119 research outputs found
Detailed X-ray spectroscopy of the magnetar 1E 2259+586
Magnetic field geometry is expected to play a fundamental role in magnetar
activity. The discovery of a phase-variable absorption feature in the X-ray
spectrum of SGR 0418+5729, interpreted as cyclotron resonant scattering,
suggests the presence of very strong non-dipolar components in the magnetic
fields of magnetars. We performed a deep XMM-Newton observation of pulsar 1E
2259+586, to search for spectral features due to intense local magnetic fields.
In the phase-averaged X-ray spectrum, we found evidence for a broad absorption
feature at very low energy (0.7 keV). If the feature is intrinsic to the
source, it might be due to resonant scattering/absorption by protons close to
star surface. The line energy implies a magnetic field of ~ 10^14 G, roughly
similar to the spin-down measure, ~ 6x10^13 G. Examination of the X-ray
phase-energy diagram shows evidence for a further absorption feature, the
energy of which strongly depends on the rotational phase (E >~ 1 keV ). Unlike
similar features detected in other magnetar sources, notably SGR 0418+5729, it
is too shallow and limited to a small phase interval to be modeled with a
narrow phase-variable cyclotron absorption line. A detailed phase-resolved
spectral analysis reveals significant phase-dependent variability in the
continuum, especially above 2 keV. We conclude that all the variability with
phase in 1E 2259+586 can be attributed to changes in the continuum properties
which appear consistent with the predictions of the Resonant Compton Scattering
model
Simultaneous Multi-band Radio & X-ray Observations of the Galactic Center Magnetar SGR 17452900
We report on multi-frequency, wideband radio observations of the Galactic
Center magnetar (SGR 17452900) with the Green Bank Telescope for 100
days immediately following its initial X-ray outburst in April 2013. We made
multiple simultaneous observations at 1.5, 2.0, and 8.9 GHz, allowing us to
examine the magnetar's flux evolution, radio spectrum, and interstellar medium
parameters (such as the dispersion measure (DM), the scattering timescale and
its index). During two epochs, we have simultaneous observations from the
Chandra X-ray Observatory, which permitted the absolute alignment of the radio
and X-ray profiles. As with the two other radio magnetars with published
alignments, the radio profile lies within the broad peak of the X-ray profile,
preceding the X-ray profile maximum by 0.2 rotations. We also find that
the radio spectral index is significantly negative between 2 and
9 GHz; during the final 30 days of our observations ,
which is typical of canonical pulsars. The radio flux has not decreased during
this outburst, whereas the long-term trends in the other radio magnetars show
concomitant fading of the radio and X-ray fluxes. Finally, our wideband
measurements of the DMs taken in adjacent frequency bands in tandem are
stochastically inconsistent with one another. Based on recent theoretical
predictions, we consider the possibility that the dispersion measure is
frequency-dependent. Despite having several properties in common with the other
radio magnetars, such as , an
increase in the radio flux during the X-ray flux decay has not been observed
thus far in other systems.Comment: 15 pages, 9 figures, 3 tables; accepted to Ap
The discovery, monitoring and environment of SGR J1935+2154
We report on the discovery of a new member of the magnetar class, SGR
J1935+2154, and on its timing and spectral properties measured by an extensive
observational campaign carried out between July 2014 and March 2015 with
Chandra and XMM-Newton (11 pointings). We discovered the spin period of SGR
J1935+2154 through the detection of coherent pulsations at a period of about
3.24s. The magnetar is slowing-down at a rate of 1.43(1)x10^{-11} s/s and with
a decreasing trend due to a negative second period derivative of
-3.5(7)x10^{-19} s/s^2. This implies a surface dipolar magnetic field strength
of about 2.2x10^{14} G, a characteristic age of about 3.6kyr and, a spin-down
luminosity L_{sd} of about 1.7x10^{34} erg/s. The source spectrum is well
modelled by a blackbody with temperature of about 500eV plus a power-law
component with photon index of about 2. The source showed a moderate long-term
variability, with a flux decay of about 25\% during the first four months since
its discovery, and a re-brightening of the same amount during the second four
months. The X-ray data were also used to study the source environment. In
particular, we discovered a diffuse emission extending on spatial scales from
about 1" up to at least 1' around SGR J1935+2154 both in Chandra and XMM-Newton
data. This component is constant in flux (at least within uncertainties) and
its spectrum is well modelled by a power-law spectrum steeper than that of the
pulsar. Though a scattering halo origin seems to be more probable we cannot
exclude that part, or all, of the diffuse emission is due to a pulsar wind
nebula.Comment: To appear in MNRAS; 10 pages, 3 color figures, 4 table
Engulfing a radio pulsar: the case of PSR J1023+0038
The binary millisecond radio pulsar PSR J1023+0038 has been recently the
subject of multiwavelength monitoring campaigns which revealed that an
accretion disc has formed around the neutron star (since 2013 June). We present
here the results of X-ray and UV observations carried out by the Swift
satellite between 2013 October and 2014 May, and of optical and NIR
observations performed with the REM telescope, the Liverpool Telescope, the
2.1-m telescope at the San Pedro M\'artir Observatory and the 1.52-m telescope
at the Loiano observing station. The X-ray spectrum is well described by an
absorbed power law, which is softer than the previous quiescent epoch (up to
2013 June). The strong correlation between the X-ray and the UV emissions
indicates that the same mechanism should be responsible for part of the
emission in these bands. Optical and infrared photometric observations show
that the companion star is strongly irradiated. Double-peaked emission lines in
the optical spectra provide compelling evidence for the presence of an outer
accretion disc too. The spectral energy distribution from IR to X-rays is well
modelled if the contributions from the companion, the disc and the intra-binary
shock emission are all considered. Our extensive data set can be interpreted in
terms of an engulfed radio pulsar: the radio pulsar is still active, but
undetectable in the radio band due to a large amount of ionized material
surrounding the compact object. X-rays and gamma-rays are produced in an
intra-binary shock front between the relativistic pulsar wind and matter from
the companion and an outer accretion disc. The intense spin-down power
irradiates the disc and the companion star, accounting for the UV and optical
emissions.Comment: 11 pages, 8 figures, 5 tables; accepted for publication on MNRA
Magnetar-like activity from the central compact object in the SNR RCW103
The 6.67 hr periodicity and the variable X-ray flux of the central compact object (CCO) at the center of the supernova remnant RCW 103, named 1E 161348–5055, have been always difficult to interpret within the standard scenarios of an isolated neutron star (NS) or a binary system. On 2016 June 22, the Burst Alert Telescope (BAT) on board Swift detected a magnetar-like short X-ray burst from the direction of 1E 161348–5055, also coincident with a large long-term X-ray outburst. Here, we report on Chandra, Nuclear Spectroscopic Telescope Array, and Swift (BAT and XRT) observations of this peculiar source during its 2016 outburst peak. In particular, we study the properties of this magnetar-like burst, we discover a hard X-ray tail in the CCO spectrum during outburst, and we study its long-term outburst history (from 1999 to 2016 July). We find the emission properties of 1E 161348–5055 consistent with it being a magnetar. However, in this scenario, the 6.67 hr periodicity can only be interpreted as the rotation period of this strongly magnetized NS, which therefore represents the slowest pulsar ever detected, by orders of magnitude. We briefly discuss the viable slow-down scenarios, favoring a picture involving a period of fall-back accretion after the supernova explosion, similarly to what is invoked (although in a different regime) to explain the "anti-magnetar" scenario for other CCOs
The X-ray outburst of the Galactic Center magnetar over six years of Chandra observations
The magnetar SGR J1745-2900 discovered at parsecs distance from the Milky Way
central black hole, Sagittarius A*, represents the closest pulsar to a
supermassive black hole ever detected. Furthermore, its intriguing radio
emission has been used to study the environment of the black hole, as well as
to derive a precise position and proper motion for this object. The discovery
of SGR J1745-2900 has opened interesting debates about the number, age and
nature of pulsars expected in the Galactic center region. In this work, we
present extensive X-ray monitoring of the outburst of SGR J1745-2900 using the
Chandra X-ray Observatory, the only instrument with the spatial resolution to
distinguish the magnetar from the supermassive black hole (2.4" angular
distance). It was monitored from its outburst onset in April 2013 until August
2019, collecting more than fifty Chandra observations for a total of more than
2.3 Ms of data. Soon after the outburst onset, the magnetar emission settled
onto a purely thermal emission state that cooled from a temperature of about
0.9 to 0.6 keV over 6 years. The pulsar timing properties showed at least two
changes in the period derivative, increasing by a factor of about 4 during the
outburst decay. We find that the long-term properties of this outburst
challenge current models for the magnetar outbursts.Comment: 11 pages, 6 figures. Accepted by Ap
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