261 research outputs found
Towards fast machine-learning-assisted Bayesian posterior inference of microseismic event location and source mechanism
Bayesian inference applied to microseismic activity monitoring allows the accurate location of microseismic events from recorded seismograms and the estimation of the associated uncertainties. However, the forward modelling of these microseismic events, which is necessary to perform Bayesian source inversion, can be prohibitively expensive in terms of computational resources. A viable solution is to train a surrogate model based on machine learning techniques, to emulate the forward model and thus accelerate Bayesian inference. In this paper, we substantially enhance previous work, which considered only sources with isotropic moment tensors. We train a machine learning algorithm on the power spectrum of the recorded pressure wave and show that the trained emulator allows complete and fast event locations for any source mechanism. Moreover, we show that our approach is computationally inexpensive, as it can be run in less than 1Â hour on a commercial laptop, while yielding accurate results using less than 104 training seismograms. We additionally demonstrate how the trained emulators can be used to identify the source mechanism through the estimation of the Bayesian evidence. Finally, we demonstrate that our approach is robust to real noise as measured in field data. This work lays the foundations for efficient, accurate future joint determinations of event location and moment tensor, and associated uncertainties, which are ultimately key for accurately characterising human-induced and natural earthquakes, and for enhanced quantitative seismic hazard assessments
Path Integral Marginalization for Cosmology: Scale Dependent Galaxy Bias & Intrinsic Alignments
We present a path-integral likelihood formalism that extends parameterized
likelihood analyses to include continuous functions. The method finds the
maximum likelihood point in function-space, and marginalizes over all possible
functions, under the assumption of a Gaussian-distributed function-space. We
apply our method to the problem of removing unknown systematic functions in two
topical problems for dark energy research : scale-dependent galaxy bias in
redshift surveys; and galaxy intrinsic alignments in cosmic shear surveys. We
find that scale-dependent galaxy bias will degrade information on cosmological
parameters unless the fractional variance in the bias function is known to 10%.
Measuring and removing intrinsic alignments from cosmic shear surveys with a
flat-prior can reduce the dark energy Figure-of-Merit by 20%, however provided
that the scale and redshift-dependence is known to better than 10% with a
Gaussian-prior, the dark energy Figure-of-Merit can be enhanced by a factor of
two with no extra assumptions.Comment: 11 pages, 4 figures, submitted to MNRA
Cosmological systematics beyond nuisance parameters: form-filling functions
In the absence of any compelling physical model, cosmological systematics are often misrepresented as statistical effects and the approach of marginalizing over extra nuisance systematic parameters is used to gauge the effect of the systematic. In this article, we argue that such an approach is risky at best since the key choice of function can have a large effect on the resultant cosmological errors. As an alternative we present a functional form-filling technique in which an unknown, residual, systematic is treated as such. Since the underlying function is unknown, we evaluate the effect of every functional form allowed by the information available (either a hard boundary or some data). Using a simple toy model, we introduce the formalism of functional form filling. We show that parameter errors can be dramatically affected by the choice of function in the case of marginalizing over a systematic, but that in contrast the functional form-filling approach is independent of the choice of basis set. We then apply the technique to cosmic shear shape measurement systematics and show that a shear calibration bias of |m(z)| ≲ 10−3 (1 +z)0.7 is required for a future all-sky photometric survey to yield unbiased cosmological parameter constraints to per cent accuracy. A module associated with the work in this paper is available through the open source icosmo code available at http://www.icosmo.or
Galaxy alignments: An overview
The alignments between galaxies, their underlying matter structures, and the
cosmic web constitute vital ingredients for a comprehensive understanding of
gravity, the nature of matter, and structure formation in the Universe. We
provide an overview on the state of the art in the study of these alignment
processes and their observational signatures, aimed at a non-specialist
audience. The development of the field over the past one hundred years is
briefly reviewed. We also discuss the impact of galaxy alignments on
measurements of weak gravitational lensing, and discuss avenues for making
theoretical and observational progress over the coming decade.Comment: 43 pages excl. references, 16 figures; minor changes to match version
published in Space Science Reviews; part of a topical volume on galaxy
alignments, with companion papers at arXiv:1504.05546 and arXiv:1504.0546
Galaxy alignments: Observations and impact on cosmology
Galaxy shapes are not randomly oriented, rather they are statistically
aligned in a way that can depend on formation environment, history and galaxy
type. Studying the alignment of galaxies can therefore deliver important
information about the physics of galaxy formation and evolution as well as the
growth of structure in the Universe. In this review paper we summarise key
measurements of galaxy alignments, divided by galaxy type, scale and
environment. We also cover the statistics and formalism necessary to understand
the observations in the literature. With the emergence of weak gravitational
lensing as a precision probe of cosmology, galaxy alignments have taken on an
added importance because they can mimic cosmic shear, the effect of
gravitational lensing by large-scale structure on observed galaxy shapes. This
makes galaxy alignments, commonly referred to as intrinsic alignments, an
important systematic effect in weak lensing studies. We quantify the impact of
intrinsic alignments on cosmic shear surveys and finish by reviewing practical
mitigation techniques which attempt to remove contamination by intrinsic
alignments.Comment: 52 pages excl. references, 16 figures; minor changes to match version
published in Space Science Reviews; part of a topical volume on galaxy
alignments, with companion papers arXiv:1504.05456 and arXiv:1504.0554
Weak gravitational lensing with the Square Kilometre Array
We investigate the capabilities of various stages of the SKA to perform
world-leading weak gravitational lensing surveys. We outline a way forward to
develop the tools needed for pursuing weak lensing in the radio band. We
identify the key analysis challenges and the key pathfinder experiments that
will allow us to address them in the run up to the SKA. We identify and
summarize the unique and potentially very powerful aspects of radio weak
lensing surveys, facilitated by the SKA, that can solve major challenges in the
field of weak lensing. These include the use of polarization and rotational
velocity information to control intrinsic alignments, and the new area of weak
lensing using intensity mapping experiments. We show how the SKA lensing
surveys will both complement and enhance corresponding efforts in the optical
wavebands through cross-correlation techniques and by way of extending the
reach of weak lensing to high redshift.Comment: 19 pages, 6 figures. Cosmology Chapter, Advancing Astrophysics with
the SKA (AASKA14) Conference, Giardini Naxos (Italy), June 9th-13th 201
Cosmological Systematics Beyond Nuisance Parameters : Form Filling Functions
In the absence of any compelling physical model, cosmological systematics are
often misrepresented as statistical effects and the approach of marginalising
over extra nuisance systematic parameters is used to gauge the effect of the
systematic. In this article we argue that such an approach is risky at best
since the key choice of function can have a large effect on the resultant
cosmological errors. As an alternative we present a functional form filling
technique in which an unknown, residual, systematic is treated as such. Since
the underlying function is unknown we evaluate the effect of every functional
form allowed by the information available (either a hard boundary or some
data). Using a simple toy model we introduce the formalism of functional form
filling. We show that parameter errors can be dramatically affected by the
choice of function in the case of marginalising over a systematic, but that in
contrast the functional form filling approach is independent of the choice of
basis set. We then apply the technique to cosmic shear shape measurement
systematics and show that a shear calibration bias of |m(z)|< 0.001(1+z)^0.7 is
required for a future all-sky photometric survey to yield unbiased cosmological
parameter constraints to percent accuracy. A module associated with the work in
this paper is available through the open source iCosmo code available at
http://www.icosmo.org .Comment: 24 pages, 18 figures, accepted to MNRA
Accelerating Bayesian microseismic event location with deep learning
We present a series of new open-source deep-learning algorithms to accelerate Bayesian full-waveform point source inversion of microseismic
events. Inferring the joint posterior probability distribution of moment tensor components and source location is key for rigorous uncertainty
quantification. However, the inference process requires forward modelling of microseismic traces for each set of parameters explored by the sampling
algorithm, which makes the inference very computationally intensive. In this paper we focus on accelerating this process by training deep-learning
models to learn the mapping between source location and seismic traces for a given 3D heterogeneous velocity model and a fixed isotropic moment
tensor for the sources. These trained emulators replace the expensive solution of the elastic wave equation in the inference process.
We compare our results with a previous study that used emulators based on Gaussian processes to invert microseismic events. For fairness of
comparison, we train our emulators on the same microseismic traces and using the same geophysical setting. We show that all of our models provide
more accurate predictions, ∼ 100 times faster predictions than the method based on Gaussian processes, and a (105) speed-up
factor over a pseudo-spectral method for waveform generation. For example, a 2 s long synthetic trace can be generated in ∼ 10 ms on a
common laptop processor, instead of ∼ 1 h using a pseudo-spectral method on a high-profile graphics processing unit card. We also
show that our inference results are in excellent agreement with those obtained from traditional location methods based on travel time estimates. The
speed, accuracy, and scalability of our open-source deep-learning models pave the way for extensions of these emulators to generic source mechanisms
and application to joint Bayesian inversion of moment tensor components and source location using full waveforms.</p
Flat-sky pseudo-cls analysis for weak gravitational lensing
We investigate the use of estimators of weak lensing power spectra based on a
flat-sky implementation of the Pseudo-Cl (PCl) technique, where the masked
shear field is transformed without regard for masked regions of sky. This
masking mixes power, and E-convergence and B-modes. To study the accuracy of
forward-modelling and full-sky power spectrum recovery we consider both
large-area survey geometries, and small-scale masking due to stars and a
checkerboard model for field-of-view gaps. The power spectrum for the
large-area survey geometry is sparsely-sampled and highly oscillatory, which
makes modelling problematic. Instead, we derive an overall calibration for
large-area mask bias using simulated fields. The effects of small-area star
masks can be accurately corrected for, while the checkerboard mask has
oscillatory and spiky behaviour which leads to percent biases. Apodisation of
the masked fields leads to increased biases and a loss of information. We find
that we can construct an unbiased forward-model of the raw PCls, and recover
the full-sky convergence power to within a few percent accuracy for both
Gaussian and lognormal-distributed shear fields. Propagating this through to
cosmological parameters using a Fisher-Matrix formalism, we find we can make
unbiased estimates of parameters for surveys up to 1,200 deg with 30
galaxies per arcmin, beyond which the percent biases become larger than the
statistical accuracy. This implies a flat-sky PCl analysis is accurate for
current surveys but a Euclid-like survey will require higher accuracy.Comment: 25 pages, 14 figure
Group-scale intrinsic galaxy alignments in the Illustris-TNG and MassiveBlack-II simulations
We study the alignments of satellite galaxies, and their anisotropic
distribution, with respect to location and orientation of their host central
galaxy in MassiveBlack-II and IllustrisTNG simulations. We find that: the shape
of the satellite system in halos of mass () is well
aligned with the shape of the central galaxy at with the mean
alignment between the major axes being when
compared to a uniform random distribution; that satellite galaxies tend to be
anisotropically distributed along the major axis of the central galaxy with a
stronger alignment in halos of higher mass or luminosity; and that the
satellite distribution is more anisotropic for central galaxies with lower star
formation rate, which are spheroidal, and for red central galaxies.Radially we
find that satellites tend to be distributed along the major axis of the shape
of the stellar component of central galaxies at smaller scales and the dark
matter component on larger scales. We find that the dependence of satellite
anisotropy on central galaxy properties and the radial distance is similar in
both the simulations with a larger amplitude in MassiveBlack-II. The
orientation of satellite galaxies tends to point toward the location of the
central galaxy at small scales and this correlation decreases with increasing
distance, and the amplitude of satellite alignment is higher in high mass
halos. However, the projected ellipticities do not exhibit a scale-dependent
radial alignment, as has been seen in some observational measurements.Comment: 15 pages, 9 figures, revised after referee comments, accepted for
publication in MNRA
- …