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1. An emission-state-switching radio transient with a 54-minute period

Author

Caleb, M., Lenc, E., Kaplan, D. L., Murphy, T., Men, Y. P., Shannon, R. M., Ferrario, L., Rajwade, K. M., Clarke, T. E., Giacintucci, S., Hurley-Walker, N., Hyman, S. D., Lower, M. E., McSweeney, Sam, Ravi, V., Barr, E. D., Buchner, S., Flynn, C. M. L., Hessels, J. W. T., Kramer, M., Pritchard, J., and Stappers, B. W.

Published
2024
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2. Genetic loci regulating the concentrations of anthocyanins and proanthocyanidins in the pericarps of purple and red rice

Author

Ming‐Hsuan Chen, Shannon R. M. Pinson, Aaron K. Jackson, and Jeremy D. Edwards

Subjects
Plant culture, SB1-1110, Genetics, QH426-470
Abstract

Abstract The pigmented flavonoids, anthocyanins and proanthocyanidins, have health promoting properties. Previous work determined that the genes Pb and Rc turn on and off the biosynthesis of anthocyanins (purple) and proanthocyanidins (red), respectively. Not yet known is how the concentrations of these pigmented flavonoids are regulated in grain pericarps. Quantitative trait locus (QTL) analysis in a population of rice (Oryza sativa L.) F5 recombinant inbred lines from white pericarp “IR36ae” x red+purple pericarp “242” revealed three QTLs associated with grain concentrations of anthocyanins (TAC) or proanthocyanidins (PA). Both TAC and PA independently mapped to a 1.5 Mb QTL region on chromosome 3 between RM3400 (at 15.8 Mb) and RM15123 (17.3 Mb), named qPR3. Across 2 years, qPR3 explained 36.3% of variance in TAC and 35.8% in PA variance not attributable to Pb or Rc. The qPR3 region encompasses Kala3, a MYB transcription factor previously known to regulate purple grain characteristics. Study of PbPbRcrc progeny showed that TAC of RcRc near isogenic lines (NILs) was 2.1–4.5x that of rcrc. Similarly, study of PbPbRcRc NILs, which had 70% higher PA than pbpbRcRc NILs, revealed a mutual enhancement, not a trade‐off between these compounds that share precursors. This suggests that Pb and Rc upregulate genes in a shared pathway as they activate TAC and PA synthesis, respectively. This study provides molecular markers for facilitating marker‐assisted selection of qPR3, qPR5, and qPR7 to enhance grain concentrations of pigmented flavonoids and documented that stacking Rc and Pb genes further increases both flavonoid compounds.

Published
2023
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3. Investigating the Malting Suitability and Brewing Quality of Different Rice Cultivars

Author

Bernardo P. Guimaraes, Florian Schrickel, Nils Rettberg, Shannon R. M. Pinson, Anna M. McClung, Kaushik Luthra, Griffiths G. Atungulu, Xueyan Sha, Christian de Guzman, and Scott Lafontaine

Subjects
rice varieties, malt, rice malt, gluten free, beer, Nutrition. Foods and food supply, TX341-641, Nutritional diseases. Deficiency diseases, RC620-627
Abstract

Nineteen globally diverse rice cultivars were analyzed for various chemical parameters important to malting, including germination energy, protein, apparent amylose content, and gelatinization temperatures (GT). The rice cultivars were then malted, and congress mashes were produced. Several parameters important to brewing were then assessed in the malts and worts (i.e., extract, soluble protein, free amino nitrogen (FAN), GT, etc.). The rice malts produced were saccharified to varying degrees, had high limit dextrinase activities, and contained sufficient FAN/protein concentrations. This suggests their potential to yield robust fermentations in beer styles with high adjunct inclusions without requiring additional nitrogen supplementation. Rice cultivars with purple-pigmented bran were found to yield unique wort colors and could serve as novel natural gluten-free colorants for future recipes. Overall, these findings suggest that malted rice could offer a more local and gluten-free source of starch for brewers and beverage/food producers.

Published
2024
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4. Identification of quantitative trait loci for tillering, root, and shoot biomass at the maximum tillering stage in rice

Author

Jinyoung Y. Barnaby, Anna M. McClung, Jeremy D. Edwards, and Shannon R. M. Pinson

Subjects
Medicine, Science
Abstract

Abstract Tillering and plant biomass are key determinants of rice crop productivity. Tillering at the vegetative stage is associated with weed competition, nutrient uptake, and methane emissions. However, little information is available on quantitative trait loci (QTLs) associated with tiller number (qTN), root biomass (qRB), and shoot biomass (qSB) at the active tillering stage which occurs approximately 6 weeks after planting. Here, we mapped tiller and biomass QTLs with ~ 250 recombinant inbred lines derived from a ‘Francis’ by ‘Rondo’ cross using data collected at the maximum tillering stage from two years of greenhouse study, and further compared these QTLs with those mapped at the harvest stage from a field study. Across these three studies, we discovered six qTNs, two qRBs, and three qSBs. Multiple linear regression further indicated that qTN1-2, qTN3-3, qTN4-1, qRB3-1, and qRB5-1 were significant at the maximum tillering stage while qTN3-2 was detected only at the harvest stage. Moreover, qTN3-1 was consistently significant across different developmental stages and growing environments. The genes identified from the peak target qTN regions included a carotenoid metabolism enzyme, a MYB transcription factor, a CBS domain-containing protein, a SAC3/GANP family protein, a TIFY motif containing protein, and an ABC transporter protein. Two genes in the qRB peak target regions included an expressed protein and a WRKY gene. This knowledge of the QTLs, associated markers, candidate genes, and germplasm resources with high TN, RB and SB is of value to rice cultivar improvement programs.

Published
2022
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5. Assessment of Rice Sheath Blight Resistance Including Associations with Plant Architecture, as Revealed by Genome-Wide Association Studies

Author

Danting Li, Fantao Zhang, Shannon R. M. Pinson, Jeremy D. Edwards, Aaron K. Jackson, Xiuzhong Xia, and Georgia C. Eizenga

Subjects
Rice, Sheath blight disease, Genome-wide association mapping, Tillering, Rhizoctonia solani, Oryza sativa, Plant culture, SB1-1110
Abstract

Abstract Background Sheath blight (ShB) disease caused by Rhizoctonia solani Kühn, is one of the most economically damaging rice (Oryza sativa L.) diseases worldwide. There are no known major resistance genes, leaving only partial resistance from small-effect QTL to deploy for cultivar improvement. Many ShB-QTL are associated with plant architectural traits detrimental to yield, including tall plants, late maturity, or open canopy from few or procumbent tillers, which confound detection of physiological resistance. Results To identify QTL for ShB resistance, 417 accessions from the Rice Diversity Panel 1 (RDP1), developed for association mapping studies, were evaluated for ShB resistance, plant height and days to heading in inoculated field plots in Arkansas, USA (AR) and Nanning, China (NC). Inoculated greenhouse-grown plants were used to evaluate ShB using a seedling-stage method to eliminate effects from height or maturity, and tiller (TN) and panicle number (PN) per plant. Potted plants were used to evaluate the RDP1 for TN and PN. Genome-wide association (GWA) mapping with over 3.4 million SNPs identified 21 targeted SNP markers associated with ShB which tagged 18 ShB-QTL not associated with undesirable plant architecture traits. Ten SNPs were associated with ShB among accessions of the Indica subspecies, ten among Japonica subspecies accessions, and one among all RDP1 accessions. Across the 18 ShB QTL, only qShB4-1 was not previously reported in biparental mapping studies and qShB9 was not reported in the GWA ShB studies. All 14 PN QTL overlapped with TN QTL, with 15 total TN QTL identified. Allele effects at the five TN QTL co-located with ShB QTL indicated that increased TN does not inevitably increase disease development; in fact, for four ShB QTL that overlapped TN QTL, the alleles increasing resistance were associated with increased TN and PN, suggesting a desirable coupling of alleles at linked genes. Conclusions Nineteen accessions identified as containing the most SNP alleles associated with ShB resistance for each subpopulation were resistant in both AR and NC field trials. Rice breeders can utilize these accessions and SNPs to develop cultivars with enhanced ShB resistance along with increased TN and PN for improved yield potential.

Published
2022
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8. MeerKAT observations of pair-plasma induced birefringence in the double pulsar eclipses.

Author

Lower, M E, Kramer, M, Johnston, S, Breton, R P, Wex, N, Bailes, M, Buchner, S, Camilo, F, Oswald, L S, Reardon, D J, Shannon, R M, Serylak, M, and Krishnan, V Venkatraman

Abstract

PSR J0737−3039A/B is unique among double neutron star systems. Its near-perfect edge-on orbit causes the fast spinning pulsar A to be eclipsed by the magnetic field of the slow spinning pulsar B. Using high-sensitivity MeerKAT radio observations combined with updated constraints on the system geometry, we studied the impact of these eclipses on the incident polarization properties of pulsar A. Averaging light curves together after correcting for the rotation of pulsar B revealed enormous amounts of circular polarization and rapid changes in the linear polarization position angle, which occur at phases where emission from pulsar A is partially transmitted through the magnetosphere of pulsar B. These behaviours confirm that the eclipse mechanism is the result of synchrotron absorption in a relativistic pair-plasma confined to the closed-field region of pulsar B's truncated dipolar magnetic field. We demonstrate that changes in circular polarization handedness throughout the eclipses are directly tied to the average line of sight magnetic field direction of pulsar B, from which we unambiguously determine the complete magnetic and viewing geometry of the pulsar. [ABSTRACT FROM AUTHOR]

Published
2024
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10. Relationships Among Arsenic-Related Traits, Including Rice Grain Arsenic Concentration and Straighthead Resistance, as Revealed by Genome-Wide Association

Author

Shannon R. M. Pinson, D. Jo Heuschele, Jeremy D. Edwards, Aaron K. Jackson, Santosh Sharma, and Jinyoung Y. Barnaby

Subjects
rice, arsenic, straighthead disorder, genome-wide association, bayesian network, QTL, Genetics, QH426-470
Abstract

There is global concern that rice grains and foods can contain harmful amounts of arsenic (As), motivating breeders to produce cultivars that restrict As accumulation in grains to protect human health. Arsenic is also toxic to plants, with straighthead disorder (StHD), causing panicle sterility, being observed in rice. The genetic variation in StHD resistance suggests that plants have evolved mechanisms that reduce As toxicity, possibly via regulation of As uptake, transport, or detoxification/sequestration. Because these mechanisms could also underlie the wide (3- to 100-fold) differences in grain As concentration (grain-As) observed among diverse rice genotypes, it was hypothesized that some genes reduce both grain-As content and StHD susceptibility and may be detectable as co-located StDH and As quantitative trait loci (QTL). We used a machine-learning Bayesian network approach plus high-resolution genome-wide association study (GWAS) to identify QTL for grain-As and StHD resistance within the USDA Rice Minicore Collection (RMC). Arsenic enters roots through phosphorus (P) and silica (Si) transporters, As detoxification involves sulfur (S), and cell signaling to activate stress tolerance mechanisms is impacted by Si, calcium (Ca), and copper (Cu). Therefore, concentrations of Si, P, S, Ca, and Cu were included in this study to elucidate physiological mechanisms underlying grain-As and StHD QTL. Multiple QTL (from 9 to 33) were identified for each of the investigated As-associated traits. Although the QTL for StHD, Si, and grain-As did not overlap as heavily as our hypothesis predicted (4/33 StHD and 4/15 As QTL co-located), they do provide useful guidance to future research. Furthermore, these are the first StHD and Si QTL to be identified using high-density mapping, resulting in their being mapped to shorter, more precise genomic regions than previously reported QTL. The candidate genes identified provide guidance for future research, such as gene editing or mutation studies to further investigate the role of antioxidants and ROS scavenging to StHD resistance, as indicated by candidate genes around the commonly reported qStHD8-2 QTL. Other genes indicated for future study for improving grain-As and StHD include several multidrug and toxic compound extrusion (MATE) genes, F-box genes, and NIPs not documented to date to transport As.

Published
2022
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12. Genome-wide association studies of ionomic and agronomic traits in USDA mini core collection of rice and comparative analyses of different mapping methods

Author

Shuai Liu, Hua Zhong, Xiaoxi Meng, Tong Sun, Yangsheng Li, Shannon R. M. Pinson, Sam K. C. Chang, and Zhaohua Peng

Subjects
Rice, Ionomic traits, Agronomic traits, Multivariate GWAS, Botany, QK1-989
Abstract

Abstract Background Rice is an important human staple food vulnerable to heavy metal contamination leading to serious concerns. High yield with low heavy metal contamination is a common but highly challenging goal for rice breeders worldwide due to lack of genetic knowledge and markers. Results To identify candidate QTLs and develop molecular markers for rice yield and heavy metal content, a total of 191 accessions from the USDA Rice mini-core collection with over 3.2 million SNPs were employed to investigate the QTLs. Sixteen ionomic and thirteen agronomic traits were analyzed utilizing two univariate (GLM and MLM) and two multivariate (MLMM and FarmCPU) GWAS methods. 106, 47, and 97 QTLs were identified for ionomics flooded, ionomics unflooded, and agronomic traits, respectively, with the criterium of p-value

Published
2020
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14. Socio-Technical Changes for Sustainable Rice Production: Rice Husk Amendment, Conservation Irrigation, and System Changes

Author

Benjamin R. K. Runkle, Angelia L. Seyfferth, Matthew C. Reid, Matthew A. Limmer, Beatriz Moreno-García, Colby W. Reavis, Jasquelin Peña, Michele L. Reba, M. Arlene A. Adviento-Borbe, Shannon R. M. Pinson, and Chris Isbell

Subjects
rice, sustainability, circular food system, conservation agriculture, grain quality, silicon, Agriculture, Plant culture, SB1-1110
Abstract

Rice is a staple food and primary source of calories for much of the world. However, rice can be a dietary source of toxic metal(loid)s to humans, and its cultivation creates atmospheric greenhouse gas emissions and requires high water use. Because rice production consumes a significant amount of natural resources and is a large part of the global agricultural economy, increasing its sustainability could have substantial societal benefits. There are opportunities for more sustainable field production through a combination of silicon (Si) management and conservation irrigation practices. As a Si-rich soil amendment, rice husks can limit arsenic and cadmium uptake, while also providing plant vigor in drier soil conditions. Thus, husk addition and conservation irrigation may be more effective to attenuate the accumulation of toxic metal(loid)s, manage water usage and lower climate impacts when implemented together than when either is implemented separately. This modified field production system would take advantage of rice husks, which are an underutilized by-product of milled rice that is widely available near rice farm sites, and have ~10% Si content. Husk application could, alongside alternate wetting and drying or furrow irrigation management, help resolve multiple sustainability challenges in rice production: (1) limit arsenic and cadmium accumulation in rice; (2) minimize greenhouse gas emissions from rice production; (3) decrease irrigation water use; (4) improve nutrient use efficiency; (5) utilize a waste product of rice processing; and (6) maintain plant-accessible soil Si levels. This review presents the scientific basis for a shift in rice production practices and considers complementary rice breeding efforts. It then examines socio-technical considerations for how such a shift in production practices could be implemented by farmers and millers together and may bring rice production closer to a bio-circular economy. This paper's purpose is to advocate for a changed rice production method for consideration by community stakeholders, including producers, millers, breeders, extension specialists, supply chain organizations, and consumers, while highlighting remaining research and implementation questions.

Published
2021
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15. MeerKAT Pulsar Timing Array parallaxes and proper motions.

Author

Shamohammadi, M, Bailes, M, Flynn, C, Reardon, D J, Shannon, R M, Buchner, S, Cameron, A D, Camilo, F, Coronigu, A, Geyer, M, Kramer, M, Miles, M, and Spiewak, R

Subjects
ORBITAL velocity, PULSARS, MEERKAT, GLOBULAR clusters, PARALLAX, RADIO telescopes, VELOCITY
Abstract

We have determined positions, proper motions, and parallaxes of 77 millisecond pulsars (MSPs) from ∼3 yr of MeerKAT radio telescope observations. Our timing and noise analyses enable us to measure 35 significant parallaxes (12 of them for the first time) and 69 significant proper motions. Eight pulsars near the ecliptic have an accurate proper motion in ecliptic longitude only. PSR J0955−6150 has a good upper limit on its very small proper motion (<0.4 mas yr−1). We used pulsars with accurate parallaxes to study the MSP velocities. This yields 39 MSP transverse velocities, and combined with MSPs in the literature (excluding those in Globular Clusters) we analyse 66 MSPs in total. We find that MSPs have, on average, much lower velocities than normal pulsars, with a mean transverse velocity of only 78(8) km s−1 (MSPs) compared with 246(21) km s−1 (normal pulsars). We found no statistical differences between the velocity distributions of isolated and binary MSPs. From Galactocentric cylindrical velocities of the MSPs, we derive 3D velocity dispersions of σρ, σϕ, σ z  = 63(11), 48(8), 19(3) km s−1. We measure a mean asymmetric drift with amplitude 38(11) km s−1, consistent with expectation for MSPs, given their velocity dispersions and ages. The MSP velocity distribution is consistent with binary evolution models that predict very few MSPs with velocities >300 km s−1 and a mild anticorrelation of transverse velocity with orbital period. [ABSTRACT FROM AUTHOR]

Published
2024
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16. Investigating the Malting Suitability and Brewing Quality of Different Rice Cultivars.

Author

Guimaraes, Bernardo P., Schrickel, Florian, Rettberg, Nils, Pinson, Shannon R. M., McClung, Anna M., Luthra, Kaushik, Atungulu, Griffiths G., Sha, Xueyan, de Guzman, Christian, and Lafontaine, Scott

Subjects
MALTING, RICE quality, CULTIVARS, RICE products, RICE starch, PULLULANASE, OLIVE oil, MALT
Abstract

Nineteen globally diverse rice cultivars were analyzed for various chemical parameters important to malting, including germination energy, protein, apparent amylose content, and gelatinization temperatures (GT). The rice cultivars were then malted, and congress mashes were produced. Several parameters important to brewing were then assessed in the malts and worts (i.e., extract, soluble protein, free amino nitrogen (FAN), GT, etc.). The rice malts produced were saccharified to varying degrees, had high limit dextrinase activities, and contained sufficient FAN/protein concentrations. This suggests their potential to yield robust fermentations in beer styles with high adjunct inclusions without requiring additional nitrogen supplementation. Rice cultivars with purple-pigmented bran were found to yield unique wort colors and could serve as novel natural gluten-free colorants for future recipes. Overall, these findings suggest that malted rice could offer a more local and gluten-free source of starch for brewers and beverage/food producers. [ABSTRACT FROM AUTHOR]

Published
2024
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17. Genomic prediction and QTL mapping of root system architecture and above-ground agronomic traits in rice (Oryza sativa L.) with a multitrait index and Bayesian networks

Author

Santosh Sharma, Shannon R M Pinson, David R Gealy, and Jeremy D Edwards

Subjects
Genetics, QH426-470
Abstract

AbstractRoot system architecture (RSA) is a crucial factor in resource acquisition and plant productivity. Roots are difficult to phenotype in the field, thus new tools for predicting phenotype from genotype are particularly valuable for plant breeders aiming to improve RSA. This study identifies quantitative trait loci (QTLs) for RSA and agronomic traits in a rice (Oryza sativa

Published
2021
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18. Univariate and Multivariate QTL Analyses Reveal Covariance Among Mineral Elements in the Rice Ionome

Author

Huan Liu, Su-Xian Long, Shannon R. M. Pinson, Zhong Tang, Mary Lou Guerinot, David E. Salt, Fang-Jie Zhao, and Xin-Yuan Huang

Subjects
Rice, ionome, mineral nutrient, QTL, principal component analysis, Genetics, QH426-470
Abstract

Rice provides more than one fifth of daily calories for half of the world’s human population, and is a major dietary source of both essential mineral nutrients and toxic elements. Rice grains are generally poor in some essential nutrients but may contain unsafe levels of some toxic elements under certain conditions. Identification of quantitative trait loci (QTLs) controlling the concentrations of mineral nutrients and toxic trace metals (the ionome) in rice will facilitate development of nutritionally improved rice varieties. However, QTL analyses have traditionally considered each element separately without considering their interrelatedness. In this study, we performed principal component analysis (PCA) and multivariate QTL analyses to identify the genetic loci controlling the covariance among mineral elements in the rice ionome. We resequenced the whole genomes of a rice recombinant inbred line (RIL) population, and performed univariate and multivariate QTL analyses for the concentrations of 16 elements in grains, shoots and roots of the RIL population grown in different conditions. We identified a total of 167 unique elemental QTLs based on analyses of individual elemental concentrations as separate traits, 53 QTLs controlling covariance among elemental concentrations within a single environment/tissue (PC-QTLs), and 152 QTLs which determined covariation among elements across environments/tissues (aPC-QTLs). The candidate genes underlying the QTL clusters with elemental QTLs, PC-QTLs and aPC-QTLs co-localized were identified, including OsHMA4 and OsNRAMP5. The identification of both elemental QTLs and PC QTLs will facilitate the cloning of underlying causal genes and the dissection of the complex regulation of the ionome in rice.

Published
2021
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22. An insight into chromatic behaviour of jitter in pulsars and its modelling: a case study of PSR J0437−4715.

Author

Kulkarni, A D, Shannon, R M, Reardon, D J, Miles, M T, Bailes, M, and Shamohammadi, M

Subjects
*PULSARS, *GRAVITATIONAL waves, *WHITE noise, *COVARIANCE matrices, *SURFACE waves (Seismic waves), *RADIO frequency
Abstract

Pulse-to-pulse profile shape variations introduce correlations in pulsar times of arrival across radio frequency measured at the same observational epoch. This leads to a broad-band noise in excess of radiometer noise, which is termed as pulse jitter noise. The presence of jitter noise limits the achievable timing precision and decreases the sensitivity of pulsar timing data sets to signals of interest such as nanohertz-frequency gravitational waves. Current white noise models used in pulsar timing analyses attempt to account for this, assuming complete correlation of uncertainties through the arrival times collected in a unique observation and no frequency dependence of jitter (which corresponds to a rank-one covariance matrix). However, previous studies show that the brightest millisecond pulsar at decimetre wavelengths, PSR J0437−4715, shows decorrelation and frequency dependence of jitter noise. Here, we present a detailed study of the decorrelation of jitter noise in PSR J0437−4715 and implement a new technique to model it. We show that the rate of decorrelation due to jitter can be expressed as a power law in frequency. We analyse the covariance matrix associated with the jitter noise process and find that a higher rank approximation is essential to account for the decorrelation and to account for frequency dependence of jitter noise. We show that the use of this novel method significantly improves the estimation of other chromatic noise parameters such as dispersion measure variations. However, we find no significant improvement in errors and estimation of other timing model parameters suggesting that current methods are not biased for other parameters, for this pulsar due to this misspecification. We show that pulse energy variations show a similar decorrelation to the jitter noise, indicating a common origin for both observables. [ABSTRACT FROM AUTHOR]

Published
2024
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23. The impact of the FREDDA dedispersion algorithm on H0 estimations with fast radio bursts.

Author

Hoffmann, J, James, C W, Qiu, H, Glowacki, M, Bannister, K W, Gupta, V, Prochaska, J X, Bera, A, Deller, A T, Gourdji, K, Marnoch, L, Ryder, S D, Scott, D R, Shannon, R M, and Tejos, N

Subjects
HUBBLE constant, POPULATION statistics, SIGNAL-to-noise ratio, SOLAR radio bursts, ALGORITHMS
Abstract

Fast radio bursts (FRBs) are transient radio signals of extragalactic origins that are subjected to propagation effects such as dispersion and scattering. It follows then that these signals hold information regarding the medium they have traversed and are hence useful as cosmological probes of the Universe. Recently, FRBs were used to make an independent measure of the Hubble constant H 0, promising to resolve the Hubble tension given a sufficient number of detected FRBs. Such cosmological studies are dependent on FRB population statistics, cosmological parameters, and detection biases, and thus it is important to accurately characterize each of these. In this work, we empirically characterize the sensitivity of the Fast Real-time Engine for Dedispersing Amplitudes (FREDDA) which is the current detection system for the Australian Square Kilometre Array Pathfinder (ASKAP). We coherently redisperse high-time resolution data of 13 ASKAP-detected FRBs and inject them into FREDDA to determine the recovered signal-to-noise ratios as a function of dispersion measure. We find that for 11 of the 13 FRBs, these results are consistent with injecting idealized pulses. Approximating this sensitivity function with theoretical predictions results in a systematic error of 0.3 km s−1 Mpc−1 on H 0 when it is the only free parameter. Allowing additional parameters to vary could increase this systematic by up to |$\sim 1\,$| km s−1 Mpc−1. We estimate that this systematic will not be relevant until ∼400 localized FRBs have been detected, but will likely be significant in resolving the Hubble tension. [ABSTRACT FROM AUTHOR]

Published
2024
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24. A MeerKAT view of the double pulsar eclipses: Geodetic precession of pulsar B and system geometry.

Author

Lower, M. E., Kramer, M., Shannon, R. M., Breton, R. P., Wex, N., Johnston, S., Bailes, M., Buchner, S., Hu, H., Venkatraman Krishnan, V., Blackmon, V. A., Camilo, F., Champion, D. J., Freire, P. C. C., Geyer, M., Karastergiou, A., van Leeuwen, J., McLaughlin, M. A., Reardon, D. J., and Stairs, I. H.

Subjects
PULSARS, NEUTRON stars, MEERKAT, LIGHT curves, GENERAL relativity (Physics)
Abstract

The double pulsar system, PSR J0737−3039A/B, consists of two neutron stars bound together in a highly relativistic orbit that is viewed nearly edge-on from the Earth. This alignment results in brief radio eclipses of the fast-rotating pulsar A when it passes behind the toroidal magnetosphere of the slow-rotating pulsar B. The morphology of these eclipses is strongly dependent on the geometric orientation and rotation phase of pulsar B, and their time evolution can be used to constrain the geodetic precession rate of the pulsar. We demonstrate a Bayesian inference framework for modelling high-sensitivity eclipse light curves obtained with MeerKAT between 2019 and 2023. Using a hierarchical inference approach, we obtained a precession rate of ΩSOB = 5.16°−0.34°+0.32° yr−1 (68% confidence intervals) for pulsar B, consistent with predictions from general relativity to a relative uncertainty of 6.5%. This updated measurement provides a 6.1% test of relativistic spin-orbit coupling in the strong-field regime. We show that a simultaneous fit to all of our observed eclipses can in principle return a ∼1.5% test of spin-orbit coupling. However, systematic effects introduced by the current geometric orientation of pulsar B along with inconsistencies between the observed and predicted eclipse light curves result in difficult to quantify uncertainties when using this approach. Assuming the validity of general relativity, we definitively show that the spin axis of pulsar B is misaligned from the total angular momentum vector by 40.6° ±0.1° and that the orbit of the system is inclined by approximately 90.5° from the direction of our line of sight. Our measured geometry for pulsar B suggests the largely empty emission cone contains an elongated horseshoe-shaped beam centred on the magnetic axis, and that it may not be re-detected as a radio pulsar until early 2035. [ABSTRACT FROM AUTHOR]

Published
2024
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25. The High Time Resolution Universe Pulsar survey – XVIII. The reprocessing of the HTRU-S Low Lat survey around the Galactic Centre using a Fast Folding Algorithm pipeline for accelerated pulsars.

Author

Wongphechauxsorn, J, Champion, D J, Bailes, M, Balakrishnan, V, Barr, E D, Bernadich, M C i, Bhat, N D R, Burgay, M, Cameron, A D, Chen, W, Flynn, C M L, Jameson, A, Johnston, S, Keith, M J, Kramer, M, Ng, C, Possenti, A, Sengar, R, Shannon, R M, and Stappers, B

Subjects
PULSAR detection, MAGNETIC flux density, FAST Fourier transforms, UNIVERSE, BINARY pulsars, LINEAR polarization, PULSARS
Abstract

The HTRU-S Low Latitude survey data within 1° of the Galactic Centre (GC) were searched for pulsars using the Fast Folding Algorithm (FFA). Unlike traditional Fast Fourier Transform (FFT) pipelines, the FFA optimally folds the data for all possible periods over a given range, which is particularly advantageous for pulsars with low-duty cycles. For the first time, a search over acceleration was included in the FFA to improve its sensitivity to binary pulsars. The steps in dispersion measure (DM) and acceleration were optimized, resulting in a reduction of the number of trials by 86 per cent. This was achieved over a search period range from 0.6 to 432-s, i.e. 10 per cent of the observation time (4320s), with a maximum DM of 4000 pc cm−3 and an acceleration range of ±128 m s−2. The search resulted in the re-detections of four known pulsars, including a pulsar that was missed in the previous FFT processing of this survey. This result indicates that the FFA pipeline is more sensitive than the FFT pipeline used in the previous processing of the survey within our parameter range. Additionally, we discovered a 1.89-s pulsar, PSR J1746-2829, with a large DM, located 0.5 from the GC. Follow-up observations revealed that this pulsar has a relatively flat spectrum (α = −0.9 ± 0.1) and has a period derivative of ∼1.3 × 10−12 s s−1, implying a surface magnetic field of ∼5.2 × 1013 G and a characteristic age of ∼23 000 yr. While the period, spectral index, and surface magnetic field strength are similar to many radio magnetars, other characteristics such as high linear polarization are absent. [ABSTRACT FROM AUTHOR]

Published
2024
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26. Spectropolarimetric variability in the repeating fast radio burst source FRB 20180301A.

Author

Kumar, P, Luo, R, Price, D C, Shannon, R M, Deller, A T, Bhandari, S, Feng, Y, Flynn, C, Jiang, J C, Uttarkar, P A, Wang, S Q, and Zhang, S B

Subjects
POLARIMETRY, FARADAY effect, RADIO telescopes, LINEAR polarization, BREWSTER'S angle, SAMPLE size (Statistics)
Abstract

As the sample size of repeating fast radio bursts (FRBs) has grown, an increasing diversity of phenomenology has emerged. Through long-term multi-epoch studies of repeating FRBs, it is possible to assess which phenomena are common to the population and which are unique to individual sources. We present a multi-epoch monitoring campaign of the repeating FRB source 20180301A using the ultra-wideband low (UWL) receiver observations with Murriyang , the Parkes 64-m radio telescope. The observations covered a wide frequency band spanning approximately 0.7–4 GHz, and yielded the detection of 46 bursts. None of the repeat bursts displayed radio emission in the range of 1.8–4 GHz, while the burst emission peaked at 1.1 GHz. We discover evidence for secular trends in the burst dispersion measure, indicating a decline at a rate of |$-2.7\pm 0.2\, {\rm pc\, cm^{-3}\, yr^{-1}}$|⁠. We also found significant variation in the Faraday rotation measure of the bursts across the follow-up period, including evidence of a sign reversal. While a majority of bursts did not exhibit any polarization, those that did show a decrease in the linear polarization fraction as a function of frequency, consistent with spectral depolarization due to scattering, as observed in other repeating FRB sources. Surprisingly, no significant variation in the polarization position angles was found, which is in contrast with earlier measurements reported for the FRB source. We measure the burst rate and sub-pulse drift rate variation and compare them with the previous results. These novel observations, along with the extreme polarization properties observed in other repeating FRBs, suggest that a sub-sample of FRB progenitors possess highly dynamic magneto-ionic environments. [ABSTRACT FROM AUTHOR]

Published
2023
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27. Flux density monitoring of 89 millisecond pulsars with MeerKAT.

Author

Gitika, P, Bailes, M, Shannon, R M, Reardon, D J, Cameron, A D, Shamohammadi, M, Miles, M T, Flynn, C M L, Corongiu, A, and Kramer, M

Subjects
ACTINIC flux, MEERKAT, GRAVITATIONAL waves
Abstract

We present a flux density study of 89 millisecond pulsars (MSPs) regularly monitored as part of the MeerKAT Pulsar Timing Array (MPTA) using the L -Band receiver with an approximately two week cadence between 2019 and 2022. For each pulsar, we have determined the mean flux densities at each epoch in eight ∼97 MHz sub-bands ranging from 944 to 1625 MHz. From these we have derived their modulation indices, their average and peak-to-median flux densities in each sub-band, as well as their mean spectral indices across the entire frequency range. We find that the vast majority of the MSPs have spectra that are well described by a simple power law, with a mean spectral index of –1.86(6). Using the temporal variation of the flux densities, we measured the structure functions and determined the refractive scintillation time-scale for seven. The structure functions provide strong evidence that the intrinsic radio luminosities of MSPs are stable. As a population, the average modulation index at 20 cm wavelengths peaks near unity at dispersion measures (DMs) of ∼20 pc cm−3 and by a DM of 100 pc cm−3 are closer to 0.2, due to refractive scintillation. We find that timing arrays can improve their observing efficiency by reacting to scintillation maxima, and that 20 cm FRB surveys should prioritize highly scintillating mid-latitude regions of the Galactic sky where they will find ∼30 per cent more events and bursts at greater distances. [ABSTRACT FROM AUTHOR]

Published
2023
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28. Rotational and radio emission properties of PSR J0738-4042 over half a century

Author

Lower, M. E., Johnston, S., Karastergiou, A., Brook, P. R., Bailes, M., Buchner, S., Deller, A. T., Dunn, L., Flynn, C., Kerr, M., Manchester, R. N., Mandlik, A., Oswald, L. S., Parthasarathy, A., Shannon, R. M., Sobey, C., and Weltevrede, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a comprehensive study of the rotational and emission properties of PSR J0738$-$4042 using a combination of observations taken by the Deep Space Network, Hartebeesthoek, Parkes (Murriyang) and Molonglo observatories between 1972 and 2023. Our timing of the pulsar is motivated by previously reported profile/spin-down events that occurred in September 2005 and December 2015, which result in an anomalously large braking index of $n = 23300 \pm 1800$. Using a Gaussian process regression framework, we develop continuous models for the evolution of the pulsar spin-down rate ($\dot{\nu}$) and profile shape. We find that the pulse profile variations are similar regardless of radio observing frequency and polarisation. Small-scale differences can be ascribed to changes in the interstellar medium along the line of sight and frequency-dependent changes in magnetospheric radio emission height. No new correlated spin-down or profile events were identified in our extended dataset. However, we found that the disappearance of a bright emission component in the leading edge of archival profiles between 1981-1988 was not associated with a substantial change in $\dot{\nu}$. This marks a notable departure from the previous profile/spin-down events in this pulsar. We discuss the challenges these observations pose for physical models and conclude that interactions between the pulsar and in-falling asteroids or a form of magnetospheric state-switching with a long periodicity are plausible explanations., Comment: 14 pages, 8 figures. Accepted for publication in MNRAS

Published
2023

29. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

Author

Falxa, M, Babak, S, Baker, P T, Bécsy, B, Chalumeau, A, Chen, S, Chen, Z, Cornish, N J, Guillemot, L, Hazboun, J S, Mingarelli, C M F, Parthasarathy, A, Petiteau, A, Pol, N S, Sesana, A, Spolaor, S B, Taylor, S R, Theureau, G, Vallisneri, M, Vigeland, S J, Witt, C A, Zhu, X, Antoniadis, J, Arzoumanian, Z, Bailes, M, Bhat, N D R, Blecha, L, Brazier, A, Brook, P R, Caballero, N, Cameron, A D, Casey-Clyde, J A, Champion, D, Charisi, M, Chatterjee, S, Cognard, I, Cordes, J M, Crawford, F, Cromartie, H T, Crowter, K, Dai, S, DeCesar, M E, Demorest, P B, Desvignes, G, Dolch, T, Drachler, B, Feng, Y, Ferrara, E C, Fiore, W, Fonseca, E, Garver-Daniels, N, Glaser, J, Goncharov, B, Good, D C, Griessmeier, J, Guo, Y J, Gültekin, K, Hobbs, G, Hu, H, Islo, K, Jang, J, Jennings, R J, Johnson, A D, Jones, M L, Kaczmarek, J, Kaiser, A R, Kaplan, D L, Keith, M, Kelley, L Z, Kerr, M, Key, J S, Laal, N, Lam, M T, Lamb, W G, Lazio, T J W, Liu, K, Liu, T, Luo, J, Lynch, R S, Madison, D R, Main, R, Manchester, R, McEwen, A, McKee, J, McLaughlin, M A, Ng, C, Nice, D J, Ocker, S, Olum, K D, Osłowski, S, Pennucci, T T, Perera, B B P, Perrodin, D, Porayko, N, Possenti, A, Quelquejay-Leclere, H, Ransom, S M, Ray, P S, Reardon, D J, Russell, C J, Samajdar, A, Sarkissian, J, Schult, L, Shaifullah, G, Shannon, R M, Shapiro-Albert, B J, Siemens, X, Simon, J J, Siwek, M, Smith, T L, Speri, L, Spiewak, R, Stairs, I H, Stappers, B, Stinebring, D R, Swiggum, J K, Tiburzi, C, Turner, J, Vecchio, A, Verbiest, Joris, Wahl, H, Wang, S Q, Wang, J, Wang, Jun, Wu, Ziwei, Zhang, L, Zhang, S, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and IPTA

Subjects
noise, data analysis method, gravitational radiation, orbit: circle, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), sensitivity, frequency: high, General Relativity and Quantum Cosmology, confidence limit, frequency: low, black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), pulsar
Abstract

The International Pulsar Timing Array 2nd data release is the combination ofdatasets from worldwide collaborations. In this study, we search for continuouswaves: gravitational wave signals produced by individual supermassive blackhole binaries in the local universe. We consider binaries on circular orbitsand neglect the evolution of orbital frequency over the observational span. Wefind no evidence for such signals and set sky averaged 95% upper limits ontheir amplitude h 95 . The most sensitive frequency is 10nHz with h 95 = 9.110-15 . We achieved the best upper limit to date at low and high frequencies ofthe PTA band thanks to improved effective cadence of observations. In ouranalysis, we have taken into account the recently discovered common red noiseprocess, which has an impact at low frequencies. We also find that the peculiarnoise features present in some pulsars data must be taken into account toreduce the false alarm. We show that using custom noise models is essential insearching for continuous gravitational wave signals and setting the upperlimit.

Published
2023

30. The dispersion–brightness relation for fast radio bursts from a wide-field survey

Author

Shannon, R. M., Macquart, J.-P., Bannister, K. W., Ekers, R. D., James, C. W., Osłowski, S., Qiu, H., Sammons, M., Hotan, A. W., Voronkov, M. A., Beresford, R. J., Brothers, M., Brown, A. J., Bunton, J. D., Chippendale, A. P., Haskins, C., Leach, M., Marquarding, M., McConnell, D., Pilawa, M. A., Sadler, E. M., Troup, E. R., Tuthill, J., Whiting, M. T., Allison, J. R., Anderson, C. S., Bell, M. E., Collier, J. D., Gürkan, G., Heald, G., and Riseley, C. J.

Published
2018
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31. Two-screen scattering in CRAFT FRBs.

Author

Sammons, Mawson W, Deller, Adam T, Glowacki, Marcin, Gourdji, Kelly, James, C W, Prochaska, J Xavier, Qiu, Hao, Scott, Danica R, Shannon, R M, and Trott, C M

Subjects
MILKY Way, INTERSTELLAR medium, SOLAR radio bursts, GALAXIES
Abstract

Temporal broadening is a commonly observed property of fast radio bursts (FRBs), associated with turbulent media which cause radiowave scattering. Similarly to dispersion, scattering is an important probe of the media along the line of sight to an FRB source, such as the circumburst or circumgalactic media (CGM). Measurements of characteristic scattering times alone are insufficient to constrain the position of the dominant scattering media along the line of sight. However, where more than one scattering screen exists, Galactic scintillation can be leveraged to form strong constraints. We quantify the scattering and scintillation in 10 FRBs with (1) known host galaxies and redshifts and (2) captured voltage data enabling high-time resolution analysis. We find strong evidence for two screens in three cases. For FRBs 20190608B and 20210320C, we find evidence for scattering screens less than approximately 16.7 and 3000 kpc, respectively, from their sources, consistent with the scattering occurring in the circumburst environment, the host interstellar medium (ISM) or the CGM. For FRB 20201124A, we find a low modulation index that evolves over the burst's scattering tail, indicating the presence of a scattering screen ≈9 kpc from the host, and excluding the circumburst environment from potential scattering sites. By assuming that pulse broadening is contributed by the host galaxy ISM or circumburst environment, the lack of observed scintillation in four FRBs in our sample suggests that existing models may be poor estimators of scattering times associated with the Milky Way's ISM, similar to the anomalously low scattering observed for FRB 20201124A. [ABSTRACT FROM AUTHOR]

Published
2023
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32. Rotational and radio emission properties of PSR J0738−4042 over half a century.

Author

Lower, M E, Johnston, S, Karastergiou, A, Brook, P R, Bailes, M, Buchner, S, Deller, A T, Dunn, L, Flynn, C, Kerr, M, Manchester, R N, Mandlik, A, Oswald, L S, Parthasarathy, A, Shannon, R M, Sobey, C, and Weltevrede, P

Subjects
KRIGING, INTERSTELLAR medium, ASTEROIDS, PULSARS, RADIO frequency
Abstract

We present a comprehensive study of the rotational and emission properties of PSR J0738−4042 using a combination of observations taken by the Deep Space Network, Hartebeesthoek, Parkes (Murriyang) and Molonglo observatories between 1972 and 2023. Our timing of the pulsar is motivated by previously reported profile/spin-down events that occurred in 2005 September and 2015 December, which result in an anomalously large braking index of n  = 23 300 ± 1800. Using a Gaussian process regression framework, we develop continuous models for the evolution of the pulsar spin-down rate (⁠|$\dot{\nu }$|⁠) and profile shape. We find that the pulse profile variations are similar regardless of radio observing frequency and polarization. Small-scale differences can be ascribed to changes in the interstellar medium along the line of sight and frequency-dependent changes in magnetospheric radio emission height. No new correlated spin-down or profile events were identified in our extended data set. However, we found that the disappearance of a bright emission component in the leading edge of archival profiles between 1981 and 1988 was not associated with a substantial change in |$\dot{\nu }$|⁠. This marks a notable departure from the previous profile/spin-down events in this pulsar. We discuss the challenges these observations pose for physical models and conclude that interactions between the pulsar and in-falling asteroids or a form of magnetospheric state-switching with a long periodicity are plausible explanations. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

33. CELEBI: The CRAFT Effortless Localisation and Enhanced Burst Inspection Pipeline

Author

Scott, D. R., Cho, H., Day, C. K., Deller, A. T., Glowacki, M., Gourdji, K., Bannister, K. W., Bera, A., Bhandari, S., James, C. W., and Shannon, R. M.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Fast radio bursts (FRBs) are being detected with increasing regularity. However, their spontaneous and often once-off nature makes high-precision burst position and frequency-time structure measurements difficult without specialised real-time detection techniques and instrumentation. The Australian Square Kilometre Array Pathfinder (ASKAP) has been enabled by the Commensal Real-time ASKAP Fast Transients Collaboration (CRAFT) to detect FRBs in real-time and save raw antenna voltages containing FRB detections. We present the CRAFT Effortless Localisation and Enhanced Burst Inspection pipeline (CELEBI), an automated software pipeline that extends CRAFT's existing software to process ASKAP voltages in order to produce sub-arcsecond precision localisations and polarimetric data at time resolutions as fine as 3 ns of FRB events. We use Nextflow to link together Bash and Python code that performs software correlation, interferometric imaging, and beamforming, making use of common astronomical software packages., 17 pages, 13 figures, minor revisions, accepted for publication in Astronomy & Computing

Published
2023

34. Mass measurements and 3D orbital geometry of PSR J1933$-$6211

Author

Geyer, M., Krishnan, V. Venkatraman, Freire, P. C. C., Kramer, M., Antoniadis, J., Bailes, M., Bernadich, M. C. i, Buchner, S., Cameron, A. D., Champion, D. J., Karastergiou, A., Keith, M. J., Lower, M. E., Osłowski, S., Possenti, A., Parthasarathy, A., Reardon, D. J., Serylak, M., Shannon, R. M., Spiewak, R., van Straten, W., and Verbiest, Joris

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

PSR J1933$-$6211 is a 3.5-ms pulsar in a 12.8-d orbit with a white dwarf (WD). Its high proper motion and low dispersion measure result in such significant interstellar scintillation that high signal-to-noise detections require long observing durations or fortuitous timing. We turn to the sensitive MeerKAT telescope and, combined with historic Parkes data, leverage PSR J1933$-$6211's kinematic and relativistic effects to constrain its 3D orbital geometry and the component masses. We obtain precise proper motion and parallax estimates, and measure their effects as secular changes in the Keplerian orbital parameters: a variation in orbital period of $7(1) \times 10^{-13}$ s s$^{-1}$ and a change in projected semi-major axis of $1.60(5) \times 10^{-14}$ s s$^{-1}$. A self-consistent analysis of all kinematic and relativistic effects yields a distance of $1.6^{+0.2}_{-0.3}$ kpc, an orbital inclination, $i = 55(1)$ deg and a longitude of the ascending node, $\Omega = 255^{+8}_{-14}$ deg. The probability densities for $\Omega$ and $i$ and their symmetric counterparts, ($180-i$, $360-\Omega$), are seen to depend on the fiducial orbit used to measure the time of periastron passage. We investigate this unexpected dependence and rule out software-related causes using simulations. Nevertheless, we constrain the pulsar and WD masses to $1.4^{+0.3}_{-0.2}$ M$_\odot$ and $0.43(5)$ M$_\odot$ respectively. These strongly disfavour a helium-dominated WD. The orbital similarities between PSRs J1933$-$6211 and J1614$-$2230 suggest they underwent Case A Roche lobe overflow, an extended evolution while the companion star is still on the Main Sequence. However, with a mass of $\sim 1.4$ M$_\odot$, PSR J1933$-$6211 has not accreted significant matter. This highlights the low accretion efficiency of the spin-up process and suggests that observed neutron star masses are mostly a result of supernova physics., Comment: 16 pages, 7 figures. Abstract shortened to adhere to ArXiv limit

Published
2023

36. Epigenetic Regulation via Altered Histone Acetylation Results in Suppression of Mast Cell Function and Mast Cell-Mediated Food Allergic Responses

Author

Dylan Krajewski, Edwin Kaczenski, Jeffrey Rovatti, Stephanie Polukort, Chelsea Thompson, Catherine Dollard, Jennifer Ser-Dolansky, Sallie S. Schneider, Shannon R. M. Kinney, and Clinton B. Mathias

Subjects
mast cells, food allergy, trichostatin A, histone deacetylase (HDAC) inhibitors, epigenetics, Immunologic diseases. Allergy, RC581-607
Abstract

Mast cells are highly versatile cells that perform a variety of functions depending on the immune trigger, context of activation, and cytokine stimulus. Antigen-mediated mast cell responses are regulated by transcriptional processes that result in the induction of numerous genes contributing to mast cell function. Recently, we also showed that exposure to dietary agents with known epigenetic actions such as curcumin can suppress mast cell-mediated food allergy, suggesting that mast cell responses in vivo may be epigenetically regulated. To further assess the effects of epigenetic modifications on mast cell function, we examined the behavior of bone marrow-derived mast cells (BMMCs) in response to trichostatin A (TSA) treatment, a well-studied histone deacetylase inhibitor. IgE-mediated BMMC activation resulted in enhanced expression and secretion of IL-4, IL-6, TNF-α, and IL-13. In contrast, pretreatment with TSA resulted in altered cytokine secretion. This was accompanied by decreased expression of FcεRI and mast cell degranulation. Interestingly, exposure to non-IgE stimuli such as IL-33, was also affected by TSA treatment. Furthermore, continuous TSA exposure contributed to mast cell apoptosis and a decrease in survival. Further examination revealed an increase in I-κBα and a decrease in phospho-relA levels in TSA-treated BMMCs, suggesting that TSA alters transcriptional processes, resulting in enhancement of I-κBα transcription and decreased NF-κB activation. Lastly, treatment of wild-type mice with TSA in a model of ovalbumin-induced food allergy resulted in a significant attenuation in the development of food allergy symptoms including decreases in allergic diarrhea and mast cell activation. These data therefore suggest that the epigenetic regulation of mast cell activation during immune responses may occur via altered histone acetylation, and that exposure to dietary substances may induce epigenetic modifications that modulate mast cell function.

Published
2018
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37. Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run

Author

Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adhikari, N., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Angelova, V, Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koji, Arai, Koya, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arene, M., Aritomi, N., Arnaud, N., Aronson, S. M., Arun, K. G., Asada, H., Asali, Y., Ashton, G., Aso, Y., Assiduo, M., Aston, S. M., Astone, P., Aubin, F., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Badger, C., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Bailes, M., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I, Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Becsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I, Benedetto, V, Beniwal, D., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Are, R., Bhardwaj, U., Bhattacharjee, D., Bhaumik, S., Bilenko, I. A., Billingsley, G., Bini, S., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M-A, Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Bogaert, G., Boldrini, M., Bonavena, L. D., Bondu, F., Bonilla, E., Bonn, Booker, P., Boom, B. A., Bork, R., Boschi, V, Bose, N., Bose, S., Bossilkov, V, Boudart, V, Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Calderon Bustillo, J., Callaghan, J. D., Callister, T. A., Calloni, E., Cameron, J., Camp, J. B., Canepa, M., Canevarolo, S., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carrillo, G., Carullo, G., Carver, T. L., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Ceasar, M., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, W., Chakravarti, K., Subrahmanya, S. Chalathadka, Champion, E., Chan, C-H, Chan, C., Chan, C. L., Chan, K., Chan, M., Ra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chass, e-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y-B, Chen, Y-R, Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y, Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y-K, Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Codazzo, E., Cohadon, P-F, Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colombo, A., Colpi, M., Compton, C. M., Constancio, J, R., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I, Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coulon, J-P, Countryman, S. T., Cousins, B., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cunningham, L., Cuoco, E., Dabadie, P., Dal Canton, T., Dall'Osso, S., Dalya, G., Dana, A., Daneshgaranbajastani, L. M., Danilishin, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Datta, S., Dattilo, V, Dave, I, Davier, M., Davies, G. S., Davis, D., Davis, M. C., Daw, E. J., Dean, R., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Favero, V, De Lillo, F., De Lillo, N., Del Pozzo, W., Demarchi, L. M., De Matteis, F., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., De Simone, R., Dhur, Har, S., Diaz, M. C., Diaz-Ortiz, Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I, Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I, Drago, M., Driggers, J. C., Drori, Y., Ducoin, J-G, Dupej, P., Durante, O., Duverne, P-A, Dwyer, S. E., Eassa, C., Easter, P. J., Ebersold, M., Eckhardt, T., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Engelby, E., Enomoto, Y., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V, Fair, H., Fairhurst, S., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Farrow, N. W., Fauchon-Jones, E. J., Favaro, G., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Fenyvesi, E., Ferguson, D. L., Fern, ez-Galiana, A., Ferrante, I, Ferreira, T. A., Fidecaro, F., Figura, P., Fiori, I, Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V, Flaminio, R., Floden, E., Fong, H., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Frederick, C., Freed, J. P., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fronze, G. G., Fujii, Y., Fujikawa, Y., Fukunaga, M., Fukushima, M., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D., Gaonkar, S. G., Garaventa, B., Garcia-Nunez, C., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V, G-G, Ge, Gemme, G., Gennai, A., George, J., Gerberding, O., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., Gonzalez, G., Gopakumar, A., Gosselin, M., Gouaty, R., Gould, D. W., Grace, B., Grado, A., Granata, M., Granata, V, Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W., Griggs, H. L., Grignani, G., Grimaldi, A., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guerra, D., Guidi, G. M., Guimaraes, A. R., Guixe, G., Gulati, H. K., Guo, H-K, Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, P., Gustafson, E. K., Gustafson, R., Guzman, F., Ha, S., Haegel, L., Hagiwara, A., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W-B, Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Hasskew, R. K., Haster, C-J, Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heidt, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Hern, A. G., Ez, Vivanco, F. Hern, Heurs, M., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hiranuma, Y., Hirata, N., Hirose, E., W. C. G., Ho, Hochheim, S., Hofman, D., Hohmann, J. N., Holcomb, D. G., Holl, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Z., Hopkins, P., Hough, J., Hourihane, S., Howell, E. J., Hoy, C. G., Hoyl, Hreibi, A., Hsieh, B-H, Hsu, Y., Huang, G-Z, Huang, H-Y, Huang, P., Huang, Y-C, Huang, Y-J, Huang, Y., Hubner, M. T., Huddart, A. D., Hughey, B., Hui, D. C. Y., Hui, V, Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Ide, S., Idzkowski, B., Iess, A., Ikenoue, B., Imam, S., Inayoshi, K., Ingram, C., Inoue, Y., Ioka, K., Isi, M., Isleif, K., Ito, K., Itoh, Y., Iyer, B. R., Izumi, K., Jaberianhamedan, V, Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janquart, J., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jenner, K., Jeon, C., Jeunon, M., Jia, W., Jin, H-B, Johns, G. R., Jones, A. W., Jones, I, Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Jung, P., Jung, K., Junker, J., Juste, V, Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, Kalogera, V, Kamai, B., Kamiizumi, M., K, A, N., Hasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karat, S., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kawaguchi, K., Kawai, N., Kawasaki, T., Kefelian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, J., Kim, K., Kim, W. S., Kim, Y-M, Kimball, C., Kimura, N., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kita, N., Kitazawa, H., Kleybolte, L., Klimenko, S., Knee, A. M., Knowles, T. D., Knyazev, E., Koch, P., Koekoek, G., Kojima, Y., Kokeyama, K., Koley, S., Kolitsidou, P., Kolstein, M., Komori, K., Kondrashov, V, Kong, A. K. H., Kontos, A., Koper, N., Korobko, M., Kotake, K., Kovalam, M., Kozak, D. B., Kozakai, C., Kozu, R., Kringel, V, Krishnendu, Krolak, A., Kuehn, G., Kuei, F., Kuijer, P., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuo, C., Kuo, H-S, Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kuwahara, S., Kwak, K., Lagabbe, P., Laghi, D., Lal, E, E., Lam, T. L., Lamberts, A., L, Ry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., La Rosa, I, Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lee, R., Lehmann, J., Lemaitre, A., Leonardi, M., Leroy, N., Letendre, N., Levesque, C., Levin, Y., Leviton, J. N., Leyde, K., A. K. Y., Li, Li, B., Li, J., K. L., Li, T. G. F., Li, Li, X., Lin, C-Y, Lin, F-K, Lin, F-L, Lin, H. L., Lin, L. C-C, Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, G. C., Liu, J., Liu, K., Liu, X., Llamas, F., Llorens-Monteagudo, M., R. K. L., Lo, Lockwood, A., London, L. T., Longo, A., Lopez, D., Portilla, M. Lopez, Lorenzini, M., Loriette, V, Lorm, Losurdo, G., Lott, T. P., Lough, J. D., Lousto, C. O., Lovelace, G., Lucaccioni, J. F., Luck, H., Lumaca, D., Lundgren, A. P., Luo, L-W, Lynam, J. E., Macas, R., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., I. Magana, Ez, Magazzu, C., Magee, R. M., Maggiore, R., Magnozzi, M., Mahesh, S., Majorana, E., Makarem, C., Maksimovic, I, Maliakal, S., Malik, A., Man, N., M, Ic, V, Mangano, V, Mango, J. L., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marchio, M., Marion, F., Mark, Z., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, M., Martinez, V. A., Martinez, V, Martinovic, K., Martynov, Marx, E. J., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matichard, F., Matiushechkina, M., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclell, D. E., Mcclincy, P. K., Mccormick, S., Mcculler, L., Mcghee, Mcguire, S. C., Mcisaac, C., Mciver, J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Meijer, Q., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I, Michel, C., Michimura, Y., Middleton, H., Milano, L., Miller, A. L., Miller, A., Miller, B., Millhouse, M., Mills, J. C., Milotti, E., Minazzoli, O., Minenkov, Y., Mio, N., Mir, Ll M., Miravet-Tenes, M., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Geoffrey, Mo, Modafferi, L. M., Moguel, E., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina, I, Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moragues, J., Moraru, D., Morawski, F., More, A., Moreno, C., Moreno, G., Mori, Y., Morisaki, S., Moriwaki, Y., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, Arunava, Mukherjee, D., Mukherjee, Soma, Mukherjee, Subroto, Mukherjee, Suvodip, Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Murray, P. G., Musenich, R., Muusse, S., Nadji, S. L., Nagano, K., Nagano, S., Nagar, A., Nakamura, K., Nakano, H., Nakano, M., Nakashima, R., Nakayama, Y., Napolano, V, Nardecchia, I, Narikawa, T., Naticchioni, L., Nayak, B., Nayak, R. K., Negishi, R., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neubauer, P., Neunzert, A., K. Y., Ng, S. W. S., Ng, Nguyen, C., Nguyen, P., Nguyen, T., Quynh, L. Nguyen, W-T, Ni, Nichols, S. A., Nishizawa, A., Nissanke, S., Nitoglia, E., Nocera, F., Norman, M., North, C., Nozaki, S., Nuttall, L. K., Oberling, J., Obuchi, Y., Oelker, E., Ogaki, W., Oganesyan, G., J. J., Oh, Oh, K., S. H., Oh, Ohashi, M., Ohishi, N., Ohkawa, M., Ohme, F., Ohta, H., Okada, M. A., Okutani, Y., Okutomi, K., Olivetto, C., Oohara, K., Ooi, C., Oram, R., Ormiston, R. G., Ormsby, N. D., Ortega, L. F., Oshino, S., Ossokine, S., Osthelder, C., Otabe, S., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Pan, K., P, P. K., A, Pang, H., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Panther, F. H., Paoletti, F., Paoli, A., Paolone, A., Parisi, A., Park, H., Park, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Pathak, M., Patricelli, B., Patron, A. S., Patrone, S., Paul, S., Payne, E., Pedraza, M., Pegoraro, M., Pele, A., Arellano, F. E. Pena, Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Perigois, C., Perkins, C. C., Perreca, A., Perries, S., Petermann, J., Petterson, D., Pfeiffer, H. P., Pham, K. A., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierini, L., Pierro, V, Pillant, G., Pillas, M., Pilo, F., Pinard, L., Pinto, I. M., Pinto, M., Piotrzkowski, K., Pirello, M., Pitkin, M. D., Placidi, E., Planas, L., Plastino, W., Pluchar, C., Poggiani, R., Polini, E., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Poulton, R., Powell, J., Pracchia, M., Pradier, T., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Principe, M., Prodi, G. A., Prokhorov, L., Prosposito, P., Prudenzi, L., Puecher, A., Punturo, M., Puosi, F., Puppo, P., Purrer, M., Qi, H., Quetschke, V, Quitzow-James, R., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rail, S. X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, J., Rapagnani, P., Rapol, U. D., Ray, A., Raymond, V, Raza, N., Razzano, M., Read, J., Rees, L. A., Regimbau, T., Rei, L., Reid, S., Reid, S. W., Reitze, D. H., Relton, P., Renzini, A., Rettegno, P., Rezac, M., Ricci, F., Richards, D., Richardson, J. W., Richardson, L., Riemenschneider, G., Riles, K., Rinaldi, S., Rink, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rodriguez, S., Roll, Rollins, J. G., Romanelli, M., Romano, R., Romel, C. L., Romero-Rodriguez, A., Romero-Shaw, I. M., Romie, J. H., Ronchini, S., Rosa, L., Rose, C. A., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, S., Roy, Santosh, Roy, Soumen, Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakellariadou, M., Sakuno, Y., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., S, Ers, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sassolas, B., Satari, H., Sato, S., Sato, T., Sauter, O., Savage, R. L., Sawada, T., Sawant, D., Sawant, H. L., Sayah, S., Schaetzl, D., Scheel, M., Scheuer, J., Schiworski, M., Schmidt, P., Schmidt, S., Schnabel, R., Schneewind, M., Schofield, R. M. S., Schonbeck, A., Schulte, B. W., Schutz, B. F., Schwartz, E., Scott, J., Scott, S. M., Seglar-Arroyo, M., Sekiguchi, T., Sekiguchi, Y., Sellers, D., Sengupta, A. S., Sentenac, D., Seo, E. G., Sequino, V, Sergeev, A., Setyawati, Y., Shaffer, T., Shahriar, M. S., Shams, B., Shao, L., Sharma, A., Sharma, P., Shawhan, P., Shcheblanov, N. S., Shibagaki, S., Shikauchi, M., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Sintes, A. M., Sipala, V, Skliris, V, Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Soldateschi, J., Somala, S. N., Somiya, K., Son, E. J., Soni, K., Soni, S., Sordini, V, Sorrentino, F., Sorrentino, N., Sotani, H., Soulard, R., Souradeep, T., Sowell, E., Spagnuolo, V, Spencer, A. P., Spera, M., Srinivasan, R., Srivastava, A. K., Srivastava, V, Staats, K., Stachie, C., Steer, D. A., Steinlechner, J., Steinlechner, S., Stops, D. J., Stover, M., Strain, K. A., Strang, L. C., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V, Sugimoto, R., Suh, H. G., Summerscales, T. Z., Sun, H., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Suzuki, Takamasa, Suzuki, Toshikazu, Swinkels, B. L., Szewczyk, P., Tacca, M., Tagoshi, H., Tait, S. C., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Talbot, C. J., Talbot, C., Tanaka, H., Tanaka, Kazuyuki, Tanaka, Kenta, Tanaka, Taiki, Tanaka, Takahiro, Tanasijczuk, A. J., Tanioka, S., Tanner, D. B., Tao, D., Tao, L., San Martin, E. N. Tapia, Taranto, C., Tasson, J. D., Telada, S., Tenorio, R., Terhune, J. E., Terkowski, L., Thirugnanasamb, M. P., Am, Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V, Toivonen, A. M., Tol, Tolley, A. E., Tomaru, T., Tomigami, Y., Tomura, T., Tonelli, M., Torres-Forne, A., Torrie, Melo, I. Tosta E., Toyra, D., Trapananti, A., Travasso, F., Traylor, G., Trevor, M., Tringali, M. C., Tripathee, A., Troiano, L., Trovato, A., Trozzo, L., Trudeau, R. J., Tsai, D. S., Tsai, D., Tsang, K. W., Tsang, T., Tsao, J-S, Tse, M., Tso, R., Tsubono, K., Tsuchida, S., Tsukada, L., Tsuna, D., Tsutsui, T., Tsuzuki, T., Turbang, K., Turconi, M., Tuyenbayev, D., Ubhi, A. S., Uchikata, N., Uchiyama, T., Udall, R. P., Ueda, A., Uehara, T., Ueno, K., Ueshima, G., Unnikrishnan, C. S., Uraguchi, F., Urban, A. L., Ushiba, T., Utina, A., Vahlbruch, H., Vajente, G., Vajpeyi, A., Valdes, G., Valentini, M., Valsan, V., van Bakel, N., van Beuzekom, M., van den Br, J. F. J., Van den Broeck, C., er-Hyde, D. C., van der Schaaf, L., Van, Heijningen, Vanosky, J., van Putten, M. H. P. M., van Remortel, N., Vardaro, M., Vargas, A. F., Varma, V., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venneberg, J., Venugopalan, G., Verkindt, D., Verma, P., Verma, Y., Veske, D., Vetrano, F., Vicere, A., Vidyant, S., Viets, A. D., Vijaykumar, A., Villa-Ortega, V., Vinet, J-Y, Virtuoso, A., Vitale, S., Vo, T., Vocca, H., von Reis, E. R. G., von Wrangel, J. S. A., Vorvick, C., Vyatchanin, S. P., Wade, L. E., Wade, M., Wagner, K. J., Walet, R. C., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J., Wang, J. Z., Wang, W. H., Ward, R. L., Warner, J., Was, M., Washimi, T., Washington, N. Y., Watchi, J., Weaver, B., Webster, S. A., Weinert, M., Weinstein, A. J., Weiss, R., Weller, C. M., Wellmann, F., Wen, L., Wessels, P., Wette, K., Whelan, J. T., White, D. D., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, M. J., Williamson, A. R., Willis, J. L., Willke, B., Wilson, D. J., Winkler, W., Wipf, C. C., Wlodarczyk, T., Woan, G., Woehler, J., Wofford, J. K., Wong, I. C. F., Wu, C., D. S., Wu, Wu, H., Wu, S., Wysocki, D. M., Xiao, L., W-R, Xu, Yamada, T., Yamamoto, H., Yamamoto, Kazuhiro, Yamamoto, Kohei, Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, F. W., Yang, L., Yang, Y., Yang, Yang, Yang, Z., Yap, M. J., Yeeles, D. W., Yelikar, A. B., Ying, M., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoo, J., Yoshioka, T., Hang, Yu, Haocun, Yu, Yuzurihara, H., Zanolin, M., Zeidler, S., Zelenova, T., Zendri, J-P, Zevin, M., Zhan, M., Zhang, H., Zhang, J., Zhang, L., Zhang, T., Zhang, Y., Zhao, C., Zhao, G., Zhao, Y., Zhao, Yue, Zhou, R., Zhou, Z., Zhu, X. J., Zhu, Z-H, Zucker, M. E., Zweizig, J., Antonopoulou, D., Arzoumanian, Z., Basu, A., Bogdanov, S., Cognard, I, Crowter, K., Enoto, T., Espinoza, C. M., Flynn, C. M. L., Fonseca, E., Good, D. C., Guillemot, L., Guillot, S., Harding, A. K., Keith, M. J., Kuiper, L., Lower, M. E., Lyne, A. G., Mckee, J. W., Meyers, B. W., Ng, C., Palfreyman, J. L., Shannon, R. M., Shaw, B., Stairs, I. H., Stappers, B. W., Tan, C. M., Theureau, G., Weltevrede, P., LIGO Sci Collaboration, Virgo, Collaboration, Kagra, Collaboration, Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adhikari, N., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Allocca, A., Altin, P. A., Amato, A., Anand, C., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Andrić, T., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koji, Arai, Koya, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Aronson, S. M., Arun, K. G., Asada, H., Asali, Y., Ashton, G., Aso, Y., Assiduo, M., Aston, S. M., Astone, P., Aubin, F., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Badger, C., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Bailes, M., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Bécsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Bhandare, R., Bhardwaj, U., Bhattacharjee, D., Bhaumik, S., Bilenko, I. A., Billingsley, G., Bini, S., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M. -A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Bogaert, G., Boldrini, M., Bonavena, L. D., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Cameron, J., Camp, J. B., Canepa, M., Canevarolo, S., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carrillo, G., Carullo, G., Carver, T. L., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Ceasar, M., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Chakravarti, K., Subrahmanya, S. Chalathadka, Champion, E., Chan, C. -H., Chan, C., Chan, C. L., Chan, K., Chan, M., Chandra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. -B., Chen, Y. -R., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y., Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y-K., Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Codazzo, E., Cohadon, P. -F., Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colombo, A., Colpi, M., Compton, C. M., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coulon, J. -P., Countryman, S. T., Cousins, B., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cunningham, L., Cuoco, E., Curyło, M., Dabadie, P., Canton, T. Dal, Dall’Osso, S., Dálya, G., Dana, A., Daneshgaranbajastani, L. M., D’Angelo, B., Danilishin, S., D’Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Datta, S., Dattilo, V., Dave, I., Davier, M., Davies, G. S., Davis, D., Davis, M. C., Daw, E. J., Dean, R., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Del Pozzo, W., Demarchi, L. M., De Matteis, F., D’Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., De Simone, R., Dhurandhar, S., Díaz, M. C., Diaz-Ortiz, M., Didio, N. A., Dietrich, T., Fiore, L. Di, Fronzo, C. Di, Giorgio, C. Di, Giovanni, F. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Ding, B., Pace, S. Di, Palma, I. Di, Renzo, F. Di, Divakarla, A. K., Dmitriev, A., Doctor, Z., D’Onofrio, L., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Drago, M., Driggers, J. C., Drori, Y., Ducoin, J. -G., Dupej, P., Durante, O., D’Urso, D., Duverne, P. -A., Dwyer, S. E., Eassa, C., Easter, P. J., Ebersold, M., Eckhardt, T., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Engelby, E., Enomoto, Y., Errico, L., Essick, R. C., Estellés, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fair, H., Fairhurst, S., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Farrow, N. W., Fauchon-Jones, E. J., Favaro, G., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, T. A., Fidecaro, F., Figura, P., Fiori, I., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Fong, H., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Frederick, C., Freed, J. P., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fronzé, G. G., Fujii, Y., Fujikawa, Y., Fukunaga, M., Fukushima, M., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D., Gaonkar, S. G., Garaventa, B., García-Núñez, C., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Ge, G. -G., Gemme, G., Gennai, A., George, J., Gerberding, O., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., González, G., Gopakumar, A., Gosselin, M., Gouaty, R., Gould, D. W., Grace, B., Grado, A., Granata, M., Granata, V., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W., Griggs, H. L., Grignani, G., Grimaldi, A., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guerra, D., Guidi, G. M., Guimaraes, A. R., Guixé, G., Gulati, H. K., Guo, H. -K., Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, P., Gustafson, E. K., Gustafson, R., Guzman, F., Ha, S., Haegel, L., Hagiwara, A., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W. -B., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Hasskew, R. K., Haster, C. -J., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heidt, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Hernandez, A. G., Vivanco, F. Hernandez, Heurs, M., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hiranuma, Y., Hirata, N., Hirose, E., Ho, W. C. G., Hochheim, S., Hofman, D., Hohmann, J. N., Holcomb, D. G., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Z., Hopkins, P., Hough, J., Hourihane, S., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsieh, B-H., Hsu, Y., Huang, G-Z., Huang, H-Y., Huang, P., Huang, Y-C., Huang, Y. -J., Huang, Y., Hübner, M. T., Huddart, A. D., Hughey, B., Hui, D. C. Y., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Ide, S., Idzkowski, B., Iess, A., Ikenoue, B., Imam, S., Inayoshi, K., Ingram, C., Inoue, Y., Ioka, K., Isi, M., Isleif, K., Ito, K., Itoh, Y., Iyer, B. R., Izumi, K., Jaberianhamedan, V., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jan, A. Z., Jani, K., Janquart, J., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jenner, K., Jeon, C., Jeunon, M., Jia, W., Jin, H. -B., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Jung, P., Jung, K., Junker, J., Juste, V., Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karat, S., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kawaguchi, K., Kawai, N., Kawasaki, T., Kéfélian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, J., Kim, K., Kim, W. S., Kim, Y. -M., Kimball, C., Kimura, N., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kita, N., Kitazawa, H., Kleybolte, L., Klimenko, S., Knee, A. M., Knowles, T. D., Knyazev, E., Koch, P., Koekoek, G., Kojima, Y., Kokeyama, K., Koley, S., Kolitsidou, P., Kolstein, M., Komori, K., Kondrashov, V., Kong, A. K. H., Kontos, A., Koper, N., Korobko, M., Kotake, K., Kovalam, M., Kozak, D. B., Kozakai, C., Kozu, R., Kringel, V., Krishnendu, N. V., Królak, A., Kuehn, G., Kuei, F., Kuijer, P., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuo, C., Kuo, H-S., Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kuwahara, S., Kwak, K., Lagabbe, P., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Rosa, I. La, Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lee, R., Lehmann, J., Lemaître, A., Leonardi, M., Leroy, N., Letendre, N., Levesque, C., Levin, Y., Leviton, J. N., Leyde, K., Li, A. K. Y., Li, B., Li, J., Li, K. L., Li, T. G. F., Li, X., Lin, C-Y., Lin, F-K., Lin, F-L., Lin, H. L., Lin, L. C. -C., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, G. C., Liu, J., Liu, K., Liu, X., Llamas, F., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., London, L. T., Longo, A., Lopez, D., Portilla, M. Lopez, Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lott, T. P., Lough, J. D., Lousto, C. O., Lovelace, G., Lucaccioni, J. F., Lück, H., Lumaca, D., Lundgren, A. P., Luo, L. -W., Lynam, J. E., Macas, R., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., Hernandez, I. Magaña, Magazzù, C., Magee, R. M., Maggiore, R., Magnozzi, M., Mahesh, S., Majorana, E., Makarem, C., Maksimovic, I., Maliakal, S., Malik, A., Man, N., Mandic, V., Mangano, V., Mango, J. L., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marchio, M., Marion, F., Mark, Z., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, M., Martinez, V. A., Martinez, V., Martinovic, K., Martynov, D. V., Marx, E. J., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matichard, F., Matiushechkina, M., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mcclincy, P. K., Mccormick, S., Mcculler, L., Mcghee, G. I., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Meijer, Q., Melatos, A., Melchor, D. A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Michimura, Y., Middleton, H., Milano, L., Miller, A. L., Miller, A., Miller, B., Millhouse, M., Mills, J. C., Milotti, E., Minazzoli, O., Minenkov, Y., Mio, N., Mir, Ll. M., Miravet-Tenés, M., Mishra, C., Mishra, T., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Mo, Geoffrey, Modafferi, L. M., Moguel, E., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina, I., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moragues, J., Moraru, D., Morawski, F., More, A., Moreno, C., Moreno, G., Mori, Y., Morisaki, S., Moriwaki, Y., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, Arunava, Mukherjee, D., Mukherjee, Soma, Mukherjee, Subroto, Mukherjee, Suvodip, Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Murray, P. G., Musenich, R., Muusse, S., Nadji, S. L., Nagano, K., Nagano, S., Nagar, A., Nakamura, K., Nakano, H., Nakano, M., Nakashima, R., Nakayama, Y., Napolano, V., Nardecchia, I., Narikawa, T., Naticchioni, L., Nayak, B., Nayak, R. K., Negishi, R., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neubauer, P., Neunzert, A., Ng, K. Y., Ng, S. W. S., Nguyen, C., Nguyen, P., Nguyen, T., Quynh, L. Nguyen, Ni, W. -T., Nichols, S. A., Nishizawa, A., Nissanke, S., Nitoglia, E., Nocera, F., Norman, M., North, C., Nozaki, S., Nuttall, L. K., Oberling, J., O’Brien, B. D., Obuchi, Y., O’Dell, J., Oelker, E., Ogaki, W., Oganesyan, G., Oh, J. J., Oh, K., Oh, S. H., Ohashi, M., Ohishi, N., Ohkawa, M., Ohme, F., Ohta, H., Okada, M. A., Okutani, Y., Okutomi, K., Olivetto, C., Oohara, K., Ooi, C., Oram, R., O’Reilly, B., Ormiston, R. G., Ormsby, N. D., Ortega, L. F., O’Shaughnessy, R., O’Shea, E., Oshino, S., Ossokine, S., Osthelder, C., Otabe, S., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Pan, K., Panda, P. K., Pang, H., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Panther, F. H., Paoletti, F., Paoli, A., Paolone, A., Parisi, A., Park, H., Park, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Pathak, M., Patricelli, B., Patron, A. S., Patrone, S., Paul, S., Payne, E., Pedraza, M., Pegoraro, M., Pele, A., Arellano, F. E. Peña, Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Périgois, C., Perkins, C. C., Perreca, A., Perriès, S., Petermann, J., Petterson, D., Pfeiffer, H. P., Pham, K. A., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierini, L., Pierro, V., Pillant, G., Pillas, M., Pilo, F., Pinard, L., Pinto, I. M., Pinto, M., Piotrzkowski, K., Pirello, M., Pitkin, M. D., Placidi, E., Planas, L., Plastino, W., Pluchar, C., Poggiani, R., Polini, E., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Poulton, R., Powell, J., Pracchia, M., Pradier, T., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Principe, M., Prodi, G. A., Prokhorov, L., Prosposito, P., Prudenzi, L., Puecher, A., Punturo, M., Puosi, F., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quitzow-James, R., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rail, S. X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, J., Rapagnani, P., Rapol, U. D., Ray, A., Raymond, V., Raza, N., Razzano, M., Read, J., Rees, L. A., Regimbau, T., Rei, L., Reid, S., Reid, S. W., Reitze, D. H., Relton, P., Renzini, A., Rettegno, P., Rezac, M., Ricci, F., Richards, D., Richardson, J. W., Richardson, L., Riemenschneider, G., Riles, K., Rinaldi, S., Rink, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rodriguez, S., Rolland, L., Rollins, J. G., Romanelli, M., Romano, R., Romel, C. L., Romero-Rodríguez, A., Romero-Shaw, I. M., Romie, J. H., Ronchini, S., Rosa, L., Rose, C. A., Rosińska, D., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, S., Roy, Santosh, Roy, Soumen, Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakellariadou, M., Sakuno, Y., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sassolas, B., Satari, H., Sato, S., Sato, T., Sauter, O., Savage, R. L., Sawada, T., Sawant, D., Sawant, H. L., Sayah, S., Schaetzl, D., Scheel, M., Scheuer, J., Schiworski, M., Schmidt, P., Schmidt, S., Schnabel, R., Schneewind, M., Schofield, R. M. S., Schönbeck, A., Schulte, B. W., Schutz, B. F., Schwartz, E., Scott, J., Scott, S. M., Seglar-Arroyo, M., Sekiguchi, T., Sekiguchi, Y., Sellers, D., Sengupta, A. S., Sentenac, D., Seo, E. G., Sequino, V., Sergeev, A., Setyawati, Y., Shaffer, T., Shahriar, M. S., Shams, B., Shao, L., Sharma, A., Sharma, P., Shawhan, P., Shcheblanov, N. S., Shibagaki, S., Shikauchi, M., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Soldateschi, J., Somala, S. N., Somiya, K., Son, E. J., Soni, K., Soni, S., Sordini, V., Sorrentino, F., Sorrentino, N., Sotani, H., Soulard, R., Souradeep, T., Sowell, E., Spagnuolo, V., Spencer, A. P., Spera, M., Srinivasan, R., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Steer, D. A., Steinlechner, J., Steinlechner, S., Stops, D. J., Stover, M., Strain, K. A., Strang, L. C., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V., Sugimoto, R., Suh, H. G., Summerscales, T. Z., Sun, H., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Suzuki, Takamasa, Suzuki, Toshikazu, Swinkels, B. L., Szczepańczyk, M. J., Szewczyk, P., Tacca, M., Tagoshi, H., Tait, S. C., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Talbot, C. J., Talbot, C., Tanaka, H., Tanaka, Kazuyuki, Tanaka, Kenta, Tanaka, Taiki, Tanaka, Takahiro, Tanasijczuk, A. J., Tanioka, S., Tanner, D. B., Tao, D., Tao, L., San Martín, E. N. Tapia, Taranto, C., Tasson, J. D., Telada, S., Tenorio, R., Terhune, J. E., Terkowski, L., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toivonen, A. M., Toland, K., Tolley, A. E., Tomaru, T., Tomigami, Y., Tomura, T., Tonelli, M., Torres-Forné, A., Torrie, C. I., e Melo, I. 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J., Venneberg, J., Venugopalan, G., Verkindt, D., Verma, P., Verma, Y., Veske, D., Vetrano, F., Viceré, A., Vidyant, S., Viets, A. D., Vijaykumar, A., Villa-Ortega, V., Vinet, J. -Y., Virtuoso, A., Vitale, S., Vo, T., Vocca, H., Reis, E. R. G. von, Wrangel, J. S. A. von, Vorvick, C., Vyatchanin, S. P., Wade, L. E., Wade, M., Wagner, K. J., Walet, R. C., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J., Wang, J. Z., Wang, W. H., Ward, R. L., Warner, J., Was, M., Washimi, T., Washington, N. Y., Watchi, J., Weaver, B., Webster, S. A., Weinert, M., Weinstein, A. J., Weiss, R., Weller, C. M., Wellmann, F., Wen, L., Weßels, P., Wette, K., Whelan, J. T., White, D. D., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, M. J., Williamson, A. R., Willis, J. L., Willke, B., Wilson, D. J., Winkler, W., Wipf, C. C., Wlodarczyk, T., Woan, G., Woehler, J., Wofford, J. K., Wong, I. C. F., Wu, C., Wu, D. S., Wu, H., Wu, S., Wysocki, D. M., Xiao, L., Xu, W-R., Yamada, T., Yamamoto, H., Yamamoto, Kazuhiro, Yamamoto, Kohei, Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, F. W., Yang, L., Yang, Y., Yang, Yang, Yang, Z., Yap, M. J., Yeeles, D. W., Yelikar, A. B., Ying, M., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoo, J., Yoshioka, T., Yu, Hang, Yu, Haocun, Yuzurihara, H., Zadrożny, A., Zanolin, M., Zeidler, S., Zelenova, T., Zendri, J. -P., Zevin, M., Zhan, M., Zhang, H., Zhang, J., Zhang, L., Zhang, T., Zhang, Y., Zhao, C., Zhao, G., Zhao, Y., Zhao, Yue, Zhou, R., Zhou, Z., Zhu, X. J., Zhu, Z. -H., Zucker, M. E., Zweizig, J., Antonopoulou, D., Arzoumanian, Z., Basu, A., Bogdanov, S., Cognard, I., Crowter, K., Enoto, T., Espinoza, C. M., Flynn, C. M. L., Fonseca, E., Good, D. C., Guillemot, L., Guillot, S., Harding, A. K., Keith, M. J., Kuiper, L., Lower, M. E., Lyne, A. G., Mckee, J. W., Meyers, B. W., Ng, C., Palfreyman, J. L., Shannon, R. M., Shaw, B., Stairs, I. H., Stappers, B. W., Tan, C. M., Theureau, G., Weltevrede, P., Andri??, T., Ar??ne, M., B??csy, B., Bustillo, J. Calder??n., Casanueva Diaz, J., Cavagli??, M., Cerd??-Dur??n, P., Chalathadka Subrahmanya, S., Cie??lar, M., Cordero-Carri??n, I., Cury??o, M., Dal Canton, T., Dall???osso, S., D??lya, G., D???angelo, B., D???antonio, S., Del??glise, S., D???emilio, V., D??az, M. C., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., D???onofrio, L., D???urso, D., Estell??s, H., Fronz??, G. G., Garc??a-N????ez, C., Garc??a-Quir??s, C., Gonz??lez, G., Guix??, G., Hernandez Vivanco, F., H??bner, M. T., K??f??lian, F., Kr??lak, A., La Rosa, I., Lema??tre, A., Lopez Portilla, M., L??ck, H., Hernandez, I. Maga??a., Magazz??, C., M??rka, S., M??rka, Z., Miravet-Ten??s, M., Mu??iz, E. A., Nguyen Quynh, L., O???brien, B. D., O???dell, J., O???reilly, B., O???shaughnessy, R., O???shea, E., Arellano, F. E. 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(UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Abbott, R, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andri??, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Ar??ne, M, Aritomi, N, Arnaud, N, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Aston, S, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Bailes, M, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, B??csy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhardwaj, U, Bhattacharjee, D, Bhaumik, S, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavagli??, M, Cavalier, F, Cavalieri, R, Ceasar, M, Cella, G, Cerd??-Dur??n, P, Cesarini, E, Chaibi, W, Chakravarti, K, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cie??lar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carri??n, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Cury??o, M, Dabadie, P, Dal Canton, T, Dall???osso, S, D??lya, G, Dana, A, Daneshgaranbajastani, L, D???angelo, B, Danilishin, S, D???antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Davis, M, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Del??glise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, Demarchi, L, De Matteis, F, D???emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, D??az, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D???onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Ducoin, J, Dupej, P, Durante, O, D???urso, D, Duverne, P, Dwyer, S, Eassa, C, Easter, P, Ebersold, M, Eckhardt, T, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Engelby, E, Enomoto, Y, Errico, L, Essick, R, Estell??s, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, V, Fair, H, Fairhurst, S, Farah, A, Farinon, S, Farr, B, Farr, W, Farrow, N, Fauchon-Jones, E, Favaro, G, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Fong, H, Font, J, Fornal, B, Forsyth, P, Franke, A, Frasca, S, Frasconi, F, Frederick, C, Freed, J, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fronz??, G, Fujii, Y, Fujikawa, Y, Fukunaga, M, Fukushima, M, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gair, J, Gais, J, Galaudage, S, Gamba, R, Ganapathy, D, Ganguly, A, Gao, D, Gaonkar, S, Garaventa, B, Garc??a-N????ez, C, Garc??a-Quir??s, C, Garufi, F, Gateley, B, Gaudio, S, Gayathri, V, Ge, G, Gemme, G, Gennai, A, George, J, Gerberding, O, Gergely, L, Gewecke, P, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giacoppo, L, Giaime, J, Giardina, K, Gibson, D, Gier, C, Giesler, M, Giri, P, Gissi, F, Glanzer, J, Gleckl, A, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonz??lez, G, Gopakumar, A, Gosselin, M, Gouaty, R, Gould, D, Grace, B, Grado, A, Granata, M, Granata, V, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, A, Gretarsson, E, Griffith, D, Griffiths, W, Griggs, H, Grignani, G, Grimaldi, A, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guerra, D, Guidi, G, Guimaraes, A, Guix??, G, Gulati, H, Guo, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Guzman, F, Ha, S, Haegel, L, Hagiwara, A, Haino, S, Halim, O, Hall, E, Hamilton, E, Hammond, G, Han, W, Haney, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, H, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hartwig, D, Hasegawa, K, Haskell, B, Hasskew, R, Haster, C, Hattori, K, Haughian, K, Hayakawa, H, Hayama, K, Hayes, F, Healy, J, Heidmann, A, Heidt, A, Heintze, M, Heinze, J, Heinzel, J, Heitmann, H, Hellman, F, Hello, P, Helmling-Cornell, A, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Hennig, M, Hernandez, A, Hernandez Vivanco, F, Heurs, M, Hild, S, Hill, P, Himemoto, Y, Hines, A, Hiranuma, Y, Hirata, N, Hirose, E, Ho, W, Hochheim, S, Hofman, D, Hohmann, J, Holcomb, D, Holland, N, Hollows, I, Holmes, Z, Holt, K, Holz, D, Hong, Z, Hopkins, P, Hough, J, Hourihane, S, Howell, E, Hoy, C, Hoyland, D, Hreibi, A, Hsieh, B, Hsu, Y, Huang, G, Huang, H, Huang, P, Huang, Y, H??bner, M, Huddart, A, Hughey, B, Hui, D, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Ide, S, Idzkowski, B, Iess, A, Ikenoue, B, Imam, S, Inayoshi, K, Ingram, C, Inoue, Y, Ioka, K, Isi, M, Isleif, K, Ito, K, Itoh, Y, Iyer, B, Izumi, K, Jaberianhamedan, V, Jacqmin, T, Jadhav, S, James, A, Jan, A, Jani, K, Janquart, J, Janssens, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jenner, K, Jeon, C, Jeunon, M, Jia, W, Jin, H, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Jung, P, Jung, K, Junker, J, Juste, V, Kaihotsu, K, Kajita, T, Kakizaki, M, Kalaghatgi, C, Kalogera, V, Kamai, B, Kamiizumi, M, Kanda, N, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaur, T, Kawabe, K, Kawaguchi, K, Kawai, N, Kawasaki, T, K??f??lian, F, Keitel, D, Key, J, Khadka, S, Khalili, F, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, Kimura, N, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kita, N, Kitazawa, H, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, Knyazev, E, Koch, P, Koekoek, G, Kojima, Y, Kokeyama, K, Koley, S, Kolitsidou, P, Kolstein, M, Komori, K, Kondrashov, V, Kong, A, Kontos, A, Koper, N, Korobko, M, Kotake, K, Kovalam, M, Kozak, D, Kozakai, C, Kozu, R, Kringel, V, Krishnendu, N, Kr??lak, A, Kuehn, G, Kuei, F, Kuijer, P, Kumar, A, Kumar, P, Kumar, R, Kume, J, Kuns, K, Kuo, C, Kuo, H, Kuromiya, Y, Kuroyanagi, S, Kusayanagi, K, Kuwahara, S, Kwak, K, Lagabbe, P, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, La Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lee, R, Lehmann, J, Lema??tre, A, Leonardi, M, Leroy, N, Letendre, N, Levesque, C, Levin, Y, Leviton, J, Leyde, K, Li, A, Li, B, Li, J, Li, K, Li, T, Li, X, Lin, C, Lin, F, Lin, H, Lin, L, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, G, Liu, J, Liu, K, Liu, X, Llamas, F, Llorens-Monteagudo, M, Lo, R, Lockwood, A, London, L, Longo, A, Lopez, D, Lopez Portilla, M, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lott, T, Lough, J, Lousto, C, Lovelace, G, Lucaccioni, J, L??ck, H, Lumaca, D, Lundgren, A, Luo, L, Lynam, J, Macas, R, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magazz??, C, Magee, R, Maggiore, R, Magnozzi, M, Mahesh, S, Majorana, E, Makarem, C, Maksimovic, I, Maliakal, S, Malik, A, Man, N, Mandic, V, Mangano, V, Mango, J, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marchio, M, Marion, F, Mark, Z, M??rka, S, M??rka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, M, Martinez, V, Martinovic, K, Martynov, D, Marx, E, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Mateu-Lucena, M, Matichard, F, Matiushechkina, M, Mavalvala, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mcclincy, P, Mccormick, S, Mcculler, L, Mcghee, G, Mcguire, S, Mcisaac, C, Mciver, J, Mcrae, T, Mcwilliams, S, Meacher, D, Mehmet, M, Mehta, A, Meijer, Q, Melatos, A, Melchor, D, Mendell, G, Menendez-Vazquez, A, Menoni, C, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merritt, J, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, P, Meylahn, F, Mhaske, A, Miani, A, Miao, H, Michaloliakos, I, Michel, C, Michimura, Y, Middleton, H, Milano, L, Miller, A, Miller, B, Millhouse, M, Mills, J, Milotti, E, Minazzoli, O, Minenkov, Y, Mio, N, Mir, L, Miravet-Ten??s, M, Mishra, C, Mishra, T, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Miyakawa, O, Miyamoto, A, Miyazaki, Y, Miyo, K, Miyoki, S, Mo, G, Modafferi, L, Moguel, E, Mogushi, K, Mohapatra, S, Mohite, S, Molina, I, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moragues, J, Moraru, D, Morawski, F, More, A, Moreno, C, Moreno, G, Mori, Y, Morisaki, S, Moriwaki, Y, Mours, B, Mow-Lowry, C, Mozzon, S, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Mu??iz, E, Murray, P, Musenich, R, Muusse, S, Nadji, S, Nagano, K, Nagano, S, Nagar, A, Nakamura, K, Nakano, H, Nakano, M, Nakashima, R, Nakayama, Y, Napolano, V, Nardecchia, I, Narikawa, T, Naticchioni, L, Nayak, B, Nayak, R, Negishi, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neubauer, P, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nguyen, T, Nguyen Quynh, L, Ni, W, Nichols, S, Nishizawa, A, Nissanke, S, Nitoglia, E, Nocera, F, Norman, M, North, C, Nozaki, S, Nuttall, L, Oberling, J, O???brien, B, Obuchi, Y, O???dell, J, Oelker, E, Ogaki, W, Oganesyan, G, Oh, J, Oh, K, Oh, S, Ohashi, M, Ohishi, N, Ohkawa, M, Ohme, F, Ohta, H, Okada, M, Okutani, Y, Okutomi, K, Olivetto, C, Oohara, K, Ooi, C, Oram, R, O???reilly, B, Ormiston, R, Ormsby, N, Ortega, L, O???shaughnessy, R, O???shea, E, Oshino, S, Ossokine, S, Osthelder, C, Otabe, S, Ottaway, D, Overmier, H, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, H, Pan, K, Panda, P, Pang, H, Pang, P, Pankow, C, Pannarale, F, Pant, B, Panther, F, Paoletti, F, Paoli, A, Paolone, A, Parisi, A, Park, H, Park, J, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patel, M, Pathak, M, Patricelli, B, Patron, A, Patrone, S, Paul, S, Payne, E, Pedraza, M, Pegoraro, M, Pele, A, Arellano, F, Penn, S, Perego, A, Pereira, A, Pereira, T, Perez, C, P??rigois, C, Perkins, C, Perreca, A, Perri??s, S, Petermann, J, Petterson, D, Pfeiffer, H, Pham, K, Phukon, K, Piccinni, O, Pichot, M, Piendibene, M, Piergiovanni, F, Pierini, L, Pierro, V, Pillant, G, Pillas, M, Pilo, F, Pinard, L, Pinto, I, Pinto, M, Piotrzkowski, K, Pirello, M, Pitkin, M, Placidi, E, Planas, L, Plastino, W, Pluchar, C, Poggiani, R, Polini, E, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Poulton, R, Powell, J, Pracchia, M, Pradier, T, Prajapati, A, Prasai, K, Prasanna, R, Pratten, G, Principe, M, Prodi, G, Prokhorov, L, Prosposito, P, Prudenzi, L, Puecher, A, Punturo, M, Puosi, F, Puppo, P, P??rrer, M, Qi, H, Quetschke, V, Quitzow-James, R, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Rail, S, Raja, S, Rajan, C, Ramirez, K, Ramirez, T, Ramos-Buades, A, Rana, J, Rapagnani, P, Rapol, U, Ray, A, Raymond, V, Raza, N, Razzano, M, Read, J, Rees, L, Regimbau, T, Rei, L, Reid, S, Reitze, D, Relton, P, Renzini, A, Rettegno, P, Rezac, M, Ricci, F, Richards, D, Richardson, J, Richardson, L, Riemenschneider, G, Riles, K, Rinaldi, S, Rink, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rodriguez, S, Rolland, L, Rollins, J, Romanelli, M, Romano, R, Romel, C, Romero-Rodr??guez, A, Romero-Shaw, I, Romie, J, Ronchini, S, Rosa, L, Rose, C, Rosi??ska, D, Ross, M, Rowan, S, Rowlinson, S, Roy, S, Rozza, D, Ruggi, P, Ryan, K, Sachdev, S, Sadecki, T, Sadiq, J, Sago, N, Saito, S, Saito, Y, Sakai, K, Sakai, Y, Sakellariadou, M, Sakuno, Y, Salafia, O, Salconi, L, Saleem, M, Salemi, F, Samajdar, A, Sanchez, E, Sanchez, J, Sanchez, L, Sanchis-Gual, N, Sanders, J, Sanuy, A, Saravanan, T, Sarin, N, Sassolas, B, Satari, H, Sato, S, Sato, T, Sauter, O, Savage, R, Sawada, T, Sawant, D, Sawant, H, Sayah, S, Schaetzl, D, Scheel, M, Scheuer, J, Schiworski, M, Schmidt, P, Schmidt, S, Schnabel, R, Schneewind, M, Schofield, R, Sch??nbeck, A, Schulte, B, Schutz, B, Schwartz, E, Scott, J, Scott, S, Seglar-Arroyo, M, Sekiguchi, T, Sekiguchi, Y, Sellers, D, Sengupta, A, Sentenac, D, Seo, E, Sequino, V, Sergeev, A, Setyawati, Y, Shaffer, T, Shahriar, M, Shams, B, Shao, L, Sharma, A, Sharma, P, Shawhan, P, Shcheblanov, N, Shibagaki, S, Shikauchi, M, Shimizu, R, Shimoda, T, Shimode, K, Shinkai, H, Shishido, T, Shoda, A, Shoemaker, D, Shyamsundar, S, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singha, A, Sintes, A, Sipala, V, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smetana, J, Smith, J, Smith, R, Soldateschi, J, Somala, S, Somiya, K, Son, E, Soni, K, Soni, S, Sordini, V, Sorrentino, F, Sorrentino, N, Sotani, H, Soulard, R, Souradeep, T, Sowell, E, Spagnuolo, V, Spencer, A, Spera, M, Srinivasan, R, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Steer, D, Steinlechner, J, Steinlechner, S, Stops, D, Stover, M, Strain, K, Strang, L, Stratta, G, Strunk, A, Sturani, R, Stuver, A, Sudhagar, S, Sudhir, V, Sugimoto, R, Suh, H, Summerscales, T, Sun, H, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Suzuki, T, Swinkels, B, Szczepa??czyk, M, Szewczyk, P, Tacca, M, Tagoshi, H, Tait, S, Takahashi, H, Takahashi, R, Takamori, A, Takano, S, Takeda, H, Takeda, M, Talbot, C, Tanaka, H, Tanaka, K, Tanaka, T, Tanasijczuk, A, Tanioka, S, Tanner, D, Tao, D, Tao, L, Tapia San Mart??n, E, Taranto, C, Tasson, J, Telada, S, Tenorio, R, Terhune, J, Terkowski, L, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toivonen, A, Toland, K, Tolley, A, Tomaru, T, Tomigami, Y, Tomura, T, Tonelli, M, Torres-Forn??, A, Torrie, C, Tosta e Melo, I, T??yr??, D, Trapananti, A, Travasso, F, Traylor, G, Trevor, M, Tringali, M, Tripathee, A, Troiano, L, Trovato, A, Trozzo, L, Trudeau, R, Tsai, D, Tsang, K, Tsang, T, Tsao, J, Tse, M, Tso, R, Tsubono, K, Tsuchida, S, Tsukada, L, Tsuna, D, Tsutsui, T, Tsuzuki, T, Turbang, K, Turconi, M, Tuyenbayev, D, Ubhi, A, Uchikata, N, Uchiyama, T, Udall, R, Ueda, A, Uehara, T, Ueno, K, Ueshima, G, Unnikrishnan, C, Uraguchi, F, Urban, A, Ushiba, T, Utina, A, Vahlbruch, H, Vajente, G, Vajpeyi, A, Valdes, G, Valentini, M, Valsan, V, van Bakel, N, van Beuzekom, M, van den Brand, J, Van Den Broeck, C, Vander-Hyde, D, van der Schaaf, L, van Heijningen, J, Vanosky, J, van Putten, M, van Remortel, N, Vardaro, M, Vargas, A, Varma, V, Vas??th, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venneberg, J, Venugopalan, G, Verkindt, D, Verma, P, Verma, Y, Veske, D, Vetrano, F, Vicer??, A, Vidyant, S, Viets, A, Vijaykumar, A, Villa-Ortega, V, Vinet, J, Virtuoso, A, Vitale, S, Vo, T, Vocca, H, von Reis, E, von Wrangel, J, Vorvick, C, Vyatchanin, S, Wade, L, Wade, M, Wagner, K, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, W, Ward, R, Warner, J, Was, M, Washimi, T, Washington, N, Watchi, J, Weaver, B, Webster, S, Weinert, M, Weinstein, A, Weiss, R, Weller, C, Wellmann, F, Wen, L, We??els, P, Wette, K, Whelan, J, White, D, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, M, Williamson, A, Willis, J, Willke, B, Wilson, D, Winkler, W, Wipf, C, Wlodarczyk, T, Woan, G, Woehler, J, Wofford, J, Wong, I, Wu, C, Wu, D, Wu, H, Wu, S, Wysocki, D, Xiao, L, Xu, W, Yamada, T, Yamamoto, H, Yamamoto, K, Yamamoto, T, Yamashita, K, Yamazaki, R, Yang, F, Yang, L, Yang, Y, Yang, Z, Yap, M, Yeeles, D, Yelikar, A, Ying, M, Yokogawa, K, Yokoyama, J, Yokozawa, T, Yoo, J, Yoshioka, T, Yu, H, Yuzurihara, H, Zadro??ny, A, Zanolin, M, Zeidler, S, Zelenova, T, Zendri, J, Zevin, M, Zhan, M, Zhang, H, Zhang, J, Zhang, L, Zhang, T, Zhang, Y, Zhao, C, Zhao, G, Zhao, Y, Zhou, R, Zhou, Z, Zhu, X, Zhu, Z, Zucker, M, Zweizig, J, Antonopoulou, D, Arzoumanian, Z, Basu, A, Bogdanov, S, Cognard, I, Crowter, K, Enoto, T, Espinoza, C, Flynn, C, Fonseca, E, Good, D, Guillemot, L, Guillot, S, Harding, A, Keith, M, Kuiper, L, Lower, M, Lyne, A, Mckee, J, Meyers, B, Ng, C, Palfreyman, J, Shannon, R, Shaw, B, Stairs, I, Stappers, B, Tan, C, Theureau, G, Weltevrede, P, National Science Foundation (US), National Aeronautics and Space Administration (US), Science and Technology Facilities Council (UK), Generalitat Valenciana, Generalitat de Catalunya, European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Govern de les Illes Balears, Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, Physics, Theoretical Physics, Elementary Particle Physics, Faculty of Sciences and Bioengineering Sciences, Andric, T., Arai, K., Arene, M., Becsy, B., Bustillo, J. C., Diaz, J. C., Cavaglia, M., Cerda-Duran, P., Subrahmanya, S. C., Chatterjee, D., Chiang, C. -Y., Chu, Y. -K., Cieslar, M., Cordero-Carrion, I., Curylo, M., Canton, T. D., Dall'Osso, S., Dalya, G., D'Angelo, B., D'Antonio, S., Deleglise, S., D'Emilio, V., Diaz, M. C., Fiore, L. D., Fronzo, C. D., Giorgio, C. D., Giovanni, F. D., Giovanni, M. D., Lieto, A. D., Pace, S. D., Palma, I. D., Renzo, F. D., D'Onofrio, L., D'Urso, D., Estelles, H., Fronze, G. G., Garcia-Nunez, C., Garcia-Quiros, C., Ghosh, A., Ghosh, S., Gonzalez, G., Guixe, G., Gupta, A., Vivanco, F. H., Hsieh, B. -H., Huang, G. -Z., Huang, H. -Y., Huang, Y. -C., Hubner, M. T., Kefelian, F., Krolak, A., Kumar, R., Kuo, H. -S., Rosa, I. L., Lemaitre, A., Lin, C. -Y., Lin, F. -K., Lin, F. -L., Portilla, M. B., Luck, H., Hernandez, I. M., Magazzu, C., Marka, S., Marka, Z., Mir, L. M., Miravet-Tenes, M., Mo, G., Mukherjee, A., Mukherjee, S., Muniz, E. A., Quynh, L. N., O'Brien, B. D., O'Dell, J., O'Reilly, B., O'Shaughnessy, R., O'Shea, E., Arellano, F. E. P., Perigois, C., Perries, S., Purrer, M., Romero-Rodriguez, A., Rosinska, D., Schonbeck, A., Suzuki, T., Szczepanczyk, M. J., Tanaka, K., Tanaka, T., San Martin, E. N. T., Tiwari, S., Torres-Forne, A., E Melo, I. T., Toyra, D., Tsao, J. -S., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Der Schaaf, L., Van Heijningen, J. V., Van Putten, M. H. P. M., Van Remortel, N., Vasuth, M., Vicere, A., Reis, E. R. G. V., Wrangel, J. S. A. V., Wessels, P., Xu, W. -R., Yamamoto, K., Yu, H., Zadrozny, A., RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, and RS: FSE MSP

Subjects
Gravitational wave astronomy, Neutron stars, Pulsars, long-lived, Astronomy, frequency: time dependence, spin, General Relativity and Quantum Cosmology, PRECISE, QC350, LIGO, neutron star, QC, pulsar, QB, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, constraint: energy, gravitational radiation: time dependence, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, asymmetry, PROPER MOTION, radiation: electromagnetic, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Neutron star, O3, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, Transients, energy loss: rotation, SPIN-DOWN LIMIT, Neutron Stars, Transients, Gravitational Waves, LIGO, Virgo, O3, SDG 7 - Affordable and Clean Energy, Gravitational Waves, Science & Technology, GLITCHES, Virgo, CONSTRAINTS, Astronomy and Astrophysics, Neutron Stars, sensitivity, Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie, VIRGO, Physics and Astronomy, Space and Planetary Science, DISCOVERY, DISTANCE, ddc:520, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], EMISSION, ENERGETIC YOUNG PULSAR
Abstract

Abbott et al., Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours–months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets., This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO), for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación (AEI), the Spanish Ministerio de Ciencia e Innovación and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcció General de Política Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d'Innovació Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union—European Regional Development Fund; Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provision of computational resources. This work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF), Computing Infrastructure Project of KISTI-GSDC, Korea Astronomy and Space Science Institute (KASI), and Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. We acknowledge that CHIME is located on the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (Project 31170) and by contributions from the provinces of British Columbia, Québec, and Ontario. The CHIME/FRB Project, which enabled development in common with the CHIME/Pulsar instrument, is funded by a grant from the CFI 2015 Innovation Fund (Project 33213) and by contributions from the provinces of British Columbia and Québec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University, and the McGill Space Institute thanks to the Trottier Family Foundation, and the University of British Columbia. The CHIME/Pulsar instrument hardware was funded by NSERC RTI-1 grant EQPEQ 458893-2014. This research was enabled in part by support provided by WestGrid (www.westgrid.ca) and Compute Canada (www.computecanada.ca). We acknowledge support from the Natural Sciences and Engineering Research Council of Canada (NSERC) funding reference #CITA 490888-16, the Canadian Institute for Advanced Research, and the UBC Four Year Fellowship (6456). We acknowledge support from EPSRC/STFC fellowship (EP/T017325/1), ANID/FONDECYT grants 1171421 and 1211964, and NASA grants 80NSSC19K1444 and 80NSSC21K0091. This work is supported by NASA through the NICER mission and the Astrophysics Explorers Program, and uses data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory.

Published
2022

40. Foliar‐applied sulfate and potassium does not reduce rice grain arsenic concentrations nor straighthead severity.

Author

Pinson, Shannon R. M., Heuschele, Deborah Jo, Isbell, Chris, Li, Jifeng, Vandal, Matthew P., and Smith, Aaron P.

Subjects
*POTASSIUM sulfate, *ARSENIC, *SULFUR fertilizers, *RICE, *PLANT genetics, *FOLIAR feeding, *GRAIN, *CULTIVARS
Abstract

Arsenic (As) is naturally present in all soils and can accumulate to toxic levels in rice (Oryza sativa L.) grains under some production conditions. It can also reduce grain yields, posing a double threat to global food security. Plant genetics can affect the amount of As accumulated in grains. A growing body of evidence suggests that one mechanism plants use to detoxify As and limit As concentrations in grains (grain‐As) is to sequester As in vegetative tissues. We evaluated 17 rice cultivars previously shown to have contrastingly high or low grain‐As. Cultivars high in grain‐As commonly transferred As out of their flag leaves during grain fill, while all eight cultivars having low grain‐As retained As in flag leaves, effectively excluding it from transfer to developing grains. Sequestration of As in cell vacuoles involves several sulfur (S)‐containing compounds. We hypothesized that enhanced leaf concentration of S via foliar fertilization could further reduce grain‐As. Effect of foliar‐S on grain‐As was studied in field‐scale and plot experiments. The plot study included cultivars known to contrastingly retain As in flag leaves during grain fill grown in both As‐enriched and Native (non‐enriched) soils, and included severity ratings for rice straighthead, an As‐induced disorder. Contrary to the hypothesis, while foliar‐S did increase grain‐S concentrations, it did not prove useful for reducing grain‐As, nor did it reduce straighthead severity, possibly because soil was not deficient in S or plants used a biochemical mechanism other than S‐related As chelation and sequestration to retain As in leaves. Core Ideas: Some rice cultivars accumulate less arsenic in their grains than other rice cultivars.Cultivars with lower grain arsenic continue accumulating arsenic in flag leaves during grain fill.Cultivars with higher grain arsenic remobilize arsenic out of flag leaves during grain fill.Results suggest grain arsenic is reduced by increasing leaf sequestration, involving sulfur‐containing compounds.Foliar‐applied sulfur fertilizer did not reduce grain arsenic concentrations under study conditions. [ABSTRACT FROM AUTHOR]

Published
2023
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41. Pulsar polarization: a broad-band population view with the Parkes Ultra-Wideband receiver.

Author

Oswald, L S, Johnston, S, Karastergiou, A, Dai, S, Kerr, M, Lower, M E, Manchester, R N, Shannon, R M, Sobey, C, and Weltevrede, P

Subjects
RADIO telescopes, CIRCULAR polarization, LINEAR polarization, BREWSTER'S angle, PULSARS
Abstract

The radio polarization properties of the pulsar population are only superficially captured by the conventional picture of pulsar radio emission. We study the broadband polarization of 271 young radio pulsars, focusing particularly on circular polarization, using high-quality observations made with the Ultra-Wideband Low receiver on Murriyang, the Parkes radio telescope. We seek to encapsulate polarization behaviour on a population scale by defining broad categories for frequency- and phase-dependent polarization evolution, studying the co-occurrences of these categorizations and comparing them with average polarization measurements and spin-down energy (⁠|$\dot{E}$|⁠). This work shows that deviations of the linear polarization position angle from the rotating vector model are linked to the presence of circular polarization features and to frequency evolution of the polarization. Polarization fraction, circular polarization contribution, and profile complexity all evolve with |$\dot{E}$| across the population, with the profiles of high- |$\dot{E}$| pulsars being simple and highly linearly polarized. The relationship between polarization fraction and circular contribution is also seen to evolve such that highly polarized profiles show less variation in circular contribution with frequency than less strongly polarized profiles. This evolution is seen both across the population and across frequency for individual sources. Understanding pulsar radio polarization requires detailed study of individual sources and collective understanding of population-level trends. For the former, we provide visualizations of their phase- and frequency-resolved polarization parameters. For the latter, we have highlighted the importance of including the impact of circular polarization and of |$\dot{E}$|⁠. [ABSTRACT FROM AUTHOR]

Published
2023
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42. Searches for Shapiro delay in seven binary pulsars using the MeerKAT telescope.

Author

Shamohammadi, M, Bailes, M, Freire, P C C, Parthasarathy, A, Reardon, D J, Shannon, R M, Venkatraman Krishnan, V, Bernadich, M C i, Cameron, A D, Champion, D J, Corongiu, A, Flynn, C, Geyer, M, Kramer, M, Miles, M T, Possenti, A, and Spiewak, R

Subjects
MEERKAT, BINARY pulsars, PULSARS, NEUTRON stars, DATA quality, SPACETIME, RADIO telescopes
Abstract

Precision timing of millisecond pulsars (MSPs) in binary systems enables observers to detect the relativistic Shapiro delay induced by space–time curvature. When favourably aligned, this enables constraints to be placed on the component masses and system orientation. Here, we present the results of timing campaigns on seven binary MSPs observed with the 64-antenna MeerKAT radio telescope that show evidence of Shapiro delay: PSRs J0101−6422, J1101−6424, J1125−6014, J1514−4946, J1614−2230, J1732−5049, and J1909−3744. Evidence for Shapiro delay was found in all of the systems, and for three the orientations and data quality enabled strong constraints on their orbital inclinations and component masses. For PSRs J1125−6014, J1614−2230, and J1909−3744, we determined pulsar masses to be |$M_{\rm p} = 1.68\pm 0.17$|⁠ , |$1.94\pm 0.03$|⁠ , and |$1.45 \pm 0.03 \, {\rm M_{\odot }}$|⁠ , and companion masses to be |$M_{\rm c} = 0.33\pm 0.02$|⁠ , |$0.495\pm 0.005$|⁠ , and |$0.205 \pm 0.003 \, {\rm M_{\odot }}$|⁠ , respectively. This provides the first independent confirmation of PSR J1614−2230's mass, one of the highest known. The Shapiro delays measured for PSRs J0101−6422, J1101−6424, J1514−4946, and J1732−5049 were only weak, and could not provide interesting component mass limits. Despite a large number of MSPs being routinely timed, relatively few have accurate masses via Shapiro delays. We use simulations to show that this is expected, and provide a formula for observers to assess how accurately a pulsar mass can be determined. We also discuss the observed correlation between pulsar companion masses and spin period, and the anticorrelation between recycled pulsar mass and their companion masses. [ABSTRACT FROM AUTHOR]

Published
2023
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43. Analysis of the ionized interstellar medium and orbital dynamics of PSR J1909-3744 using scintillation arcs.

Author

Askew, J, Reardon, D J, and Shannon, R M

Subjects
INTERSTELLAR medium, RADIO telescopes, ORBITS (Astronomy), PULSARS, POWER spectra, BINARY pulsars
Abstract

Long-term studies of binary millisecond pulsars (MSPs) provide precise tests of strong-field gravity, and can be used to measure neutron-star masses. PSR J1909-3744, a binary MSP has been the subject of several pulsar timing analyses. The edge-on orbit enables measurement of its mass using the Shapiro delay; however, there is degeneracy in the sense of the inclination angle, i , and multiple solutions for the longitude of ascending node, Ω. Radio pulsars scintillate due to inhomogeneities in the ionized interstellar medium (IISM). This can result in scintillation arcs in the power spectrum of the dynamic spectrum that can use these to study the interstellar medium and constrain binary pulsar orbits. Here, we study the scintillation of PSR J1909-3744 using observations from the 64-m Parkes Radio Telescope (Murriyang) over ≈13 yr, using techniques to study scintillation in a lower signal-to-noise regime. By monitoring annual and orbital variations of the arc-curvature measurements, we are able to characterize the velocity of the IISM. We find that the statistics of the IISM remained stationary over this time and a slightly anisotropic model (axial ratio ≳1.2) is preferred. We measure the relative distance to a single dominant thin scattering screen at s  = 0.49 ± 0.04, or D s = 590 ± 50 pc, with an angle of anisotropy ζ = 85 ± 6° (East of North) and velocity in the direction of anisotropy V IISM,ζ = 14 ± 10 km s−1. By combining a physical model of the IISM and current pulsar timing results, we also constrain Ω = 225 ± 3° and i  = 86.46 ± 0.05°. [ABSTRACT FROM AUTHOR]

Published
2023
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44. The MeerKAT Pulsar Timing Array: first data release.

Author

Miles, M T, Shannon, R M, Bailes, M, Reardon, D J, Keith, M J, Cameron, A D, Parthasarathy, A, Shamohammadi, M, Spiewak, R, van Straten, W, Buchner, S, Camilo, F, Geyer, M, Karastergiou, A, Kramer, M, Serylak, M, Theureau, G, and Venkatraman Krishnan, V

Subjects
*DATA release, *PULSARS, *MEERKAT, *GRAVITATIONAL waves, *COMMUNITIES
Abstract

We present the first 2.5 yr of data from the MeerKAT Pulsar Timing Array (MPTA), part of MeerTime, a MeerKAT Large Survey Project. The MPTA aims to precisely measure pulse arrival times from an ensemble of 88 pulsars visible from the Southern hemisphere, with the goal of contributing to the search, detection, and study of nanohertz-frequency gravitational waves as part of the International Pulsar Timing Array. This project makes use of the MeerKAT telescope and operates with a typical observing cadence of 2 weeks using the L-band receiver that records data from 856 to 1712 MHz. We provide a comprehensive description of the observing system, software, and pipelines used and developed for the MeerTime project. The data products made available as part of this data release are from the 78 pulsars that had at least 30 observations between the start of the MeerTime programme in February 2019 and October 2021. These include both sub-banded and band-averaged arrival times and the initial timing ephemerides, noise models, and the frequency-dependent standard templates (portraits) used to derive pulse arrival times. After accounting for detected noise processes in the data, the frequency-averaged residuals of 67 of the pulsars achieved a root-mean-square residual precision of |$\lt 1 \, \mu \rm {s}$|⁠. We also present a novel recovery of the clock correction waveform solely from pulsar timing residuals and an exploration into preliminary findings of interest to the international pulsar timing community. The arrival times, standards, and full Stokes parameter-calibrated pulsar timing archives are publicly available. [ABSTRACT FROM AUTHOR]

Published
2023
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45. Socio-Technical Changes for Sustainable Rice Production: Rice Husk Amendment, Conservation Irrigation, and System Changes

Author

C. Reavis, Matthew C. Reid, M. Arlene A. Adviento-Borbe, Shannon R. M. Pinson, Beatriz Moreno-García, Benjamin R. K. Runkle, Jasquelin Peña, Chris Isbell, Matt A. Limmer, Angelia L. Seyfferth, and Michele L. Reba

Subjects
Irrigation, rice, Conservation agriculture, grain quality, food and beverages, silicon, Plant culture, Agriculture, Staple food, Agricultural engineering, General Medicine, sustainability, SB1-1110, conservation agriculture, circular food system, Greenhouse gas, Sustainability, Production (economics), Environmental science, Surface irrigation, Water use
Abstract

Rice is a staple food and primary source of calories for much of the world. However, rice can be a dietary source of toxic metal(loid)s to humans, and its cultivation creates atmospheric greenhouse gas emissions and requires high water use. Because rice production consumes a significant amount of natural resources and is a large part of the global agricultural economy, increasing its sustainability could have substantial societal benefits. There are opportunities for more sustainable field production through a combination of silicon (Si) management and conservation irrigation practices. As a Si-rich soil amendment, rice husks can limit arsenic and cadmium uptake, while also providing plant vigor in drier soil conditions. Thus, husk addition and conservation irrigation may be more effective to attenuate the accumulation of toxic metal(loid)s, manage water usage and lower climate impacts when implemented together than when either is implemented separately. This modified field production system would take advantage of rice husks, which are an underutilized by-product of milled rice that is widely available near rice farm sites, and have ~10% Si content. Husk application could, alongside alternate wetting and drying or furrow irrigation management, help resolve multiple sustainability challenges in rice production: (1) limit arsenic and cadmium accumulation in rice; (2) minimize greenhouse gas emissions from rice production; (3) decrease irrigation water use; (4) improve nutrient use efficiency; (5) utilize a waste product of rice processing; and (6) maintain plant-accessible soil Si levels. This review presents the scientific basis for a shift in rice production practices and considers complementary rice breeding efforts. It then examines socio-technical considerations for how such a shift in production practices could be implemented by farmers and millers together and may bring rice production closer to a bio-circular economy. This paper's purpose is to advocate for a changed rice production method for consideration by community stakeholders, including producers, millers, breeders, extension specialists, supply chain organizations, and consumers, while highlighting remaining research and implementation questions.

Published
2021
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46. Summary of session C1: pulsar timing arrays

Author

Shannon, R. M., Chamberlin, S., Cornish, N. J., Ellis, J. A., Mingarelli, C. M. F., Perrodin, D., Rosado, P., Sesana, A., Taylor, S. R., Wen, L., Bassa, C. G., Gair, J., Janssen, G. H., Karuppusamy, R., Kramer, M., Lee, K. J., Liu, K., Mandel, I., Purver, M., Sidery, T., Smits, R., Stappers, B. W., and Vecchio, A.

Published
2014
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48. Curcumin Ingestion Inhibits Mastocytosis and Suppresses Intestinal Anaphylaxis in a Murine Model of Food Allergy.

Author

Shannon R M Kinney, Logan Carlson, Jennifer Ser-Dolansky, Chelsea Thompson, Sagar Shah, Amos Gambrah, Wei Xing, Sallie S Schneider, and Clinton B Mathias

Subjects
Medicine, Science
Abstract

IgE antibodies and mast cells play critical roles in the establishment of allergic responses to food antigens. Curcumin, the active ingredient of the curry spice turmeric, has anti-inflammatory properties, and thus may have the capacity to regulate Th2 cells and mucosal mast cell function during allergic responses. We assessed whether curcumin ingestion during oral allergen exposure can modulate the development of food allergy using a murine model of ovalbumin (OVA)-induced intestinal anaphylaxis. Herein, we demonstrate that frequent ingestion of curcumin during oral OVA exposure inhibits the development of mastocytosis and intestinal anaphylaxis in OVA-challenged allergic mice. Intragastric (i.g.) exposure to OVA in sensitized BALB/c mice induced a robust IgE-mediated response accompanied by enhanced OVA-IgE levels, intestinal mastocytosis, elevated serum mMCP-1, and acute diarrhea. In contrast, mice exposed to oral curcumin throughout the experimental regimen appeared to be normal and did not exhibit intense allergic diarrhea or a significant enhancement of OVA-IgE and intestinal mast cell expansion and activation. Furthermore, allergic diarrhea, mast cell activation and expansion, and Th2 responses were also suppressed in mice exposed to curcumin during the OVA-challenge phase alone, despite the presence of elevated levels of OVA-IgE, suggesting that curcumin may have a direct suppressive effect on intestinal mast cell activation and reverse food allergy symptoms in allergen-sensitized individuals. This was confirmed by observations that curcumin attenuated the expansion of both adoptively transferred bone marrow-derived mast cells (BMMCs), and inhibited their survival and activation during cell culture. Finally, the suppression of intestinal anaphylaxis by curcumin was directly linked with the inhibition of NF-κB activation in curcumin-treated allergic mice, and curcumin inhibited the phosphorylation of the p65 subunit of NF-κB in BMMCs. In summary, our data demonstrates a protective role for curcumin during allergic responses to food antigens, suggesting that frequent ingestion of this spice may modulate the outcome of disease in susceptible individuals.

Published
2015
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