ORCID Profile
0000-0002-4824-101X
Current Organisation
University of Melbourne
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In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Atomic, Molecular, Nuclear, Particle and Plasma Physics | Nuclear And Particle Physics | Instruments And Techniques | Particle Physics | Information Storage, Retrieval And Management | Distributed and Grid Systems | Particle physics | Synchrotrons; Accelerators; Instruments and Techniques | Cloud computing | Information Systems Management | Particle and high energy physics | Instruments and techniques | Distributed Computing not elsewhere classified | Global Information Systems |
Physical sciences | Expanding Knowledge in the Physical Sciences | Information processing services | Computer software and services not elsewhere classified | Information Processing Services (incl. Data Entry and Capture) | Electronic Information Storage and Retrieval Services | Information and Communication Services not elsewhere classified | Scientific Instruments |
Publisher: Springer Science and Business Media LLC
Date: 10-2021
Abstract: Charged lepton flavor violation is forbidden in the Standard Model but possible in several new physics scenarios. In many of these models, the radiative decays τ ± → ℓ ± γ ( ℓ = e, μ ) are predicted to have a sizeable probability, making them particularly interesting channels to search at various experiments. An updated search via τ ± → ℓ ± γ using full data of the Belle experiment, corresponding to an integrated luminosity of 988 fb − 1 , is reported for charged lepton flavor violation. No significant excess over background predictions from the Standard Model is observed, and the upper limits on the branching fractions, $$ \\mathcal{B} $$ B ( τ ± → μ ± γ ) ≤ 4 . 2 × 10 − 8 and $$ \\mathcal{B} $$ B ( τ ± → e ± γ ) ≤ 5 . 6 × 10 − 8 , are set at 90% confidence level.
Publisher: American Physical Society (APS)
Date: 21-05-2007
Publisher: American Physical Society (APS)
Date: 26-04-2002
Publisher: Oxford University Press (OUP)
Date: 13-12-2022
Abstract: Neighborhood places that facilitate older residents to meet and interact (third places) receive an increasing research interest as studies have consistently shown the benefits of social engagement for older adults’ health. This scoping review synthesized the findings of studies examining the role of third places in older adults’ social engagement. Searching 5 databases (CINAHL, Medline, PsycInfo, Scopus, and Web of Science) in October 2021, this study identified quantitative and qualitative studies that examined the relationships between third places and social engagement (interaction and network) among older adults. A total of 32 studies (12 quantitative and 20 qualitative studies) met the eligibility criteria. These studies examined 4 types of third place, namely, community facilities, local businesses, open/green spaces, and transition spaces. More than two thirds of the studies reviewed found that access to community facilities, local businesses, and open/green spaces were related to older adults’ social interaction. For the relationships between third places and social networks, the importance of accessible local businesses and the quality of open/green spaces was supported by fewer studies. The findings of quantitative and qualitative studies suggest that local places that are convenient to visit and comfortable to stay in for older adults are likely to enhance their social interaction and network. However, more specific evidence is needed to inform the planning and design of third places. The review discusses future research topics that address the gaps identified in the current literature.
Publisher: American Physical Society (APS)
Date: 18-01-2019
Publisher: Physical Society of Japan
Date: 15-07-2007
Publisher: Springer Science and Business Media LLC
Date: 27-04-2021
Publisher: American Physical Society (APS)
Date: 06-2007
Publisher: American Physical Society (APS)
Date: 08-04-2002
Publisher: American Physical Society (APS)
Date: 25-01-2018
Publisher: American Physical Society (APS)
Date: 09-06-2006
Publisher: Elsevier BV
Date: 2002
Publisher: American Physical Society (APS)
Date: 24-03-2011
Publisher: American Physical Society (APS)
Date: 22-02-2007
Publisher: American Physical Society (APS)
Date: 09-06-2006
Publisher: Springer Science and Business Media LLC
Date: 19-01-2202
Publisher: American Physical Society (APS)
Date: 28-01-2004
Publisher: American Physical Society (APS)
Date: 28-09-2010
Publisher: American Physical Society (APS)
Date: 29-06-2006
Publisher: American Physical Society (APS)
Date: 10-11-2010
Publisher: American Physical Society (APS)
Date: 13-05-2008
Publisher: American Physical Society (APS)
Date: 08-09-2021
Publisher: American Physical Society (APS)
Date: 18-09-2007
Publisher: American Physical Society (APS)
Date: 26-10-2010
Publisher: American Physical Society (APS)
Date: 1997
Publisher: American Physical Society (APS)
Date: 20-05-1991
Publisher: American Physical Society (APS)
Date: 27-02-2202
Publisher: American Physical Society (APS)
Date: 13-07-2004
Publisher: Elsevier BV
Date: 2019
Publisher: American Physical Society (APS)
Date: 29-04-2004
Publisher: Springer Science and Business Media LLC
Date: 30-11-2021
DOI: 10.1007/S41781-021-00075-X
Abstract: Quantum computers have the potential to speed up certain computational tasks. A possibility this opens up within the field of machine learning is the use of quantum techniques that may be inefficient to simulate classically but could provide superior performance in some tasks. Machine learning algorithms are ubiquitous in particle physics and as advances are made in quantum machine learning technology there may be a similar adoption of these quantum techniques. In this work a quantum support vector machine (QSVM) is implemented for signal-background classification. We investigate the effect of different quantum encoding circuits, the process that transforms classical data into a quantum state, on the final classification performance. We show an encoding approach that achieves an average Area Under Receiver Operating Characteristic Curve (AUC) of 0.848 determined using quantum circuit simulations. For this same dataset the best classical method tested, a classical Support Vector Machine (SVM) using the Radial Basis Function (RBF) Kernel achieved an AUC of 0.793. Using a reduced version of the dataset we then ran the algorithm on the IBM Quantum ibmq_casablanca device achieving an average AUC of 0.703. As further improvements to the error rates and availability of quantum computers materialise, they could form a new approach for data analysis in high energy physics.
Publisher: American Physical Society (APS)
Date: 17-11-2006
Publisher: American Physical Society (APS)
Date: 21-08-2001
Publisher: American Physical Society (APS)
Date: 20-11-2001
Publisher: Elsevier BV
Date: 12-2005
Publisher: Elsevier BV
Date: 02-1993
Publisher: American Physical Society (APS)
Date: 03-02-2004
Publisher: American Physical Society (APS)
Date: 04-2011
Publisher: American Physical Society (APS)
Date: 30-11-2020
Publisher: American Physical Society (APS)
Date: 28-06-2010
Publisher: Elsevier BV
Date: 2008
Publisher: American Physical Society (APS)
Date: 28-10-2008
Publisher: Elsevier BV
Date: 08-1998
Publisher: American Physical Society (APS)
Date: 07-1988
Publisher: Elsevier BV
Date: 03-2012
Publisher: American Physical Society (APS)
Date: 12-09-2008
Publisher: Elsevier BV
Date: 05-2011
Publisher: American Physical Society (APS)
Date: 27-06-2013
Publisher: American Physical Society (APS)
Date: 12-04-2010
Publisher: Elsevier BV
Date: 04-1995
Publisher: American Physical Society (APS)
Date: 14-04-2021
Publisher: Springer Science and Business Media LLC
Date: 03-2021
Abstract: We present measurements of the branching fractions for the decays B → Kμ + μ − and B → Ke + e − , and their ratio ( R K ), using a data s le of 711 fb − 1 that contains 772 × 10 6 $$ B\\overline{B} $$ B B ¯ events. The data were collected at the ϒ(4 S ) resonance with the Belle detector at the KEKB asymmetric-energy e + e − collider. The ratio R K is measured in five bins of dilepton invariant-mass-squared ( q 2 ): q 2 ∈ (0 . 1 , 4 . 0) , (4 . 00 , 8 . 12) , (1 . 0 , 6 . 0), (10 . 2 , 12 . 8) and ( 14 . 18) GeV 2 /c 4 , along with the whole q 2 region. The R K value for q 2 ∈ (1 . 0 , 6 . 0) GeV 2 /c 4 is $$ {1.03}_{-0.24}^{+0.28} $$ 1.03 − 0.24 + 0.28 ± 0 . 01. The first and second uncertainties listed are statistical and systematic, respectively. All results for R K are consistent with Standard Model predictions. We also measure CP -averaged isospin asymmetries in the same q 2 bins. The results are consistent with a null asymmetry, with the largest difference of 2.6 standard deviations occurring for the q 2 ∈ (1 . 0 , 6 . 0) GeV 2 /c 4 bin in the mode with muon final states. The measured differential branching fractions, $$ d\\mathrm{\\mathcal{B}} $$ d ℬ /dq 2 , are consistent with theoretical predictions for charged B decays, while the corresponding values are below the expectations for neutral B decays. We have also searched for lepton-flavor-violating B → Kμ ± e ∓ decays and set 90% confidence-level upper limits on the branching fraction in the range of 10 − 8 for B + → K + μ ± e ∓ , and B 0 → K 0 μ ± e ∓ modes.
Publisher: American Physical Society (APS)
Date: 03-1998
Publisher: American Physical Society (APS)
Date: 26-07-2004
Publisher: Elsevier BV
Date: 11-2008
Publisher: American Physical Society (APS)
Date: 09-03-2018
Publisher: Elsevier BV
Date: 10-1985
Publisher: Elsevier BV
Date: 06-1985
Publisher: American Physical Society (APS)
Date: 14-10-2020
Publisher: American Physical Society (APS)
Date: 07-08-2009
Publisher: American Physical Society (APS)
Date: 03-04-2008
Publisher: American Physical Society (APS)
Date: 12-07-2021
Publisher: American Physical Society (APS)
Date: 12-07-2021
Publisher: Elsevier BV
Date: 10-2000
Publisher: Springer Science and Business Media LLC
Date: 2003
Publisher: American Physical Society (APS)
Date: 19-07-2019
Publisher: American Physical Society (APS)
Date: 25-08-2010
Publisher: Elsevier BV
Date: 08-2005
Publisher: American Physical Society (APS)
Date: 16-08-2021
Publisher: American Physical Society (APS)
Date: 10-07-2019
Publisher: American Physical Society (APS)
Date: 20-03-2009
Publisher: Springer Science and Business Media LLC
Date: 03-2008
DOI: 10.1038/NATURE06827
Publisher: American Physical Society (APS)
Date: 29-08-2002
Publisher: American Physical Society (APS)
Date: 20-05-1991
Publisher: American Physical Society (APS)
Date: 04-05-2007
Publisher: American Physical Society (APS)
Date: 31-08-2017
Publisher: American Physical Society (APS)
Date: 10-06-2011
Publisher: Springer Science and Business Media LLC
Date: 11-2014
Publisher: American Physical Society (APS)
Date: 02-1992
Publisher: American Physical Society (APS)
Date: 19-05-2008
Publisher: Oxford University Press (OUP)
Date: 02-2018
DOI: 10.1093/PTEP/PTY003
Publisher: American Physical Society (APS)
Date: 04-02-2010
Publisher: Elsevier BV
Date: 05-1998
Publisher: American Physical Society (APS)
Date: 10-08-2006
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 08-2001
DOI: 10.1109/23.958712
Publisher: American Physical Society (APS)
Date: 27-03-2008
Publisher: Elsevier BV
Date: 10-2013
Publisher: American Physical Society (APS)
Date: 12-07-2007
Publisher: American Physical Society (APS)
Date: 23-03-2011
Publisher: American Physical Society (APS)
Date: 23-10-1989
Publisher: American Physical Society (APS)
Date: 14-06-2019
Publisher: American Physical Society (APS)
Date: 06-08-2004
Publisher: Springer Science and Business Media LLC
Date: 08-2018
Publisher: Elsevier BV
Date: 12-1989
Publisher: American Physical Society (APS)
Date: 24-11-2003
Publisher: American Physical Society (APS)
Date: 07-02-2019
Publisher: Elsevier BV
Date: 09-2000
Publisher: American Physical Society (APS)
Date: 31-08-2017
Publisher: IOP Publishing
Date: 10-2017
Publisher: American Physical Society (APS)
Date: 21-02-2019
Publisher: Cold Spring Harbor Laboratory
Date: 06-06-2022
DOI: 10.1101/2022.06.01.22275851
Abstract: Heterozygous disruptions of FOXP2 were the first identified molecular cause for severe speech disorder childhood apraxia of speech (CAS), yet few cases have been reported, limiting knowledge of the condition. Here we phenotyped 29 in iduals from 18 families with pathogenic FOXP2 -only variants (13 loss-of-function, 5 missense variants 14 males aged 2 years to 62 years). Health and development (cognitive, motor, social domains) was examined, including speech and language outcomes with the first cross-linguistic analysis of English and German. Speech disorders were prevalent (24/26, 92%) and CAS was most common (23/26, 89%), with similar speech presentations across English and German. Speech was still impaired in adulthood and some speech sounds (e.g. ‘th’, ‘r’, ‘ch’, ‘j’) were never acquired. Language impairments (22/26, 85%) ranged from mild to severe. Comorbidities included feeding difficulties in infancy (10/27, 37%), fine (14/27, 52%) and gross (14/27, 52%) motor impairment, anxiety (6/28, 21%), depression (7/28, 25%), and sleep disturbance (11/15, 44%). Physical features were common (23/28, 82%) but with no consistent pattern. Cognition ranged from average to mildly impaired, and was incongruent with language ability for ex le, seven participants with severe language disorder had average non-verbal cognition. Although we identify increased prevalence of conditions like anxiety, depression and sleep disturbance, we confirm that the consequences of FOXP2 dysfunction remain relatively specific to speech disorder, as compared to other recently identified monogenic conditions associated with CAS. Thus, our findings reinforce that FOXP2 provides a valuable entrypoint for examining the neurobiological bases of speech disorder. Heterozygous disruptions of FOXP2 were the first identified molecular cause for severe speech disorder childhood apraxia of speech (CAS), yet few cases have been reported, limiting knowledge of the condition. Here we provide the most comprehensive characterisation of in iduals with pathogenic FOXP2 variants, almost doubling the number of published families to date. We provide the first cross-linguistic analysis of speech and language across German and English. We show that the phenotype for pathogenic FOXP2 variants remains relatively specific to speech disorder, compared to phenotypes associated with other monogenic conditions involving CAS. This study guides identification of cases with a FOXP2 -related disorder for a clinical genetic diagnosis, will improve prognostic counselling and lead to better targeted clinical management.
Publisher: American Physical Society (APS)
Date: 10-09-2003
Publisher: American Physical Society (APS)
Date: 10-12-2003
Publisher: Elsevier BV
Date: 05-1991
Publisher: Elsevier BV
Date: 04-2008
Publisher: Ovid Technologies (Wolters Kluwer Health)
Date: 28-04-2020
DOI: 10.1212/WNL.0000000000009441
Abstract: Determining the genetic basis of speech disorders provides insight into the neurobiology of human communication. Despite intensive investigation over the past 2 decades, the etiology of most speech disorders in children remains unexplained. To test the hypothesis that speech disorders have a genetic etiology, we performed genetic analysis of children with severe speech disorder, specifically childhood apraxia of speech (CAS). Precise phenotyping together with research genome or exome analysis were performed on children referred with a primary diagnosis of CAS. Gene coexpression and gene set enrichment analyses were conducted on high-confidence gene candidates. Thirty-four probands ascertained for CAS were studied. In 11/34 (32%) probands, we identified highly plausible pathogenic single nucleotide (n = 10 CDK13 , EBF3 , GNAO1 , GNB1 , DDX3X , MEIS2 , POGZ , SETBP1 , UPF2 , ZNF142 ) or copy number (n = 1 5q14.3q21.1 locus) variants in novel genes or loci for CAS. Testing of parental DNA was available for 9 probands and confirmed that the variants had arisen de novo. Eight genes encode proteins critical for regulation of gene transcription, and analyses of transcriptomic data found CAS-implicated genes were highly coexpressed in the developing human brain. We identify the likely genetic etiology in 11 patients with CAS and implicate 9 genes for the first time. We find that CAS is often a sporadic monogenic disorder, and highly genetically heterogeneous. Highly penetrant variants implicate shared pathways in broad transcriptional regulation, highlighting the key role of transcriptional regulation in normal speech development. CAS is a distinctive, socially debilitating clinical disorder, and understanding its molecular basis is the first step towards identifying precision medicine approaches.
Publisher: American Physical Society (APS)
Date: 15-11-2018
Publisher: American Physical Society (APS)
Date: 15-10-2019
Publisher: American Physical Society (APS)
Date: 14-06-2018
Publisher: Oxford University Press (OUP)
Date: 10-05-2021
Abstract: Next-generation telescopes such as the James Webb Space Telescope (JWST) and the Nancy Grace Roman Space Telescope (NGRST) will enable us to study the first billion years of our Universe in unprecedented detail. In this work, we use the astraeus (semi-numerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dArk mattEr simUlationS) framework, which couples galaxy formation and reionization (for a wide range of reionization feedback models), to estimate the cosmic variance expected in the UV Luminosity Function (UV LF) and the stellar mass function in JWST surveys. We find that different reionization scenarios play a minor role in the cosmic variance. Most of the cosmic variance is completely driven by the underlying density field and increases above $100{{\\ \\rm per\\ cent}}$ for ${\\it M}_{\\rm UV}\\sim -17.5 ~ (-20)$ at z = 12 (6) for the JADES-deep survey (the deep JWST Advanced Extragalactic Survey with an area of 46 arcmin2) the cosmic variance decreases with an increasing survey area roughly independently of redshift. We find that the faint-end (${\\it M}_{\\rm UV}\\gtrsim -17$) slope of the Lyman Break Galaxies (LBGs) UV LF becomes increasingly shallower with increasing reionization feedback and show how JWST observations will be able to distinguish between different models of reionization feedback at z & 9, even accounting for cosmic variance. We also show the environments (in terms of density and ionization fields) of LBGs during the EoR, finding that the underlying overdensity and ionization fraction scale positively with the UV luminosity. Finally, we also provide a public software tool to allow interested readers to compute cosmic variance for different redshifts and survey areas.
Publisher: Elsevier BV
Date: 06-1986
Publisher: American Physical Society (APS)
Date: 22-07-1996
Publisher: American Physical Society (APS)
Date: 12-08-2019
Publisher: American Physical Society (APS)
Date: 19-10-2020
Publisher: American Physical Society (APS)
Date: 26-10-2020
Publisher: American Physical Society (APS)
Date: 14-04-2021
Publisher: American Physical Society (APS)
Date: 15-10-2010
Publisher: American Physical Society (APS)
Date: 22-08-2001
Publisher: American Physical Society (APS)
Date: 29-08-2002
Publisher: American Physical Society (APS)
Date: 13-01-2010
Publisher: American Physical Society (APS)
Date: 10-01-2018
Publisher: American Physical Society (APS)
Date: 19-03-2015
Publisher: American Physical Society (APS)
Date: 27-10-2021
Publisher: Elsevier BV
Date: 04-2010
Publisher: American Physical Society (APS)
Date: 10-01-2018
Publisher: American Physical Society (APS)
Date: 13-01-2009
Publisher: American Physical Society (APS)
Date: 29-01-2019
Publisher: American Physical Society (APS)
Date: 05-11-2010
Publisher: American Physical Society (APS)
Date: 25-01-2018
Publisher: American Physical Society (APS)
Date: 12-1998
Publisher: Elsevier BV
Date: 06-2008
Publisher: American Physical Society (APS)
Date: 03-12-2008
Publisher: American Physical Society (APS)
Date: 05-1990
Publisher: American Physical Society (APS)
Date: 12-05-2020
Publisher: American Physical Society (APS)
Date: 10-03-2004
Publisher: American Physical Society (APS)
Date: 11-1995
Publisher: Springer Science and Business Media LLC
Date: 10-2019
Abstract: We report a new measurement of the e + e − → ϒ( nS ) π + π − ( n = 1 , 2 , 3) cross sections at energies from 10 . 52 to 11 . 02 GeV using data collected with the Belle detector at the KEKB asymmetric-energy e + e − collider. We observe a new structure in the energy dependence of the cross sections if described by a Breit-Wigner function its mass and width are found to be $$ M=\\left(10752.7\\pm {5.9}_{-1.1}^{+0.7}\\right)\\mathrm{MeV}/{c}^2 $$ M = 10752.7 ± 5.9 − 1.1 + 0.7 MeV / c 2 and $$ \\Gamma =\\left({35.5}_{-11.3\\kern0.5em -3.3}^{+17.6+3.9}\\right) $$ Γ = 35.5 − 11.3 − 3.3 + 17.6 + 3.9 MeV, where the first error is statistical and the second is systematic. The global significance of the new structure including systematic uncertainty is 5.2 standard deviations. We also find evidence for the e + e − → ϒ (1 S ) π + π − process at the energy 10 . 52 GeV, which is below the B $$ \\overline{B} $$ B ¯ threshold.
Publisher: American Physical Society (APS)
Date: 22-05-2007
Publisher: American Physical Society (APS)
Date: 15-05-2007
Publisher: American Physical Society (APS)
Date: 09-06-2021
Publisher: American Physical Society (APS)
Date: 03-06-2021
Publisher: American Physical Society (APS)
Date: 06-2021
Publisher: American Physical Society (APS)
Date: 11-1986
Publisher: American Physical Society (APS)
Date: 07-1991
Publisher: Oxford University Press (OUP)
Date: 30-11-2022
Abstract: In this work, the sixth of a series, we use the seminumerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dark-matter simUlationS (astraeus) framework to investigate the nature of the sources that reionized the Universe. We extend astraeus, which already couples a galaxy formation semi-analytical model with a detailed seminumerical reionization scheme, to include a model for black-hole formation, growth, and the production of ionizing radiation from associated active galactic nuclei (AGNs). We calibrate our fiducial AGN model to reproduce the bolometric luminosity function at z ≃ 5, and explore the role of the resulting AGN population in reionizing the Universe. We find that in all the models yielding a reasonable AGN luminosity function, galaxies dominate overwhelmingly the ionizing budget during the Epoch of Reionization, with AGN accounting for 1–10 per cent of the ionizing budget at z = 6 and starting to play a role only below z ≲ 5.
Publisher: American Physical Society (APS)
Date: 05-1997
Publisher: American Physical Society (APS)
Date: 25-06-2004
Publisher: American Physical Society (APS)
Date: 21-12-2004
Publisher: American Physical Society (APS)
Date: 16-04-2009
Publisher: American Physical Society (APS)
Date: 03-10-2018
Publisher: American Physical Society (APS)
Date: 11-09-2019
Publisher: American Physical Society (APS)
Date: 14-06-2006
Publisher: Oxford University Press (OUP)
Date: 02-2020
DOI: 10.1093/PTEP/PTAA008
Publisher: Elsevier BV
Date: 10-1992
Publisher: American Physical Society (APS)
Date: 07-05-2010
Publisher: American Physical Society (APS)
Date: 27-02-2023
Publisher: American Physical Society (APS)
Date: 15-10-2007
Publisher: American Physical Society (APS)
Date: 30-12-2019
Publisher: American Physical Society (APS)
Date: 13-01-2000
Publisher: American Physical Society (APS)
Date: 29-03-2006
Publisher: Elsevier BV
Date: 02-2002
Publisher: American Physical Society (APS)
Date: 27-09-2001
Publisher: Elsevier BV
Date: 07-1998
Publisher: Elsevier BV
Date: 10-2007
Publisher: American Physical Society (APS)
Date: 08-06-2010
Publisher: American Physical Society (APS)
Date: 13-03-2018
Publisher: American Physical Society (APS)
Date: 09-1998
Publisher: Elsevier BV
Date: 05-2007
Publisher: IOP Publishing
Date: 11-06-2014
Publisher: Elsevier BV
Date: 03-2006
Publisher: Springer Science and Business Media LLC
Date: 11-2018
Publisher: American Physical Society (APS)
Date: 25-06-2008
Publisher: Elsevier BV
Date: 11-1995
Publisher: Elsevier BV
Date: 2003
Publisher: American Physical Society (APS)
Date: 19-10-2021
Publisher: American Physical Society (APS)
Date: 10-11-2010
Publisher: Elsevier BV
Date: 10-1989
Publisher: Oxford University Press (OUP)
Date: 27-12-2022
Abstract: Using the astraeus (seminumerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dark matter simUlationS) framework, we explore the impact of environmental density and radiative feedback on the assembly of galaxies and their host haloes during the Epoch of Reionization. The astraeus framework allows us to study the evolution of galaxies with masses ($10^{8.2}\\,\\rm M_\\odot \\lt M_{\\rm h}\\lt 10^{13}\\,\\rm M_\\odot$) in a wide variety of environment [−0.5 & log (1 + δ) & 1.3 averaged over (2 cMpc)3]. We find that: (i) there exists a mass- and redshift- dependent ‘characteristic’ environment [${\\rm log}\\, (1+\\delta _a(M_{\\rm h}, z)) = 0.021\\times (M_{\\rm h}/\\rm M_\\odot)^{0.16} + 0.07 z -1.12$, up to $z$ ∼ 10] at which galaxies are most efficient at accreting dark matter, e.g at a rate of $0.2{{\\ \\rm per\\ cent}}$ of their mass every Myr at $z$ = 5 (ii) the number of minor and major mergers and their contributions to the dark matter assembly increases with halo mass at all redshifts and is mostly independent of the environment (iii) at $z$ = 5 minor mergers contribute slightly more (by up to $\\sim 10{{\\ \\rm per\\ cent}}$) to the dark matter assembly while for the stellar assembly, major mergers dominate the contribution from minor mergers for $M_{\\rm h}\\lesssim 10^{11.5}\\rm\\, M_\\odot$ galaxies (iv) radiative feedback quenches star formation more in low-mass galaxies ($M_{\\rm h}\\lesssim 10^{9.5}\\rm\\, M_\\odot$) in over-dense environments [log(1 + δ) & 0.5] dominated by their major branch, this yields star formation histories biased towards older ages with a slower redshift evolution.
Publisher: American Physical Society (APS)
Date: 04-1991
Publisher: Elsevier BV
Date: 02-2006
Publisher: American Physical Society (APS)
Date: 1994
Publisher: American Physical Society (APS)
Date: 02-1998
Publisher: Elsevier BV
Date: 06-2002
Publisher: American Physical Society (APS)
Date: 23-09-2004
Publisher: American Physical Society (APS)
Date: 22-09-2004
Publisher: American Physical Society (APS)
Date: 06-1997
Publisher: American Physical Society (APS)
Date: 14-03-2011
Publisher: American Physical Society (APS)
Date: 28-05-2010
Publisher: American Physical Society (APS)
Date: 13-05-2020
Publisher: Elsevier BV
Date: 10-1992
Publisher: Elsevier BV
Date: 08-2010
Publisher: American Physical Society (APS)
Date: 18-01-2008
Publisher: American Physical Society (APS)
Date: 15-03-2021
Publisher: American Physical Society (APS)
Date: 20-02-2019
Publisher: American Physical Society (APS)
Date: 27-11-2007
Publisher: American Physical Society (APS)
Date: 05-12-2008
Publisher: American Physical Society (APS)
Date: 27-12-2001
Publisher: American Physical Society (APS)
Date: 27-08-2002
Publisher: American Physical Society (APS)
Date: 12-09-2008
Publisher: American Physical Society (APS)
Date: 16-06-2021
Publisher: Elsevier BV
Date: 04-1982
Publisher: Elsevier BV
Date: 03-2001
Publisher: American Physical Society (APS)
Date: 06-07-2007
Publisher: IOP Publishing
Date: 10-2017
Publisher: Springer Science and Business Media LLC
Date: 1999
Publisher: American Physical Society (APS)
Date: 04-08-2009
Publisher: American Physical Society (APS)
Date: 30-12-2010
Publisher: American Physical Society (APS)
Date: 21-06-2010
Publisher: American Physical Society (APS)
Date: 08-11-2001
Publisher: American Physical Society (APS)
Date: 27-08-2008
Publisher: American Physical Society (APS)
Date: 25-03-2020
Publisher: American Physical Society (APS)
Date: 29-03-2021
Publisher: American Physical Society (APS)
Date: 26-05-2006
Publisher: American Physical Society (APS)
Date: 22-04-2021
Publisher: American Physical Society (APS)
Date: 07-09-1987
Publisher: American Physical Society (APS)
Date: 19-09-2008
Publisher: Springer Science and Business Media LLC
Date: 02-2013
Abstract: We search for CP violation in the decay ${D^{+}}\\to K_S^0{K^{+}}$ using a data s le with an integrated luminosity of 977 fb −1 collected with the Belle detector at the KEKB e + e − asymmetric-energy collider. No CP violation has been observed and the CP asymmetry in ${D^{+}}\\to K_S^0{K^{+}}$ decay is measured to be (−0.25 ± 0.28 ± 0.14)%, which is the most sensitive measurement to date. After subtracting CP violation due to ${K^0}-{{\\overline{K}}^0}$ mixing, the CP asymmetry in ${D^{+}}\\to {{\\overline{K}}^0}{K^{+}}$ decay is found to be (+0.08 ± 0.28 ± 0.14)%.
Publisher: American Physical Society (APS)
Date: 12-2020
Publisher: Elsevier BV
Date: 02-1989
Publisher: American Physical Society (APS)
Date: 1990
Publisher: Elsevier BV
Date: 1982
Publisher: Elsevier BV
Date: 04-2007
Publisher: American Physical Society (APS)
Date: 23-06-2023
Publisher: American Physical Society (APS)
Date: 09-1991
Publisher: American Physical Society (APS)
Date: 16-06-2010
Publisher: American Physical Society (APS)
Date: 23-03-2021
Publisher: American Physical Society (APS)
Date: 03-02-2011
Publisher: American Physical Society (APS)
Date: 22-06-2010
Publisher: American Physical Society (APS)
Date: 22-12-2006
Publisher: American Physical Society (APS)
Date: 22-12-2021
Publisher: American Physical Society (APS)
Date: 25-02-2019
Publisher: American Physical Society (APS)
Date: 24-01-2005
Publisher: American Physical Society (APS)
Date: 22-05-2003
Publisher: Elsevier BV
Date: 06-1992
Publisher: American Physical Society (APS)
Date: 12-1998
Publisher: Oxford University Press (OUP)
Date: 28-07-2023
Abstract: We use the astraeus framework to investigate how the visibility and spatial distribution of Lyman-α (Lyα) emitters (LAEs) during reionization is sensitive to a halo mass-dependent fraction of ionizing radiation escaping from the galactic environment (fesc) and the ionization topology. To this end, we consider the two physically plausible bracketing scenarios of fesc increasing and decreasing with rising halo mass. We derive the corresponding observed Lyα luminosities of galaxies for three different analytic Lyα line profiles and associated Lyα escape fraction ($f_\\mathrm{esc}^\\mathrm{Ly\\alpha }$) models: importantly, we introduce two novel analytic Lyα line profile models that describe the surrounding interstellar medium (ISM) as dusty gas clumps. They are based on parameterizing results from radiative transfer simulations, with one of them relating $f_\\mathrm{esc}^\\mathrm{Ly\\alpha }$ to fesc by assuming the ISM of being interspersed with low-density tunnels. Our key findings are: (i) for dusty gas clumps, the Lyα line profile develops from a central to double peak dominated profile as a galaxy’s halo mass increases (ii) LAEs are galaxies with $M_h\\gtrsim 10^{10}\\, {\\rm \\rm M_\\odot }$ located in overdense and highly ionized regions (iii) for this reason, the spatial distribution of LAEs is primarily sensitive to the global ionization fraction and only weakly in second-order to the ionization topology or a halo mass-dependent fesc (iv) furthermore, as the observed Lyα luminosity functions reflect the Lyα emission from more massive galaxies, there is a degeneracy between the fesc-dependent intrinsic Lyα luminosity and the Lyα attenuation by dust in the ISM if fesc does not exceed $\\sim 50~{{\\ \\rm per \\, cent}}$.
Publisher: American Physical Society (APS)
Date: 30-04-2009
Publisher: American Physical Society (APS)
Date: 03-1996
Publisher: American Physical Society (APS)
Date: 15-06-2007
Publisher: Elsevier BV
Date: 07-2007
Publisher: Informa UK Limited
Date: 12-2006
Publisher: Springer Science and Business Media LLC
Date: 06-2021
Abstract: Using a data s le of 980 fb − 1 collected with the Belle detector at the KEKB asymmetric-energy e + e − collider, we study the processes of $$ {\\Xi}_c^0\\to \\Lambda {\\overline{K}}^{\\ast 0} $$ Ξ c 0 → Λ K ¯ ∗ 0 , $$ {\\Xi}_c^0\\to {\\Sigma}^0{\\overline{K}}^{\\ast 0} $$ Ξ c 0 → Σ 0 K ¯ ∗ 0 , and $$ {\\Xi}_c^0\\to {\\Sigma}^{+}{K}^{\\ast -} $$ Ξ c 0 → Σ + K ∗ − for the first time. The relative branching ratios to the normalization mode of $$ {\\Xi}_c^0\\to {\\Xi}^{-}{\\pi}^{+} $$ Ξ c 0 → Ξ − π + are measured to be $$ {\\displaystyle \\begin{array}{c}\\mathcal{B}\\left({\\Xi}_c^0\\to \\Lambda {\\overline{K}}^{\\ast 0}\\right)/\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Xi}^{-}{\\pi}^{+}\\right)=0.18\\pm 0.02\\left(\\mathrm{stat}.\\right)\\pm 0.01\\left(\\mathrm{syst}.\\right),\\\\ {}\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Sigma}^0{\\overline{K}}^{\\ast 0}\\right)/\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Xi}^{-}{\\pi}^{+}\\right)=0.69\\pm 0.03\\left(\\mathrm{stat}.\\right)\\pm 0.03\\left(\\mathrm{syst}.\\right),\\\\ {}\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Sigma}^{+}{K}^{\\ast -}\\right)/\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Xi}^{-}{\\pi}^{+}\\right)=0.34\\pm 0.06\\left(\\mathrm{stat}.\\right)\\pm 0.02\\left(\\mathrm{syst}.\\right),\\end{array}} $$ B Ξ c 0 → Λ K ¯ ∗ 0 / B Ξ c 0 → Ξ − π + = 0.18 ± 0.02 stat . ± 0.01 syst . , B Ξ c 0 → Σ 0 K ¯ ∗ 0 / B Ξ c 0 → Ξ − π + = 0.69 ± 0.03 stat . ± 0.03 syst . , B Ξ c 0 → Σ + K ∗ − / B Ξ c 0 → Ξ − π + = 0.34 ± 0.06 stat . ± 0.02 syst . , where the uncertainties are statistical and systematic, respectively. We obtain $$ {\\displaystyle \\begin{array}{c}\\mathcal{B}\\left({\\Xi}_c^0\\to \\Lambda {\\overline{K}}^{\\ast 0}\\right)=\\left(3.3\\pm 0.3\\left(\\mathrm{stat}.\\right)\\pm 0.2\\left(\\mathrm{syst}.\\right)\\pm 1.0\\left(\\mathrm{ref}.\\right)\\right)\\times {10}^{-3},\\\\ {}\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Sigma}^0{\\overline{K}}^{\\ast 0}\\right)=\\left(12.4\\pm 0.5\\left(\\mathrm{stat}.\\right)\\pm 0.5\\left(\\mathrm{syst}.\\right)\\pm 3.6\\left(\\mathrm{ref}.\\right)\\right)\\times {10}^{-3},\\\\ {}\\mathcal{B}\\left({\\Xi}_c^0\\to {\\Sigma}^{+}{K}^{\\ast 0}\\right)=\\left(6.1\\pm 1.0\\left(\\mathrm{stat}.\\right)\\pm 0.4\\left(\\mathrm{syst}.\\right)\\pm 1.8\\left(\\mathrm{ref}.\\right)\\right)\\times {10}^{-3},\\end{array}} $$ B Ξ c 0 → Λ K ¯ ∗ 0 = 3.3 ± 0.3 stat . ± 0.2 syst . ± 1.0 ref . × 10 − 3 , B Ξ c 0 → Σ 0 K ¯ ∗ 0 = 12.4 ± 0.5 stat . ± 0.5 syst . ± 3.6 ref . × 10 − 3 , B Ξ c 0 → Σ + K ∗ 0 = 6.1 ± 1.0 stat . ± 0.4 syst . ± 1.8 ref . × 10 − 3 , where the uncertainties are statistical, systematic, and from $$ \\mathcal{B}\\left({\\Xi}_c^0\\to {\\Xi}^{-}{\\pi}^{+}\\right) $$ B Ξ c 0 → Ξ − π + , respectively. The asymmetry parameters $$ \\alpha \\left({\\Xi}_c^0\\to \\Lambda {\\overline{K}}^{\\ast 0}\\right) $$ α Ξ c 0 → Λ K ¯ ∗ 0 and $$ \\alpha \\left({\\Xi}_c^0\\to {\\Sigma}^{+}{K}^{\\ast -}\\right) $$ α Ξ c 0 → Σ + K ∗ − are 0 . 15 ± 0 . 22(stat . ) ± 0 . 04(syst . ) and − 0 . 52 ± 0 . 30(stat . ) ± 0 . 02(syst . ), respectively, where the uncertainties are statistical followed by systematic.
Publisher: American Physical Society (APS)
Date: 18-07-2018
Publisher: American Physical Society (APS)
Date: 03-12-2018
Publisher: American Physical Society (APS)
Date: 18-05-1998
Publisher: American Physical Society (APS)
Date: 22-10-2010
Publisher: American Physical Society (APS)
Date: 17-04-2007
Publisher: American Physical Society (APS)
Date: 18-04-2007
Publisher: American Physical Society (APS)
Date: 02-2018
Publisher: American Physical Society (APS)
Date: 20-11-2007
Publisher: American Physical Society (APS)
Date: 12-1989
Publisher: American Physical Society (APS)
Date: 24-07-2008
Publisher: Elsevier BV
Date: 06-1985
Publisher: American Physical Society (APS)
Date: 11-08-2006
Publisher: Elsevier BV
Date: 1999
Publisher: American Physical Society (APS)
Date: 04-05-2018
Publisher: American Physical Society (APS)
Date: 28-05-2019
Publisher: Oxford University Press (OUP)
Date: 03-03-2021
Abstract: We introduce a new self-consistent model of galaxy evolution and reionization, astraeus (seminumerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dArk mattEr simUlationS), which couples a state-of-the-art N-body simulation with the semi-analytical galaxy evolution delphi and the seminumerical reionization scheme cifog. astraeus includes all the key processes of galaxy formation and evolution (including accretion, mergers, supernova, and radiative feedback) and follows the time and spatial evolution of the ionized regions in the intergalactic medium (IGM). Importantly, it explores different radiative feedback models that cover the physically plausible parameter space, ranging from a weak and delayed to a strong and immediate reduction of gas mass available for star formation. From our simulation suite that covers the different radiative feedback prescriptions and ionization topologies, we find that radiative feedback continuously reduces star formation in galaxies with $M_\\mathrm{ h}\\lesssim 10^{9.5}\\, {\\rm \\rm M_\\odot }$ upon local reionization larger mass haloes are unaffected even for the strongest and immediate radiative feedback cases during reionization. For this reason, the ionization topologies of different radiative feedback scenarios differ only on scales smaller than 1–2 comoving Mpc, and significant deviations are found only when physical parameters (e.g. the escape fraction of ionizing photons) are altered based on galactic properties. Finally, we find that observables (the ultraviolet luminosity function, stellar mass function, reionization histories and ionization topologies) are hardly affected by the choice of the used stellar population synthesis models that model either single stars or binaries.
Publisher: Informa UK Limited
Date: 04-08-2020
Publisher: American Physical Society (APS)
Date: 27-11-2017
Publisher: American Physical Society (APS)
Date: 19-12-2018
Publisher: American Physical Society (APS)
Date: 17-12-2018
Publisher: American Physical Society (APS)
Date: 08-01-2007
Publisher: American Physical Society (APS)
Date: 05-12-2017
Publisher: IOP Publishing
Date: 19-05-2011
Publisher: American Physical Society (APS)
Date: 04-01-2019
Publisher: American Physical Society (APS)
Date: 31-12-2019
Publisher: Elsevier BV
Date: 02-1987
Publisher: American Physical Society (APS)
Date: 24-12-2020
Publisher: American Physical Society (APS)
Date: 02-01-2002
Publisher: Elsevier BV
Date: 11-2009
Publisher: American Physical Society (APS)
Date: 06-01-2004
Publisher: American Physical Society (APS)
Date: 16-01-2002
Publisher: American Physical Society (APS)
Date: 02-06-2004
Publisher: American Physical Society (APS)
Date: 24-12-2003
Publisher: American Physical Society (APS)
Date: 16-03-2010
Publisher: American Physical Society (APS)
Date: 15-03-1999
Publisher: American Physical Society (APS)
Date: 19-10-2006
Publisher: American Physical Society (APS)
Date: 07-12-2009
Publisher: American Physical Society (APS)
Date: 21-12-2006
Publisher: American Physical Society (APS)
Date: 09-10-2018
Publisher: Springer Science and Business Media LLC
Date: 18-09-2023
DOI: 10.1038/S41380-022-01764-8
Abstract: Childhood apraxia of speech (CAS), the prototypic severe childhood speech disorder, is characterized by motor programming and planning deficits. Genetic factors make substantive contributions to CAS aetiology, with a monogenic pathogenic variant identified in a third of cases, implicating around 20 single genes to date. Here we aimed to identify molecular causation in 70 unrelated probands ascertained with CAS. We performed trio genome sequencing. Our bioinformatic analysis examined single nucleotide, indel, copy number, structural and short tandem repeat variants. We prioritised appropriate variants arising de novo or inherited that were expected to be damaging based on in silico predictions. We identified high confidence variants in 18/70 (26%) probands, almost doubling the current number of candidate genes for CAS. Three of the 18 variants affected SETBP1 , SETD1A and DDX3X , thus confirming their roles in CAS, while the remaining 15 occurred in genes not previously associated with this disorder. Fifteen variants arose de novo and three were inherited. We provide further novel insights into the biology of child speech disorder, highlighting the roles of chromatin organization and gene regulation in CAS, and confirm that genes involved in CAS are co-expressed during brain development. Our findings confirm a diagnostic yield comparable to, or even higher, than other neurodevelopmental disorders with substantial de novo variant burden. Data also support the increasingly recognised overlaps between genes conferring risk for a range of neurodevelopmental disorders. Understanding the aetiological basis of CAS is critical to end the diagnostic odyssey and ensure affected in iduals are poised for precision medicine trials.
Publisher: American Physical Society (APS)
Date: 27-03-2007
Publisher: American Physical Society (APS)
Date: 29-11-2021
Publisher: American Physical Society (APS)
Date: 27-07-2021
Publisher: American Physical Society (APS)
Date: 03-2006
Publisher: American Physical Society (APS)
Date: 18-05-1992
Publisher: American Physical Society (APS)
Date: 19-08-2019
Publisher: Elsevier BV
Date: 11-2006
Publisher: Elsevier BV
Date: 03-2011
Publisher: IOP Publishing
Date: 11-06-2014
Publisher: American Physical Society (APS)
Date: 06-01-2011
Publisher: American Physical Society (APS)
Date: 05-07-2011
Publisher: American Physical Society (APS)
Date: 23-04-2012
Publisher: American Physical Society (APS)
Date: 12-1998
Publisher: Oxford University Press (OUP)
Date: 30-11-2022
Abstract: In this work, we have implemented a detailed physical model of galaxy chemical enrichment into the Astraeus (seminumerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dark matter simUlationS) framework which couples galaxy formation and reionization in the first billion years. Simulating galaxies spanning over 2.5 orders of magnitude in halo mass with $M_{\\rm h} \\sim 10^{8.9}{-}10^{11.5}\\,{\\rm M_\\odot}$ ($M_{\\rm h} \\sim 10^{8.9}{-}10^{12.8}\\rm M_\\odot$) at z ∼ 10 (5), we find: (i) smooth accretion of metal-poor gas from the intergalactic medium (IGM) plays a key role in diluting the interstellar medium interstellar medium metallicity which is effectively restored due to self-enrichment from star formation (ii) a redshift averaged gas-mass loading factor that depends on the stellar mass as $\\eta _{\\rm g} \\approx 1.38 ({M_*}/{10^{10}\\, {\\rm \\rm M_\\odot }})^{-0.43}$ (iii) the mass–metallicity relation is already in place at z ∼ 10 and shows effectively no redshift evolution down to z ∼ 5 (iv) for a given stellar mass, the metallicity decreases with an increase in the star formation rate (SFR) (v) the key properties of the gas-phase metallicity (in units of 12 + log(O/H), stellar mass, SFR and redshift are linked through a high-redshift fundamental plane of metallicity (HFPZ) for which we provide a functional form (vi) the mass–metallicity–SFR relations are effectively independent of the reionization radiative feedback model for $M_* {\\,\\, \\buildrel\\gt \\over \\sim \\,\\,}10^{6.5}\\rm M_\\odot$ galaxies (vii) while low-mass galaxies ($M_{\\rm h} {\\,\\, \\buildrel\\lt \\over \\sim \\,\\,}10^9\\,\\rm M_\\odot$) are the key contributors to the metal budget of the IGM at early times, higher mass haloes provide about 50 per cent of the metal budget at lower redshifts.
Publisher: American Physical Society (APS)
Date: 20-10-2009
Publisher: American Physical Society (APS)
Date: 24-12-2003
Publisher: American Physical Society (APS)
Date: 06-07-2020
Publisher: American Physical Society (APS)
Date: 09-04-2018
Publisher: American Physical Society (APS)
Date: 16-06-1999
Publisher: American Physical Society (APS)
Date: 06-1987
Publisher: American Physical Society (APS)
Date: 30-12-2021
Publisher: American Physical Society (APS)
Date: 26-03-2020
Publisher: American Physical Society (APS)
Date: 30-11-2018
Publisher: Elsevier BV
Date: 08-2006
Publisher: American Physical Society (APS)
Date: 26-12-2018
Publisher: American Physical Society (APS)
Date: 07-1988
Publisher: American Physical Society (APS)
Date: 26-06-2006
Publisher: American Physical Society (APS)
Date: 06-03-2008
Publisher: American Physical Society (APS)
Date: 30-12-2010
Publisher: Elsevier BV
Date: 02-2008
Publisher: American Physical Society (APS)
Date: 27-11-2002
Publisher: Elsevier BV
Date: 06-2004
Publisher: American Physical Society (APS)
Date: 04-09-2009
Publisher: Springer Science and Business Media LLC
Date: 04-2021
Abstract: We present a search for the dark photon A ′ in the B 0 → A ′ A ′ decays, where A ′ subsequently decays to e + e − , μ + μ − , and π + π − . The search is performed by analyzing 772 × 10 6 $$ B\\overline{B} $$ B B ¯ events collected by the Belle detector at the KEKB e + e − energy-asymmetric collider at the ϒ(4 S ) resonance. No signal is found in the dark photon mass range 0 . 01 GeV /c 2 ≤ m A ′ ≤ 2 . 62 GeV /c 2 , and we set upper limits of the branching fraction of B 0 → A ′ A ′ at the 90% confidence level. The products of branching fractions, $$ \\mathrm{\\mathcal{B}}\\left({B}^0\\to A^{\\prime }A^{\\prime}\\right)\\times \\mathrm{\\mathcal{B}}{\\left(A\\prime \\to {e}^{+}{e}^{-}\\right)}^2 $$ ℬ B 0 → A ′ A ′ × ℬ A ′ → e + e − 2 and $$ \\mathrm{\\mathcal{B}}\\left({B}^0\\to A^{\\prime }A^{\\prime}\\right)\\times \\mathrm{\\mathcal{B}}{\\left(A\\prime \\to {\\mu}^{+}{\\mu}^{-}\\right)}^2 $$ ℬ B 0 → A ′ A ′ × ℬ A ′ → μ + μ − 2 , have limits of the order of 10 − 8 depending on the A ′ mass. Furthermore, considering A ′ decay rate to each pair of charged particles, the upper limits of $$ \\mathrm{\\mathcal{B}}\\left({B}^0\\to A^{\\prime }A^{\\prime}\\right) $$ ℬ B 0 → A ′ A ′ are of the order of 10 − 8 –10 − 5 . From the upper limits of $$ \\mathrm{\\mathcal{B}}\\left({B}^0\\to A^{\\prime }A^{\\prime}\\right) $$ ℬ B 0 → A ′ A ′ , we obtain the Higgs portal coupling for each assumed dark photon and dark Higgs mass. The Higgs portal couplings are of the order of 10 − 2 –10 − 1 at $$ {m}_{h\\prime}\\simeq {m}_{B^0} $$ m h ′ ≃ m B 0 ± 40 MeV /c 2 and 10 − 1 –1 at $$ {m}_{h\\prime}\\simeq {m}_{B^0} $$ m h ′ ≃ m B 0 ± 3 GeV /c 2 .
Publisher: Springer Science and Business Media LLC
Date: 10-2019
Abstract: We present the first model-independent measurement of the CKM unitarity triangle angle ϕ 3 using B ± → D ( $$ {K}_{\\mathrm{S}}^0 $$ K S 0 π + π − π 0 ) K ± decays, where D indicates either a D 0 or $$ \\overline{D} $$ D ¯ 0 meson. Measurements of the strong-phase difference of the D → $$ {K}_{\\mathrm{S}}^0 $$ K S 0 π + π − π 0 litude obtained from CLEO-c data are used as input. This analysis is based on the full Belle data set of 772 × 10 6 B $$ \\overline{B} $$ B ¯ events collected at the Υ(4 S ) resonance. We obtain ϕ 3 = ( $$ {5.7}_{-8.8}^{+10.2} $$ 5.7 − 8.8 + 10.2 ± 3 . 5 ± 5 . 7) ° and the suppressed litude ratio r B = 0 . 323 ± 0 . 147 ± 0 . 023 ± 0 . 051. Here the first uncertainty is statistical, the second is the experimental systematic, and the third is due to the precision of the strong-phase parameters measured from CLEO-c data. The 95% confidence interval on ϕ 3 is ( − 29 . 7 , 109 . 5) ° , which is consistent with the current world average.
Publisher: Elsevier BV
Date: 2002
Publisher: Elsevier BV
Date: 08-1995
Publisher: Elsevier BV
Date: 08-1983
Publisher: American Physical Society (APS)
Date: 03-04-2003
Publisher: American Physical Society (APS)
Date: 05-03-2010
Publisher: Oxford University Press (OUP)
Date: 10-05-2021
Abstract: In this work, we use the astraeus (seminumerical rAdiative tranSfer coupling of galaxy formaTion and Reionization in N-body dArk mattEr simUlationS) framework that couples galaxy formation and reionization in the first billion years. Exploring a number of models for reionization feedback and the escape fraction of ionizing radiation from the galactic environment (fesc), we quantify how the contribution of star-forming galaxies (with halo masses $M_\\mathrm{ h}\\gt 10^{8.2}\\, {\\rm \\rm M_\\odot }$) to reionization depends on the radiative feedback model, fesc, and the environmental overdensity. Our key findings are: (i) for constant fesc models, intermediate-mass galaxies (with halo masses of $M_\\mathrm{ h}\\simeq 10^{9-11}\\, {\\rm \\rm M_\\odot }$ and absolute UV magnitudes of MUV ∼ −15 to −20) in intermediate-density regions (with overdensity log10(1 + δ) ∼ 0−0.8 on a 2 comoving Mpc spatial scale) drive reionization (ii) scenarios where fesc increases with decreasing halo mass shift, the galaxy population driving reionization to lower mass galaxies ($M_\\mathrm{ h}\\lesssim 10^{9.5}\\, {\\rm \\rm M_\\odot }$) with lower luminosities (MUV ≳ −16) and overdensities [log10(1 + δ) ∼ 0−0.5 on a 2 comoving Mpc spatial scale] (iii) reionization imprints its topology on the ionizing emissivity of low-mass galaxies ($M_h\\lesssim 10^{9}\\, {\\rm \\rm M_\\odot }$] through radiative feedback. Low-mass galaxies experience a stronger suppression of star formation by radiative feedback and show lower ionizing emissivities in overdense regions (iv) a change in fesc with galaxy properties has the largest impact on the sources of reionization and their detectability, with the radiative feedback strength and environmental overdensity playing a sub-dominant role (v) James Webb Space Telescope-surveys (with a limiting magnitude of MUV = −16) will be able to detect the galaxies providing ${\\sim}60{-}70{{\\ \\rm per\\ cent}}$ (${\\sim}10{{\\ \\rm per\\ cent}}$) of reionization photons at z = 7 for constant fesc models (scenarios where fesc increases with decreasing halo mass).
Publisher: American Physical Society (APS)
Date: 11-1993
Publisher: American Physical Society (APS)
Date: 14-06-2002
Publisher: American Physical Society (APS)
Date: 26-07-2006
Publisher: American Physical Society (APS)
Date: 31-12-2003
Publisher: American Physical Society (APS)
Date: 04-12-2009
Publisher: American Physical Society (APS)
Date: 02-08-2018
Publisher: American Physical Society (APS)
Date: 08-02-2021
Publisher: American Physical Society (APS)
Date: 14-12-2009
Publisher: American Physical Society (APS)
Date: 15-12-2021
Publisher: American Physical Society (APS)
Date: 10-07-2019
Publisher: American Physical Society (APS)
Date: 28-12-2018
Publisher: Elsevier BV
Date: 04-2004
Publisher: American Physical Society (APS)
Date: 26-03-2008
Publisher: American Physical Society (APS)
Date: 18-08-1986
Publisher: Elsevier BV
Date: 05-2007
Publisher: American Physical Society (APS)
Date: 26-12-2018
Start Date: 2018
End Date: 03-2021
Amount: $318,048.00
Funder: Australian Research Council
View Funded ActivityStart Date: 01-2004
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Amount: $510,000.00
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Amount: $2,827,000.00
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Amount: $257,250.00
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Amount: $361,693.00
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Amount: $25,200,000.00
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Amount: $220,255.00
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Amount: $1,972,000.00
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Funder: Australian Research Council
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Funder: Australian Research Council
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