Discovery of X‐Ray Pulsations from the Compact Central Source in the Supernova Remnant 3C 58

Murray, Stephen S.; Slane, Patrick; Seward, F. D.; Ransom, S. M.; Gaensler, B. M.

doi:10.1086/338766

Cited by 115 publications

(121 citation statements)

References 13 publications

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“…Due to its similarities with the Crab Nebula, 3C58 was identified as a PWN twenty years before its pulsar was found, PSR J0205+6449, which initially was discovered by X-rays (Murray et al 2002) and only afterward detected at radio frequencies (820 and 1375 MHz; Camilo et al 2002). 3C58 was discovered by the Einstein Observatory and initially associated with the remnant of the supernova SN 1181 recorded in a.d. 1181 (Becker et al 1982), thus implying an age of 820 yr.…”

Section: Psr J0205+6449 and The Pwn 3c58mentioning

confidence: 99%

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

Anderhub¹,

Antonelli²,

Antoranz³

et al. 2010

ApJ

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The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other groundbased instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions.

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Section: Psr J0205+6449 and The Pwn 3c58mentioning

confidence: 99%

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

Anderhub¹,

Antonelli²,

Antoranz³

et al. 2010

ApJ

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“…The pulsars provide the magnetic field and relativistic particles that generate the observed center-filled synchrotron radiation fields. While a faint central X-ray point source in 3C 58 had long been suspected to be a neutron star (Becker et al 1982;Helfand et al 1995), it was only recently identified as a pulsar, first through X-rays (P ¼ 65:7 ms, PSR J0205+6449; Murray et al 2002) and then quickly confirmed in the radio (Camilo et al 2002;Malofeev et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)

Fesen

Rudie

Hurford

et al. 2008

ASTROPHYS J SUPPL S

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We present a comprehensive imaging and spectroscopic survey of optical emission knots associated with the young Galactic supernova remnant 3C 58. H images show hundreds of clumpy filaments and knots arranged in a complex structure covering a nearly circular area roughly 400 00 in diameter. A quite different emission structure is seen in [O iii], where the brightest features are less clumpy and largely confined to the remnant's northwest quadrant. Measured radial velocities of over 450 knots reveal two distinct kinematic populations; one with average and peak expansion velocities of 770 and 1100 km s À1 , respectively, forming a thick shell, and the other showing jvj 250 km s À1 . High-velocity knots (jvj ! 500 km s À1 ) exhibit a strong bipolar expansion pattern with redshifted and blueshifted knots located in northeastern and southwestern regions, respectively. These knots also show strong [N ii]/H line emission ratios, suggesting enhanced N/H. In contrast, the slower expanding knot population shows much lower [N ii]/H line ratios and likely represents circumstellar mass loss material from the 3C 58 progenitor. Proper-motion estimates using images spanning a 28 yr time interval suggest positional shifts of between 0.5 00 and 2.0 00 , implying proper motions of 0.02 00 Y0.07 00 yr À1 . These values agree with previous estimates but are much less than the %0.2 00 yr À1 expected if 3C 58 were associated with historic guest star of 1181 CE. Subject headingg s: ISM: individual (3C 58) -ISM: kinematics and dynamics -supernova remnants

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“…It is centered on PSR J0205+6449, a pulsar discovered in 2002 with the Chandra X-ray observatory [2]. It is widely assumed that 3C 58 is located at a distance of 3.2 kpc [3], but recent H I measurements suggest a distance of 2 kpc [4].…”

Section: General Descriptionmentioning

confidence: 99%

Discovery of TeV gamma-ray emission from the pulsar wind nebula 3C 58 by MAGIC

Canales¹,

Barrio

González

et al. 2016

EPJ Web of Conferences

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Abstract. The pulsar wind nebula (PWN) 3C 58 is one of the historical very-high-energy (VHE; E>100 GeV) gamma-ray source candidates. It has been compared to the Crab Nebula due to their morphological similarities. This object was detected by Fermi-LAT with a spectrum extending beyond 100 GeV. We analyzed 81 hours of 3C 58 data taken with the MAGIC telescopes and we detected VHE gamma-ray emission for the first time at TeV energies with a significance of 5.7 sigma and an integral flux of 0.65% C.U. above 1 TeV. According to our results 3C 58 is the least luminous PWN ever detected at VHE and the one with the lowest flux at VHE to date. We compare our results with the expectations of time-dependent models in which electrons up-scatter photon fields. The best representation favors a distance to the PWN of 2 kpc and Far Infrared (FIR) comparable to CMB photon fields. Hadronic contribution from the hosting supernova remnant (SNR) requires unrealistic energy budget given the density of the medium, disfavoring cosmic ray acceleration in the SNR as origin of the VHE gammaray emission.

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Discovery of X‐Ray Pulsations from the Compact Central Source in the Supernova Remnant 3C 58

Cited by 115 publications

References 13 publications

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

Search for Very High Energy Gamma-Ray Emission From Pulsar-Pulsar Wind Nebula Systems With the Magic Telescope

Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)

Discovery of TeV gamma-ray emission from the pulsar wind nebula 3C 58 by MAGIC

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