Abstract
Abstract PSR J1813–1749 has peculiarities that make it a very interesting object of study. It is one of the most energetic and the most scattered pulsars known. It is associated with HESS J1813–178, one of the brightest and most compact TeV sources in the sky. Recently, Ho et al. used archival X-ray Chandra observations separated by more than 10 yr and determined that the total proper motion of PSR J1813–1749 is ∼66 mas yr−1, corresponding to a velocity of ∼1900 km s−1 for a distance of 6.2 kpc. These results would imply that this pulsar is the fastest neutron star known in the Galaxy and, by estimating the angular separation with respect to the center of the associated supernova remnant, has an age of only ∼300 yr, making it one of the youngest pulsars known. Using archival high angular resolution VLA observations taken over 12 yr we have estimated the radio proper motions of PSR J1813–1748 to be much smaller: ( μ α · cos ( δ ) , μ δ ) = (−5.0 ± 3.7, −13.2 ± 6.7) mas yr−1, or a total proper motion of 14.8 ± 5.9 mas yr−1. The positions referenced against quasars make our results reliable. We conclude that PSR J1813–1749 is not a very fast moving source. Its kinematic age using the new total proper motion is ∼1350 yr. This age is consistent within a factor of a few with the characteristic age of the pulsar and with the age estimated from the broadband spectral energy distribution of HESS J1813–178, as well as the age of the associated supernova remnant.
Highlights
PSR J1813–1749 (=CXOU J181335.1−174957) is the most scattered and the second most energetic pulsar in the Milky Way (Halpern et al 2012; Camilo et al 2021)
The total proper motion of PSR J1814–1749 is an interesting subject to study, and in this paper we present the proper motions measured with archival high angular resolution observations taken with the Very Large Array (VLA) by us and by other groups
The proper motions of PSR J1813–1749 determined from the X-ray observations are = (−64 ± 9, −14 ± 7) mas yr−1
Summary
PSR J1813–1749 (=CXOU J181335.1−174957) is the most scattered and the second most energetic pulsar in the Milky Way (Halpern et al 2012; Camilo et al 2021). As the pulsar is at an angular distance of ∼20′′ from the center of the SNR G12.82–0.02 the large proper motions would indicate a young age of around 300 yr, making it one of the youngest pulsars known This age, while consistent at the lower end of the age range of 285–2500 yr for SNR G12.82–0.02 (Brogan et al 2005), is, in conflict with the age estimated for HESS J1813–178 of 2500 yr (Zhu et al 2018) and the characteristic age of the pulsar of 5600 yr (Halpern et al 2012). As discussed by Camilo et al (2021), the total proper motion of ∼66 mas yr−1 would imply a tangential velocity of the order of 2000 km s−1 at 6.2 kpc, the lower limit of the distance This velocity is larger than that of any well-measured velocity for a neutron star (see Deller et al 2019). The total proper motion of PSR J1814–1749 is an interesting subject to study, and in this paper we present the proper motions measured with archival high angular resolution observations taken with the VLA by us and by other groups
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