Optical Observations of PSR J2021+3651 in the Dragonfly Nebula With the GTC

Kirichenko, A.; Danilenko, A.; Shternin, P. S.; Shibanov, Yuriy; Ryspaeva, E. B.; Zyuzin, D.; Durant, Martin; Kargaltsev, Oleg; Pavlov, G. G.; Cabrera-Lavers, A.

doi:10.1088/0004-637x/802/1/17

Cited by 38 publications

(36 citation statements)

References 49 publications

(64 reference statements)

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“…A simultaneous fitting to the spectra from different observations leads to consistent results. The spectrum of the nebula was fitted with an absorbed power-law, leading to N H =(6.9±0.5) × 10 21 cm −2 , photon index Γ= 1.45±0.06, and a flux level in the 0.2-10 keV band of 7.47 +0.17 −0.18 ×10 −13 erg cm −2 s −1 , values which are consistent with previously published results (Kirichenko et al 2015;Van Etten et al 2008;Hessels et al 2004). As suggested by previous studies, the pulsar was modelled with an absorbed sum of the power-law and blackbody components.…”

Section: Psr J1747-2958: Detection Of the Pulsar In The 'Mouse' Nebulasupporting

confidence: 89%

“…We used the archival Chandra observations (obs. ID 3901, 7603, 8502) for the spectral analysis of PSR J2021+3651, adopting similar methods to those described in Kirichenko et al (2015) and Van Etten et al (2008). The pulsar spectrum was extracted from all three observations using a source region of radius 1.5 pixels (0.74 arcsec).…”

Section: Psr J1747-2958: Detection Of the Pulsar In The 'Mouse' Nebulamentioning

confidence: 99%

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Theoretically Motivated Search and Detection of Non-thermal Pulsations from PSRs J1747-2958, J2021+3651, and J1826-1256

Torres

Zelati

et al. 2018

ApJL

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Based on a theoretical selection of pulsars as candidates for detection at X-ray energies, we present an analysis of archival X-ray observations done with Chandra and XMM-Newton of PSR J1747-2958 (the pulsar in the 'Mouse' nebula), PSR J2021+3651 (the pulsar in the 'Dragonfly' nebula), and PSR J1826-1256. X-ray pulsations from PSR J1747-2958 and PSR J1826-1256 are detected for the first time, and a previously reported hint of an X-ray pulsation from PSR J2021+3651 is confirmed with a higher significance. We analyze these pulsars' spectra in regards to the theoretically predicted energy distribution, finding a remarkable agreement, and provide here a refined calculation of the model parameters taking into account the newly derived X-ray spectral data.

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Section: Psr J1747-2958: Detection Of the Pulsar In The 'Mouse' Nebulasupporting

confidence: 89%

Section: Psr J1747-2958: Detection Of the Pulsar In The 'Mouse' Nebulamentioning

confidence: 99%

Theoretically Motivated Search and Detection of Non-thermal Pulsations from PSRs J1747-2958, J2021+3651, and J1826-1256

Torres

Zelati

et al. 2018

ApJL

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“…We obtained 100000 samples which is enough compared with autocorrelation time (50-80). The procedure is similar to that utilised by Kirichenko et al (2015). Posterior median values of the spectral parameters with 90 per cent credible intervals are presented in Table 2, where the models differ only by the thermal components applied and are named according to that.…”

Section: Analysis Of the X-ray Spectramentioning

confidence: 99%

Constraining the parameters of the pulsar wind nebula DA 495 and its pulsar withChandraandXMM–Newton

Карпова

Zyuzin

Danilenko

et al. 2015

Mon. Not. R. Astron. Soc.

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We present spectral and timing analyses of the X-ray emission from the pulsar wind nebula DA 495 and its central object, J1952.2+2925, suggested to be the pulsar, using archival Chandra and XMM-Newton data. J1952.2+2925 has a pure thermal spectrum which is equally well fitted either by the blackbody model with a temperature of ≈ 215 eV and an emitting area radius of ≈ 0.6 km or by magnetized neutron star atmosphere models with temperatures of 80-90 eV. In the latter case the thermal emission can come from the entire neutron star surface which temperature is consistent with standard neutron star cooling scenarios. We place also an upper limit on the J1952.2+2925 nonthermal flux. The derived spectral parameters are generally compatible with published ones based only on the Chandra data, but they are much more accurate due to the inclusion of XMM-Newton data. No pulsations were found and we placed an upper limit for the J1952.2+2925 pulsed emission fraction of 40 per cent. Utilizing the interstellar absorption-distance relation, we estimated the distance to DA 495, which can be as large as 5 kpc if J1952.2+2925 emission is described by the atmosphere models. We compiled possible multi-wavelength spectra of the nebula including radio data; they depend on the spectral model of the central object.Comparing the results with other pulsar plus wind nebula systems we set reasonable constraints on the J1952.2+2925 spin-down luminosity and age. We suggest that the Fermi source 3FGL J1951.6+2926 is the likely γ-ray counterpart of J1952.2+2925.

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“…Fermi-LAT (Abdo et al 2009) detected emissions from PSR J2021+3651 and gave an upper limit on the extended GeV γ-ray emissions around it, consistent with the hard spectrum of VER J2019+368 in the TeV band. Although the distance to the pulsar is inferred from the radio data to be ≥10 kpc (Roberts et al 2002), this conclusion remains controversial (e.g., Van Etten et al 2008) and does not coincide with a detailed study of the distance by Kirichenko et al (2015).…”

Section: Introductionmentioning

confidence: 99%

X-Ray Studies of the Extended TeV Gamma-Ray Source VER J2019+368

Mizuno

Tanaka

Takahashi

et al. 2017

ApJ

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This article reports the results of X-ray studies of the extended TeV γ-ray source VER J2019+368. Suzaku observations conducted to examine properties of the X-ray pulsar wind nebula (PWN) around PSR J2021+3651 revealed that the western region of the X-ray PWN has a source extent of 15 ′ × 10 ′ with the major axis oriented to that of the TeV emission. The PWN-west spectrum was closely fitted by a power-law for absorption at N (H) = (8.2 +1.3 −1.1 ) × 10 21 cm −2 and a photon index of Γ = 2.05 ± 0.12, with no obvious change in the index within the X-ray PWN. The measured X-ray absorption indicates that the distance to the source is much less than 10 kpc inferred by radio data. Aside from the PWN, no extended emission was observed around PSR J2021+3651 even by Suzaku. Archival data from the XMM-Newton were also analyzed to complement the Suzaku observations, indicating that the eastern region of the X-ray PWN has a similar spectrum (N (H) = (7.5 ± 0.9)× 10 21 cm −2 and Γ = 2.03 ± 0.10) and source extent up to at least 12 ′ along the major axis. The lack of significant change in the photon index and the source extent in X-ray are used to constrain the advection velocity or the diffusion coefficient for accelerated X-ray-producing electrons. A mean magnetic field of ∼3 µG is required to account for the measured X-ray spectrum and reported TeV γ-ray spectrum. A model calculation of synchrotron radiation and inverse Compton scattering was able to explain ∼80% of the reported TeV flux, indicating that the X-ray PWN is a major contributor of VER J2019+368.

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Optical Observations of PSR J2021+3651 in the Dragonfly Nebula With the GTC

Cited by 38 publications

References 49 publications

Theoretically Motivated Search and Detection of Non-thermal Pulsations from PSRs J1747-2958, J2021+3651, and J1826-1256

Theoretically Motivated Search and Detection of Non-thermal Pulsations from PSRs J1747-2958, J2021+3651, and J1826-1256

Constraining the parameters of the pulsar wind nebula DA 495 and its pulsar withChandraandXMM–Newton

X-Ray Studies of the Extended TeV Gamma-Ray Source VER J2019+368

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