The alignments and clustering of galaxies in wide-area photometric galaxy surveys

The upcoming decades will see the transformation of our understanding of the Universe. New experiments, soon to come online, aim to observe the evolution of large-scale structures traced by billions of galaxies, throughout much of cosmic time. The volume of data soon to be at our disposal comes with responsibility; with unprecedented levels of statistical power, we must identify and control sources of systematic error in our analyses to an ever greater degree, lest we waste newfound precision upon inaccurate inferences. This thesis explores the impacts of such errors upon our understanding of galaxy data, and proposes methods for their mitigation. First, I detail my study of the intrinsic alignments of galaxies (Ch. 2). The study of weak cosmological lensing (or `cosmic shear') posits that the distribution of intrinsic galaxy shapes should be random, and thus that we can learn about the Universe by attributing shape correlations to the effects of gravitational lensing by the large-scale structure. However, we observe different galaxies to be intrinsically aligned with structure in complex ways; violating the assumption of randomness and forming the primary astrophysical systematic for cosmic shear analyses. Using a unique set of highly-complete, spectroscopic data, I directly measure and model the projected 3D galaxy intrinsic alignments and clustering, revealing new complexity regarding the spiral/elliptical, central/satellite nature of galaxies, before forecasting the benefits of my data-driven priors for intrinsic alignment models in future cosmic shear work. The physical galaxy distribution is another powerful probe of the Universe, however, measurements of galaxy clustering must contend with spatially non-uniform observing conditions. If poor conditions result in systematic failures to detect objects, the observed clustering will not represent the true galaxy density field. I describe (in Ch. 3) a method of mitigation for such biases, centred around the retrieval of systematic density modes from galaxy data using self-organising maps (SOMs). Creating random galaxy catalogues which mimic and thereby subtract the systematic density trends, I demonstrate the accurate recovery of clustering signals from realistically deprecated synthetic data. I go on to present the first photometric angular clustering measurement from the Kilo Degree Survey, made robust by our corrective randoms. Studies of 3D, or projected, clustering and intrinsic alignments are typically limited to spectroscopic, rather than photometric, data; accurate redshifts are necessary to isolate objects in the radial dimension. The Physics of the Accelerating Universe Survey bridges this gap, offering greater depths at a small cost to redshift accuracy, by observing in 40 optical narrow-bands. In Ch. 4, I derive principled random galaxy catalogues, capable of reproducing the galaxies' redshift distribution sans structure, and doing so robustly for arbitrary galaxy sample selections. With these randoms, I explore the projected 3D clustering and intrinsic alignments of these data, finding quite remarkable support for the conclusions of my previous work (Ch 2), and extending the study of intrinsic alignments to yet fainter objects and smaller scales

The Decomposition of Cellulose by Soil Fungi

Author Institution: Biology Department, Wilmington College, Wilmington, Ohi

The Niger Basin and Bungo park 1

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Alien Registration- Johnston, Harry E. (Portland, Cumberland County)

https://digitalmaine.com/alien_docs/21518/thumbnail.jp

Alien Registration- Johnston, Harry E. (Portland, Cumberland County)

https://digitalmaine.com/alien_docs/21518/thumbnail.jp

Does early surgery improve outcomes for periprosthetic fractures of the hip and knee? : A systematic review and meta-analysis

Open access via Springer Compact AgreementPeer reviewedPublisher PD

Intrinsic correlations of galaxy sizes in a hydrodynamical cosmological simulation

Residuals between measured galactic radii and those predicted by the Fundamental Plane (FP) are possible tracers of weak lensing magnification. However, observations have shown these to be systematically correlated with the large-scale structure. We use the Horizon-AGN hydrodynamical cosmological simulation to analyse these intrinsic size correlations (ISCs) for both elliptical (early-type) and spiral (late-type) galaxies at $z=0.06$. We fit separate FPs to each sample, finding similarly distributed radius residuals, $\lambda$, in each case. We find persistent $\lambda\lambda$ correlations over three-dimensional separations $0.5-17\,h^{-1}{\rm{Mpc}}$ in the case of spiral galaxies, at $>3\sigma$ significance. When relaxing a mass-selection, applied for better agreement with galaxy clustering constraints, the spiral $\lambda\lambda$ detection strengthens to $9\sigma$; we detect a $5\sigma$ density-$\lambda$ correlation; and we observe intrinsically-large spirals to cluster more strongly than small spirals over scales $\lesssim10\,h^{-1}{\rm{Mpc}}$, at $>5\sigma$ significance. Conversely, and in agreement with the literature, we observe lower-mass, intrinsically-small ellipticals to cluster more strongly than their large counterparts over scales $0.5-17\,h^{-1}{\rm{Mpc}}$, at $>5\sigma$ significance. We model $\lambda\lambda$ correlations using a phenomenological non-linear size model, and predict the level of contamination for cosmic convergence analyses. We find the systematic contribution to be of similar order to, or dominant over the cosmological signal. We make a mock measurement of an intrinsic, systematic contribution to the projected surface mass density $\Sigma(r)$ and find statistically significant, low-amplitude, positive (negative) contributions from lower-mass spirals (ellipticals), which may be of concern for large-scale ($\gtrsim\,7\,h^{-1}$ Mpc) measurements.Comment: 23 pages, 10 figures (2 pages, 4 figures in appendix), submitted to MNRA

Intrinsic correlations of galaxy sizes in a hydrodynamical cosmological simulation

Residuals between measured galactic radii and those predicted by the Fundamental Plane (FP) are possible tracers of weak lensing magnification. However, observations have shown these to be systematically correlated with the large-scale structure. We use the Horizon-AGN hydrodynamical cosmological simulation to analyse these intrinsic size correlations (ISCs) for both elliptical (early-type) and spiral (late-type) galaxies at z = 0.06. We fit separate FPs to each sample, finding similarly distributed radius residuals, λ, in each case. We find persistent λλ correlations over three-dimensional separations 0.5–17h−1 Mpc in the case of spiral galaxies, at >3σ significance. When relaxing a mass-selection, applied for better agreement with galaxy clustering constraints, the spiral λλ detection strengthens to 9σ; we detect a 5σ density-λ correlation; and we observe intrinsically-large spirals to cluster more strongly than small spirals over scales ≲10h−1 Mpc at >5σ significance. Conversely, and in agreement with the literature, we observe lower-mass, intrinsically-small ellipticals to cluster more strongly than their large counterparts over scales 0.5–17h−1 Mpc at >5σ significance. We model λλ correlations using a phenomenological non-linear size model, and predict the level of contamination for cosmic convergence analyses. We find the systematic contribution to be of similar order to, or dominant over the cosmological signal. We make a mock measurement of an intrinsic, systematic contribution to the projected surface mass density Σ(r), and find statistically significant low-amplitude, positive (negative) contributions from lower-mass spirals (ellipticals), which may be of concern for large-scale (⁠≳7h−1 Mpc) measurements