470 research outputs found
On the Statistical Properties of Cospectra
In recent years, the cross-spectrum has received considerable attention as a means of characterizing the variability of astronomical sources as a function of wavelength. The cospectrum has only recently been understood as a means of mitigating instrumental effects dependent on temporal frequency in astronomical detectors, as well as a method of characterizing the coherent variability in two wavelength ranges on different timescales. In this paper, we lay out the statistical foundations of the cospectrum, starting with the simplest case of detecting a periodic signal in the presence of white noise, under the assumption that the same source is observed simultaneously in independent detectors in the same energy range. This case is especially relevant for detecting faint X-ray pulsars in detectors heavily affected by instrumental effects, including NuSTAR, Astrosat, and IXPE, which allow for even sampling and where the cospectrum can act as an effective way to mitigate dead time. We show that the statistical distributions of both single and averaged cospectra differ considerably from those for standard periodograms. While a single cospectrum follows a Laplace distribution exactly, averaged cospectra are approximated by a Gaussian distribution only for more than ~30 averaged segments, dependent on the number of trials. We provide an instructive example of a quasi-periodic oscillation in NuSTAR and show that applying standard periodogram statistics leads to underestimated tail probabilities for period detection. We also demonstrate the application of these distributions to a NuSTAR observation of the X-ray pulsar Hercules X-1
Evidence for a Variable Ultrafast Outflow in the Newly Discovered Ultraluminous Pulsar NGC 300 ULX-1
Ultraluminous pulsars are a definite proof that persistent super-Eddington
accretion occurs in nature. They support the scenario according to which most
Ultraluminous X-ray Sources (ULXs) are super-Eddington accretors of stellar
mass rather than sub-Eddington intermediate mass black holes. An important
prediction of theories of supercritical accretion is the existence of powerful
outflows of moderately ionized gas at mildly relativistic speeds. In practice,
the spectral resolution of X-ray gratings such as RGS onboard XMM-Newton is
required to resolve their observational signatures in ULXs. Using RGS, outflows
have been discovered in the spectra of 3 ULXs (none of which are currently
known to be pulsars). Most recently, the fourth ultraluminous pulsar was
discovered in NGC 300. Here we report detection of an ultrafast outflow (UFO)
in the X-ray spectrum of the object, with a significance of more than
3{\sigma}, during one of the two simultaneous observations of the source by
XMM-Newton and NuSTAR in December 2016. The outflow has a projected velocity of
65000 km/s (0.22c) and a high ionisation factor with a log value of 3.9. This
is the first direct evidence for a UFO in a neutron star ULX and also the first
time that this its evidence in a ULX spectrum is seen in both soft and hard
X-ray data simultaneously. We find no evidence of the UFO during the other
observation of the object, which could be explained by either clumpy nature of
the absorber or a slight change in our viewing angle of the accretion flow.Comment: 10 pages, 4 figures. Accepted to MNRA
Spectral Changes in the Hyperluminous Pulsar in NGC 5907 as a Function of Super-Orbital Phase
We present broad-band, multi-epoch X-ray spectroscopy of the pulsating
ultra-luminous X-ray source (ULX) in NGC 5907. Simultaneous XMM-Newton and
NuSTAR data from 2014 are best described by a multi-color black-body model with
a temperature gradient as a function of accretion disk radius significantly
flatter than expected for a standard thin accretion disk (T(r) ~ r^{-p}, with
p=0.608^{+0.014}_{-0.012}). Additionally, we detect a hard power-law tail at
energies above 10 keV, which we interpret as being due to Comptonization. We
compare this observation to archival XMM-Newton, Chandra, and NuSTAR data from
2003, 2012, and 2013, and investigate possible spectral changes as a function
of phase over the 78d super-orbital period of this source. We find that
observations taken around phases 0.3-0.4 show very similar temperature
profiles, even though the observed flux varies significantly, while one
observation taken around phase 0 has a significantly steeper profile. We
discuss these findings in light of the recent discovery that the compact object
is a neutron star and show that precession of the accretion disk or the neutron
star can self-consistently explain most observed phenomena.Comment: 7 pages, 5 figures, submitted to ApJ; comments welcom
MHD Simulations of Magnetospheric Accretion, Ejection and Plasma-field Interaction
We review recent axisymmetric and three-dimensional (3D) magnetohydrodynamic
(MHD) numerical simulations of magnetospheric accretion, plasma-field
interaction and outflows from the disk-magnetosphere boundary.Comment: 11 pages, 8 figures, conference proceedings: "Physics at the
Magnetospheric Boundary", Geneva, Switzerland, 25-28 June, 201
An XMM-Newton and NuSTAR study of IGR J18214-1318: a non-pulsating high-mass X-ray binary with a neutron star
IGR J18214-1318, a Galactic source discovered by the International Gamma-Ray
Astrophysics Laboratory, is a high-mass X-ray binary (HMXB) with a supergiant
O-type stellar donor. We report on the XMM-Newton and NuSTAR observations that
were undertaken to determine the nature of the compact object in this system.
This source exhibits high levels of aperiodic variability, but no periodic
pulsations are detected with a 90% confidence upper limit of 2% fractional rms
between 0.00003-88 Hz, a frequency range that includes the typical pulse
periods of neutron stars (NSs) in HMXBs (0.1-10 s). Although the lack of
pulsations prevents us from definitively identifying the compact object in IGR
J18214-1318, the presence of an exponential cutoff with e-folding energy
keV in its 0.3-79 keV spectrum strongly suggests that the compact
object is an NS. The X-ray spectrum also shows a Fe K emission line and
a soft excess, which can be accounted for by either a partial-covering absorber
with cm which could be due to the
inhomogeneous supergiant wind, or a blackbody component with
keV and km, which may originate
from NS hot spots. Although neither explanation for the soft excess can be
excluded, the former is more consistent with the properties observed in other
supergiant HMXBs. We compare IGR J18214-1318 to other HMXBs that lack
pulsations or have long pulsation periods beyond the range covered by our
observations.Comment: 15 pages, 12 figures, 4 table
Extending the and statistics to generic pulsed profiles
The search for astronomical pulsed signals within noisy data, in the radio
band, is usually performed through an initial Fourier analysis to find
"candidate" frequencies and then refined through the folding of the time series
using trial frequencies close to the candidate. In order to establish the
significance of the pulsed profiles found at these trial frequencies, pulsed
profiles are evaluated with a chi-squared test, to establish how much they
depart from a null hypothesis where the signal is consistent with a flat
distribution of noisy measurements. In high-energy astronomy, the chi-squared
statistic has widely been replaced by the statistic and the H-test as
they are more sensitive to extra information such as the harmonic content of
the pulsed profile. The statistic and H-test were originally developed
for the use with "event data", composed of arrival times of single photons,
leaving it unclear how these methods could be used in radio astronomy. In this
paper, we present a version of the statistic and H-test for pulse
profiles with Gaussian uncertainties, appropriate for radio or even optical
pulse profiles. We show how these statistical indicators provide better
sensitivity to low-significance pulsar candidates with respect to the usual
chi-squared method, and a straightforward way to discriminate between pulse
profile shapes. Moreover, they provide an additional tool for Radio Frequency
Interference (RFI) rejection.Comment: 15 pages, 5 figure
Detection of Very Low-Frequency Quasi-Periodic Oscillations in the 2015 Outburst of V404 Cygni
In June 2015, the black hole X-ray binary (BHXRB) V404 Cygni went into
outburst for the first time since 1989. Here, we present a comprehensive search
for quasi-periodic oscillations (QPOs) of V404 Cygni during its recent
outburst, utilizing data from six instruments on board five different X-ray
missions: Swift/XRT, Fermi/GBM, Chandra/ACIS, INTEGRAL's IBIS/ISGRI and JEM-X,
and NuSTAR. We report the detection of a QPO at 18 mHz simultaneously with both
Fermi/GBM and Swift/XRT, another example of a rare but slowly growing new class
of mHz-QPOs in BHXRBs linked to sources with a high orbital inclination.
Additionally, we find a duo of QPOs in a Chandra/ACIS observation at 73 mHz and
1.03 Hz, as well as a QPO at 136 mHz in a single Swift/XRT observation that can
be interpreted as standard Type-C QPOs. Aside from the detected QPOs, there is
significant structure in the broadband power, with a strong feature observable
in the Chandra observations between 0.1 and 1 Hz. We discuss our results in the
context of current models for QPO formation.Comment: 17 pages, 9 figures, published in Ap
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