Publications

4.1 Research Agenda: NEBULA Data Plane (NDP)................................................................................ 5 4.2 What is NDP?.................................................................................................................................... 6 Figure 1: NDP packet format....................................................................................................................... 7 4.3 What properties does NDP uphold?............................................................................................... 7

We recently described a new method to determine total body creatine pool size and skeletal muscle mass based on dilution of an oral dose of D 3 ‐creatine in urinary creatinine. Enrichment of D 3 ‐ creatinine was measured by isotope ratio mass spectrometry. Here we adapt the method to LC‐MS/MS, and investigate the potential for repeated application over time. Rats were given an oral tracer dose of D 3 ‐creatine (1.0 mg/kg body weight) at 10 weeks of age. Urine D 3 ‐creatinine enrichment was determined 72 hr after tracer administration and creatine pool size was calculated. Lean body mass (LBM) measured by quantitative magnetic resonance correlated with creatine pool size ( r = 0.92, P = 0.0002). The rate constant for decline in urinary D 3 ‐creatinine enrichment was slow and linear (2.73 ± 0.06 %/day). Subtracting background urinary D 3 ‐creatinine enrichment from the enrichment following a second dose of D 3 ‐creatine at 17 weeks permitted repeat calculations of creatine pool size. As at 10 weeks, 17 week LBM correlated with creatine pool size ( r = 0.98, P < 0.0001). In addition, the change in creatine pool size was correlated with the change in LBM during the 7 weeks of somatic growth between measurements ( r = 0.96, P < 0.0001). Thus, the LC‐MS/MS‐based D 3 ‐creatine dilution method can be applied repeatedly to measure skeletal muscle mass change in longitudinal studies. These studies were funded by GlaxoSmithKline.

Playing Fields presents the profound reflections of a group of international scholars on how games, sports, and motor practices interact with global-local processes, inequality, gender relations, identity, representation, performance, and emotion through varied modes of analysis, approaches, and styles.

We present the synthesis, properties, and biological applications of Peroxyfluor-1 (PF1), a new type of optical probe for intracellular imaging of hydrogen peroxide in living biological samples. PF1 utilizes a boronate deprotection mechanism to provide unprecedented selectivity and optical dynamic range for detecting H2O2 in aqueous solution over similar reactive oxygen species including superoxide, nitric oxide, tert-butyl hydroperoxide, and hydroxyl radical. We further demonstrate the value of this reagent for biological applications by imaging changes in [H2O2] in living mammalian cells.

An emerging challenge in modern distributed querying is to efficiently process multiple continuous aggregation queries simultaneously. Processing each query independently may be infeasible, so multi-query optimizations are critical for sharing work across queries. The challenge is to identify overlapping computations that may not be obvious in the queries themselves. In this paper, we reveal new opportunities for sharing work in the context of distributed aggregation queries that vary in their selection predicates. We identify settings in which a large set of q such queries can be answered by executing k . The k queries are revealed by analyzing a boolean matrix capturing the connection between data and the queries that they satisfy, in a manner akin to familiar techniques like Gaussian elimination. Indeed, we identify a class of linear aggregate functions (including SUM, COUNT and AVERAGE), and show that the sharing potential for such queries can be optimally recovered using standard matrix decompositions from computational linear algebra. For some other typical aggregation functions (including MIN and MAX) we find that optimal sharing maps to the NP-hard set basis problem. However, for those scenarios, we present a family of heuristic algorithms and demonstrate that they perform well for moderate-sized matrices. We also present a dynamic distributed system architecture to exploit sharing opportunities, and experimentally evaluate the benefits of our techniques via a novel, flexible random workload generator we develop for this setting.

An entry from the Cambridge Structural Database, the world’s repository for small molecule crystal structures. The entry contains experimental data from a crystal diffraction study. The deposited dataset for this entry is freely available from the CCDC and typically includes 3D coordinates, cell parameters, space group, experimental conditions and quality measures.

Much excitement surrounds the intense mass loss that seems to take place in some massive stars immediately before core collapse. However, occurring too late, it has a negligible impact on the star's evolution or the final yields, which are influenced instead by the longer-term, quasi-steady mass loss taking place during H and He burning. Late-time observations of core-collapse supernovae interacting with the progenitor wind are one means to constrain this secular mass loss. Here, we present radiative transfer calculations for a Type II SN with and without this interaction power, focusing on the phase between 350 and 1000d after explosion. Without interaction power, the ejecta are powered through radioactive decay whose exponential decline produces an ever-fading SN. Instead, with a constant interaction power of $10^{40}$ erg s$^{-1}$ (representative of an SN II ramming into a steady-state $10^{-6} M_\odot$ yr$^{-1}$ wind), the spectrum morphs from decay powered at 350d, with narrow lines forming in the inner metal-rich ejecta, to interaction powered at 1000d, with broad boxy lines forming in the outer H-rich ejecta. Intermediate times are characterized by a hybrid and complex spectrum made of overlapping narrow and broad lines. While interaction boosts primarily the flux in the ultraviolet, which remains largely unobserved today, a knee in the $R$-band light curve or a $U$-band boost are clear signatures of interaction at late times. The model predictions compare favorably with a number of Type II supernovae including SN 2004et or SN 2017eaw at 500-1000d after explosion.

Herein we analyse late-time (post-plateau; 103 < t < 1229 d) optical spectra of low-redshift (z < 0.016), hydrogen-rich Type IIP supernovae (SNe IIP). Our newly constructed sample contains 91 nebular spectra of 38 SNe IIP, which is the largest dataset of its kind ever analysed in one study, and many of the objects have complementary photometric data. We determined the peak and total luminosity, velocity of the peak, HWHM intensity, and profile shape for many emission lines. Temporal evolution of these values and various flux ratios are studied. We also investigate the correlations between these measurements and photometric observables, such as the peak and plateau absolute magnitudes and the late-time light curve decline rates in various optical bands. The strongest and most robust result we find is that the luminosities of all spectral features (except those of helium) tend to be higher in objects with steeper late-time V-band decline rates. A steep late-time V-band slope likely arises from less efficient trapping of gamma-rays and positrons, which could be caused by multidimensional effects such as clumping of the ejecta or asphericity of the explosion itself. Furthermore, if gamma-rays and positrons can escape more easily, then so can photons via the observed emission lines, leading to more luminous spectral features. It is also shown that SNe IIP with larger progenitor stars have ejecta with a more physically extended oxygen layer that is well-mixed with the hydrogen layer. In addition, we find a subset of objects with evidence for asymmetric Ni-56 ejection, likely bipolar in shape. We also compare our observations to theoretical late-time spectral models of SNe IIP from two separate groups and find moderate-to-good agreement with both sets of models. Our SNe IIP spectra are consistent with models of 12-15 M_Sun progenitor stars having relatively low metallicity (Z $\le$ 0.01).

&lt;p&gt;PDF file - 226K, Relative Abundance of Indicator Bacterial Phylotypes in Mice Fecal bacteria of age- and litter-matched SPF-N and SPF-S mice (n = 4-5 for each type) were subjected to an indicator analysis.&lt;/p&gt;