The Proper Motion of the Pulsar J1124–5916 in the Galactic Supernova Remnant G292.0+1.8

Long, Xuejun; Patnaude, Daniel; Plucinsky, Paul P.; Gaetz, T. J.

doi:10.3847/1538-4357/ac704b

Cited by 9 publications

(7 citation statements)

References 41 publications

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“…To obtain astrometric corrections for each observation, we first needed to obtain precise point-source positions that took the detector point-spread function (PSF) into account. For this, we followed the methods of past papers (e.g., Mayer et al 2020;Long et al 2022). We produce PSF simulations using the CIAO Chandra Ray Tracer (ChaRT) tool, 3 generating five iterations of each point source with a monochromatic spectrum of 1 keV with 0.01 photons cm −2 s −1 .…”

Section: Point-spread Function Modeling and Fittingmentioning

confidence: 99%

“…Only Chandra has sufficient spatial resolution to measure the proper motions of NSs, and doing so requires baselines of at least a decade for all but the closest objects. There are currently ∼20 velocity measurements of NSs embedded within SNRs, found using a mix of direct proper-motion measurements (e.g., Auchettl et al 2015;Temim et al 2017;Shternin et al 2019;Mayer & Becker 2021;Long et al 2022) and measuring the distances between NS positions and estimated SNR explosion sites (e.g., Winkler et al 2009;Banovetz et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Updated Proper Motion of the Neutron Star in the Supernova Remnant Cassiopeia A

Holland-Ashford,

Slane,

Long

2024

ApJ

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In this paper, we present updated estimates of the velocity of the neutron star (NS) in the supernova remnant Cassiopeia A using over two decades of Chandra observations. We use two methods: (1) recording the NS positions from dozens of Chandra observations, including the astrometric uncertainty estimates on the data points, but not correcting the astrometry of the observations; and (2) correcting the astrometry of the 13 Chandra observations that have a sufficient number of point sources with identified Gaia counterparts. For method #1, we observe a heliocentric velocity of 275 ± 121 km s−1, with an angle of 177° ± 22° east of north. For method #2, we observe a heliocentric velocity of 436 ± 89 km s−1 at an angle of 158° ± 12°. Correcting for galactic rotation and the Sun’s peculiar motion decreases these estimates to 256 km s−1 at 167° and 433 km s−1 at 151°, respectively. Both of our estimates match with the explosion-center-estimated velocity of ∼350 km s−1 and the previous 10 yr baseline proper-motion measurement of 570 ± 260 km s−1, but our use of additional data over a longer baseline has led to a smaller uncertainty by a factor of 2–3. Our estimates rule out velocities ≳600 km s−1 and better match with simulations of Cassiopeia A that include NS kick mechanisms.

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Section: Point-spread Function Modeling and Fittingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Updated Proper Motion of the Neutron Star in the Supernova Remnant Cassiopeia A

Holland-Ashford,

Slane,

Long

2024

ApJ

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“…The gold standard for making such claims is accurate pulsar proper motion and parallax measurements. Often both the magnitude and direction of the proper motion can reinforce the claimed association by showing that the pulsar likely originated near the geometric center of the SNR (Deller et al 2012;Van Etten et al 2012;Shternin et al 2019;Johnston & Lower 2021;Long et al 2022). In other cases, proper motion measurements either exclude an association or require more complex scenarios to remain tenable (Brisken et al 2006;de Vries et al 2021;Espinoza et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Cannonball or Bowling Ball: Proper Motion and Parallax for PSR J0002+6216

Bruzewski,

Schinzel,

Taylor

et al. 2023

ApJ

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We report the results of careful astrometric measurements of the cannonball pulsar J0002+6216 carried out over 3 yr using the High Sensitivity Array. We significantly refine the proper motion to μ = 35.3 ± 0.6 mas yr−1 and place new constraints on the distance, with the overall effect of lowering the velocity and increasing the inferred age to 47.60 ± 0.80 kyr. Although the pulsar is brought more in line with the standard natal kick distribution, this new velocity has implications for the morphology of the pulsar wind nebula that surrounds it, the density of the interstellar medium through which it travels, and the age of the supernova remnant (CTB 1) from which it originates.

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“…Tracking metal-rich ejecta over many years and measuring their proper motions enable estimates of the center of expansion (CoE) and explosion age, as well as information about the progenitor system's circumstellar material (CSM) environment via ejecta interaction. The CoE and explosion age are important values for determining the kick velocity of compact objects (Vogt et al 2018;Banovetz et al 2021;Long et al 2022), searching for surviving companions (Kerzendorf et al 2019;Li et al 2021), and measuring differences between optical and X-ray centers (Katsuda et al 2018). These values can also serve as important tests for increasingly sophisticated 2D and 3D supernova simulations (e.g., Wongwathanarat et al 2015;Janka et al 2016;Burrows et al 2019;Ferrand et al 2021;Orlando et al 2021Orlando et al , 2022.…”

Section: Introductionmentioning

confidence: 99%

Hubble Space Telescope Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age

Banovetz

Milisavljevic

Sravan

et al. 2023

ApJ

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We present proper motion measurements of the oxygen-rich ejecta of the LMC supernova remnant N132D using two epochs of Hubble Space Telescope Advanced Camera for Surveys data spanning 16 years. The proper motions of 120 individual knots of oxygen-rich gas were measured and used to calculate a center of expansion (CoE) of α = 5h25m01.ˢ71 and δ = −69°38′41.″64 (J2000) with a 1σ uncertainty of 2.″90. This new CoE measurement is 9.″2 and 10.″8 from two previous CoE estimates based on the geometry of the optically emitting ejecta. We also derive an explosion age of 2770 ± 500 yr, which is consistent with recent age estimates of ≈2500 yr made from 3D ejecta reconstructions. We verified our estimates of the CoE and age using a new automated procedure that detected and tracked the proper motions of 137 knots, with 73 knots that overlap with the visually identified knots. We find that the proper motions of the ejecta are still ballistic, despite the remnant’s age, and are consistent with the notion that the ejecta are expanding into an interstellar medium cavity. Evidence for explosion asymmetry from the parent supernova is also observed. Using the visually measured proper motion measurements and corresponding CoE and age, we compare N132D to other supernova remnants with proper motion ejecta studies.

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The Proper Motion of the Pulsar J1124–5916 in the Galactic Supernova Remnant G292.0+1.8

Cited by 9 publications

References 41 publications

Updated Proper Motion of the Neutron Star in the Supernova Remnant Cassiopeia A

Updated Proper Motion of the Neutron Star in the Supernova Remnant Cassiopeia A

Cannonball or Bowling Ball: Proper Motion and Parallax for PSR J0002+6216

Hubble Space Telescope Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age

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