A new study towards PSR J1826–1334 and PSR J1826–1256 in the region of HESS J1825–137 and HESS J1826–130

Isolated neutron stars are prime targets for continuous−wave (CW) searches by ground−based gravitational−wave interferometers. Results are presented from a CW search targeting ten pulsars. The search uses a semi−coherent algorithm, which combines the maximum−likelihood F−statistic with a hidden Markov model (HMM) to efficiently detect and track quasi−monochromatic signals which wander randomly in frequency. The targets, which are associated with TeV sources detected by the High Energy Stereoscopic System (H.E.S.S.), are chosen to test for gravitational radiation from young, energetic pulsars with strong γ−ray emission, and take maximum advantage of the frequency tracking capabilities of HMM compared to other CW search algorithms. The search uses data from the second observing run of the Advanced Laser Interferometer Gravitational−Wave Observatory (aLIGO). It scans 1−Hz sub−bands around f * , 4f * /3, and 2f * , where f * denotes the star's rotation frequency, in order to accommodate a physically plausible frequency mismatch between the electromagnetic and gravitational−wave emission. The 24 sub−bands searched in this study return 5,256 candidates above the Gaussian threshold with a false alarm probability of 1% per sub−band per target. Only 12 candidates survive the three data quality vetoes which are applied to separate non−Gaussian artifacts from true astrophysical signals. CW searches using the data from subsequent observing runs will clarify the status of the remaining candidates.

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“…source. This is also consistent with TeV γ−rays originating from the inverse Compton mechanism within the PWN powered by PSR J1826−1256 [78].…”

Section: Hess J1718−385supporting

confidence: 86%

Search for continuous gravitational waves from ten H.E.S.S. sources using a hidden Markov model

et al. 2021

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“…The CMB photon field provides u CMB ∼0.26 eV cm −3 . Electron Lorentz factors of γ e ∼ 1.3 × 10 8 and γ e ∼ 3.6 × 10 7 would be required to reach the VHE γ-ray fluxes reported here for CMB and IR seed photons, respectively, in agreement with the estimates in Duvidovich et al (2019).…”

Section: Discussionsupporting

confidence: 86%

“…An estimate for the magnetic field inside the Eel Nebula of ∼20-30 µG is provided in Keogh (2010). Recently, Duvidovich et al (2019) made use of XMM-Newton observations of the region around PSR J1826-1256 and discussed such a possibility. Based on the spectral softening found along the nebula, they considered X-rays produced by electrons with energies E e 150 TeV radiating synchrotron emission in a magnetic field B > 2µG.…”

Section: Discussionmentioning

confidence: 99%

An extreme particle accelerator in the Galactic plane: HESS J1826−130

Abdalla

Adam²,

Aharonian³

et al. 2020

A&A

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The unidentified very-high-energy (VHE; E>0.1 TeV)-ray source, HESS J1826−130, was discovered with the High Energy Stereoscopic System(HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady-ray flux from HESS J1826−130, which appears extendedwith a half-width of 0.21•±0.02•stat±0.05•sys. The source spectrum is best fit with either a power-law function with a spectral indexΓ =1.78±0.10stat±0.20sysand an exponential cut-offat 15.2+5.5−3.2TeV, or a broken power-law withΓ1=1.96±0.06stat±0.20sys,Γ2=3.59±0.69stat±0.20sysfor energies below and aboveEbr=11.2±2.7 TeV, respectively. The VHE flux from HESS J1826−130 is contaminated by the extended emission ofthe bright, nearby pulsar wind nebula (PWN), HESS J1825−137, particularly at the low end of the energy spectrum. Leptonic scenarios for theorigin of HESS J1826−130 VHE emission related to PSR J1826−1256 are confronted by our spectral and morphological analysis. In a hadronicframework, taking into account the properties of dense gas regions surrounding HESS J1826−130, the source spectrum would imply an astrophysicalobject capable of accelerating the parent particle population up to200 TeV. Our results are also discussed in a multiwavelength context, accountingfor both the presence of nearby supernova remnants (SNRs), molecular clouds, and counterparts detected in radio, X-rays, and TeV energies

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“…After this paper submission, the work by Duvidovich et al (2019) was published. Authors used the same XMM-Newton data to analyse the PSR J1826−1256 and Eel emission.…”

Section: Discussionmentioning

confidence: 99%

X-ray studies of the gamma-ray pulsar J1826−1256 and its pulsar wind nebula with Chandra and XMM–Newton

Карпова

Zyuzin

Shibanov

2019

Monthly Notices of the Royal Astronomical Society

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We have analyzed archival XMM-Newton and Chandra observations of the γ-ray radioquiet pulsar J1826−1256 and its pulsar wind nebula. The pulsar spectrum can be described by a power-law model with a photon index Γ ≈ 1. We find that the nebular spectrum softens with increasing distance from the pulsar, implying synchrotron cooling. The empirical interstellar absorption-distance relation gives a distance of ≈ 3.5 kpc to J1826−1256. We also discuss the nebula geometry and association between the pulsar, the very high energy source HESS J1826−130, the supernova remnant candidate G18.45−0.42 and the open star cluster Bica 3.

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A new study towards PSR J1826–1334 and PSR J1826–1256 in the region of HESS J1825–137 and HESS J1826–130

Cited by 17 publications

References 35 publications

Search for continuous gravitational waves from ten H.E.S.S. sources using a hidden Markov model

Search for continuous gravitational waves from ten H.E.S.S. sources using a hidden Markov model

An extreme particle accelerator in the Galactic plane: HESS J1826−130

X-ray studies of the gamma-ray pulsar J1826−1256 and its pulsar wind nebula with Chandra and XMM–Newton

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