Discovery of a radio nebula around PSR J0855−4644

Maitra, Chandreyee; Roy, Sthitadhi; Acero, Fabio; Gupta, Yashwant

doi:10.1093/mnrasl/sly038

Cited by 4 publications

(2 citation statements)

References 20 publications

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“…The PWN lies projectionally near the south-eastern rim of the SNR Vela Junior (Maitra, Acero, & Venter 2017). As seen in radio, G266.97−1.00 is a bow shock PWN (Maitra et al 2018) with a faint trailing tail. Since the faint tail has blent into the background noise, the tail might be much longer than seen.…”

Section: The Synchrotron Radiation Of the Pwnmentioning

confidence: 87%

“…The origin of jet-like features in bow shock PWNe have been detailedly studied in recent years; Olmi & Bucciantini (2019) show that the jets can be explained as the major tunnel of the escaping high energy electrons. The projective distance from the pulsar to the bow shock apex is ∼ 20 ′′ (∼ 0.3 pc) in the radio observation (Maitra et al 2018). The standoff distance, however, is smaller than the projective value by about 10%, 20%, and 50% for inclination angles 60 • , 45 • , and 20 • , respectively (Ng et al 2017), and therefore, the double torus/jet sturcture could be thought to lie within the unshocked pulsar wind 2 .…”

Section: The Synchrotron Radiation Of the Pwnmentioning

confidence: 90%

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Is PSR J0855$-$4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

Bao,

Chen,

Liu

2020

Preprint

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DAMPE observation on the cosmic ray electron spectrum hints a narrow excess at ∼ 1.4 TeV. Although the excess can be ascribed to dark matter particles, pulsars and pulsar wind nebulae are believed to be a more natural astrophysical origin: electrons injected from nearby pulsars at their early ages can form a bump-like feature in the spectrum due to radiative energy losses. In this paper, with a survey of nearby pulsars, we find 4 pulsars that may have notable contributions to ∼ 1.4 TeV cosmic ray electrons. Among them, PSR J0855−4644 has a spin down luminosity more than 50 times higher than others and presumably dominates the electron fluxes from them. X-ray observations on the inner compact part (which may represent a tunnel for the transport of electrons from the pulsar) of PWN G267.0−01.0 are then used to constrain the spectral index of high energy electrons injected by the pulsar. We show that high-energy electrons released by PSR J0855−4644 could indeed reproduce the 1.4 TeV spectral feature hinted by the DAMPE with reasonable parameters.

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Section: The Synchrotron Radiation Of the Pwnmentioning

confidence: 87%

Section: The Synchrotron Radiation Of the Pwnmentioning

confidence: 90%

Is PSR J0855$-$4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

Bao,

Chen,

Liu

2020

Preprint

View full text Add to dashboard Cite

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SRG/eROSITA and XMM-Newton observations of Vela Jr

Camilloni¹,

Becker²,

Predehl³

et al. 2023

A&A

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Context. The Vela supernova remnant (SNR) complex is a region containing at least three SNRs: Vela, Puppis A, and Vela Jr. With the launch of the spectro-imaging X-ray telescope eROSITA on board the Spectrum-Röntgen-Gamma (SRG) mission, it became possible to observe the one degree wide Vela Jr in its entirety. Although several previous pointed Chandra and XMM-Newton observations are available, it is only the second time after the ROSAT all-sky survey that the whole remnant was observed in X-rays with homogeneous sensitivity. Aims. Vela Jr is one of the few remnants emitting in the TeV band, making it an important object in shock acceleration studies. However, the age and distance determination using X-ray emission is largely hampered by the presence of the Vela SNR along the same line. With the eROSITA data set our aim is to characterize the emission of Vela Jr and distinguish it from Vela emission, and also to characterize the spectral emission of the inner remnant. Methods. We processed the eROSITA data dividing the whole remnant into seven different regions. In addition, images of the whole remnant were employed to pinpoint the position of the geometric center and constrain the proper motion of the CCO. We also employed archival XMM-Newton pointed observations of the NW rim to determine the cutoff energy of the electrons and the expansion velocity. Results. We find the magnetic field can vary between 2 µG and 16 µG in the NW rim. We also find that the remnant spectrum is uniformly featureless in most regions, except for two inner regions where an extra thermal model component improves the fit. We obtain new coordinates for the geometric remnant center, resulting in a separation of only 35.2 ± 15.8″ from the position of the CCO. As a result, we reinforce the association between the CCO and a proposed faint optical–IR counterpart.

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Is PSR J0855−4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

Bao

Chen

Liu

2020

Monthly Notices of the Royal Astronomical Society

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DAMPE observation on the cosmic ray electron spectrum hints a narrow excess at ∼1.4 TeV. Although the excess can be ascribed to dark matter particles, pulsars and pulsar wind nebulae are believed to be a more natural astrophysical origin: electrons injected from nearby pulsars at their early ages can form a bump-like feature in the spectrum due to radiative energy losses. In this paper, with a survey of nearby pulsars, we find 4 pulsars that may have notable contributions to ∼1.4 TeV cosmic ray electrons. Among them, PSR J0855−4644 has a spin down luminosity more than 50 times higher than others and presumably dominates the electron fluxes from them. X-ray observations on the inner compact part (which may represent a tunnel for the transport of electrons from the pulsar) of PWN G267.0−01.0 are then used to constrain the spectral index of high energy electrons injected by the pulsar. We show that high-energy electrons released by PSR J0855−4644 could indeed reproduce the 1.4 TeV spectral feature hinted by the DAMPE with reasonable parameters.

show abstract

Discovery of a radio nebula around PSR J0855−4644

Cited by 4 publications

References 20 publications

Is PSR J0855$-$4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

Is PSR J0855$-$4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

SRG/eROSITA and XMM-Newton observations of Vela Jr

Is PSR J0855−4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?

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