995 research outputs found
The Fermi LAT detection of magnetar-like pulsar PSR J1846-0258 at high-energy gamma-rays
We report the detection of the pulsed signal of the radio-quiet magnetar-like
pulsar PSR J1846-0258 in the high-energy \gr-ray data of the Fermi Large Area
Telescope (Fermi LAT). We produced phase-coherent timing models exploiting RXTE
PCA and Swift XRT monitoring data for the post- (magnetar-like) outburst period
from 2007 August 28 to 2016 September 4, with independent verification using
INTEGRAL ISGRI and Fermi GBM data. Phase-folding barycentric arrival times of
selected Fermi LAT events from PSR J1846-0258, resulted in a 4.2 sigma
detection (30--100 MeV) of a broad pulse consistent in shape and aligned in
phase with the profiles that we measured with Swift XRT (2.5--10 keV), INTEGRAL
ISGRI (20--150 keV) and Fermi GBM (20--300 keV). The pulsed flux (30--100 MeV)
is (3.91 +/- 0.97)E-9 photons/(cm^2 s MeV). Declining significances of the
INTEGRAL ISGRI 20--150 keV pulse profiles suggest fading of the pulsed hard
X-ray emission during the post-outburst epochs. We revisited with greatly
improved statistics the timing and spectral characteristics of PSR B1509-58 as
measured with the Fermi LAT. The broad-band pulsed emission spectra (from 2 keV
up to GeV energies) of PSR J1846-0258 and PSR B1509-58 can be accurately
described with similarly curved shapes, with maximum luminosities at 3.5 +/-
1.1 MeV (PSR J1846-0258) and 2.23 +/- 0.11 MeV (PSR B1509-58). We discuss
possible explanations for observational differences between Fermi LAT detected
pulsars that reach maximum luminosities at GeV energies, like the second
magnetar-like pulsar PSR J1119-6127, and pulsars with maximum luminosities at
MeV energies, which might be due to geometric differences rather than exotic
physics in high-B fields.Comment: 13 pages, 8 figures, accepted by MNRAS on 2017 November 3
The 2-10 keV emission properties of PSR B1937+21
We present the results of a BeppoSAX observation of the fastest pulsar known:
PSR B1937+21. The ~ 200 ks observation (78.5 (34) ks MECS (LECS) exposure
times) allowed us to investigate with high statistical significance both the
spectral properties and the pulse profile shape. The absorbed power law
spectral model gave a photon index of ~ 1.7 and N_H ~ 2.3 x 10^22 cm^-2. These
values explain both a) the ROSAT non-detection and b) the deviant estimate of a
photon index of ~ 0.8 obtained by ASCA. The pulse profile appears, for the
first time, clearly double peaked with the main component much stronger than
the other. The statistical significance is 10 sigma (main peak) and 5 sigma
(secondary peak). The 1.6-10 keV pulsed fraction is consistent with 100%; only
in the 1.6-4 keV band there is a ~ 2 sigma indication for a DC component. The
secondary peak is detected significantly only for energies above 3 / 4 keV. The
unabsorbed (2-10 keV) flux is F_2-10 = 3.7 x 10^-13 erg cm^-2 s^-1, implying a
luminosity of L_X = 4.6 x 10^31 Theta (d/3.6 kpc)^2 erg s^-1 and an X-ray
efficiency of eta = 4 x 10^-5 Theta, where Theta is the solid angle spanned by
the emission beam. These results are in agreement with those obtained by ASCA.Comment: 4 pages, 4 figures, 2 tables. To appear in the Proceedings of the
270. WE-Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants,
Jan. 21-25, 2002, Physikzentrum Bad Honnef, eds W. Becker, H. Lesch & J.
Truemper. Proceedings are available as MPE-Report 27
A large spin-up glitch detected in the 70.5 ms pulsar AX J1838.0-0655 associated with HESS J1837-069
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