The Distance to the Crab Nebula and NP 0532

Trimble, Virginia

doi:10.1086/129507

Cited by 98 publications

(60 citation statements)

References 11 publications

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“…Thus, we assign the error of 10 days in the recorded dates. The estimated observed magnitudes are corrected to the absolute ones with the distance of 2 kpc (Trimble 1973;Davidson & Fesen 1985) and the extinction of A V = 1.6 mag (Miller 1973). Our LC models show that the explosion of an ecSN within super-AGB wind can explain the major characteristics of The star was recorded to appear in late May in 1054 in Japanese literature (Meigetsuki), but it is likely that there is an error in the recorded month.…”

Section: Sn 1054 (Crab Nebula)mentioning

confidence: 83%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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The most massive stars on the asymptotic giant branch (AGB), or the so-called super-AGB stars, are thought to produce supernovae triggered by electron captures in their degenerate O+Ne+Mg cores. Super-AGB stars are expected to have slow winds with high mass-loss rates, so their circumstellar density is high. The explosions of super-AGB stars are therefore presumed to occur in this dense circumstellar environment. We provide the first synthetic light curves for such events by exploding realistic electron-capture supernova progenitors within their super-AGB winds. We find that the early light curve -that is, before the recombination wave reaches the bottom of the hydrogen-rich envelope of supernova ejecta (the plateau phase) -is not affected by the dense wind. However, after the luminosity drop following the plateau phase, the luminosity remains much higher when the super-AGB wind is taken into account. We compare our results to the historical light curve of SN 1054, the progenitor of the Crab Nebula, and show that the explosion of an electron-capture supernova within an ordinary super-AGB wind can explain the observed light curve features. We conclude that SN 1054 could have been a Type IIn supernova without any extra extreme mass loss, which was previously suggested to be necessary to account for its early high luminosity. We also show that our light curves match Type IIn supernovae with an early plateau phase or the so-called Type IIn-P supernovae, and suggest that they are electron-capture supernovae within super-AGB winds. Although some electron-capture supernovae can be bright in the optical spectral range due to the large progenitor radius, their X-ray luminosity from the interaction does not necessarily get as bright as other Type IIn supernovae whose optical luminosities are also powered by the interaction. Thus, we suggest that optically bright X-ray-faint Type IIn supernovae can emerge from electron-capture supernovae. Optically faint Type IIn supernovae, such as SN 2008S, can also originate from electron-capture supernovae if their hydrogen-rich envelope masses are small. We argue that some of them can be observed as Type IIn-b supernovae due to the small hydrogen-rich envelope mass.

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Section: Sn 1054 (Crab Nebula)mentioning

confidence: 83%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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“…It shows a rotation period of T 33.7 » ms, slowly increasing by T 4.2 10 13 =´-. Its distance is still rather poorly determined (Trimble 1973) and generally stated as 2.0±0.5kpc (Kaplan et al 2008). The Crab Pulsar phaseogram (defined as flux-or simply count rate-as a function of the pulsar phase f) shows increased emission in two phase ranges: the main pulse P1, which has been used to define the zero phase value, and the inter-pulse P2 at 0.4 f » .…”

Section: The Data Setmentioning

confidence: 99%

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

Ahnen¹,

Ansoldi²,

Antonelli³

et al. 2017

ApJS

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Spontaneous breaking of Lorentz symmetry at energies on the order of the Planck energy or lower is predicted by many quantum gravity theories, implying non-trivial dispersion relations for the photon in vacuum. Consequently, gamma-rays of different energies, emitted simultaneously from astrophysical sources, could accumulate measurable differences in their time of flight until they reach the Earth. Such tests have been carried out in the past using fast variations of gamma-ray flux from pulsars, and more recently from active galactic nuclei and gamma-ray bursts. We present new constraints studying the gamma-ray emission of the galactic Crab Pulsar, recently observed up to TeV energies by the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) collaboration. A profile likelihood analysis of pulsar events reconstructed for energies above 400GeV finds no significant variation in arrival time as their energy increases.Ninety-five percent CL limits are obtained on the ) for a quadratic scenario, for the subluminal and the superluminal cases, respectively. A substantial part of this study is dedicated to calibration of the test statistic, with respect to bias and coverage properties. Moreover, the limits take into account systematic uncertainties, which are found to worsen the statistical limits by about 36%-42%. Our constraints would have been much more stringent if the intrinsic pulse shape of the pulsar between 200GeV and 400GeV was understood in sufficient detail and allowed inclusion of events well below 400GeV.

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“…As a very bright object located at a distance of 2 kpc (Trimble 1973), it is an advantageous target to investigate physical processes in PWNe as well as in supernova remnants (SNRs). Thousands of articles have been published reporting multiwavelength observations and theoretical models describing and interpreting the Crab Nebula.…”

Section: Introductionmentioning

confidence: 99%

Morphological Properties of the Crab Nebula: A Detailed Multiwavelength Study Based on New VLA, HST, Chandra, and XMM-Newton Images

Dubner

Castelletti

Kargaltsev

et al. 2017

ApJ

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We present a detailed analysis of the morphological properties of the Crab Nebula across the electromagnetic spectrum based on new and previous high-quality data from radio to X-rays. In the radio range we obtained an image of the entire nebula at 3 GHz with subarcsecond angular resolution using the VLA (NRAO) and an image at 100 GHz of the central region using the ALMA array.Simultaneously with the VLA observations we performed HST WFPC3 near infrared (λ ∼ 1.5µm) and Chandra X-ray (0.5-8 keV band) observations of the central region of the nebula. In addition we produced a new UV image of the Crab nebula at 291 nm by co-adding 75 individual exposures of the Optical-UV Monitor on board XMM-Newton. The high-angular resolution and high-dynamic range radio image at 3 GHz allowed us to improve the detection and characterization of peculiar morphological features including arches with foot brightening and intercrossed loop-like structures, likely originating in plasma confined to magnetic field lines. Based on the new radio image, we carried out a detailed multiwavelength correlation. In the central area, the comparison of the almost simultaneous images confirms that the wisps in the three spectral ranges do not generally coincide in location, the radio emission being the most discordant, which is suggestive of the existence of two different synchrotron components. The X-ray pulsar jet does not have a radio counterpart. Instead, another jet-like feature is seen in radio, though with different curvature and starting point.

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The Distance to the Crab Nebula and NP 0532

Cited by 98 publications

References 11 publications

Electron-capture supernovae exploding within their progenitor wind

Electron-capture supernovae exploding within their progenitor wind

Constraining Lorentz Invariance Violation Using the Crab Pulsar Emission Observed up to TeV Energies by MAGIC

Morphological Properties of the Crab Nebula: A Detailed Multiwavelength Study Based on New VLA, HST, Chandra, and XMM-Newton Images

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