Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Kim, Seungjong; An, Hongjun

doi:10.1002/asna.202023774

Cited by 6 publications

(3 citation statements)

References 43 publications

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“…We applied our phenomenological multizone emission model (Kim & An 2020b) to the broadband SED and the measured X-ray profiles of photon index and brightness of K3. In the model, the pulsar supplies electrons and magnetic field B to the PWN.…”

Section: Multizone Pwn Emission Modelingmentioning

confidence: 99%

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

Park

Kim

Woo

et al. 2023

ApJ

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We present a detailed analysis of broadband X-ray observations of the pulsar PSR J1420−6048 and its wind nebula (PWN) in the Kookaburra region with Chandra, XMM-Newton, and NuSTAR. Using the archival XMM-Newton and new NuSTAR data, we detected 68 ms pulsations of the pulsar and characterized its X-ray pulse profile, which exhibits a sharp spike and a broad bump separated by ∼0.5 in phase. A high-resolution Chandra image revealed a complex morphology of the PWN: a torus-jet structure, a few knots around the torus, one long (∼7′) and two short tails extending in the northwest direction, and a bright diffuse emission region to the south. Spatially integrated Chandra and NuSTAR spectra of the PWN out to 2.′5 are well-described by a power-law model with a photon index Γ ≈ 2. A spatially resolved spectroscopic study, as well as NuSTAR radial profiles of the 3–7 keV and 7–20 keV brightness, showed a hint of spectral softening with increasing distance from the pulsar. A multiwavelength spectral energy distribution (SED) of the source was then obtained by supplementing our X-ray measurements with published radio, Fermi-LAT, and H.E.S.S. data. The SED and radial variations of the X-ray spectrum were fit with a leptonic multizone emission model. Our detailed study of the PWN may be suggestive of (1) particle transport dominated by advection, (2) a low magnetic-field strength (B ∼ 5 μG), and (3) electron acceleration to ∼PeV energies.

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Section: Multizone Pwn Emission Modelingmentioning

confidence: 99%

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

Park

Kim

Woo

et al. 2023

ApJ

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“…Further exploration of the spatially varying PWN emission can give insights into particle transport mechanisms within the source (e.g., Tang & Chevalier 2012;Porth et al 2016;Kim & An 2020), subsequently exploring how energetic electrons are injected into the ISM. Moreover, the spectral softening could potentially manifest as a high-energy spectral break in the spatially integrated spectrum; NuSTAR's hard X-ray data may facilitate detecting a spectral break (e.g., Nynka et al 2014;Madsen et al 2015a) or a cutoff (e.g., An 2019) at energies 10 keV.…”

Section: Introductionmentioning

confidence: 99%

X-Ray Characterization of the Pulsar PSR J1849−0001 and Its Wind Nebula G32.64+0.53 Associated with TeV Sources Detected by H.E.S.S., HAWC, Tibet ASγ, and LHAASO

Kim,

Park,

Woo

et al. 2023

ApJ

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We report on the X-ray emission properties of the pulsar PSR J1849−0001 and its wind nebula (PWN), as measured by Chandra, XMM-Newton, NICER, Swift, and NuSTAR. In the X-ray data, we detected the 38 ms pulsations of the pulsar up to ∼60 keV with high significance. Additionally, we found that the pulsar's on-pulse spectral energy distribution displays significant curvature, peaking at ≈60 keV. Comparing the phase-averaged and on-pulse spectra of the pulsar, we found that the pulsar's off-pulse emission exhibits a spectral shape that is very similar to its on-pulse emission. This characterization of the off-pulse emission enabled us to measure the >10 keV spectrum of the faint and extended PWN using NuSTAR's off-pulse data. We measured both the X-ray spectrum and the radial profiles of the PWN’s brightness and photon index, and we combined these X-ray measurements with published TeV results. We then employed a multizone emission scenario to model the broadband data. The results of the modeling suggest that the magnetic field within the PWN is relatively low (≈7 μG) and that electrons are accelerated to energies ≳400 TeV within this PWN. The electrons responsible for the TeV emission outside the X-ray PWN may propagate to ∼30 pc from the pulsar in ∼10 kyr.

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“…We describe a multizone SED model (e.g., Kim & An 2020b) that we use to infer the particle energies and the flow properties in the Rabbit PWN by simultaneously fitting the radial profiles and the broadband SED (Fig. 8).…”

Section: Multizone Emission Model For the Pwnmentioning

confidence: 99%

A broadband X-ray study of the Rabbit pulsar wind nebula powered by PSR J1418-6058

Park¹,

Kim²,

Woo³

et al. 2023

Preprint

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We report on broadband X-ray properties of the Rabbit pulsar wind nebula (PWN) associated with the pulsar PSR J1418−6058 using archival Chandra and XMM-Newton data, and a new NuSTAR observation. NuSTAR data above 10 keV allowed us to detect the 110-ms spin period of the pulsar, characterize its hard X-ray pulse profile, and resolve hard X-ray emission from the PWN after removing contamination from the pulsar and other overlapping point sources. The extended PWN was detected up to ∼20 keV and is well described by a power-law model with a photon index Γ ≈2. The PWN shape does not vary significantly with energy, and its X-ray spectrum shows no clear evidence of softening away from the pulsar. We modeled the spatial profile of X-ray spectra and broadband spectral energy distribution in the radio to TeV band to infer the physical properties of the PWN. We found that a model with low magnetic field strength (B ∼ 10 µG) and efficient diffusion (D ∼ 10 27 cm 2 s −1 ) fits the PWN data well. The extended hard X-ray and TeV emission, associated respectively with synchrotron radiation and inverse Compton scattering by relativistic electrons, suggests that particles are accelerated to very high energies ( 500 TeV), indicating that the Rabbit PWN is a Galactic PeVatron candidate.

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Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Cited by 6 publications

References 43 publications

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

X-Ray Studies of the Pulsar PSR J1420–6048 and Its TeV Pulsar Wind Nebula in the Kookaburra Region

X-Ray Characterization of the Pulsar PSR J1849−0001 and Its Wind Nebula G32.64+0.53 Associated with TeV Sources Detected by H.E.S.S., HAWC, Tibet ASγ, and LHAASO

A broadband X-ray study of the Rabbit pulsar wind nebula powered by PSR J1418-6058

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