190 research outputs found
Different twins in the millisecond pulsar recycling scenario: optical polarimetry of PSR J1023+0038 and XSS J12270-4859
We present the first optical polarimetric study of the two transitional
pulsars PSR J1023+0038 and XSS J12270-4859. This work is focused on the search
for intrinsical linear polarisation (LP) in the optical emission from the two
systems. We carried out multiband optical and NIR photo-polarimetry of the two
systems using the ESO NTT at La Silla (Chile), equipped with the EFOSC2 and the
SOFI instruments. XSS J12270-4859 was observed during its radio-pulsar state;
we did not detect LP in all bands, with 3 sigma upper limits of, e.g., 1.4% in
the R-band. We built the NIR-optical averaged spectral energy distribution
(SED) of the system, that could be well described by an irradiated black body
with radius and albedo ,
without the need of further components (thus excluding the visible presence of
an extended accretion disc and/or of relativistic jets). The case was different
for PSR J1023+0038, that was in its accretion phase during our campaign. We
measured a LP of and in the V and R bands,
respectively. The phase-resolved polarimetric curve of the source in the R-band
reveals a hint of a sinusoidal modulation at the source 4.75 hr orbital period,
peaked at the same orbital phase as the light curve. The measured LP of PSR
J1023+0038 could in principle be interpreted as scattering with free electrons
(that can be found in the accretion disc of the system or even in the hot
corona that surrounds the disc itself) or to synchrotron emission from a
relativistic particles jet or outflow. However, the NIR-optical SED of the
system built starting from our dataset did not suggest the presence of a jet.
We conclude that the optical LP observed for PSR J1023+0038 is possibly due to
Thomson scattering with electrons in the disc, as also suggested from the
possible modulation of the R-band LP at the system orbital period.Comment: 10 pages, 8 figures, 4 tables. Accepted for publication in Sec. 7.
Stellar structure and evolution of Astronomy and Astrophysic
Renewed activity from the magnetar CXOU J164710.2-455216
On 2018 February 5 at 19:27:11 UT, Swift BAT detected a new burst from a direction consistent with the magnetar CXOU J164710.2-455216 (trigger=808755; Barthelmy et al. 2018, GCN #22389)
Multiwavelength study of RX J2015.6+3711: a magnetic cataclysmic variable with a 2-hr spin period
The X-ray source RX J2015.6+3711 was discovered by ROSAT in 1996 and recently
proposed to be a cataclysmic variable (CV). Here we report on an XMM-Newton
observation of RX J2015.6+3711 performed in 2014, where we detected a coherent
X-ray modulation at a period of 7196+/-11 s, and discovered other significant
(>6sigma) small-amplitude periodicities which we interpret as the CV spin
period and the sidebands of a possible ~12 hr periodicity, respectively. The
0.3-10 keV spectrum can be described by a power law (Gamma = 1.15+/-0.04) with
a complex absorption pattern, a broad emission feature at 6.60+/-0.01 keV, and
an unabsorbed flux of (3.16+/-0.05)x10^{-12} erg/s/cm^2. We observed a
significant spectral variability along the spin phase, which can be ascribed
mainly to changes in the density of a partial absorber and the power law
normalization. Archival X-ray observations carried out by the Chandra
satellite, and two simultaneous X-ray and UV/optical pointings with Swift,
revealed a gradual fading of the source in the soft X-rays over the last 13
years, and a rather stable X-ray-to-optical flux ratio (F_X/F_V ~1.4-1.7).
Based on all these properties, we identify this source with a magnetic CV, most
probably of the intermediate polar type. The 2 hr spin period makes RX
J2015.6+3711 the second slowest rotator of the class, after RX J0524+4244
("Paloma", P_spin~2.3 hr). Although we cannot unambiguously establish the true
orbital period with these observations, RX J2015.6+3711 appears to be a key
system in the evolution of magnetic CVs.Comment: 11 pages, 8 figures, accepted for publication on MNRA
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
- …