THE RADIO-2 mm SPECTRAL INDEX OF THE CRAB NEBULA MEASURED WITH GISMO

Arendt, Richard G.; George, Jithin V.; Staguhn, Johannes; Benford, Dominic J.; Devlin, Mark J.; Dicker, Simon; Fixsen, D. J.; Irwin, K. D.; Jhabvala, Christine A.; Korngut, Phillip; Kovács, A.; Maher, Stephen F.; Mason, B. S.; Miller, Timothy M.; Moseley, S. H.; Vilanova, Santiago; Sievers, A.; Sievers, Jonathan; Sharp, Elmer H.; Wollack, Edward J.

doi:10.1088/0004-637x/734/1/54

Cited by 15 publications

(27 citation statements)

References 42 publications

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“…4 We indicate in the plot the SNR (870 yr, Bietenholz & Bartel 2008) and spindown (4800 yr, Camilo et al 2006) ages for this PWN. 5 A mid-IR bump over the power-law fit in the Crab spectrum in the mid-IR at ∼50 μm is due to thermal emission from the warm dust generated by the SN (Temim et al 2006;Arendt et al 2011;Temim et al 2012). 6 The optical-IR part of the 3C 58 torus spectrum is confirmed by near-UV and near-IR observations (Zyuzin et al, in prep.).…”

Section: Multiwavelength Spectrum Of the Torus-like Pwnmentioning

confidence: 88%

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The PSR J1124-5916 wind nebula in the near-infrared

Zharikov

Zyuzin²,

Shibanov

et al. 2013

A&A

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Context. The young radio pulsar J1124-5916 is associated with the Cas A like supernova remnant G292.0+1.8. It powers a compact torus-like pulsar wind nebula with a jet first detected in X-rays and then identified in the optical and mid-infrared. Aims. We carried out deep near-infrared observations of the pulsar field to identify the pulsar and its nebula in this range. Methods. The direct-imaging mode of the NACO adaptive optics instrument at the ESO VLT in the H and K s bands was used.Results. We detected a faint, H = 21.30(10) and K s = 20.45(10), extended elliptical object in both bands, whose center position is consistent with the X-ray position of the pulsar. The morphology of the object and the orientation of its major axis agree well with those observed for the pulsar torus-like nebula in the mid-infrared, optical, and X-rays. This suggests that it is the near-infrared counterpart of the nebula. The measured fluxes compiled with the data in other ranges show a complicated unabsorbed power-law spectrum of the torus-like nebula with several steep breaks between the near-infrared and mid-infrared, the optical and X-rays, and possibly in the mid-infrared. This implies a multiple relativistic particle population responsible for the synchrotron emission of the nebula in different spectral ranges. We have not resolved the pulsar counterpart from its nebula and place only upper limits on its brightness, H ≥ 23.9 and K s ≥ 22.7. Based on that, its contribution to the total near-infrared flux of the pulsar+nebula system is ≤10%, which is comparable with the expected contribution in the optical.

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Section: Multiwavelength Spectrum Of the Torus-like Pwnmentioning

confidence: 88%

“…This cannot be excluded even for the Crab, where, in addition to the significant X-ray-optical slope change, some small breaks may exist between the optical and near-IR and/or between the near-IR and mid-IR (Arendt et al 2011). In Fig.…”

Section: Multiwavelength Spectrum Of the Torus-like Pwnmentioning

confidence: 99%

The PSR J1124-5916 wind nebula in the near-infrared

Zharikov

Zyuzin²,

Shibanov

et al. 2013

A&A

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“…One way to estimate B is based on the synchrotron break frequency in the integrated spectrum (Equation (7)). However, the break is not a sharp feature and it is difficult to locate the synchrotron break frequency of the Crab and 3C 58 based on current observational data (Slane et al 2008;Arendt et al 2011). Another way is to model the high-energy inverse Compton emission.…”

Section: Pure Diffusion Modelmentioning

confidence: 99%

Particle Transport in Young Pulsar Wind Nebulae

Tang

Chevalier

2012

ApJ

103

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The model for pulsar wind nebulae (PWNe) as a result of the magnetohydrodynamic (MHD) downstream flow from a shocked, relativistic pulsar wind has been successful in reproducing many features of the nebulae observed close to central pulsars. However, observations of well-studied young nebulae like the Crab Nebula, 3C 58, and G21.5-0.9 do not show the toroidal magnetic field on a larger scale that might be expected in the MHD flow model; in addition, the radial variation of spectral index due to synchrotron losses is smoother than expected in the MHD flow model. We find that pure diffusion models can reproduce the basic data on nebular size and spectral index variation for the Crab, 3C 58, and G21.5-0.9. Most of our models use an energy-independent diffusion coefficient; power-law variations of the coefficient with energy are degenerate with variation in the input particle energy distribution index in the steady state, transmitting boundary case. Energy-dependent diffusion is a possible reason for the smaller diffusion coefficient inferred for the Crab. Monte Carlo simulations of the particle transport allowing for advection and diffusion of particles suggest that diffusion dominates over much of the total nebular volume of the Crab. Advection dominates close to the pulsar and is likely to play a role in the X-ray half-light radius. The source of diffusion and mixing of particles is uncertain, but may be related to the Rayleigh-Taylor instability at the outer boundary of a young PWN or to instabilities in the toroidal magnetic field structure.

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“…In the millimetre wavelength range, we used the Goddard-IRAM Superconducting 2 Millimeter Observer (GISMO, Staguhn et al 2006) 2 mm data observed on the IRAM 30 m telescope, and Multiplexed Squid TES Array at Ninety GHz (MUSTANG, Dicker et al 2008) 3.3 mm observations obtained with the Green Bank Telescope (GBT). The data sets, observational details and data reduction strategy have been presented in detail in Arendt et al (2011). At 2 mm, Arendt et al (2011) reported a total integrated flux density of 244±24 Jy.…”

Section: Millimetre and Radio Observationsmentioning

confidence: 99%

“…The data sets, observational details and data reduction strategy have been presented in detail in Arendt et al (2011). At 2 mm, Arendt et al (2011) reported a total integrated flux density of 244±24 Jy. The total flux density at 3.3 mm was less well constrained due to the small field of view (FOV=40 × 40 ) and the loss of large scale emission.…”

Section: Millimetre and Radio Observationsmentioning

confidence: 99%

The dust content of the Crab Nebula

Looze

Barlow

Bandiera

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have modelled the near-infrared to radio images of the Crab Nebula with a Bayesian SED model to simultaneously fit its synchrotron, interstellar and supernova dust emission. We infer an interstellar dust extinction map with an average A V = 1.08 ± 0.38 mag, consistent with a small contribution ( 22%) to the Crab's overall infrared emission. The Crab's supernova dust mass is estimated to be between 0.032 and 0.049 M (for amorphous carbon grains) with an average dust temperature T dust =41±3 K, corresponding to a dust condensation efficiency of 8-12%. This revised dust mass is up to an order of magnitude lower than some previous estimates, which can be attributed to our different interstellar dust corrections, lower SPIRE flux densities, and higher dust temperatures than were used in previous studies. The dust within the Crab is predominantly found in dense filaments south of the pulsar, with an average V band dust extinction of A V = 0.20 − 0.39 mag, consistent with recent optical dust extinction studies. The modelled synchrotron power-law spectrum is consistent with a radio spectral index α radio =0.297±0.009 and an infrared spectral index α IR =0.429±0.021. We have identified a millimetre excess emission in the Crab's central regions, and argue that it most likely results from two distinct populations of synchrotron emitting particles. We conclude that the Crab's efficient dust condensation (8-12%) provides further evidence for a scenario where supernovae can provide substantial contributions to the interstellar dust budgets in galaxies.

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THE RADIO-2 mm SPECTRAL INDEX OF THE CRAB NEBULA MEASURED WITH GISMO

Cited by 15 publications

References 42 publications

The PSR J1124-5916 wind nebula in the near-infrared

The PSR J1124-5916 wind nebula in the near-infrared

Particle Transport in Young Pulsar Wind Nebulae

The dust content of the Crab Nebula

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