espinoza, Cristobal M., Haskell, B., Jaisawal, Gaurava K. and Malacaria, Christian (2020) Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER. Monthly Notices of the Royal Astronomical Society, 498 (3), 4396-4403. (doi:10.1093/mnras/staa2653).

Record type: Article

Abstract

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.

Text
2009.00031 - Accepted Manuscript
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More information

Accepted/In Press date: 27 August 2020
e-pub ahead of print date: 1 September 2020
Published date: 25 September 2020
Keywords: ISM: individual: G12.82-0.02, HESS J1813-178, ISM: supernova remnants, X-rays: stars, pulsars: general, pulsars: individual: CXOU J181335.16-174957.4, PSR J1813-1749

Identifiers

Local EPrints ID: 443784
URI: http://eprints.soton.ac.uk/id/eprint/443784
ISSN: 0035-8711
PURE UUID: d276acc0-47d8-4e6d-8d0c-be8fd06745af
ORCID for Wynn C. G. Ho: ORCID iD orcid.org/0000-0002-6089-6836

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Date deposited: 11 Sep 2020 16:41
Last modified: 26 Nov 2021 02:54

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Contributors

Author: Wynn C. G. Ho ORCID iD
Author: Sebastien Guillot
Author: P.M. Saz Parkinson
Author: B. Limyansky
Author: C.-Y. Ng
Author: Michal Bejger
Author: Cristobal M. Espinoza
Author: B. Haskell
Author: Gaurava K. Jaisawal
Author: Christian Malacaria

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