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PM2.5 and PM10 Mass Measurements in California's San Joaquin Valley
Chow, Judith C.,Watson, John G.,Lowenthal, Douglas H.,Chen, L. -W. Antony,Tropp, Richard J.,Park, Kihong,Magliano, Karen A. Taylor Francis 2006 AEROSOL SCIENCE AND TECHNOLOGY Vol.40 No.10
<P> PM2.5 and PM10 mass measurements from different sampling systems and locations within California's San Joaquin Valley (SJV) are compared to determine how well mass concentrations from a unified data set can be used to address issues such as compliance with particulate matter (PM) standards, temporal and spatial variations, and model predictions. Pairwise comparisons were conducted among 20 samplers, including four Federal Reference Method (FRM) units, battery-powered MiniVols, sequential filter samplers, dichotomous samplers, Micro-Orifice Uniform Deposit Impactors (MOUDIs), beta attenuation monitors (BAMs), tapered element oscillating microbalances (TEOMs), and nephelometers. The differences between FRM samplers were less than 10 and 20% for 70 and 92% of the pairwise comparisons, respectively. The TEOM, operating at 50°C in this study, measured less than the other samplers, consistent with other comparisons in nitrate-rich atmospheres. PM2.5 mass measured continuously with the BAM was highly correlated with filter-based PM2.5 although the absolute bias was greater than 20% in 45% of the cases. Light scattering (Bsp) was also highly correlated with filter-based PM2.5 at most sites, with mass scattering efficiencies varying by 10 and 20% for Bsp measured with Radiance Research nephelometers with and without PM2.5 size-selective inlets, respectively. Collocating continuous monitors with filter samplers was shown to be useful for evaluating short-term variability and identifying outliers in the filter-based measurements. Comparability among different PM samplers used in CRPAQS is sufficient to evaluate spatial gradients larger than about 15% when the data are pooled together for spatial and temporal analysis and comparison with models.</P>
Austermann, J. E.,Aretxaga, I.,Hughes, D. H.,Kang, Y.,Kim, S.,Lowenthal, J. D.,Perera, T. A.,Sanders, D. B.,Scott, K. S.,Scoville, N.,Wilson, G. W.,Yun, M. S. Blackwell Publishing Ltd 2009 Monthly notices of the Royal Astronomical Society Vol.393 No.4
<P>ABSTRACT</P><P>We report an overdensity of bright submillimetre galaxies (SMGs) in the 0.15 deg<SUP>2</SUP> AzTEC/COSMOS survey and a spatial correlation between the SMGs and the optical-IR galaxy density at <I>z</I>≲ 1.1. This portion of the COSMOS field shows a ∼3σ overdensity of robust SMG detections when compared to a background, or ‘blank-field’, population model that is consistent with SMG surveys of fields with no extragalactic bias. The SMG overdensity is most significant in the number of very bright detections (14 sources with measured fluxes <I>S</I><SUB>1.1 mm</SUB> > 6 mJy), which is entirely incompatible with sample variance within our adopted blank-field number densities and infers an overdensity significance of ≫ 4σ. We find that the overdensity and spatial correlation to optical-IR galaxy density are most consistent with lensing of a background SMG population by foreground mass structures along the line of sight, rather than physical association of the SMGs with the <I>z</I>≲ 1.1 galaxies/clusters. The SMG positions are only weakly correlated with weak-lensing maps, suggesting that the dominant sources of correlation are individual galaxies and the more tenuous structures in the survey region, and not the massive and compact clusters. These results highlight the important roles cosmic variance and large-scale structure can play in the study of SMGs.</P>
X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution
Johnson, S. P.,Wilson, G. W.,Wang, Q. D.,Williams, C. C.,Scott, K. S.,Yun, M. S.,Pope, A.,Lowenthal, J.,Aretxaga, I.,Hughes, D. Oxford University Press 2013 Monthly notices of the Royal Astronomical Society Vol.431 No.1
Cheng, Ann-Lii,Kang, Yoon-Koo,Lin, Deng-Yn,Park, Joong-Won,Kudo, Masatoshi,Qin, Shukui,Chung, Hyun-Cheol,Song, Xiangqun,Xu, Jianming,Poggi, Guido,Omata, Masao,Pitman Lowenthal, Susan,Lanzalone, Silvan American Society for Clinical Oncology 2013 Journal of clinical oncology Vol.31 No.32
<P><B>Purpose</B></P><P>Open-label, phase III trial evaluating whether sunitinib was superior or equivalent to sorafenib in hepatocellular cancer.</P><P><B>Patients and Methods</B></P><P>Patients were stratified and randomly assigned to receive sunitinib 37.5 mg once per day or sorafenib 400 mg twice per day. Primary end point was overall survival (OS).</P><P><B>Results</B></P><P>Early trial termination occurred for futility and safety reasons. A total of 1,074 patients were randomly assigned to the study (sunitinib arm, n = 530; sorafenib arm, n = 544). For sunitinib and sorafenib, respectively, median OS was 7.9 versus 10.2 months (hazard ratio [HR], 1.30; one-sided <I>P</I> = .9990; two-sided <I>P</I> = .0014); median progression-free survival (PFS; 3.6 <I>v</I> 3.0 months; HR, 1.13; one-sided <I>P</I> = .8785; two-sided <I>P</I> = .2286) and time to progression (TTP; 4.1 <I>v</I> 3.8 months; HR, 1.13; one-sided <I>P</I> = .8312; two-sided <I>P</I> = .3082) were comparable. Median OS was similar among Asian (7.7 <I>v</I> 8.8 months; HR, 1.21; one-sided <I>P</I> = .9829) and hepatitis B–infected patients (7.6 <I>v</I> 8.0 months; HR, 1.10; one-sided <I>P</I> = .8286), but was shorter with sunitinib in hepatitis C–infected patients (9.2 <I>v</I> 17.6 months; HR, 1.52; one-sided <I>P</I> = .9835). Sunitinib was associated with more frequent and severe adverse events (AEs) than sorafenib. Common grade 3/4 AEs were thrombocytopenia (29.7%) and neutropenia (25.7%) for sunitinib; hand-foot syndrome (21.2%) for sorafenib. Discontinuations owing to AEs were similar (sunitinib, 13.3%; sorafenib, 12.7%).</P><P><B>Conclusion</B></P><P>OS with sunitinib was not superior or equivalent but was significantly inferior to sorafenib. OS was comparable in Asian and hepatitis B–infected patients. OS was superior in hepatitis C–infected patients who received sorafenib. Sunitinib-treated patients reported more frequent and severe toxicity.</P>
The source counts of submillimetre galaxies detected at λ= 1.1 mm
Scott, K. S.,Wilson, G. W.,Aretxaga, I.,Austermann, J. E.,Chapin, E. L.,Dunlop, J. S.,Ezawa, H.,Halpern, M.,Hatsukade, B.,Hughes, D. H.,Kawabe, R.,Kim, S.,Kohno, K.,Lowenthal, J. D.,Montañ,a, A. Blackwell Publishing Ltd 2012 Monthly notices of the Royal Astronomical Society Vol.423 No.1
<P><B>ABSTRACT</B></P><P>The source counts of galaxies discovered at submillimetre and millimetre wavelengths provide important information on the evolution of infrared‐bright galaxies. We combine the data from six blank‐field surveys carried out at 1.1 mm with AzTEC, totalling 1.6 deg<SUP>2</SUP> in area with root‐mean‐square depths ranging from 0.4 to 1.7 mJy, and derive the strongest constraints to date on the 1.1 mm source counts at flux densities <I>S</I><SUB>1100</SUB>= 1–12 mJy. Using additional data from the AzTEC Cluster Environment Survey to extend the counts to <I>S</I><SUB>1100</SUB>∼ 20 mJy, we see tentative evidence for an enhancement relative to the exponential drop in the counts at <I>S</I><SUB>1100</SUB>∼ 13 mJy and a smooth connection to the bright source counts at >20 mJy measured by the South Pole Telescope; this excess may be due to strong‐lensing effects. We compare these counts to predictions from several semi‐analytical and phenomenological models and find that for most the agreement is quite good at flux densities ≳ 4 mJy; however, we find significant discrepancies (≳ 3σ) between the models and the observed 1.1‐mm counts at lower flux densities, and none of them is consistent with the observed turnover in the Euclidean‐normalized counts at <I>S</I><SUB>1100</SUB>≲ 2 mJy. Our new results therefore may require modifications to existing evolutionary models for low‐luminosity galaxies. Alternatively, the discrepancy between the measured counts at the faint end and predictions from phenomenological models could arise from limited knowledge of the spectral energy distributions of faint galaxies in the local Universe.</P>