4,337 research outputs found
Estimation and uncertainty of reversible Markov models
Reversibility is a key concept in Markov models and Master-equation models of
molecular kinetics. The analysis and interpretation of the transition matrix
encoding the kinetic properties of the model relies heavily on the
reversibility property. The estimation of a reversible transition matrix from
simulation data is therefore crucial to the successful application of the
previously developed theory. In this work we discuss methods for the maximum
likelihood estimation of transition matrices from finite simulation data and
present a new algorithm for the estimation if reversibility with respect to a
given stationary vector is desired. We also develop new methods for the
Bayesian posterior inference of reversible transition matrices with and without
given stationary vector taking into account the need for a suitable prior
distribution preserving the meta- stable features of the observed process
during posterior inference. All algorithms here are implemented in the PyEMMA
software - http://pyemma.org - as of version 2.0
Active phase and amplitude fluctuations of flagellar beating
The eukaryotic flagellum beats periodically, driven by the oscillatory
dynamics of molecular motors, to propel cells and pump fluids. Small, but
perceivable fluctuations in the beat of individual flagella have physiological
implications for synchronization in collections of flagella as well as for
hydrodynamic interactions between flagellated swimmers. Here, we characterize
phase and amplitude fluctuations of flagellar bending waves using shape mode
analysis and limit cycle reconstruction. We report a quality factor of
flagellar oscillations, (means.e.). Our analysis shows
that flagellar fluctuations are dominantly of active origin. Using a minimal
model of collective motor oscillations, we demonstrate how the stochastic
dynamics of individual motors can give rise to active small-number fluctuations
in motor-cytoskeleton systems.Comment: accepted for publication in Physical Review Letter
Chandra and Hubble Study of a New Transient X-ray Source in M31
We present X-ray and optical observations of a new transient X-ray source in
M31 first detected 23-May-2004 at R.A.=00:43:09.940 +/- 0.65'',
Dec.=41:23:32.49 +/- 0.66''. The X-ray lightcurve shows two peaks separated by
several months, reminiscent of many Galactic X-ray novae. The location and
X-ray spectrum of the source suggest it is a low mass X-ray binary (LMXB).
Follow-up HST ACS observations of the location both during and after the
outburst provide a high-confidence detection of variability for one star within
the X-ray position error ellipse. This star has B ~ 1 mag, and there is
only a ~1% chance of finding such a variable in the error ellipse. We consider
this star a good candidate for the optical counterpart of the X-ray source. The
luminosity of this candidate provides a prediction for the orbital period of
the system of 2.3 days.Comment: 17 pages, 3 figures, 4 tables, accepted for publication in Ap
A Deep XMM-Newton Survey of M33: Point Source Catalog, Source Detection and Characterization of Overlapping Fields
We have obtained a deep 8-field XMM-Newton mosaic of M33 covering the galaxy
out to the D isophote and beyond to a limiting 0.2--4.5 keV unabsorbed
flux of 510 erg cm s (L410
erg s at the distance of M33). These data allow complete coverage of the
galaxy with high sensitivity to soft sources such as diffuse hot gas and
supernova remnants. Here we describe the methods we used to identify and
characterize 1296 point sources in the 8 fields. We compare our resulting
source catalog to the literature, note variable sources, construct hardness
ratios, classify soft sources, analyze the source density profile, and measure
the X-ray luminosity function. As a result of the large effective area of
XMM-Newton below 1 keV, the survey contains many new soft X-ray sources. The
radial source density profile and X-ray luminosity function for the sources
suggests that only 15% of the 391 bright sources with
L3.610 erg s are likely to be associated with M33,
and more than a third of these are known supernova remnants. The log(N)--log(S)
distribution, when corrected for background contamination, is a relatively flat
power-law with a differential index of 1.5, which suggests many of the other
M33 sources may be high-mass X-ray binaries. Finally, we note the discovery of
an interesting new transient X-ray source, which we are unable to classify.Comment: 26 pages, 6 tables, 13 figures, accepted for publication in ApJ
SXP214, an X-ray Pulsar in the Small Magellanic Cloud, Crossing the Circumstellar Disk of the Companion
Located in the Small Magellanic Cloud (SMC), SXP214 is an X-ray pulsar in a
high mass X-ray binary system with a Be-star companion. A recent survey of the
SMC under a Chandra X-ray Visionary program found the source in a transition
when the X-ray flux was on a steady rise. The Lomb-Scargle periodogram revealed
a pulse period of 211.49 +/- 0.42 s, which is significantly (>5sigma) shorter
than the previous measurements with XMM-Newton and RXTE. This implies that the
system has gone through sudden spin-up episodes recently. The pulse profile
shows a sharp eclipse-like feature with a modulation amplitude of >95%. The
linear rise of the observed X-ray luminosity from <~2x to 7x10^35 erg s^-1 is
correlated with steady softening of the X-ray spectrum, which can be described
by the changes in the local absorption from N_H ~ 10^24 to <~10^20 cm^-2 for an
absorbed power-law model. The soft X-ray emission below 2 keV was absent in the
early part of the observation when only the pulsating hard X-ray component was
observed, whereas at later times both soft and hard X-ray components were
observed pulsating. A likely explanation is that the neutron star was initially
hidden in the circumstellar disk of the companion, and later came out of the
disk with the accreted material that continued fueling the observed pulsation.Comment: 8 pages, 4 figures, 1 table, accepted for publication in Ap
Optical Constraints on an X-ray Transient Source in M31
We have detected a transient X-ray source in the M31 bulge through a
continuing monitoring campaign with the Chandra ACIS-I camera. The source was
detected at R.A.=00:42:33.428 +/- 0.11'', Dec.=+41:17:03.37 +/- 0.11'' in only
a single observation taken 2004 May 23. Fortuitous optical HST/ACS imaging of
the transient location prior to the X-ray outburst, along with follow-up
HST/ACS imaging during and after the outburst, reveals no transient optical
source brighter than B (equivalent) = 25.5. The location of the source and its
X-ray properties suggest it is a low mass X-ray binary (LMXB). Assuming the
transient is similar to many Galactic X-ray novae, the X-ray luminosity of (3.9
+/- 0.5) X 10 erg s and the upper-limit on the optical luminosity
provide a prediction of <1.6 days for the orbital period of the binary system.Comment: 15 pages, 3 figures, accepted for publication in Ap
A Soft X-ray Transient in the M31 Bulge
We have examined a probable soft X-ray transient source in the M31 bulge at
R.A.=0:42:41.814 +/- 0.08", Dec. = 41:16:35.86 +/- 0.07". On the three
occasions we observed the source, its spectrum was soft (kT_{in} ~1 keV). The
brightest detection of the source was 2004 July 17 with a 0.3-7 keV luminosity
of ~5 X 10^{37} erg/s. The only previous detection of the source was in 1979 by
the Einstein observatory. The multiple detections over 25 years suggest the
duty cycle of the source is in the range 0.02-0.06. Coordinated HST/ACS imaging
before, during, and after the outburst revealed no variable optical source
within the position errors of the X-ray source. The optical data place a firm
upper limit on the brightness of the counterpart of the X-ray outburst of
B>24.7, suggesting the binary has a period <5.2 days. The X-ray spectrum and
lack of bright stars at the source location indicate the source was a soft
transient event occurring in a low-mass X-ray binary, making this source a good
black hole candidate in M31.Comment: 18 pages, 4 tables, 3 figures, accepted for publication in Ap
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