<i>Chandra</i>X‐Ray Imaging Spectroscopy of the Young Supernova Remnant Kesteven 75

Helfand, D. J.; Collins, Benjamin F.; Gotthelf, E. V.

doi:10.1086/344725

Cited by 84 publications

(144 citation statements)

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“…Total and pulsed (unabsorbed) high-energy spectrum (∼1-300 keV) of Kes75/PSR J1846−0258 from pre-outburst RXTE PCA and HEXTE (both pulsed) and INTEGRAL IBIS ISGRI (pulsed and total) observations in an E 2 F representation. The spectral coverage is extended towards 1 keV using the Chandra spectral-fit results (1-7 keV; unabsorbed) obtained by Helfand et al (2003) for the total emission spectrum of the pulsar and the PWN. Note that both the PWN contribution and DC emission from PSR J1846−0258 drop to undetectable levels at energies near 150 keV: the total emission is consistent with being 100% pulsed above ∼150 keV.…”

Section: Analysis Methodsmentioning

confidence: 99%

“…We barycentered the PCA event arrival times using the Chandra X-ray observatory (CXO) sub-arcsecond position of PSR J1846−0258, (α, δ) = (18 h 46 m 24. s 94, −02 • 58 30 . 1) for epoch J2000 (Helfand et al 2003), which corresponds to (l, b) = (29.712015, −0.240245) in Galactic coordinates. In each of these sub-observations a coherent pulsed signal at a rate of ∼3.0827 Hz (see also Gotthelf et al 2000) could be detected in the barycentered time series.…”

Section: Timing Solutions: Ephemeridesmentioning

confidence: 99%

“…The individual PCA, HEXTE and ISGRI spectra are mutually consistent in overlapping energy bands. 3 An absorbing hydrogen column of N H = 3.96 × 10 22 cm −2 has been assumed for the PCA spectral analysis (see Helfand et al 2003) and in all PCA spectra shown in this paper the interstellar absorption has been modeled out.…”

Section: Pulsed Pre-outburst 3-300 Kev Spectrummentioning

confidence: 99%

“…6 the spectral model fits obtained from Chandra data in the soft X-ray band (1-7 keV) by Helfand et al (2003) (see for recent analyses Ng et al 2008) for the total emission from PSR J1846−0258 (Γ = 1.39 ± 0.04; pulsed plus unpulsed/DC; solid orange line) and the PWN (Γ = 1.92 ± 0.04; dashed orange line), separately. We also show the sum of these two models as a dotted orange line representing the total emission from PSR J1846−0258/PWN in the 1-7 keV band, to be compared with the total emission as measured by ISGRI above 20 keV.…”

Section: Pulsed Fractionsmentioning

confidence: 99%

“…We also show the sum of these two models as a dotted orange line representing the total emission from PSR J1846−0258/PWN in the 1-7 keV band, to be compared with the total emission as measured by ISGRI above 20 keV. Dividing the pulsed emission estimated in the 0.5-10 keV band through extrapolation to lower energies of the ∼3-300 keV pulsed spectrum, (2.98±0.03)×10 −12 erg/cm 2 s, by the total point-source emission 9.50×10 −12 erg/cm 2 s (Helfand et al 2003) from PSR J1846−0258 in the Chandra 0.5-10 keV band we obtained an average pulsed fraction of 31%. Therefore, comparing this value with the lower-limit of 44% derived for the 20-100 keV band, the pulsed fraction is steadily growing with energy to become within the large errors consistent with ∼100% near 150 keV.…”

Section: Pulsed Fractionsmentioning

confidence: 99%

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High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

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Aims. PSR J1846−0258 is a young rotation-powered pulsar with one of the highest surface magnetic field strengths, located in the centre of SN-remnant Kes-75. In June 2006 a magnetar-like outburst took place. Using multi-year RXTE and INTEGRAL observations covering the epoch of the outburst, we aim to study the temporal and spectral characteristics of PSR J1846−0258 over a broad ∼3-300 keV energy range to derive constraints on theoretical scenarios aiming to explain this schizophrenic behaviour. Methods. We explored all publically available RXTE observations of PSR J1846−0258 to generate accurate ephemerides over the period January 30, 2000-November 7, 2007. Phase-folding procedures yielded pulse profiles for RXTE PCA (∼3-30 keV), RXTE HEXTE (∼15-250 keV) and INTEGRAL ISGRI (∼20-300 keV). The pulsed spectrum over the full ∼3-300 keV energy range was derived, as well as the total spectrum (including the pulsar wind nebula) over the 20-300 keV band with the ISGRI. The timing, spatial, and spectral analyses were applied for epochs before, during, and after the magnetar-like outburst to study the evolution of the high-energy characteristics. Results. ISGRI detected PSR J1846−0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20-300 keV energy range with photon index Γ = 1.80 ± 0.06 and energy flux (20-300 keV) of (6.62 ± 0.35) × 10 −11 erg/cm 2 s. More than 90 days after the onset of the outburst, still during the decay phase, the same spectral shape was measured (Γ = 1.75 +0.27 −0.31 ) with an indication for a 52% (2.3σ) enhanced total emission, while one year after the outburst the hard X-ray non-thermal emission of PSR J1846−0258/Kes-75 was found to be back to its pre-outburst values. PCA monitoring of PSR J1846−0258 before the outburst yielded phase-coherent ephemerides confirming the earlier derived breaking index of the spindown. During the outburst, incoherent solutions have been derived. We show that the radiative outburst was triggered by a major spin-up glitch near MJD 53 883 ± 3 with a glitch size Δν/ν in the range (2.0−4.4) × 10 −6 . Using all pre-outburst observations of ISGRI and HEXTE for the first time pulse profiles have been obtained up to 150 keV with a broad single asymmetric pulse. The pulse shape did not vary with energy over the 2.9-150 keV energy range, nor did it change during the magnetar-like outburst. The time-averaged pre-outburst ∼3-300 keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Γ = 1.20 ± 0.01. A fit with a curved power-law model gives an improved fit. Around 150 keV the pulsed fraction approaches 100%. For the first 32 days of the magnetarlike outburst, the 3-30 keV pulsed spectrum can be represented with two power laws, a soft component with index Γ s = 2.96 ± 0.06 and a hard component with the pre-outburst value Γ h ∼ 1.2. Above ∼9 keV, all spectra during outburst are consistent with the latter single power-law shape with index ∼1.2. The 2-10 keV flux increased by a factor ∼5 and the 10...

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Section: Analysis Methodsmentioning

confidence: 99%

Section: Timing Solutions: Ephemeridesmentioning

confidence: 99%

Section: Pulsed Pre-outburst 3-300 Kev Spectrummentioning

confidence: 99%

Section: Pulsed Fractionsmentioning

confidence: 99%

Section: Pulsed Fractionsmentioning

confidence: 99%

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High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

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The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75

2014

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By studying composite supernova remnants (SNRs), remnants which contain a pulsar wind nebula (PWN), it is possible to estimate physical properties of the progenitor explosion, central neutron star, and its pulsar wind that are difficult to measure directly. This is best done by fitting the dynamical and broadband spectral properties of a PWN with an evolutionary model for a PWN inside an SNR. We apply such a model to the composite SNR Kes 75, whose associated pulsar PSR J1846-0258 is thought to have an extremely strong surface magnetic field. If ∼ 3 M of mass was ejected in the supernova, our model suggests a normal or slightly subenergetic supernova in a low density environment. Additionally, for the measured pre-outburst braking index of p = 2.65, our model prefers an age of ∼ 430 years and an initial spin period P0 ∼ 0.2 s. Lastly, the magnetization of the pulsar wind and energy spectrum of particles injected at the termination shock are similar to those observed from other PWNe powered by less magnetized neutron stars. While further study is needed to verify these results, they are nominally inconsistent with strong neutron star magnetic fields resulting from very fast initial rotation.

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PSR J1119–6127 and the X-ray emission from high magnetic field radio pulsars

Gonzalez¹,

Kaspi²,

Camilo³

et al. 2007

Isolated Neutron Stars: From the Surface to the Interior

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The existence of radio pulsars having inferred magnetic fields in the magnetar regime suggests that possible transition objects could be found in the radio pulsar population. The discovery of such an object would contribute greatly to our understanding of neutron star physics. Here we report on unusual X-ray emission detected from the radio pulsar PSR J1119-6127 using XMMNewton. The pulsar has a characteristic age of 1,700 yrs and inferred surface dipole magnetic field strength of 4.1×10 13 G. In the 0.5-2.0 keV range, the emission shows a single, narrow pulse with an unusually high pulsed fraction of ∼70%. No pulsations are detected in the 2.0-10.0 keV range, where we derive an upper limit at the 99% level for the pulsed fraction of 28%. The pulsed emission is well described by a thermal blackbody model with a high temperature of ∼2.4×10 6 K. While no unambiguous signature of magnetar-like emission has been found in high-magnetic-field radio pulsars, the X-ray characteristics of PSR J1119-6127 require alternate models from those of conventional thermal emission from neutron stars. In addition, PSR J1119-6127 is now the radio pulsar with the smallest characteristic age from which thermal X-ray emission has been detected.

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ChandraX‐Ray Imaging Spectroscopy of the Young Supernova Remnant Kesteven 75

Cited by 84 publications

References 31 publications

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75

PSR J1119–6127 and the X-ray emission from high magnetic field radio pulsars

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