Nonstationary radio luminosity of the remnant of Supernova 1181 (3C 58)

Иванов, В. П.; Rakhimov, I. A.; Smolentsev, Sergey; Stankevich, K. S.; Finkelstein, A. M.

doi:10.1134/1.1695084

Cited by 5 publications

(4 citation statements)

References 15 publications

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“…Radio observations of 3C58 suggested a flux evolution. Ivanov et al (2004) found non-stationary variations of the flux densities at 1.5 − 8.5 GHz. Although they found a frequency independent increase of the radio flux ∼ 0.3%yr −1 during the period 1965 − 1986, they also found a frequency dependent variation during the period 1966 − 2003, where both increase and decrease of fluxes are found ranging from -0.3 to 0.5 %yr −1 .…”

Section: Discussionmentioning

confidence: 90%

Properties of young pulsar wind nebulae: TeV detectability and pulsar properties

Tanaka

Takahara

2013

Monthly Notices of the Royal Astronomical Society

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Among dozens young pulsar wind nebulae, some have been detected in TeV γ-rays (TeV PWNe), while others have not (non-TeV PWNe). The TeV emission detectability is not correlated either with the spin-down power or with the characteristic age of their central pulsars, and it is an open problem what determines the detectability. To study this problem, we investigate spectral evolution of five young non-TeV PWNe, 3C58, G310.6-1.6, G292.0+1.8, G11.2-0.3 and SNR B0540-69.3. We use a spectral evolution model which has been developed to be applied to young TeV PWNe in our previous works. TeV γ-ray flux upper limits of non-TeV PWNe give upper or lower limits on parameters, such as the age of the PWN and the fraction of the spin-down power going to the magnetic energy injection (the fraction parameter). Combined with other independent observational and theoretical studies, we can guess a plausible value of the parameters for each object. For 3C58, we prefer the parameters with an age of 2.5 kyr old and the fraction parameter of 3.0 × 10 −3 , although the spectral modeling alone does not rule out a shorter age and a higher fraction parameter. The fraction parameter of 3.0 × 10 −3 is also consistent for other non-TeV PWNe and then the value is regarded as common to young PWNe including TeV PWNe. Moreover, we find that the intrinsic properties of the central pulsars are similar, 10 48−50 erg for the initial rotational energy and 10 42−44 erg for the magnetic energy (2 × 10 12 − 3 × 10 13 G for the dipole magnetic field strength at their surfaces). The TeV detectability is correlated with the total injected energy and the energy density of the interstellar radiation field around PWNe. Except for G292.0+1.8, a broken power-law injection of the particles well reproduces the broadband emission from non-TeV PWNe.

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Section: Discussionmentioning

confidence: 90%

Properties of young pulsar wind nebulae: TeV detectability and pulsar properties

Tanaka

Takahara

2013

Monthly Notices of the Royal Astronomical Society

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“…But the two objects differ significantly both in luminosity and in size. The radio nebula of 3C 58, although ∼ 2 times larger, is less luminous than the Crab by an order of magnitude (Ivanov et al 2004), while its X-ray luminosity is ∼ 2000 times smaller (Torii et al 2000). These disparities could be explained by a different age.…”

Section: Introductionmentioning

confidence: 92%

DISCOVERY OF PULSATIONS FROM THE PULSAR J0205+6449 IN SNR 3C 58 WITH THE FERMI GAMMA-RAY SPACE TELESCOPE

Abdo¹,

Ackermann²,

Ajello³

et al. 2009

ApJ

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We report the discovery of γ -ray pulsations ( 0.1 GeV) from the young radio and X-ray pulsar PSR J0205 + 6449 located in the Galactic supernova remnant 3C 58. Data in the γ -ray band were acquired by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope (formerly GLAST), while the radio rotational ephemeris used to fold γ -rays was obtained using both the Green Bank Telescope and the Lovell telescope at Jodrell Bank. The light curve consists of two peaks separated by 0.49 ± 0.01 ± 0.01 cycles which are aligned with the X-ray peaks. The first γ -ray peak trails the radio pulse by 0.08 ± 0.01 ± 0.01, while its amplitude decreases with increasing energy as for the other γ -ray pulsars. Spectral analysis of the pulsed γ -ray emission suggests a simple power law of index −2.1 ± 0.1 ± 0.2 with an exponential cutoff at 3.0 +1.1 −0.7 ± 0.4 GeV. The first uncertainty is statistical and the second is systematic. The integral γ -ray photon flux above 0.1 GeV is (13.7 ± 1.4 ± 3.0) × 10 −8 cm −2 s −1 , which implies for a distance of 3.2 kpc and assuming a broad fan-like beam a luminosity of 8.3 × 10 34 erg s −1 and an efficiency η of 0.3%. Finally, we report a 95% upper limit on the flux of 1.7 × 10 −8 cm −2 s −1 for off-pulse emission from the object.

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“…Total exposure times were typically 3000 s. The 1996 2.4 m telescope images were taken through the H and off-band (k c ¼ 6450 8) filters and consisted of two 800 s exposures in each filter for the four image regions. Wilson & Weiler 1976;(8) Reynolds & Aller 1988;(9) Davidson & Fesen 1985;(10) Green & Gull 1982;(11) Roberts et al 1993;(12) Clark et al 1983;(13) Fesen & Ketelsen 1985;(14) Lawrence et al 1995;(15) Fesen et al 1988;(16) this paper; (17) Green 1986;(18) Green 2004;(19) Green 1994;(20) Ivanov et al 2004;(21) Toor & Seward 1974;(22) Torii et al 2000;(23) Wu 1981;(24) Blair et al 1992;(25) Sollerman et al 2000;(26) Fesen et al 1988. A set of H filter images ( FWHM ¼ 90 8) were also taken on 2005 October 6 with the MDM 2.4 m telescope in order to measure proper motions of the remnant's emission features. A 2048 ; 2048 Tektronix CCD detector was used with 0.275 00 pixels and an effective 7:5 0 ; 7:5 0 field of view.…”

Section: Imagingmentioning

confidence: 97%

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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Nonstationary radio luminosity of the remnant of Supernova 1181 (3C 58)

Cited by 5 publications

References 15 publications

Properties of young pulsar wind nebulae: TeV detectability and pulsar properties

Properties of young pulsar wind nebulae: TeV detectability and pulsar properties

DISCOVERY OF PULSATIONS FROM THE PULSAR J0205+6449 IN SNR 3C 58 WITH THE FERMI GAMMA-RAY SPACE TELESCOPE

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

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