Kyr psr. PDF | The characteristic age of PSR J1734$-$3333 estimated from its current spin down rate implies that it is a young pulsar ($\tau_c | Find, read and cite all the research you need on ResearchGate

PSR B0740-28 has a spin-frequency of 6 Hz and a characteristic (spin-down) age of 160 kyr. We monitor PSR B0740-28 for 1 hour per day with the 42-ft telescope and approximately weekly with the Lovell telescope.

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acteristic age τ ≡P/2P˙ ∼17 kyr, PSR J2021+3651 is still energetic, with E˙ ∼3.4 ×1036 erg s−1. PSR J2021+3651 is detected in X-ray as a soft (mostly) ther-mal (kT BB= 0.16±0.02 keV) point source by Chandra (Hessels et al.(2004) andVan Etten et al.(2008)). The authors of both works reported the detection of X-ray pulsations to be ...

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Pulsations from PSR J1617-5055 (J1617 hereafter) ... {12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab, as well as ...PSR B0540-69 is the first young pulsar detected to have a spin-down rate transition. It results in a delayed brightening of its pulsar wind nebula ... with a characteristic age kyr. PSR B1931+24 shows periodical emission behavior, which could switch off in 10 s (Kramer et al. 2006).Specialties: Top rated in Chino We Specialize in: - Musical Instrument Lessons - Musical Instrument Rental - Musical Instruments - Music Instruction-Instrumental - Musical Instruments-Repair - Music Sheet - Music Stores Established in 2002. KYR is the realization of a dream of Karen and Richard. Richard started playing at age 10, like many of today's kids, and understands the need of a strong ...The same conclusion is reached by comparing every 400-kyr-long interval in increments of 100 kyr with the 0-800 kyr period . These results point out the absence of any dominant stable periodicity.Some basketball fans are so excited for the coming NBA season that they are paying upwards of $300 for tickets to the draft at the Barclays Center in Brooklyn on Thursday. By click...View a PDF of the paper titled Extended Very-High-Energy Gamma-Ray Emission Surrounding PSR J0622 + 3749 Observed by LHAASO-KM2A, by LHAASO Collaboration View PDF Abstract: We report the discovery of an extended very-high-energy (VHE) gamma-ray source around the location of the middle-aged (207.8 kyr) pulsar PSR J0622+3749 with the Large High ...3.1 PSR B0154+61 (J0157+6212, τ=200 kyr) Although data on PSR B0154+61 have been collected at Jodrell Bank for more than 10 yr since MJD 46866, this pulsar suffered its first observed glitch near MJD 48504. The glitch was quite small with the size of the frequency jump equal to 2.46 × 10 −9. The frequency and timing residuals are shown in lower and …We report the discovery of an extended very-high-energy (VHE) gamma-ray source around the location of the middle-aged (207.8 kyr) pulsar PSR J 0622 +3749 with the Large High-Altitude Air Shower Observatory (LHAASO). The source is detected with a significance of 8.2 σ for E >25 TeV assuming a Gaussian template. The best-fit location is (right ascension, declination) =(95.47 ° ±0.11 ° ,37 ...

Analysts rate ASX-listed companies QBE Insurance Group (AU:QBE) and Allkem Limited (AU:AKE) as Buy. Analysts are overall bullish on both stocks... Analysts rate ASX-listed companie...Abstract. We describe a sensitive targeted search campaign at Parkes to find faint young radio pulsars using the center beam of the 20-cm multi-beam receiver. The high …PSR J1928 + 1746, a 69-ms pulsar with a characteristic age of 82 kyr, is a plausible candidate for association with the unidentified EGRET source 3EG J1928 + 1733. PSR J1906 + 0746 is a 144-ms, non-recycled pulsar in a relativistic binary with an orbital period of 3.98 hr. The rate of periastron advance implies a total system mass of 2.4 M ...young pulsar PSR J1813−1749, located close to the center of ... PSR J1813−1749 has a spindown luminosity of E-dot = 6.8 x10e37 erg s−1, a characteristic age of 3.3-7.5 kyr (Gotthelf & Halpern 2009), and an estimated distance of 4.8 kpc (Halpern et al. 2012)." - "Closer to the measured HAWC location is SNR G013.5+00.2 (0.2deg

The best fit 21 kyr 21 kiloyear 21\,$\mathrm{kyr}$ and 40 kyr 40 kiloyear 40\,$\mathrm{kyr}$ Model 1 consisted of a pulsar injecting electrons into the surrounding medium with a spin-down conversion factor of 10.7 10.7 10.7 and 0.14 % percent 0.14 0.14\% respectively, indicating that the true age of the system is older than the …

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The survey has so far resulted in the discovery of 15 radio pulsars, including a pulsar with a characteristic age of ∼18 kyr, PSR J2004+3429, and a highly eccentric, binary millisecond pulsar ...PSR J2032+4127 is co-located with the extended TeV gamma-ray source, TeV J2032+4130, and may be physically associated with it. Source Information: From VERITAS and MAGIC Collaborations (2018): - "We report on observations of the pulsar / Be star binary system. PSR J2032+4127 / MT91 213 in the energy range between 100 GeV and 20 TeV.The timing solution, reported by Levin et al. , implies a very high surface magnetic field of B≈ 2.8 × 10 14 G and a characteristic age of τ c ≈ 4 kyr. PSR J1622-4950 has a flat radio spectrum and a highly variable flux density and pulse profile [8 - 10, 16, 89], which is similar to other radio magnetars.produced by the birth supernova of PSR J1734-3333 could have already faded to undetectable brightness, estimates of which suggest timescales of 10-100 kyr. This and other considerations lead us to conclude that the pulsar is possibly older than 45-100 kyr. PSR J1734-3333 is a pulsar with rotational properties that place it between

Here's how to get those travel vibes without leaving town. For many students, spring break represents the perfect school holiday. While Thanksgiving and Christmas are fun, they oft...and GeV γ-ray bands. W44 hosts the pulsar PSR B1853+01, a 20 kyr pulsar with dE/dt= 4.3 x 10e35 erg s-1 located approx. 3 kpc away. W44 has not been detected by H.E.S.S. during the HGPS, but H.E.S.S. reported significant emission with only one of their analysis chains at the location of W44, without claiming a detection (Abdalla et al., 2018)."Enter the email address you signed up with and we'll email you a reset link.We report the discovery of PSR J2022+3842, a 24 ms radio and X-ray pulsar in the supernova remnant G76.9+1.0, in observations with the Chandra X-ray telescope, the Robert C. Byrd Green Bank Radio Telescope, and the Rossi X-ray Timing Explorer (RXTE). The pulsar's spin-down rate implies a rotation-powered luminosity Edot = 1.2 x 10^{38} erg/s, a surface dipole magnetic field strength B_s = 1.0 ...up to ∼100 kyr. PSR B1706−44 is recently detected in VHE gamma-rays (Hoppe et al. 2009), and it has largely extended X-ray emission (Romani et al. 2005). However, no X-ray observation covered the entire emission, and we could not measure the extension. There are some other PWNe with known large extended X-ray nebulae, such as PSR J1016−5857with an estimated characteristic age of 77 kyr2 and a spin-down 2 There is a significant discrepancy between the characteristic spin-down age of PSR J2021+4026 and the estimated age of SNR G 78.2+2.1 of <10 kyr (Leahy et al. 2013). Article number, page 1 of 12The pulsar's spin-down rate implies a rotation-powered luminosity E-dot = 1.2x10{sup 38} erg s{sup -1}, a surface dipole magnetic field strength B{sub s} = 1.0 x 10{sup 12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab pulsar, as well as the most rapidly rotating ...PSR J2139+4716 has the lowest spin-down power (3 × 10 33 erg s -1 ) among all non-recycled gamma-ray pulsars ever found. Despite extensive multi-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars.c = 42:9 kyr) rotation-powered pulsar (Gotthelf et al.2011;Kuiper & Hermsen 2015). The source exhibits a non-sinusoidal single pulse per rotation with width ˘0:5 in rotation phase at both ... PSR J1412+7922 and PSR J1849 0001 are only seen to be pulsed in X-rays, the timing models presented here will enable LIGO/Virgo to search for GWs from these two …tic age τ = 10 −100 kyr) pulsars are often associated with very-high-energy (VHE, above 1 TeV) sources (e.g., H.E.S.S. Collaboration et al.(2018)). Many of them are luminous above a hundred TeV without a hint of a spectral cutoff (e.g.,Abeysekara et al.(2020) andSu-doh et al.(2021)). Recently, the higher energy regimeFrom Cao et al. (2021): - This list contains "Nearby teraelectronvolt sources within 1deg of the centre of the LHAASO source". - TeV J2032+4130 / 2HWC J2031+415 / VER J2032+414. - ARGO J2031+4157. - MGRO J2031+41. Pevatron: From Mitchell (2021): - this source is included in a list of Galactic sources currently known.PSR B0656+14 (P= 385 ms;マ・/font>= 1.1 テ・105yr), located at the distance of 288 ツア 30 pc (Brisken et al. 2003), is the brightest of middle-aged pulsars, in both X-rays and optical. 4Bignami et al. (1996) claimed a feature in the optical窶填V spectrum of Geminga (see also Mignani et al. 1998), but this was not supported by ...Jan 1, 2005 · The pulsar is very young, with a characteristic age τ c ≡ P / 2 P ˙ ∼ 5 kyr, and its spin-period of 16 ms makes it the fastest non-recycled pulsar known. PSR J0537−6910 is one of only a handful of young ( τ c < 10 kyr), energetic pulsars (of which the Crab pulsar is the prototype) that are known.coincident with PSR J1928+1746, which at an age of 8.2 x10e4 years and a spin-down luminosity of 1.6 x10e36 erg s-1 is both older and less energetic than PSR J1930+1852 (Cordes et al. 2006). The flux of 3FGL J1928.9+1739 follows a log parabola shape, and its extrapolation to energies larger than 1 TeV lies far below the flux of 2HWC J1928+177.We present the discovery of the Vela-like radio pulsar J1856 0245 in the Arecibo PALFA survey. PSR J1856 0245 has a spin period of 81 ms, a characteristic age of 21 kyr, and a spin-down luminosity ergs s . It isE˙ p 4.6 #1036 1 positionally coincident with the TeV g-ray source HESS J1857 026, which has no other known counterparts. Young,Join the KYR Membership and you'll get Birthday Discount, Cashback every purchases, & many more!whose characteristic age tº~PP217 kyr, PSR J2021 +3651 is still energetic, with E ~´3.4 10 erg s36 1-. PSR J2021+3651 is detected in X-ray as a soft (mostly) thermal (kT BB =0.16±0.02 keV) point source by Chandra (Hessels et al. 2004; Van Etten et al. 2008). The authors of both works reported the detection of X-ray pulsations to be ...

At the pulsar's characteristic age of 17 kyr, the association can be preserved through a combination of progenitor wind, birth kick, and PWN outflow. Associated TeV emission may, however, indicate an explosion in an earlier supernova. ... PSR J1709-4429 is a young (yr) pulsar, with spindown luminosity erg s −1, ...In turn, all of them present characteristic age around a few tens of kyr, similar to that displayed by detected PWNe. Basic information from these pulsars, taken from the ATNF pulsar catalogue Footnote 1 ... using the values from the Distance column when available. In cases where the distance is not well define, as for PSR J2111+4606, …PSR (kyr) ⁄(ergs−1) J1406-6121 61.7 2.2×1035 J1410-6132 24.8 1×1037 J1412-6145 50.4 1.2×1035 J1413-6141 13.6 5.6×1035 J1413-6205 62.8 8.3×1035 2. Analysis method 2.1 Data selection and preparation DatawereprocessedwiththeH.E.S.S.analysispackage(HAP),applyingaHillas-typeshower …The characteristic age of PSR J1734$-$3333 estimated from its current spin down rate implies that it is a young pulsar ($\tau_c<10$ kyr). ... This and other considerations lead us to conclude that ...Dec 9, 2021 · For the pulsar PSR J1734-3333, both the estimated SNR age (23 kyr) [35] and proper motion age (45-100 kyr) [94] are much older than its characteristic age (8.1 kyr), which might hint at the fact ...Abstract. We present the discovery and timing of the young (age ∼28.6 kyr) pulsar PSR J0837–2454. Based on its high latitude ( b = 98) and dispersion measure (DM = 143 pc cm −3 ), the pulsar appears to be at a z -height of >1 kpc above the Galactic plane, but near the edge of our Galaxy.

acteristic age τ ≡P/2P˙ ∼17 kyr, PSR J2021+3651 is still energetic, with E˙ ∼3.4 ×1036 erg s−1. PSR J2021+3651 is detected in X-ray as a soft (mostly) ther-mal (kT BB= 0.16±0.02 keV) point source by Chandra (Hessels et al.(2004) andVan Etten et al.(2008)). The authors of both works reported the detection of X-ray pulsations to be ...PWNe with ages up to several kyr. Recent X-ray observations have shown the presence 1 SchoolofCosmicPhysics ... Uchiyama et al. (2009) found a largely extended nebula from PSR B1823-13 as-sociated with HESS J1825−137, which could not be detected with Chandra (Pavlov et al. 2008) or XMM-Newton(Gaensler et al. 2003) observations. ...01:00:09 UTC. Now observing the Crab pulsar PSR B0531+21 with the 42ft telescope. Rotation period: 33.4 ms Age: 1 kYr Distance: 2.0 kpc. 23 Jan 2022The pulsar's spin-down rate implies a rotation-powered luminosity E-dot = 1.2x10{sup 38} erg s{sup -1}, a surface dipole magnetic field strength B{sub s} = 1.0 x 10{sup 12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab pulsar, as well as the most rapidly …PSR B0355+54 (J0358+5413; hereafter B0355) is a radio-loud pulsar with characteristic age ˝= 564 kyr and spin-down power E_ = 4:5 1034 erg s 1. Using very long baseline interferometry, Chatterjee et al.(2004) derived a parallax-determined distance of 1:04+0:21 0:16 kpc and transverse proper velocity of 61+12 9 km swith an estimated characteristic age of 77 kyr2 and a spin-down 2 There is a significant discrepancy between the characteristic spin-down age of PSR J2021+4026 and the estimated age of SNR G 78.2+2.1 of <10 kyr (Leahy et al. 2013). Article number, page 1 of 12Because no glitches were found in the latest 7.1 yr of timing data, this extends the time without a detected glitch for PSR B1509−58 to 28.4 yr. While the youngest pulsars (τ c < 2 kyr) tend to have smaller and fewer glitches than somewhat older pulsars (τ c ∼ 5–10 kyr), PSR B1509−58 is extreme in its lack of glitches.We present results of the timing observations of the 143 ms pulsar PSR J0538+2817 that provide a proper-motion measurement clearly showing an association of the pulsar with the supernova remnant S147. We measure a proper motion of 67 mas yr-1, implying a transverse velocity of v = 385 km s-1. We derive an age of the pulsar and S147 of only 30 ± 4 kyr, which is a factor of 20 times less than ...PSR J1446-4701 turned out to be a non-eclipser with possibly low (face-on) orbital inclination, with emission from both the pulsar and the intra-binary shock observable throughout the binary orbit. PSR J1311-3430 is a known eclipser, in which hints of spectral variability have been found, between pulsar superior and inferior conjunction phases.We report the discovery of PSR J2022+3842, a 24 ms radio and X-ray pulsar in the supernova remnant G76.9+1.0, in observations with the Chandra X-ray telescope, …We present radio observations of a region in the vicinity of the young pulsar PSR B1853+01 in the supernova remnant W44. The pulsar is located at the apex of an extended feature with cometary morphology. We argue on the basis of its morphology and its spectral index and polarization properties that this is a synchrotron nebula produced by the spin-down energy of the pulsar. The geometry and ...We present radio observations of a region in the vicinity of the young pulsar PSR B1853+01 in the supernova remnant W44. The pulsar is located at the apex of an extended feature with cometary morphology. We argue on the basis of its morphology and its spectral index and polarization properties that this is a synchrotron nebula produced …pulsar with a characteristic age of ˘18 kyr, PSR J2004+3429, and a highly eccentric, binary millisecond pulsar, PSR J1946+3417. All newly discovered pulsars are timed us-ing the 76-m Lovell radio telescope at the Jodrell Bank Observatory and the Effelsberg ... PSR J1719 1438 (Bailes et al. 2011), with its Jupiter-mass CO white dwarf companion; and most …Kyr is a Nord bandit leader who plays a small part in the quest "The Pale Lady." Kyr's Log can be found in Frostmere Crypt, where the quest takes place. He wears steel armor, an iron war axe and a hide shield. Prior to the Dragonborn's first visit to the crypt, Kyr tells the gatekeeper that no one can go through and he is not to be disturbed. He then enters the crypt with Ra'jirr. The bandits ...For the newly discovered fast energetic young pulsar, PSR J0058−7218, ... The remnant has an age of 10-30 kyr (García et al. 2012), which implies that PSR J1101−6101 is a fast-moving pulsar (Tomsick et al. 2012) with a velocity of 800-2400 km s −1, which is consistent with its weak proper-motion upper limit (Pavan et al. 2016).around PSR J1906+0746. If PSR J1906+0746 were the prod-uct of an SN explosion of massive core, then it would be most likely to produce a detectable SNR born in such a short time (˘113 kyr) and a distance from 5 kpc to 10 kpc. DNSs are not disrupted in the case of two SNs, this places strict limits on the nature of these systems' second SN ...The pulsar's spin-down rate implies a rotation-powered luminosity Edot = 1.2 x 10^{38} erg/s, a surface dipole magnetic field strength B_s = 1.0 x 10^{12} G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab, as well as the most rapidly-rotating young, radio-bright pulsar ...

ch <15 kyr) follow a log-normal distribution, indicating that only the B ch of young pulsars is close to real B fields. (ii) In the directly measured B-field range of NS-HMXBs ... PSR J1734−3333 (Espinoza et al. 2011)(or ∼0.03 in PSR B0540−69; Marshall et al. 2016) to ∼3.15 in PSR J1640 −4631 (Archibald et al. 2016; Wang et al ...

The age of PSR J1814[1744, if P > P and n \ 3, Especially noteworthy is the proximity of PSR 0 is 85 kyr. It is unlikely that any associated supernova J1814[1744 to the cluster of AXPs and SGRs at the upper remnant would still be observable, and indeed there is none right corner of Figure 3.

result in a PWN age of 5 -10 kyr. However large overestimates may occur as the pulsar characteristic age is estimated assuming that the initial spin period is negligible (i.e. for high spin-down energy loss rate of pulsar); e.g. case of PSR J1400-6326 where true age is 1-2 kyr as compared to characteristic age of 12.7 kyr. Size and efficiency ...The Association also exists to support and enhance the ability of local Board members to succeed in their business in an ethical and competent manner. Kentucky REALTORS® is located at 2708 Old Rosebud Road, Suite 200, Lexington, KY 40509, (800) 264-2185, or e-mail, [email protected]. Since its inception in 1922, Kentucky REALTORS® has ...for PSR J0058−7218 and PSR J1101−6101 covering time baselines of 8 months and 1.7 years, respec-tively. The baselines of the phase-connected timing models of PSR J0537−6910, PSR J1412+7922, and PSR J1849−0001 are extended up to three to four times those previously reported, and four new glitches of PSR J0537−6910 are presented.The pulsar's spin-down rate implies a rotation-powered luminosity E = 1.2 X 10(exp 38) erg/s, a surface dipole magnetic field strength B(sub S), = 1.0 X 10(exp 12) G, and a characteristic age of 8.9 kyr. PSR J2022+3842 is thus the second-most energetic Galactic pulsar known, after the Crab, as well as the most rapidly-rotating young, radio ...PSR J1838-0655 is a rotation-powered pulsar with spin-down luminosity Ė = 5.5 × 10 36 ergs s-1, characteristic age τ c ≡ P/2dot P = 23 kyr, and surface dipole magnetic field strength B s = 1.9 × 10 12 G. It coincides with an unresolved INTEGRAL source and the extended TeV source HESS J1837-069.For PSR J1901+0658, the Shapiro delay would be only approximately 0.1 ms for a very edge-on orbit (sin ⁡ i = 0.999 𝑖 0.999 \sin{i}=0.999 roman_sin italic_i = 0.999). Good luck is needed for measuring the Shapiro delay of this weak pulsar over the 14.5-day orbit because the current TOA uncertainties measured by FAST are in the range of 0.03 ...PSR J1907+0602 PSR J1907+0631: Source Type: UNID: R.A.: 19 08 12 (hh mm ss) Dec.: +06 21 00 (dd mm ss) Gal Long: 40.49 (deg) Gal Lat:-0.81 (deg) Distance: Flux: 1.36 (Crab Units) Energy Threshold: ... Age: approx. 10-20 kyr - PSR J1907+0602, Pulsar, Distance: 2.4 kpc, Age: 19.5 kyr, L_s: 2.8 x10e36 - PSR J1907+0631, Pulsar, Distance: 3.4 kpc, …c > 220 kyr. The latter is much longer than the SNR age, indicating that PSR J0821−4300 was born spinning near its present period. Its properties are remarkably similar to those of the two other known CCO pulsars, demonstrating the existence of a class of neutron stars born with weak magnetic fields related to a slow original spin.Summed 64-bin pulse profile for PSR B1509−58 for all 14 Cycles of RXTE data for the 2-50 keV energy range. We found no significant difference between individual pulse profiles and the average ...

3rd art expansionclima de 10 dias para madison tennesseebuc eepercent27s crossville reviewsbuy here pay here macon ga dollar500 down Kyr psr python programmieren lernen [email protected] & Mobile Support 1-888-750-4577 Domestic Sales 1-800-221-8273 International Sales 1-800-241-3139 Packages 1-800-800-9146 Representatives 1-800-323-4807 Assistance 1-404-209-8089. vectors. Our measurements show that PSR J1906+0746 is a young object with a characteristic age of 112 kyr. From the measured rate of orbital periastron advance (7.57 ± 0.03 yr−1), we infer a total system mass of 2.61 ± 0.02 M ⊙. While these parameters suggest that the PSR J1906+0746 binary system might. www ikoreantv com We report the discovery of an extended very-high-energy (VHE) gamma-ray source around the location of the middle-aged (207.8 kyr) pulsar PSR J 0622 +3749 with the Large High-Altitude Air Shower Observatory (LHAASO). The source is detected with a significance of 8.2 σ for E >25 TeV assuming a Gaussian template. The best-fit location is (right ascension, declination) =(95.47 ° ±0.11 ° ,37 ...In comparison to τ c , the 10-30 kyr age estimated for MSH 11-61A suggests that the pulsar was born in the SNR with initial period in the range 54 <= P 0 <= 60 ms. PSR J1101-6101 is the least energetic of the 15 rotation-powered pulsars detected by INTEGRAL, and has a high efficiency of hard X-ray radiation and jet power. locate arbytoby keith ~ 154 kyr) • v Ʇ,PSR ~ 400 km/s • Ė = 5.1 × 10 35 erg/s • P = 89 ms • radio + γ-ray pulsar • 370 ks ACIS-I exposure • Features: • “hollow” compact nebula (CN): jets + deformed equatorial outflow, • tail: X-ray tail dims with distance, 11 pc radio tail reaches peak brightness in the middle; CN not seen in radio fe galvaowhy is someone New Customers Can Take an Extra 30% off. There are a wide variety of options. The characteristic age of PSR J1734$-$3333 estimated from its current spin down rate implies that it is a young pulsar ($τ_c<10$ kyr). But the time derivative of its spin down rate differs markedly from that assumed for normal radio pulsars, meaning its actual age is uncertain. G354.8$-$0.8 is a supernova remnant (SNR) whose centre is located 21 arcmin away of the pulsar, and with a ...Timing observations of PSR J2021+3651 revealed that al-though it is dim, it is young and energetic (characteristic age c P=2P˙ ¼ 17 kyr and spin-down energy E˙ 4 2IP˙=P3 ¼ 3:6 ;1036 ergs s 1, assuming a moment of inertia I ¼ 1045 g cm2) and a likely counterpart to the ASCA X-ray source AX J2021.1+3651 and the EGRET -ray source GeV J2020 ...Abstract. We present the discovery and timing of the young (age ∼28.6 kyr) pulsar PSR J0837–2454. Based on its high latitude ( b = 98) and dispersion measure (DM = 143 pc cm −3 ), the pulsar appears to be at a z -height of >1 kpc above the Galactic plane, but near the edge of our Galaxy.