ORCID Profile
0000-0001-9434-3837
Current Organisation
Swinburne University of Technology
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Research Topics
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.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
Astronomical and Space Sciences | Cosmology and Extragalactic Astronomy | Astronomical and Space Instrumentation | High Energy Astrophysics; Cosmic Rays | Astronomical sciences | Space instrumentation | Stellar Astronomy and Planetary Systems | General Relativity and Gravitational Waves | Cosmology and extragalactic astronomy | Lasers and quantum electronics | General relativity and gravitational waves |
ANZSRC Socio-Economic Objective (SEO)
Expanding Knowledge in the Physical Sciences | Scientific Instruments | Network Infrastructure Equipment | Command, Control and Communications |
Related Links
Publications
RADIO IMAGING OBSERVATIONS of PSR J1023+0038 in AN LMXB STATE
Publisher: American Astronomical Society
Date: 04-08-2015
Observation of the
B 0 →
Publisher:
American Physical Society (APS)
Date:
20-04-2022
Publisher: American Physical Society (APS)
Date: 20-04-2022
THE PROPER MOTION OF PSR J1550-5418 MEASURED WITH VLBI: A SECOND MAGNETAR VELOCITY MEASUREMENT
Publisher: American Astronomical Society
Date: 27-02-2012
Measurement of the Time-Integrated
C P
Publisher:
American Physical Society (APS)
Date:
29-08-2023
Publisher: American Physical Society (APS)
Date: 29-08-2023
Wide-field VLBA observations of theChandradeep field South
Publisher: EDP Sciences
Date: 23-12-2010
WALLABY Pilot Survey
Publisher: American Astronomical Society
Date: 05-2023
Abstract: We report on the commensal ASKAP detection of a fast radio burst (FRB), FRB 20211127I, and the detection of neutral hydrogen (H i ) emission in the FRB host galaxy, WALLABY J131913–185018 (hereafter W13–18). This collaboration between the CRAFT and WALLABY survey teams marks the fifth, and most distant, FRB host galaxy detected in H i , not including the Milky Way. We find that W13–18 has an H i mass of M HI = 6.5 × 10 9 M ⊙ , an H i -to-stellar mass ratio of 2.17, and coincides with a continuum radio source of flux density at 1.4 GHz of 1.3 mJy. The H i global spectrum of W13–18 appears to be asymmetric, albeit the H i observation has a low signal-to-noise ratio (S/N), and the galaxy itself appears modestly undisturbed. These properties are compared to the early literature of H i emission detected in other FRB hosts to date, where either the H i global spectra were strongly asymmetric, or there were clearly disrupted H i intensity map distributions. W13–18 lacks a sufficient S/N to determine whether it is significantly less asymmetric in its H i distribution than previous ex les of FRB host galaxies. However, there are no strong signs of a major interaction in the optical image of the host galaxy that would stimulate a burst of star formation and hence the production of putative FRB progenitors related to massive stars and their compact remnants.
50 picoarcsec astrometry of pulsar emission
Publisher: Oxford University Press (OUP)
Date: 14-02-2014
VLBI observations of the radio quasar J2228+0110 atz= 5.95 and other field sources in multiple-phase-centre mode
Publisher: EDP Sciences
Date: 03-2014
The Millimeter Continuum Size–Frequency Relationship in the UZ Tau E Disk
Publisher: American Astronomical Society
Date: 03-07-2018
Measuring a Cherenkov ring in the radio emission from air showers at 110–190MHz with LOFAR
Publisher: Elsevier BV
Date: 05-2015
A novel search for gravitationally lensed radio sources in wide-field VLBI imaging from the mJIVE-20 survey
Publisher: Oxford University Press (OUP)
Date: 27-11-2019
Centrality determination in heavy-ion collisions with the LHCb detector
Publisher: IOP Publishing
Date: 05-2022
DOI: 10.1088/1748-0221/17/05/P05009
Abstract: The centrality of heavy-ion collisions is directly related to the created medium in these interactions. A procedure to determine the centrality of collisions with the LHCb detector is implemented for lead-lead collisions at √ s NN = 5 TeV and lead-neon fixed-target collisions at √ s NN = 69 GeV. The energy deposits in the electromagnetic calorimeter are used to determine and define the centrality classes. The correspondence between the number of participants and the centrality for the lead-lead collisions is in good agreement with the correspondence found in other experiments, and the centrality measurements for the lead-neon collisions presented here are performed for the first time in fixed-target collisions at the LHC.
TIMING OBSERVATIONS OF PSR J1023+0038 DURING A LOW-MASS X-RAY BINARY STATE
Publisher: American Astronomical Society
Date: 17-10-2016
Wide-field LOFAR imaging of the field around the double-double radio galaxy B1834+620
Publisher: EDP Sciences
Date: 12-2015
First observation of the
B + →
Publisher:
American Physical Society (APS)
Date:
14-08-2023
Publisher: American Physical Society (APS)
Date: 14-08-2023
Very long baseline interferometry detection of an Infrared-Faint Radio Source
Publisher: Oxford University Press (OUP)
Date: 16-06-2007
Potential kick velocity distribution of black hole X-ray binaries and implications for natal kicks
Publisher: Oxford University Press (OUP)
Date: 30-08-2019
Abstract: We use very long baseline interferometry to measure the proper motions of three black hole X-ray binaries (BHXBs). Using these results together with data from the literature and Gaia DR2 to collate the best available constraints on proper motion, parallax, distance, and systemic radial velocity of 16 BHXBs, we determined their three-dimensional Galactocentric orbits. We extended this analysis to estimate the probability distribution for the potential kick velocity (PKV) a BHXB system could have received on formation. Constraining the kicks imparted to BHXBs provides insight into the birth mechanism of black holes (BHs). Kicks also have a significant effect on BH–BH merger rates, merger sites, and binary evolution, and can be responsible for spin–orbit misalignment in BH binary systems. 75 per cent of our systems have potential kicks $\\gt 70\\, \\rm {km\\,s^{-1}}$. This suggests that strong kicks and hence spin–orbit misalignment might be common among BHXBs, in agreement with the observed quasi-periodic X-ray variability in their power density spectra. We used a Bayesian hierarchical methodology to analyse the PKV distribution of the BHXB population, and suggest that a unimodal Gaussian model with a mean of 107 $\\pm \\,\\,16\\, \\rm {km\\,s^{-1}}$ is a statistically favourable fit. Such relatively high PKVs would also reduce the number of BHs likely to be retained in globular clusters. We found no significant correlation between the BH mass and PKV, suggesting a lack of correlation between BH mass and the BH birth mechanism. Our python code allows the estimation of the PKV for any system with sufficient observational constraints.
Locating the intense interstellar scattering towards the inner Galaxy
Publisher: Oxford University Press (OUP)
Date: 19-07-2017
Searching for the Sources of Excess Extragalactic Dispersion of FRBs
Publisher: American Astronomical Society
Date: 23-08-2023
Abstract: The FLIMFLAM survey is collecting spectroscopic data of field galaxies near fast radio burst (FRB) sight lines to constrain key parameters describing the distribution of matter in the Universe. In this work, we leverage the survey data to determine the source of the excess extragalactic dispersion measure (DM), compared to Macquart relation estimates of four FRBs: FRB20190714A, FRB20200906A, FRB20200430A, and FRB20210117A. By modeling the gas distribution around the foreground galaxy halos and galaxy groups of the sight lines, we estimate DM halos , their contribution to the FRB DMs. The FRB20190714A sight line shows a clear excess of foreground halos which contribute roughly two-thirds of the observed excess DM, thus implying a sight line that is baryon dense. FRB20200906A shows a smaller but nonnegligible foreground halo contribution, and further analysis of the intergalactic medium is necessary to ascertain the true cosmic contribution to its DM. FRB20200430A and FRB20210117A show negligible foreground contributions, implying a large host galaxy excess and/or progenitor environment excess.
VLBI imaging throughout the primary beam using accurate UV shifting
Publisher: EDP Sciences
Date: 12-01-2011
Observation of New Resonances Decaying to
J / ψ
Publisher:
American Physical Society (APS)
Date:
17-08-2021
Publisher: American Physical Society (APS)
Date: 17-08-2021
Quasi-simultaneous radio and X-ray observations of Aql X-1 : probing low luminosities
Publisher: Oxford University Press (OUP)
Date: 06-12-2019
Abstract: Aql X-1 is one of the best-studied neutron star low-mass X-ray binaries. It was previously targeted using quasi-simultaneous radio and X-ray observations during at least seven different accretion outbursts. Such observations allow us to probe the interplay between accretion inflow (X-ray) and jet outflow (radio). Thus far, these combined observations have only covered one order of magnitude in radio and X-ray luminosity range this means that any potential radio–X-ray luminosity correlation, LR ∝ LXβ, is not well constrained (β ≈ 0.4–0.9, based on various studies) or understood. Here we present quasi-simultaneous Very Large Array and Swift-XRT observations of Aql X-1’s 2016 outburst, with which we probe one order of magnitude fainter in radio and X-ray luminosity compared to previous studies (6 × 1034 erg s−1 & LX & × 1035 erg s−1, i.e. the intermediate to low-luminosity regime between outburst peak and quiescence). The resulting radio non-detections indicate that Aql X-1’s radio emission decays more rapidly at low X-ray luminosities than previously assumed – at least during the 2016 outburst. Assuming similar behaviour between outbursts, and combining all available data in the hard X-ray state, this can be modelled as a steep β =$1.17^{+0.30}_{-0.21}$ power-law index or as a sharp radio cut-off at LX ≲ 5 × 1035 erg s−1 (given our deep radio upper limits at X-ray luminosities below this value). We discuss these results in the context of other similar studies.
Evidence for a New Structure in the
J / ψ p
Publisher: American Physical Society (APS)
Date: 07-02-2022
Erratum: “Very Long Baseline Astrometry of PSR J1012+5307 and its Implications on Alternative Theories of Gravity” (2020, ApJ, 896, 85)
Publisher: American Astronomical Society
Date: 03-09-2020
Subarcsecond international LOFAR radio images of Arp 220 at 150 MHz
Publisher: EDP Sciences
Date: 05-2018
A search for supernova-like optical counterparts to ASKAP-localised fast radio bursts
Publisher: EDP Sciences
Date: 07-2020
DOI: 10.1051/0004-6361/202038076
Abstract: Fast radio bursts (FRBs) are millisecond-scale radio pulses, which originate in distant galaxies and are produced by unknown sources. The mystery remains partially because of the typical difficulty in localising FRBs to host galaxies. Accurate localisations delivered by the Commensal Real-time ASKAP Fast Transients (CRAFT) survey now provide an opportunity to study the host galaxies and potential transient counterparts of FRBs at a large range of wavelengths. In this work, we investigate whether the first three FRBs accurately localised by CRAFT have supernova-like transient counterparts. We obtained two sets of imaging epochs with the Very Large Telescope for three host galaxies, one soon after the burst detection and one several months later. After subtracting these images no optical counterparts were identified in the associated FRB host galaxies, so we instead place limits on the brightness of any potential optical transients. A Monte Carlo approach, in which supernova light curves were modelled and their base properties randomised, was used to estimate the probability of a supernova associated with each FRB going undetected. We conclude that Type Ia and IIn supernovae are unlikely to accompany every apparently non-repeating FRB.
Identification of charm jets at LHCb
Publisher: IOP Publishing
Date: 02-2022
DOI: 10.1088/1748-0221/17/02/P02028
Abstract: The identification of charm jets is achieved at LHCb for data collected in 2015–2018 using a method based on the properties of displaced vertices reconstructed and matched with jets. The performance of this method is determined using a dijet calibration dataset recorded by the LHCb detector and selected such that the jets are unbiased in quantities used in the tagging algorithm. The charm-tagging efficiency is reported as a function of the transverse momentum of the jet. The measured efficiencies are compared to those obtained from simulation and found to be in good agreement.
LOFAR MSSS: detection of a low-frequency radio transient in 400 h of monitoring of the North Celestial Pole
Publisher: Oxford University Press (OUP)
Date: 31-12-2015
First Constraints on Compact Dark Matter from Fast Radio Burst Microstructure
Publisher: American Astronomical Society
Date: 08-09-2020
Binary Pulsar Distances and Velocities from Gaia Data Release 2
Publisher: American Astronomical Society
Date: 27-08-2018
A Machine Learning Classifier for Fast Radio Burst Detection at the VLBA
Publisher: IOP Publishing
Date: 22-06-2016
A single fast radio burst localized to a massive galaxy at cosmological distance.
Publisher: American Association for the Advancement of Science (AAAS)
Date: 09-08-2019
Abstract: Fast radio bursts (FRBs) are brief radio emissions from distant astronomical sources. Some are known to repeat, but most are single bursts. Nonrepeating FRB observations have had insufficient positional accuracy to localize them to an in idual host galaxy. We report the interferometric localization of the single-pulse FRB 180924 to a position 4 kiloparsecs from the center of a luminous galaxy at redshift 0.3214. The burst has not been observed to repeat. The properties of the burst and its host are markedly different from those of the only other accurately localized FRB source. The integrated electron column density along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.
Low-frequency radio absorption in Cassiopeia A
Publisher: EDP Sciences
Date: 04-2018
DOI: 10.1051/0004-6361/201732411
Abstract: Context. Cassiopeia A is one of the best-studied supernova remnants. Its bright radio and X-ray emission is due to shocked ejecta. Cas A is rather unique in that the unshocked ejecta can also be studied: through emission in the infrared, the radio-active decay of 44 Ti, and the low-frequency free-free absorption caused by cold ionised gas, which is the topic of this paper. Aims. Free-free absorption processes are affected by the mass, geometry, temperature, and ionisation conditions in the absorbing gas. Observations at the lowest radio frequencies can constrain a combination of these properties. Methods. We used Low Frequency Array (LOFAR) Low Band Antenna observations at 30–77 MHz and Very Large Array (VLA) L -band observations at 1–2 GHz to fit for internal absorption as parametrised by the emission measure. We simultaneously fit multiple UV-matched images with a common resolution of 17″ (this corresponds to 0.25 pc for a source at the distance of Cas A). The le frequency coverage allows us separate the relative contributions from the absorbing gas, the unabsorbed front of the shell, and the absorbed back of the shell to the emission spectrum. We explored the effects that a temperature lower than the ~100–500 K proposed from infrared observations and a high degree of clumping can have on the derived physical properties of the unshocked material, such as its mass and density. We also compiled integrated radio flux density measurements, fit for the absorption processes that occur in the radio band, and considered their effect on the secular decline of the source. Results. We find a mass in the unshocked ejecta of M = 2.95 ± 0.48 M ⊙ for an assumed gas temperatureof T = 100 K. This estimate is reduced for colder gas temperatures and, most significantly, if the ejecta are clumped. We measure the reverse shock to have a radius of 114″± 6″ and be centred at 23:23:26, +58:48:54 (J2000). We also find that a decrease in the amount of mass in the unshocked ejecta (as more and more material meets the reverse shock and heats up) cannot account for the observed low-frequency behaviour of the secular decline rate. Conclusions. To reconcile our low-frequency absorption measurements with models that reproduce much of the observed behaviour in Cas A and predict little mass in the unshocked ejecta, the ejecta need to be very clumped or the temperature in the cold gas needs to be low (~10 K). Both of these options are plausible and can together contribute to the high absorption value that we find.
LIMITS ON THE EVENT RATES OF FAST RADIO TRANSIENTS FROM THE V-FASTR EXPERIMENT
Publisher: American Astronomical Society
Date: 26-06-2012
Vintage telescope rebooted in the hunt for FRBs
Publisher: Springer Science and Business Media LLC
Date: 12-03-2020
Simultaneous determination of CKM angle γ and charm mixing parameters
Publisher: Springer Science and Business Media LLC
Date: 12-2021
Abstract: A combination of measurements sensitive to the CP violation angle γ of the Cabibbo-Kobayashi-Maskawa unitarity triangle and to the charm mixing parameters that describe oscillations between D 0 and $$ \\overline{D} $$ D ¯ 0 mesons is performed. Results from the charm and beauty sectors, based on data collected with the LHCb detector at CERN’s Large Hadron Collider, are combined for the first time. This method provides an improvement on the precision of the charm mixing parameter y by a factor of two with respect to the current world average. The charm mixing parameters are determined to be $$ x=\\left({0.400}_{-0.053}^{+0.052}\\right)\\% $$ x = 0.400 − 0.053 + 0.052 % and y = $$ \\left({0.630}_{-0.030}^{+0.033}\\right)\\% $$ 0.630 − 0.030 + 0.033 % . The angle γ is found to be γ = $$ \\left({65.4}_{-4.2}^{+3.8}\\right){}^{\\circ} $$ 65.4 − 4.2 + 3.8 ° and is the most precise determination from a single experiment.
Quasi-simultaneous Radio/X-Ray Observations of the Candidate Transitional Millisecond Pulsar 3FGL J1544.6−1125 during its Low-luminosity Accretion-disk State
Publisher: American Astronomical Society
Date: 12-2021
Abstract: 3FGL J1544.6−1125 is a candidate transitional millisecond pulsar (tMSP). Similar to the well-established tMSPs—PSR J1023+0038, IGR J18245−2452, and XSS J12270−4859—3FGL J1544.6−1125 shows γ -ray emission and discrete X-ray “low” and “high” modes during its low-luminosity accretion-disk state. Coordinated radio/X-ray observations of PSR J1023+0038 in its current low-luminosity accretion-disk state showed rapidly variable radio continuum emission—possibly originating from a compact, self-absorbed jet, the “propellering” of accretion material, and/or pulsar moding. 3FGL J1544.6−1125 is currently the only other (candidate) tMSP system in this state, and can be studied to see whether tMSPs are typically radio-loud compared to other neutron star binaries. In this work, we present a quasi-simultaneous Very Large Array and Swift radio/X-ray c aign on 3FGL J1544.6−1125. We detect 10 GHz radio emission varying in flux density from 47.7 ± 6.0 μ Jy down to ≲15 μ Jy (3 σ upper limit) at four epochs spanning three weeks. At the brightest epoch, the radio luminosity is L 5 GHz = (2.17 ± 0.17) × 10 27 erg s −1 for a quasi-simultaneous X-ray luminosity L 2–10 keV = (4.32 ± 0.23) × 10 33 erg s −1 (for an assumed distance of 3.8 kpc). These luminosities are close to those of PSR J1023+0038, and the results strengthen the case that 3FGL J1544.6−1125 is a tMSP showing similar phenomenology to PSR J1023+0038.
The Panchromatic Afterglow of GW170817: The Full Uniform Data Set, Modeling, Comparison with Previous Results, and Implications
Publisher: American Astronomical Society
Date: 26-11-2021
Abstract: We present the full panchromatic afterglow light-curve data of GW170817, including new radio data as well as archival optical and X-ray data, between 0.5 and 940 days post-merger. By compiling all archival data and reprocessing a subset of it, we have evaluated the impact of differences in data processing or flux determination methods used by different groups and attempted to mitigate these differences to provide a more uniform data set. Simple power-law fits to the uniform afterglow light curve indicate a t 0.86±0.04 rise, a t −1.92±0.12 decline, and a peak occurring at 155 ± 4 days. The afterglow is optically thin throughout its evolution, consistent with a single spectral index (−0.584 ± 0.002) across all epochs. This gives a precise and updated estimate of the electron power-law index, p = 2.168 ± 0.004. By studying the diffuse X-ray emission from the host galaxy, we place a conservative upper limit on the hot ionized interstellar medium density, .01 cm −3 , consistent with previous afterglow studies. Using the late-time afterglow data we rule out any long-lived neutron star remnant having a magnetic field strength between 10 10.4 and 10 16 G. Our fits to the afterglow data using an analytical model that includes Very Long Baseline Interferometry proper motion from Mooley et al., and a structured jet model that ignores the proper motion, indicates that the proper-motion measurement needs to be considered when seeking an accurate estimate of the viewing angle.
Microwave spectroscopy of the 1snp PJ 3 fine structure of high Rydberg states in He 4 MICROWAVE SPECTROSCOPY of the 1snp 3PJ ... A. DELLER and S. D. HOGAN
Publisher: American Physical Society (APS)
Date: 12-01-2018
Measurement of
C P
Publisher:
American Physical Society (APS)
Date:
02-03-2021
Publisher: American Physical Society (APS)
Date: 02-03-2021
Disentangling the Cosmic Web toward FRB 190608
Publisher: American Astronomical Society
Date: 30-09-2020
A Nonrepeating Fast Radio Burst in a Dwarf Host Galaxy
Publisher: American Astronomical Society
Date: 05-2023
Abstract: We present the discovery of an as yet nonrepeating fast radio burst (FRB), FRB 20210117A, with the Australian Square Kilometre Array Pathfinder (ASKAP), as a part of the Commensal Real-time ASKAP Fast Transients Survey. The subarcsecond localization of the burst led to the identification of its host galaxy at z = 0.214(1). This redshift is much lower than what would be expected for a source dispersion measure (DM) of 729 pc cm −3 , given typical contributions from the intergalactic medium and the host galaxy. Optical observations reveal the host to be a dwarf galaxy with little ongoing star formation—very different to the dwarf host galaxies of the known repeating FRBs 20121102A and 20190520B. We find an excess DM contribution from the host and attribute it to the FRB’s local environment. We do not find any radio emission from the FRB site or host galaxy. The low magnetized environment and the lack of a persistent radio source indicate that the FRB source is older than those found in other dwarf host galaxies, establishing the ersity of FRB sources in dwarf galaxy environments. We find our observations to be fully consistent with the “hypernebula” model, where the FRB is powered by an accretion jet from a hyperaccreting black hole. Finally, our high time resolution analysis reveals burst characteristics similar to those seen in repeating FRBs. We encourage follow-up observations of FRB 20210117A to establish any repeating nature.
Spectropolarimetric Analysis of FRB 181112 at Microsecond Resolution: Implications for Fast Radio Burst Emission Mechanism
Publisher: American Astronomical Society
Date: 12-03-2020
Measurement of
C P
Publisher:
American Physical Society (APS)
Date:
27-08-2021
Publisher: American Physical Society (APS)
Date: 27-08-2021
Sub-arcsecond imaging of Arp 299-A at 150 MHz with LOFAR: Evidence for a starburst-driven outflow
Publisher: EDP Sciences
Date: 02-2018
DOI: 10.1051/0004-6361/201732543
Abstract: We report on the first sub-arcsecond (0.44 × 0.41 arcsec 2 ) angular resolution image at 150 MHz of the A-nucleus in the luminous infrared galaxy Arp 299, from International Low Frequency Array (LOFAR) Telescope observations. The most remarkable finding is that of an intriguing two-sided, filamentary structure emanating from the A-nucleus, which we interpret as an outflow that extends up to at least 14 arcsec from the A-nucleus in the N–S direction ( ≈5 kpc deprojected size) and accounts for almost 40% of the extended emission of the entire galaxy system. We also discuss HST/NICMOS [FeII] 1.64 μ m and H 2 2.12 μ m images of Arp 299-A, which show similar features to those unveiled by our 150 MHz LOFAR observations, providing strong morphological support for the outflow scenario. Finally, we discuss unpublished Na I D spectra that confirm the outflow nature of this structure. From energetic arguments, we rule out the low-luminosity active galactic nucleus in Arp 299-A as a driver for the outflow. On the contrary, the powerful, compact starburst in the central regions of Arp 299-A provides plenty of mechanical energy to sustain an outflow, and we conclude that the intense supernova (SN) activity in the nuclear region of Arp 299-A is driving the observed outflow. We estimate that the starburst wind can support a mass-outflow rate in the range (11–63 M ⊙ yr −1 ) at speeds of up to 370–890 km s −1 , and is relatively young, with an estimated kinematic age of 3–7 Myr. Those results open an avenue to the use of low-frequency (150 MHz), sub-arcsecond imaging with LOFAR to detect outflows in the central regions of local luminous infrared galaxies.
The LOFAR Multifrequency Snapshot Sky Survey (MSSS)
Publisher: EDP Sciences
Date: 10-2015
The Host Galaxies and Progenitors of Fast Radio Bursts Localized with the Australian Square Kilometre Array Pathfinder
Publisher: American Astronomical Society
Date: 06-2020
e-VLBI observations of GHz-peaked spectrum radio sources in nearby galaxies from the AT20G survey
Publisher: Oxford University Press (OUP)
Date: 21-08-2009
Putting carbon markets into practice: A case study of financial accounting in Europe
Publisher: SAGE Publications
Date: 2013
DOI: 10.1068/C1275
Abstract: In this paper we explore how carbon markets have entered the world of financial accounting. The advent of the European Union Emissions Trading System (EU ETS) in 2005 provided the opportunity for global climate change concerns to be translated from policy into something that could, and should, be recognised within financial accounting. That is, the EU ETS provided a mechanism whereby greenhouse gas emission allowances acquired a financial value, simultaneously creating an obligation (or liability) on certain European organisations when they emit greenhouse gases. Prima facie, this process created the need for financial accounts of companies covered by the EU ETS to reflect the new commodity of carbon. Disagreement amongst accountants about how to treat emission allowances has arisen, with the initial international accounting guidance issued in late 2004 subsequently being withdrawn, and not yet replaced. Taking this absence of guidance as a starting point, we undertake an empirical project (through a survey, consultation analysis, and interviews) to establish what financial reporting practices are being adopted by participants in the EU ETS, and the level of momentum for standardisation. We draw on sociological theories about accounting, measurement, and markets.
A population analysis of pulse broadening in ASKAP fast radio bursts
Publisher: Oxford University Press (OUP)
Date: 06-07-2020
Abstract: The pulse morphology of fast radio bursts (FRBs) provides key information in both understanding progenitor physics and the plasma medium through which the burst propagates. We present a study of the profiles of 33 bright FRBs detected by the Australian Square Kilometre Array Pathfinder. We identify seven FRBs with measureable intrinsic pulse widths, including two FRBs that have been seen to repeat. In our modest s le, we see no evidence for bimodality in the pulse width distribution. We also identify five FRBs with evidence of millisecond time-scale pulse broadening caused by scattering in inhomogeneous plasma. We find no evidence for a relationship between pulse broadening and extragalactic dispersion measure. The scattering could be either caused by extreme turbulence in the host galaxy or chance propagation through foreground galaxies. With future high time resolution observations and detailed study of host galaxy properties, we may be able to probe line-of-sight turbulence on gigaparsec scales.
Two-screen scattering in CRAFT FRBs
Publisher: Oxford University Press (OUP)
Date: 09-2023
Low-frequency pulse profile variation in PSR B2217+47: evidence for echoes from the interstellar medium
Publisher: Oxford University Press (OUP)
Date: 13-02-2018
DOI: 10.1093/MNRAS/STY368
Universality of free fall from the orbital motion of a pulsar in a stellar triple system
Publisher: Springer Science and Business Media LLC
Date: 07-2018
DOI: 10.1038/S41586-018-0265-1
Abstract: Einstein's theory of gravity-the general theory of relativity
Branching Fraction Measurements of the Rare
B s 0
Publisher: American Physical Society (APS)
Date: 05-10-2021
Revealing two radio-active galactic nuclei extremely near PSR J0437−4715
Publisher: Oxford University Press (OUP)
Date: 27-02-2018
DOI: 10.1093/MNRAS/STY210
Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Publisher: American Astronomical Society
Date: 31-08-2023
Abstract: Studies of the time-domain structure of fast radio bursts (FRBs) require an accurate estimate of the FRB dispersion measure in order to recover the intrinsic burst shape. Furthermore, the exact dispersion measure is itself of interest when studying the time evolution of the medium through which multiple bursts from repeating FRBs propagate. A commonly used approach to obtain the dispersion measure is to take the value that maximizes the FRB structure in the time domain. However, various authors use differing methods to obtain this structure parameter and do not document the smoothing method used. Furthermore, there are no quantitative estimates of the error in this procedure in the FRB literature. In this article, we present a smoothing filter based on the discrete cosine transform, and show that computing the structure parameter by summing the squares of the derivatives and taking the square root (that is, the 2-norm, Σ ( d / dt ) 2 ) immediately lends itself to the calculation of the uncertainty of the structure parameter. We illustrate this with FRB 20181112A and FRB 20210117A data, which were detected by the Australian Square Kilometre Array Pathfinder, and for which high-time-resolution data are available.
CONSTRAINTS ON THE RADIAL VARIATION OF GRAIN GROWTH IN THE AS 209 CIRCUMSTELLAR DISK
Publisher: American Astronomical Society
Date: 02-11-2012
Tracking of an electron beam through the solar corona with LOFAR
Publisher: EDP Sciences
Date: 03-2018
DOI: 10.1051/0004-6361/201629017
Abstract: The Sun’s activity leads to bursts of radio emission, among other phenomena. An ex le is type-III radio bursts. They occur frequently and appear as short-lived structures rapidly drifting from high to low frequencies in dynamic radio spectra. They are usually interpreted as signatures of beams of energetic electrons propagating along coronal magnetic field lines. Here we present novel interferometric LOFAR (LOw Frequency ARray) observations of three solar type-III radio bursts and their reverse bursts with high spectral, spatial, and temporal resolution. They are consistent with a propagation of the radio sources along the coronal magnetic field lines with nonuniform speed. Hence, the type-III radio bursts cannot be generated by a monoenergetic electron beam, but by an ensemble of energetic electrons with a spread distribution in velocity and energy. Additionally, the density profile along the propagation path is derived in the corona. It agrees well with three-fold coronal density model by (1961, ApJ, 133, 983).
Software correlators in radio astronomy
Publisher: SPIE-Intl Soc Optical Eng
Date: 2009
Dissecting the Local Environment of FRB 190608 in the Spiral Arm of its Host Galaxy
Publisher: American Astronomical Society
Date: 29-11-2021
Abstract: We present a high-resolution analysis of the host galaxy of fast radio burst (FRB) 190608, an SB(r)c galaxy at z = 0.11778 (hereafter HG 190608), to dissect its local environment and its contributions to the FRB properties. Our Hubble Space Telescope Wide Field Camera 3 ultraviolet and visible light image reveals that the subarcsecond localization of FRB 190608 is coincident with a knot of star formation (Σ SFR = 1.5 × 10 −2 M ⊙ yr −1 kpc −2 ) in the northwest spiral arm of HG 190608. Using H β emission present in our Keck Cosmic Web Imager integral field spectrum of the galaxy with a surface brightness of μ H β = ( 3.36 ± 0.21 ) × 10 − 17 erg s − 1 cm − 2 arcsec − 2 , we infer an extinction-corrected H α surface brightness and compute a dispersion measure (DM) from the interstellar medium of HG 190608 of DM Host,ISM = 94 ± 38 pc cm −3 . The galaxy rotates with a circular velocity v circ = 141 ± 8 km s −1 at an inclination i gas = 37° ± 3°, giving a dynamical mass M halo dyn ≈ 10 11.96 ± 0.08 M ⊙ . This implies a halo contribution to the DM of DM Host,Halo = 55 ± 25 pc cm −3 subject to assumptions on the density profile and fraction of baryons retained. From the galaxy rotation curve, we infer a bar-induced pattern speed of Ω p = 34 ± 6 km s −1 kpc −1 using linear resonance theory. We then calculate the maximum time since star formation for a progenitor using the furthest distance to the arm’s leading edge within the localization, and find t enc = 21 − 6 + 25 Myr. Unlike previous high-resolution studies of FRB environments, we find no evidence of disturbed morphology, emission, or kinematics for FRB 190608.
Lunar occultation of the diffuse radio sky: LOFAR measurements between 35 and 80 MHz
Publisher: Oxford University Press (OUP)
Date: 06-05-2015
DOI: 10.1093/MNRAS/STV746
COORDINATED X-RAY, ULTRAVIOLET, OPTICAL, AND RADIO OBSERVATIONS OF THE PSR J1023+0038 SYSTEM IN A LOW-MASS X-RAY BINARY STATE
Publisher: American Astronomical Society
Date: 15-06-2015
The LOFAR long baseline snapshot calibrator survey
Publisher: EDP Sciences
Date: 28-01-2015
Measurement of χc1(3872) production in proton-proton collisions at $$ \sqrt{s} $$ = 8 and 13 TeV
Publisher: Springer Science and Business Media LLC
Date: 2022
Abstract: The production cross-section of the χ c 1 (3872) state relative to the ψ (2 S ) meson is measured using proton-proton collision data collected with the LHCb experiment at centre-of-mass energies of $$ \\sqrt{s} $$ s = 8 and 13 TeV, corresponding to integrated luminosities of 2.0 and 5.4 fb − 1 , respectively. The two mesons are reconstructed in the J/ψπ + π − final state. The ratios of the prompt and nonprompt χ c 1 (3872) to ψ (2 S ) production cross-sections are measured as a function of transverse momentum, p T , and rapidity, y , of the χ c 1 (3872) and ψ (2 S ) states, in the kinematic range 4 p T 20 GeV/ c and 2 . 0 y 4 . 5. The prompt ratio is found to increase with p T , independently of y . For the prompt component, the double ratio of the χ c 1 (3872) and ψ (2 S ) production cross-sections between 13 and 8 TeV is observed to be consistent with unity, independent of p T and centre-of-mass energy.
Spectropolarimetric variability in the repeating fast radio burst source FRB 20180301A
Publisher: Oxford University Press (OUP)
Date: 28-09-2023
A strong magnetic field around the supermassive black hole at the centre of the Galaxy
Publisher: Springer Science and Business Media LLC
Date: 14-08-2013
DOI: 10.1038/NATURE12499
Abstract: Earth's nearest candidate supermassive black hole lies at the centre of the Milky Way. Its electromagnetic emission is thought to be powered by radiatively inefficient accretion of gas from its environment, which is a standard mode of energy supply for most galactic nuclei. X-ray measurements have already resolved a tenuous hot gas component from which the black hole can be fed. The magnetization of the gas, however, which is a crucial parameter determining the structure of the accretion flow, remains unknown. Strong magnetic fields can influence the dynamics of accretion, remove angular momentum from the infalling gas, expel matter through relativistic jets and lead to synchrotron emission such as that previously observed. Here we report multi-frequency radio measurements of a newly discovered pulsar close to the Galactic Centre and show that the pulsar's unusually large Faraday rotation (the rotation of the plane of polarization of the emission in the presence of an external magnetic field) indicates that there is a dynamically important magnetic field near the black hole. If this field is accreted down to the event horizon it provides enough magnetic flux to explain the observed emission--from radio to X-ray wavelengths--from the black hole.
Probabilistic Association of Transients to their Hosts (PATH)
Publisher: American Astronomical Society
Date: 04-2021
Abstract: We introduce a new method to estimate the probability that an extragalactic transient source is associated with a candidate host galaxy. This approach relies solely on simple observables: sky coordinates and their uncertainties, galaxy fluxes, and angular sizes. The formalism invokes Bayes’ rule to calculate the posterior probability from the galaxy prior P ( O ), observables x , and an assumed model for the true distribution of transients in/around their host galaxies. Using simulated transients placed in the well-studied Cosmic Evolution Survey field, we consider several agnostic and physically motivated priors and offset distributions to explore the method sensitivity. We then apply the methodology to the set of 13 fast radio bursts (FRBs) localized with an uncertainty of several arcseconds. Our methodology finds nine of these are securely associated to a single host galaxy, . We examine the observed and intrinsic properties of these secure FRB hosts, recovering distributions similar to those found in previous works. Furthermore, we find a strong correlation between the apparent magnitude of the securely identified host galaxies and the estimated cosmic dispersion measures of the corresponding FRBs, which results from the Macquart relation. Future work with FRBs will leverage this relation and other measures from the secure hosts as priors for future associations. The methodology is generic to transient type, localization error, and image quality. We encourage its application to other transients where host galaxy associations are critical to the science, e.g., gravitational wave events, gamma-ray bursts, and supernovae. We have encoded the technique in Python on GitHub: github.com/FRBs/astropath .
Detection of a Glitch in PSR J0908-4913 by UTMOST
Publisher: American Astronomical Society
Date: 17-12-2019
A large light-mass component of cosmic rays at 1017–1017.5 electronvolts from radio observations
Publisher: Springer Science and Business Media LLC
Date: 02-03-2016
DOI: 10.1038/NATURE16976
Abstract: Cosmic rays are the highest-energy particles found in nature. Measurements of the mass composition of cosmic rays with energies of 10(17)-10(18) electronvolts are essential to understanding whether they have galactic or extragalactic sources. It has also been proposed that the astrophysical neutrino signal comes from accelerators capable of producing cosmic rays of these energies. Cosmic rays initiate air showers--cascades of secondary particles in the atmosphere-and their masses can be inferred from measurements of the atmospheric depth of the shower maximum (Xmax the depth of the air shower when it contains the most particles) or of the composition of shower particles reaching the ground. Current measurements have either high uncertainty, or a low duty cycle and a high energy threshold. Radio detection of cosmic rays is a rapidly developing technique for determining Xmax (refs 10, 11) with a duty cycle of, in principle, nearly 100 per cent. The radiation is generated by the separation of relativistic electrons and positrons in the geomagnetic field and a negative charge excess in the shower front. Here we report radio measurements of Xmax with a mean uncertainty of 16 grams per square centimetre for air showers initiated by cosmic rays with energies of 10(17)-10(17.5) electronvolts. This high resolution in Xmax enables us to determine the mass spectrum of the cosmic rays: we find a mixed composition, with a light-mass fraction (protons and helium nuclei) of about 80 per cent. Unless, contrary to current expectations, the extragalactic component of cosmic rays contributes substantially to the total flux below 10(17.5) electronvolts, our measurements indicate the existence of an additional galactic component, to account for the light composition that we measured in the 10(17)-10(17.5) electronvolt range.
Late-time Evolution and Modeling of the Off-axis Gamma-Ray Burst Candidate FIRST J141918.9+394036
Publisher: American Astronomical Society
Date: 2022
Abstract: We present new radio and optical data, including very-long-baseline interferometry, as well as archival data analysis, for the luminous, decades-long radio transient FIRST J141918.9+394036. The radio data reveal a synchrotron self-absorption peak around 0.3 GHz and a radius of around 1.3 mas (0.5 pc) 26 yr post-discovery, indicating a blastwave energy ∼5 × 10 50 erg. The optical spectrum shows a broad [O iii ] λ 4959,5007 emission line that may indicate collisional excitation in the host galaxy, but its association with the transient cannot be ruled out. The properties of the host galaxy are suggestive of a massive stellar progenitor that formed at low metallicity. Based on the radio light curve, blastwave velocity, energetics, nature of the host galaxy and transient rates, we find that the properties of J1419+3940 are most consistent with long gamma-ray burst (LGRB) afterglows. Other classes of (optically discovered) stellar explosions as well as neutron star mergers are disfavored, and invoking any exotic scenario may not be necessary. It is therefore likely that J1419+3940 is an off-axis LGRB afterglow (as suggested by Law et al. and Marcote et al.), and under this premise the inverse beaming fraction is found to be f b − 1 ≃ 280 − 200 + 700 , corresponding to an average jet half-opening angle θ j ≃ 5 − 2 + 4 degrees (68% confidence), consistent with previous estimates. From the volumetric rate we predict that surveys with the Very Large Array, Australian Square Kilometre Array Pathfinder, and MeerKAT will find a handful of J1419+3940-like events over the coming years.
VLA Observations of Single Pulses from the Galactic Center Magnetar
Publisher: American Astronomical Society
Date: 24-04-2019
MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSRπ. I. TWO BINARY MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS
Publisher: American Astronomical Society
Date: 22-08-2016
Limits on Precursor and Afterglow Radio Emission from a Fast Radio Burst in a Star-forming Galaxy
Publisher: American Astronomical Society
Date: 24-09-2020
Microarcsecond VLBI Pulsar Astrometry with PSRπ II. Parallax Distances for 57 Pulsars
Publisher: American Astronomical Society
Date: 22-04-2019
VLBA+GBT observations of the COSMOS field and radio source counts at 1.4 GHz
Publisher: EDP Sciences
Date: 08-2018
DOI: 10.1051/0004-6361/201832969
Abstract: We present very long baseline interferometry (VLBI) observations of 179 radio sources in the COSMOS field with extremely high sensitivity using the Green Bank Telescope (GBT) together with the Very Long Baseline Array (VLBA) (VLBA+GBT) at 1.4 GHz, to explore the faint radio population in the flux density regime of tens of μJy. Here, the identification of active galactic nuclei (AGN) is based on the VLBI detection of the source, meaning that it is independent of X-ray or infrared properties. The milli-arcsecond resolution provided by the VLBI technique implies that the detected sources must be compact and have large brightness temperatures, and therefore they are most likely AGN (when the host galaxy is located at z ≥ 0.1). On the other hand, this technique only allows us to positively identify when a radio-active AGN is present, in other words, we cannot affirm that there is no AGN when the source is not detected. For this reason, the number of identified AGN using VLBI should be always treated as a lower limit. We present a catalogue containing the 35 radio sources detected with the VLBA+GBT, ten of which were not previously detected using only the VLBA. We have constructed the radio source counts at 1.4 GHz using the s les of the VLBA and VLBA+GBT detected sources of the COSMOS field to determine a lower limit for the AGN contribution to the faint radio source population. We found an AGN contribution of −75% at flux density levels between 150 μJy and 1 mJy. This flux density range is characterised by the upturn of the Euclidean-normalised radio source counts, which implies a contribution of a new population. This result supports the idea that the sub-mJy radio population is composed of a significant fraction of radio-emitting AGN, rather than solely by star-forming galaxies, in agreement with previous studies.
Angular analysis of $$ {B}^0\to {D}^{\ast -}{D}_s^{\ast +} $$ with $$ {D}_s^{\ast +}\to {D}_s^{+}\gamma $$ decays
Publisher: Springer Science and Business Media LLC
Date: 06-2021
Abstract: The first full angular analysis of the $$ {B}^0\\to {D}^{\\ast -}{D}_s^{\\ast +} $$ B 0 → D ∗ − D s ∗ + decay is performed using 6 fb − 1 of pp collision data collected with the LHCb experiment at a centre-of-mass energy of 13 TeV. The $$ {D}_s^{\\ast +}\\to {D}_s^{+}\\gamma $$ D s ∗ + → D s + γ and D * − → $$ {\\overline{D}}^0{\\pi}^{-} $$ D ¯ 0 π − vector meson decays are used with the subsequent $$ {D}_s^{+} $$ D s + → K + K − π + and $$ {\\overline{D}}^0 $$ D ¯ 0 → K + π − decays. All helicity litudes and phases are measured, and the longitudinal polarisation fraction is determined to be f L = 0 . 578 ± 0 . 010 ± 0 . 011 with world-best precision, where the first uncertainty is statistical and the second is systematic. The pattern of helicity litude magnitudes is found to align with expectations from quark-helicity conservation in B decays. The ratio of branching fractions [ℬ( $$ {B}^0\\to {D}^{\\ast -}{D}_s^{\\ast +} $$ B 0 → D ∗ − D s ∗ + ) × ℬ( $$ {D}_s^{\\ast +}\\to {D}_s^{+}\\gamma $$ D s ∗ + → D s + γ )] / ℬ( B 0 → D * − $$ {D}_s^{+} $$ D s + ) is measured to be 2 . 045 ± 0 . 022 ± 0 . 071 with world-best precision. In addition, the first observation of the Cabibbo-suppressed B s → D * − $$ {D}_s^{+} $$ D s + decay is made with a significance of seven standard deviations. The branching fraction ratio ℬ( B s → D * − $$ {D}_s^{+} $$ D s + ) / ℬ( B 0 → D * − $$ {D}_s^{+} $$ D s + ) is measured to be 0 . 049 ± 0 . 006 ± 0 . 003 ± 0 . 002, where the third uncertainty is due to limited knowledge of the ratio of fragmentation fractions.
The geometric distance and binary orbit of PSR B1259–63
Publisher: Oxford University Press (OUP)
Date: 05-07-2018
Multi-source self-calibration: Unveiling the microJy population of compact radio sources
Publisher: EDP Sciences
Date: 23-02-2016
Measurement of the photon polarization in
Λ b 0
Publisher:
American Physical Society (APS)
Date:
23-03-2022
Publisher: American Physical Society (APS)
Date: 23-03-2022
TW Hydrae: multi-wavelength interferometry of a transition disk
Publisher: Cambridge University Press (CUP)
Date: 06-2013
DOI: 10.1017/S1743921313008016
Abstract: For over a decade, the structure of the inner “hole” in the transition disk around TW Hydrae has been a subject of debate. To probe the innermost regions of the protoplanetary disk, observations at the highest possible spatial resolution are required. We present new interferometric data of TW Hya from near-infrared to millimeter wavelengths. We confront existing models of the disk structure with the complete data set and develop a new, detailed radiative-transfer model. This model is characterized by: 1) a spatial separation of the largest grains from the small disk grains and 2) a smooth inner rim structure, rather than a sharp disk edge.
J / ψ
Publisher:
American Physical Society (APS)
Date:
03-03-2022
Publisher: American Physical Society (APS)
Date: 03-03-2022
A transient, flat spectrum radio pulsar near the Galactic Centre
Publisher: Oxford University Press (OUP)
Date: 09-03-2017
DOI: 10.1093/MNRAS/STX583
Measurement of prompt charged-particle production in pp collisions at $$ \sqrt{\mathrm{s}} $$ = 13 TeV
Publisher: Springer Science and Business Media LLC
Date: 2022
Abstract: The differential cross-section of prompt inclusive production of long-lived charged particles in proton-proton collisions is measured using a data s le recorded by the LHCb experiment at a centre-of-mass energy of $$ \\sqrt{s} $$ s = 13 TeV. The data s le, collected with an unbiased trigger, corresponds to an integrated luminosity of 5 . 4 nb − 1 . The differential cross-section is measured as a function of transverse momentum and pseudorapidity in the ranges p T ∈ [80 , 10 000) MeV /c and η ∈ [2 . 0 , 4 . 8) and is determined separately for positively and negatively charged particles. The results are compared with predictions from various hadronic-interaction models.
A radio parallax to the black hole X-ray binary MAXI J1820+070
Publisher: Oxford University Press (OUP)
Date: 20-01-2020
Abstract: Using the Very Long Baseline Array and the European Very Long Baseline Interferometry Network, we have made a precise measurement of the radio parallax of the black hole X-ray binary MAXI J1820+070, providing a model-independent distance to the source. Our parallax measurement of (0.348 ± 0.033) mas for MAXI J1820+070 translates to a distance of (2.96 ± 0.33) kpc. This distance implies that the source reached (15 ± 3) per cent of the Eddington luminosity at the peak of its outburst. Further, we use this distance to refine previous estimates of the jet inclination angle, jet velocity, and the mass of the black hole in MAXI J1820+070 to be (63 ± 3)°, (0.89 ± 0.09) c, and (9.2 ± 1.3) M⊙, respectively.
A Hubble constant measurement from superluminal motion of the jet in GW170817
Publisher: Springer Science and Business Media LLC
Date: 08-07-2019
Search for $$D^{*}(2007)^{0} \rightarrow \mu ^{+} \mu ^{-}$$ in $$B^{-}\rightarrow \pi ^{-} \mu ^{+} \mu ^{-}$$ decays
Publisher: Springer Science and Business Media LLC
Date: 02-01-2202
DOI: 10.1140/EPJC/S10052-023-11759-6
Abstract: The very rare $${{D} ^*} (2007)^0\\!\\rightarrow {\\mu ^+\\mu ^-} $$ D ∗ ( 2007 ) 0 → μ + μ - decay is searched for by analysing $${{{B} ^-}} \\!\\rightarrow {{\\pi } ^-} {\\mu ^+\\mu ^-} $$ B - → π - μ + μ - decays. The analysis uses a s le of beauty mesons produced in proton–proton collisions collected with the LHCb detector between 2011 and 2018, corresponding to an integrated luminosity of 9 $$\\text {\\,fb} ^{-1}$$ \\,fb - 1 . The signal signature corresponds to simultaneous peaks in the $${\\mu ^+\\mu ^-} $$ μ + μ - and $${{\\pi } ^-} {\\mu ^+\\mu ^-} $$ π - μ + μ - invariant masses. No evidence for an excess of events over background is observed and an upper limit is set on the branching fraction of the decay at $$\\mathcal{B}({{D} ^*} (2007)^0\\!\\rightarrow {\\mu ^+\\mu ^-} ) 2.6\\times 10^{-8}$$ B ( D ∗ ( 2007 ) 0 → μ + μ - ) 2.6 × 10 - 8 at $$90\\%$$ 90 % confidence level. This is the first limit on the branching fraction of $${{D} ^*} (2007)^0\\!\\rightarrow {\\mu ^+\\mu ^-} $$ D ∗ ( 2007 ) 0 → μ + μ - decays and the most stringent limit on $${{D} ^*} (2007)^0$$ D ∗ ( 2007 ) 0 decays to leptonic final states. The analysis is the first search for a rare charm-meson decay exploiting production via beauty decays.
DiFX-2: A More Flexible, Efficient, Robust, and Powerful Software Correlator
Publisher: IOP Publishing
Date: 03-2011
DOI: 10.1086/658907
Circularly polarized radio emission from the repeating fast radio burst source FRB 20201124A
Publisher: Oxford University Press (OUP)
Date: 14-03-2022
Abstract: The mechanism that produces fast radio burst (FRB) emission is poorly understood. Targeted monitoring of repeating FRB sources provides the opportunity to fully characterize the emission properties in a manner impossible with one-off bursts. Here, we report observations of the source of FRB 20201124A, with the Australian Square Kilometre Array Pathfinder (ASKAP) and the ultra-wideband low (UWL) receiver at the Parkes 64-m radio telescope (Murriyang). The source entered a period of emitting bright bursts during early 2021 April. We have detected 16 bursts from this source. One of the bursts detected with ASKAP is the brightest burst ever observed from a repeating FRB source with an inferred fluence of 640 ± 70 Jy ms. Of the five bursts detected with the Parkes UWL, none display any emission in the range 1.1–4 GHz. All UWL bursts are highly polarized, with their Faraday rotation measures (RMs) showing apparent variations. We obtain an average RM of −614 rad m−2 for this FRB source with a standard deviation of 16 rad m−2 in the UWL bursts. In one of the UWL bursts, we see evidence of significant circularly polarized emission with a fractional extent of 47 ± 1 per cent. Such a high degree of circular polarization has never been seen before in bursts from repeating FRB sources. We also see evidence for significant variation in the linear polarization position angle in the pulse profile of this UWL repeat burst. Models for repeat burst emission will need to account for the increasing ersity in the burst polarization properties.
The ultranarrow FRB20191107B, and the origins of FRB scattering
Publisher: Oxford University Press (OUP)
Date: 24-06-2022
Abstract: We report the detection of FRB20191107B with UTMOST radio telescope at a dispersion measure (DM) of 714.9 pc cm−3. The burst consists of three components, the brightest of which has an intrinsic width of only 11.3 μs and a scattering tail with an exponentially decaying time-scale of 21.4 μs measured at 835 MHz. We model the sensitivity of UTMOST and other major fast radio burst (FRB) surveys to such narrow events. We find that $\\gt 60{{\\ \\rm per\\, cent}}$ of FRBs like FRB20191107B are being missed, and that a significant population of very narrow FRBs probably exists and remains underrepresented in these surveys. The high DM and small scattering time-scale of FRB20191107B allows us to place an upper limit on the strength of turbulence in the intergalactic medium, quantified as scattering measure (SM), of SMIGM & 8.4 × 10−7 kpc m−20/3. Almost all UTMOST FRBs have full phase information due to real-time voltage capture, which provides us with the largest s le of coherently dedispersed single burst FRBs. Our 10.24 μs time resolution data yields accurately measured FRB scattering time-scales. We combine the UTMOST FRBs with 10 FRBs from the literature and find no obvious evidence for a DM-scattering relation, suggesting that IGM is not the dominant source of scattering in FRBs. We support the results of previous studies and identify the local environment of the source in the host galaxy as the most likely region that dominates the observed scattering of our FRBs.
DISCOVERY OF EXTENDED AND VARIABLE RADIO STRUCTURE FROM THE GAMMA-RAY BINARY SYSTEM PSR B1259–63/LS 2883
Publisher: American Astronomical Society
Date: 08-04-2011
Spatially resolved studies of extragalactic jets in high redshift radio galaxies
Publisher: Cambridge University Press (CUP)
Date: 09-2014
DOI: 10.1017/S1743921315002239
Abstract: The correlation between radio spectral steepness and redshift has been successfully used to find high redshift ( z ⩾ 2) radio galaxies, but the origin of this relation is unknown. The ultra-steep spectra of high-z radio sources make them ideally suited for studies with the Low Band Antenna of the new Low Frequency Array, which covers 10–80 MHz and has baselines up to about 1300 km. As part of an ongoing survey, we use the longest baselines to map the low-frequency ( 70 MHz) spatial distributions along the jets of 5 bright extended steep spectrum high-z radio sources. From this, we will determine whether the spectra change over these spatially resolved sources, thereby constraining particle acceleration processes. We present early results from our low-frequency survey of ultra-steep spectrum radio galaxies. The first low frequency long baseline images of these objects are presented.
RadioAstron observations of pulsars and interstellar scattering
Publisher: IEEE
Date: 2014
LOFAR Observations of 4C+19.44: On the Discovery of Low-frequency Spectral Curvature in Relativistic Jet Knots
Publisher: American Astronomical Society
Date: 28-02-2019
Search for the doubly charmed baryon Ω+cc
Publisher: Springer Science and Business Media LLC
Date: 31-08-2021
DOI: 10.1007/S11433-021-1742-7
Abstract: A search for the doubly charmed baryon Ω cc + with the decay mode Ω cc + → Ξ c + K − π + is performed using proton-proton collision data at a centre-of-mass energy of 13 TeV collected by the LHCb experiment from 2016 to 2018, corresponding to an integrated luminosity of 5.4 fb −1 . No significant signal is observed within the invariant mass range of 3.6 to 4.0GeV/ c 2 . Upper limits are set on the ratio R of the production cross-section times the total branching fraction of the Ω cc + → Ξ c + K − π + decay with respect to the $$\\Xi _{cc}^{ + + } \\to \\Lambda _c^ + {K^ - }{\\pi ^ + }{\\pi ^ + }$$ Ξ c c + + → Λ c + K − π + π + decay. Upper limits at 95% credibility level for R in the range 0.005 to 0.11 are obtained for different hypotheses on the Ω cc + mass and lifetime in the rapidity range from 2.0 to 4.5 and transverse momentum range from 4 to 15 GeV/ c .
Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations
Publisher: EDP Sciences
Date: 28-03-2016
Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9-342058
Publisher: Oxford University Press (OUP)
Date: 04-07-2016
Angular Analysis of
D 0 Publisher:
American Physical Society (APS)
Date:
03-06-2022
Publisher: American Physical Society (APS)
Date: 03-06-2022
Imaging Jupiter’s radiation belts down to 127 MHz with LOFAR
Publisher: EDP Sciences
Date: 11-02-2016
Search for time-dependent
C P
Publisher:
American Physical Society (APS)
Date:
26-10-2021
Publisher: American Physical Society (APS)
Date: 26-10-2021
Measurement of the W boson mass
Publisher: Springer Science and Business Media LLC
Date: 2022
Abstract: The W boson mass is measured using proton-proton collision data at $$ \\sqrt{s} $$ s = 13 TeV corresponding to an integrated luminosity of 1.7 fb − 1 recorded during 2016 by the LHCb experiment. With a simultaneous fit of the muon q T distribution of a s le of W → μν decays and the ϕ * distribution of a s le of Z → μμ decays the W boson mass is determined to be $$ {m}_w=80354\\pm {23}_{\\mathrm{stat}}\\pm {10}_{\\mathrm{exp}}\\pm {17}_{\\mathrm{theory}}\\pm {9}_{\\mathrm{PDF}}\\mathrm{MeV}, $$ m w = 80354 ± 23 stat ± 10 exp ± 17 theory ± 9 PDF MeV , where uncertainties correspond to contributions from statistical, experimental systematic, theoretical and parton distribution function sources. This is an average of results based on three recent global parton distribution function sets. The measurement agrees well with the prediction of the global electroweak fit and with previous measurements.
Implications of a VLBI distance to the double pulsar J0737-3039A/B
Publisher: American Association for the Advancement of Science (AAAS)
Date: 06-03-2009
Abstract: The double pulsar J0737-3039A/B is a unique system with which to test gravitational theories in the strong-field regime. However, the accuracy of such tests will be limited by knowledge of the distance and relative motion of the system. Here we present very long baseline interferometry (VLBI) observations which reveal that the distance to PSR J0737-3039A/B is \\batchmode \\documentclass[fleqn,10pt,legalpaper]{article} \\usepackage{amssymb} \\usepackage{amsfonts} \\usepackage{amsmath} \\pagestyle{empty} \\begin{document} \\(1150_{-160}^{+220}\\) \\end{document} parsecs, more than double previous estimates, and confirm its low transverse velocity (∼9 kilometers per second). Combined with a decade of pulsar timing, these results will allow tests of gravitational radiation emission theories at the 0.01% uncertainty level, putting stringent constraints on theories that predict dipolar gravitational radiation. They also allow insight into the system's formation and the source of its high-energy emission.
Study of coherent J/ψ production in lead-lead collisions at $$ \sqrt{{\mathrm{s}}_{\mathrm{NN}}} $$ = 5 TeV
Publisher: Springer Science and Business Media LLC
Date: 07-2022
Abstract: Coherent production of J/ψ mesons is studied in ultraperipheral lead-lead collisions at a nucleon-nucleon centre-of-mass energy of 5 TeV, using a data s le collected by the LHCb experiment corresponding to an integrated luminosity of about 10 μb −1 . The J/ψ mesons are reconstructed in the dimuon final state and are required to have transverse momentum below 1 GeV. The cross-section within the rapidity range of 2 . 0 y 4 . 5 is measured to be 4 . 45 ± 0 . 24 ± 0 . 18 ± 0 . 58 mb, where the first uncertainty is statistical, the second systematic and the third originates from the luminosity determination. The cross-section is also measured in J/ψ rapidity intervals. The results are compared to predictions from phenomenological models.
Search for the decay B0 → ϕμ+μ−
Publisher: Springer Science and Business Media LLC
Date: 11-05-2022
Abstract: A search for the decay B 0 → ϕμ + μ − is performed using proton-proton collisions at centre-of-mass energies of 7, 8, and 13 TeV collected by the LHCb experiment and corresponding to an integrated luminosity of 9 fb − 1 . No evidence for the B 0 → ϕμ + μ − decay is found and an upper limit on the branching fraction, excluding the ϕ and charmonium regions in the dimuon spectrum, of 4 . 4 × 10 − 3 at a 90% credibility level, relative to that of the $$ {B}_s^0 $$ B s 0 → ϕμ + μ − decay, is established. Using the measured $$ {B}_s^0 $$ B s 0 → ϕμ + μ − branching fraction and assuming a phase-space model, the absolute branching fraction of the decay B 0 → ϕμ + μ − in the full q 2 range is determined to be less than 3 . 2 × 10 − 9 at a 90% credibility level.
A millisecond pulsar in a stellar triple system
Publisher: Springer Science and Business Media LLC
Date: 2014
DOI: 10.1038/NATURE12917
Abstract: Gravitationally bound three-body systems have been studied for hundreds of years and are common in our Galaxy. They show complex orbital interactions, which can constrain the compositions, masses and interior structures of the bodies and test theories of gravity, if sufficiently precise measurements are available. A triple system containing a radio pulsar could provide such measurements, but the only previously known such system, PSR B1620-26 (refs 7, 8 with a millisecond pulsar, a white dwarf, and a planetary-mass object in an orbit of several decades), shows only weak interactions. Here we report precision timing and multiwavelength observations of PSR J0337+1715, a millisecond pulsar in a hierarchical triple system with two other stars. Strong gravitational interactions are apparent and provide the masses of the pulsar M[Symbol: see text](1.4378(13), where M[Symbol: see text]is the solar mass and the parentheses contain the uncertainty in the final decimal places) and the two white dwarf companions (0.19751(15)M[Symbol: see text] and 0.4101(3))M[Symbol: see text], as well as the inclinations of the orbits (both about 39.2°). The unexpectedly coplanar and nearly circular orbits indicate a complex and exotic evolutionary past that differs from those of known stellar systems. The gravitational field of the outer white dwarf strongly accelerates the inner binary containing the neutron star, and the system will thus provide an ideal laboratory in which to test the strong equivalence principle of general relativity.
A magnetar parallax
Publisher: Oxford University Press (OUP)
Date: 21-08-2020
Abstract: XTE J1810−197 (J1810) was the first magnetar identified to emit radio pulses, and has been extensively studied during a radio-bright phase in 2003–2008. It is estimated to be relatively nearby compared to other Galactic magnetars, and provides a useful prototype for the physics of high magnetic fields, magnetar velocities, and the plausible connection to extragalactic fast radio bursts. Upon the rebrightening of the magnetar at radio wavelengths in late 2018, we resumed an astrometric c aign on J1810 with the Very Long Baseline Array, and s led 14 new positions of J1810 over 1.3 yr. The phase calibration for the new observations was performed with two-phase calibrators that are quasi-colinear on the sky with J1810, enabling substantial improvement of the resultant astrometric precision. Combining our new observations with two archival observations from 2006, we have refined the proper motion and reference position of the magnetar and have measured its annual geometric parallax, the first such measurement for a magnetar. The parallax of 0.40 ± 0.05 mas corresponds to a most probable distance $2.5^{\\, +0.4}_{\\, -0.3}$ kpc for J1810. Our new astrometric results confirm an unremarkable transverse peculiar velocity of ≈200 $\\rm km~s^{-1}$ for J1810, which is only at the average level among the pulsar population. The magnetar proper motion vector points back to the central region of a supernova remnant (SNR) at a compatible distance at ≈70 kyr ago, but a direct association is disfavoured by the estimated SNR age of ∼3 kyr.
Nuclear Modification Factor of Neutral Pions in the Forward and Backward Regions in
p −<
Publisher: American Physical Society (APS)
Date: 24-07-2023
The low density and magnetization of a massive galaxy halo exposed by a fast radio burst
Publisher: American Association for the Advancement of Science (AAAS)
Date: 11-10-2019
Abstract: Fast radio bursts (FRBs) are millisecond flashes of radio emission from distant galaxies. It has only recently become possible to locate single bursts precisely enough to determine the host galaxy. Prochaska et al. have observed and localized a FRB using a radio interferometer. The line of sight to the host galaxy coincidentally passes through the outskirts of a closer foreground galaxy. By analyzing the propagation of the FRB, the authors put constraints on the density and magnetization of gas in the outskirts of the foreground galaxy. The technique provides complementary information to existing methods using background quasars. Science , this issue p. 231
A census of baryons in the Universe from localized fast radio bursts
Publisher: Springer Science and Business Media LLC
Date: 27-05-2020
The triggering of local AGN and their role in regulating star formation
Publisher: Oxford University Press (OUP)
Date: 08-07-2015
Evidence of a J / ψ Λ
Publisher: Elsevier BV
Date: 07-2021
Erratum: Constraining properties of neutron star merger outflows with radio observations
Publisher: Oxford University Press (OUP)
Date: 03-06-2021
Measurement of the charm mixing parameter
y C P
Publisher:
American Physical Society (APS)
Date:
25-05-2022
Publisher: American Physical Society (APS)
Date: 25-05-2022
Study of $$ {\mathrm{B}}_{\mathrm{c}}^{+} $$ decays to charmonia and three light hadrons
Publisher: Springer Science and Business Media LLC
Date: 2022
Abstract: Using proton-proton collision data, corresponding to an integrated luminosity of 9 fb − 1 collected with the LHCb detector, seven decay modes of the $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + meson into a J / ψ or ψ(2S) meson and three charged hadrons, kaons or pions, are studied. The decays $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + → (ψ(2S) → J / ψπ + π − )π + , $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + → ψ(2S)π + π − π + , $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + → J / ψK + π − π + and $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + → J / ψK + K − K + are observed for the first time, and evidence for the $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + → ψ(2S)K + K − π + , decay is found, where J / ψ and ψ(2S) mesons are reconstructed in their dimuon decay modes. The ratios of branching fractions between the different $$ {\\mathrm{B}}_{\\mathrm{c}}^{+} $$ B c + decays are reported as well as the fractions of the decays proceeding via intermediate resonances. The results largely support the factorisation approach used for a theoretical description of the studied decays.
The VLBA fast radio transient experiment: Progress and early results
Publisher: Cambridge University Press (CUP)
Date: 09-2011
DOI: 10.1017/S1743921312001299
Abstract: Motivated by recent discoveries of isolated, dispersed radio pulses of possible extragalactic origin, we are performing a commensal search for short-duration (ms) continuum radio pulses using the Very Long Baseline Array (VLBA). The geographically separated antennæ of the VLBA make the system robust to local RFI and allow events to be verified and localised on the sky with milli-arcsec accuracy. We report sky coverage and detection limits from the experiment to date.
LIMITS ON FAST RADIO BURSTS FROM FOUR YEARS OF THE V-FASTR EXPERIMENT
Publisher: American Astronomical Society
Date: 02-08-2016
Search for the radiative $$ {\Xi}_b^{-} $$ → Ξ−γ decay
Publisher: Springer Science and Business Media LLC
Date: 2022
Abstract: The first search for the rare radiative decay $$ {\\Xi}_b^{-} $$ Ξ b − → Ξ − γ is performed using data collected by the LHCb experiment in proton-proton collisions at a center-of-mass energy of 13 TeV, corresponding to an integrated luminosity of 5.4 fb − 1 . The $$ {\\Xi}_b^{-} $$ Ξ b − → Ξ − J/ψ channel is used as normalization. No $$ {\\Xi}_b^{-} $$ Ξ b − → Ξ − γ signal is found and an upper limit of $$ \\mathcal{B} $$ B ( $$ {\\Xi}_b^{-} $$ Ξ b − → Ξ − γ ) 1 . 3 × 10 − 4 at 95% confidence level is obtained.
Propagation of a fast radio burst through a birefringent relativistic plasma
Publisher: American Physical Society (APS)
Date: 14-08-2023
A wider audience: Turning VLBI into a survey instrument
Publisher: Wiley
Date: 06-2012
Abstract: Radio observations using the Very Long Baseline Interferometry (VLBI) technique typically have fields of view of only a few arcseconds, due to the computational problems inherent in imaging larger fields. Furthermore, sensitivity limitations restrict observations to very compact and bright objects, which are few and far between on the sky. Thus, while most branches of observational astronomy can carry out sensitive, wide‐field surveys, VLBI observations are limited to targeted observations of carefully selected objects. However, recent advances in technology have made it possible to carry out the computations required to target hundreds of sources simultaneously. Furthermore, sensitivity upgrades have dramatically increased the number of objects accessible to VLBI observations. The combination of these two developments have enhanced the survey capabilities of VLBI observations such that it is now possible to observe (almost) any point in the sky with milli‐arcsecond resolution. In this talk I review the development of wide‐field VLBI, which has made significant progress over the last three years (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Delayed triggering of radio active galactic nuclei in gas-rich minor mergers in the local Universe
Publisher: Oxford University Press (OUP)
Date: 05-10-2016
Very Long Baseline Astrometry of PSR J1012+5307 and its Implications on Alternative Theories of Gravity
Publisher: American Astronomical Society
Date: 16-06-2020
VLBI STRUCTURE OF PSR B1259-63/LS 2883 DURING THE 2007 AND 2010 PERIASTORN PASSAGES
Publisher: World Scientific Pub Co Pte Lt
Date: 2012
DOI: 10.1142/S2010194512004527
Abstract: PSR B1259-63 is a 48 ms pulsar in a highly eccentric 3.4-year orbit around the young massive star LS 2883. During the periastron passage the system displays transient non-thermal unpulsed emission from radio to very high energy gamma rays. We observed PSR B1259-63 with the Australian Long Baseline Array (LBA) at 2.3 GHz to trace the milliarcsecond (mas) structure of the source at three different epochs during the 2007 periastron passage. We have discovered extended and variable radio structure. The peak of the radio emission is detected at distances between 23 and 46 AU from the system assuming a distance to the system of 2.3 kpc, and the total extent of the emission is 120 AU. This is the first observational evidence that non-accreting pulsars orbiting massive stars can produce variable extended radio emission at AU scales. We also present the new LBA c aign covering five different orbital phases during the 2010–2011 periastron passage. These observations will allow us to separate the pulsed radio component from the transient extended emission.
Clumpy Star Formation and AGN Activity in the Dwarf–Dwarf Galaxy Merger Mrk 709
Publisher: American Astronomical Society
Date: 05-2021
Abstract: Nearby, low-metallicity dwarf starburst galaxies hosting active galactic nuclei (AGNs) offer the best local analogs to study the early evolution of galaxies and their supermassive black holes (BHs). Here we present a detailed multiwavelength investigation of star formation and BH activity in the low-metallicity dwarf–dwarf galaxy merger Mrk 709. Using Hubble Space Telescope H α and continuum imaging combined with Keck spectroscopy, we determine that the two dwarf galaxies are likely in the early stages of a merger (i.e., their first pass) and discover a spectacular ∼10 kpc long string of young massive star clusters ( t ≲ 10 Myr M ⋆ ≳ 10 5 M ⊙ ) between the galaxies triggered by the interaction. We find that the southern galaxy, Mrk 709 S, is undergoing a clumpy mode of star formation resembling that seen in high-redshift galaxies, with multiple young clusters/clumps having stellar masses between 10 7 and 10 8 M ⊙ . Furthermore, we present additional evidence for a low-luminosity AGN in Mrk 709 S (first identified by Reines et al. using radio and X-ray observations), including the detection of the coronal [Fe x ] optical emission line. The work presented here provides a unique glimpse into processes key to hierarchical galaxy formation and BH growth in the early universe.
Simultaneous Chandra and VLA Observations of the Transitional Millisecond Pulsar PSR J1023+0038: Anti-correlated X-Ray and Radio Variability
Publisher: American Astronomical Society
Date: 23-03-2018
Micro-arcsecond structure of Sagittarius A∗ revealed by high-sensitivity 86 GHz VLBI observations
Publisher: EDP Sciences
Date: 2019
DOI: 10.1051/0004-6361/201834148
Abstract: Context . The compact radio source Sagittarius A ∗ (Sgr A ∗ ) in the Galactic centre is the primary supermassive black hole candidate. General relativistic magnetohydrodynamical (GRMHD) simulations of the accretion flow around Sgr A ∗ predict the presence of sub-structure at observing wavelengths of ∼3 mm and below (frequencies of 86 GHz and above). For very long baseline interferometry (VLBI) observations of Sgr A ∗ at this frequency the blurring effect of interstellar scattering becomes sub-dominant, and arrays such as the high sensitivity array (HSA) and the global mm-VLBI array (GMVA) are now capable of resolving potential sub-structure in the source. Such investigations help to improve our understanding of the emission geometry of the mm-wave emission of Sgr A ∗ , which is crucial for constraining theoretical models and for providing a background to interpret 1 mm VLBI data from the Event Horizon Telescope (EHT). Aims . Following the closure phase analysis in our first paper, which indicates asymmetry in the 3 mm emission of Sgr A ∗ , here we have used the full visibility information to check for possible sub-structure. We extracted source size information from closure litude analysis, and investigate how this constrains a combined fit of the size-frequency relation and the scattering law for Sgr A ∗ . Methods . We performed high-sensitivity VLBI observations of Sgr A ∗ at 3 mm using the Very Long Baseline Array (VLBA) and the Large Millimeter Telescope (LMT) in Mexico on two consecutive days in May 2015, with the second epoch including the Greenbank Telescope (GBT). Results . We confirm the asymmetry for the experiment including GBT. Modelling the emission with an elliptical Gaussian results in significant residual flux of ∼10 mJy in south-eastern direction. The analysis of closure litudes allows us to precisely constrain the major and minor axis size of the main emission component. We discuss systematic effects which need to be taken into account. We consider our results in the context of the existing body of size measurements over a range of observing frequencies and investigate how well-constrained the size-frequency relation is by performing a simultaneous fit to the scattering law and the size-frequency relation. Conclusions . We find an overall source geometry that matches previous findings very closely, showing a deviation in fitted model parameters less than 3% over a time scale of weeks and suggesting a highly stable global source geometry over time. The reported sub-structure in the 3 mm emission of Sgr A ∗ is consistent with theoretical expectations of refractive noise on long baselines. However, comparing our findings with recent results from 1 mm and 7 mm VLBI observations, which also show evidence for east-west asymmetry, we cannot exclude an intrinsic origin. Confirmation of persistent intrinsic substructure will require further VLBI observations spread out over multiple epochs.
Study of
Z
Publisher: American Physical Society (APS)
Date: 24-02-2022
Rotational and radio emission properties of PSR J0738−4042 over half a century
Publisher: Oxford University Press (OUP)
Date: 27-07-2023
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.
Analysis of Neutral
B
Publisher: American Physical Society (APS)
Date: 25-01-2022
Host Galaxy Properties and Offset Distributions of Fast Radio Bursts: Implications for Their Progenitors
Publisher: American Astronomical Society
Date: 12-11-2020
The Bow Shock and Kinematics of PSR J1959+2048
Publisher: American Astronomical Society
Date: 05-2022
Abstract: Pulsar H α bow shocks provide rare opportunities to constrain the energetics and kinematics of the relativistic pulsar wind. We have acquired optical imaging and integral field unit spectroscopy of the bow shock of the millisecond pulsar PSR J1959+2048, measuring the shock symmetry axis at a position angle = 213.2 ± 0.°2 and showing that this slow nonradiative shock has a broad-to-narrow line component ratio I b / I n = 4. The data show that the pulsar’s velocity lies 2.°2 out of the plane of the sky. Coupled with a new fit for its timing proper motion, giving μ tot = 30.05 mas yr −1 and a Very Long Baseline Array (VLBA) interferometric parallax measurement giving d = 2.57 − 0.77 + 1.84 kpc (90% range), we have unusually complete information on the pulsar kinematics. The bow shock constraints on the wind momentum flux imply that, at the best-fit parallax distance, the pulsar moment of inertia must be very large and/or the H α efficiency at its modest shock velocity must be very high.
Performance of Oversampled Polyphase Filterbank Inversion via Fourier Transform
Publisher: World Scientific Pub Co Pte Ltd
Date: 26-02-2020
DOI: 10.1142/S225117172050004X
Abstract: Frequency channelization is a fundamental signal processing operation employed across various domains, including communications and radio astronomy. The polyphase filterbank (PFB) represents an efficient and versatile means of channelization. When strict constraints are placed on the allowable spectral leakage between neighboring channels, an overs led PFB design is advantageous. A helpful consequence of the overs ling is that inversion of the PFB to recover high temporal resolution is simplified and can be accomplished accurately using Fourier transforms. We describe this inversion approach and identify key design considerations. We examine the residual error and spectral/temporal leakage behavior when a channelizer and its corresponding inverter are cascaded, concluding that near-perfect reconstruction can be approached with appropriate selection of PFB and inverter design parameters.
A framework for interpreting fast radio transients search experiments: Application to the V-FASTR experiment
Publisher: American Astronomical Society
Date: 19-03-2013
Search for CP violation in $$ {D}_{(s)}^{+}\to {h}^{+}{\pi}^0 $$ and $$ {D}_{(s)}^{+}\to {h}^{+}\eta $$ decays
Publisher: Springer Science and Business Media LLC
Date: 06-2021
Abstract: Searches for CP violation in the two-body decays $$ {D}_{(s)}^{+}\\to {h}^{+}{\\pi}^0 $$ D s + → h + π 0 and $$ {D}_{(s)}^{+}\\to {h}^{+}\\eta $$ D s + → h + η (where h + denotes a π + or K + meson) are performed using pp collision data collected by the LHCb experiment corresponding to either 9 fb − 1 or 6 fb − 1 of integrated luminosity. The π 0 and η mesons are reconstructed using the e + e − γ final state, which can proceed as three-body decays π 0 → e + e − γ and η → e + e − γ , or via the two-body decays π 0 → γγ and η → γγ followed by a photon conversion. The measurements are made relative to the control modes $$ {D}_{(s)}^{+}\\to {K}_{\\mathrm{S}}^0{h}^{+} $$ D s + → K S 0 h + to cancel the production and detection asymmetries. The CP asymmetries are measured to be $$ {\\displaystyle \\begin{array}{c}{\\mathcal{A}}_{CP}\\left({D}^{+}\\to {\\pi}^{+}{\\pi}^0\\right)=\\left(-1.3\\pm 0.9\\pm 0.6\\right)\\%,\\\\ {}{\\mathcal{A}}_{CP}\\left({D}^{+}\\to {K}^{+}{\\pi}^0\\right)=\\left(-3.2\\pm 4.7\\pm 2.1\\right)\\%,\\\\ {}\\begin{array}{c}{\\mathcal{A}}_{CP}\\left({D}^{+}\\to {\\pi}^{+}\\eta \\right)=\\left(-0.2\\pm 0.8\\pm 0.4\\right)\\%,\\\\ {}{\\mathcal{A}}_{CP}\\left({D}^{+}\\to {K}^{+}\\eta \\right)=\\left(-6\\pm 10\\pm 4\\right)\\%,\\\\ {}\\begin{array}{c}{\\mathcal{A}}_{CP}\\left({D}_s^{+}\\to {K}^{+}{\\pi}^0\\right)=\\left(-0.8\\pm 3.9\\pm 1.2\\right)\\%,\\\\ {}\\begin{array}{c}{\\mathcal{A}}_{CP}\\left({D}_s^{+}\\to {\\pi}^{+}\\eta \\right)=\\left(0.8\\pm 0.7\\pm 0.5\\right)\\%,\\\\ {}{\\mathcal{A}}_{CP}\\left({D}_s^{+}\\to {K}^{+}\\eta \\right)=\\left(0.9\\pm 3.7\\pm 1.1\\right)\\%,\\end{array}\\end{array}\\end{array}\\end{array}} $$ A CP D + → π + π 0 = − 1.3 ± 0.9 ± 0.6 % , A CP D + → K + π 0 = − 3.2 ± 4.7 ± 2.1 % , A CP D + → π + η = − 0.2 ± 0.8 ± 0.4 % , A CP D + → K + η = − 6 ± 10 ± 4 % , A CP D s + → K + π 0 = − 0.8 ± 3.9 ± 1.2 % , A CP D s + → π + η = 0.8 ± 0.7 ± 0.5 % , A CP D s + → K + η = 0.9 ± 3.7 ± 1.1 % , where the first uncertainties are statistical and the second systematic. These results are consistent with no CP violation and mostly constitute the most precise measurements of $$ {\\mathcal{A}}_{CP} $$ A CP in these decay modes to date.
mJIVE-20: A SURVEY FOR COMPACT mJy RADIO OBJECTS WITH THE VERY LONG BASELINE ARRAY
Publisher: American Astronomical Society
Date: 06-12-2013
Fast Radio Bursts as Probes of Magnetic Fields in Galaxies at z < 0.5
Publisher: American Astronomical Society
Date: 09-2023
Angular analysis of the rare decay $$ {B}_s^0 $$ → ϕμ+μ−
Publisher: Springer Science and Business Media LLC
Date: 11-2021
Abstract: An angular analysis of the rare decay $$ {B}_s^0 $$ B s 0 → ϕμ + μ − is presented, using proton-proton collision data collected by the LHCb experiment at centre-of-mass energies of 7, 8 and 13 TeV, corresponding to an integrated luminosity of 8.4 fb − 1 . The observables describing the angular distributions of the decay $$ {B}_s^0 $$ B s 0 → ϕμ + μ − are determined in regions of q 2 , the square of the dimuon invariant mass. The results are consistent with Standard Model predictions.
Detection of a Glitch in the Pulsar J1709−4429
Publisher: American Astronomical Society
Date: 07-08-2018
A Search for Bursts from FRB 191228 in Breakthrough Listen Archival Data
Publisher: American Astronomical Society
Date: 07-2020
Observation of a Resonant Structure near the
D s +
Publisher:
American Physical Society (APS)
Date:
14-08-2023
Publisher: American Physical Society (APS)
Date: 14-08-2023
Constraints on Weak Supernova Kicks from Observed Pulsar Velocities
Publisher: American Astronomical Society
Date: 10-2021
A luminous fast radio burst that probes the Universe at redshift 1
Publisher: American Association for the Advancement of Science (AAAS)
Date: 20-10-2023
GRAIN GROWTH IN THE CIRCUMSTELLAR DISKS OF THE YOUNG STARS CY Tau AND DoAr 25
Publisher: American Astronomical Society
Date: 27-10-2015
Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks
Publisher: EDP Sciences
Date: 17-03-2016
Computational Intelligence in Radio Astronomy: Using Computational Intelligence Techniques to Tune Geodesy Models
Publisher: Springer Berlin Heidelberg
Date: 2008
Wide-band, low-frequency pulse profiles of 100 radio pulsars with LOFAR
Publisher: EDP Sciences
Date: 29-01-2016
A PARALLAX DISTANCE AND MASS ESTIMATE FOR THE TRANSITIONAL MILLISECOND PULSAR SYSTEM J1023+0038
Publisher: American Astronomical Society
Date: 17-08-2012
The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Publisher: American Astronomical Society
Date: 24-08-2023
Abstract: We present a comprehensive catalog of observations and stellar population properties for 23 highly secure host galaxies of fast radio bursts (FRBs). Our s le comprises 6 repeating FRBs and 17 apparent nonrepeaters. We present 82 new photometric and 8 new spectroscopic observations of these hosts. Using stellar population synthesis modeling and employing nonparametric star formation histories (SFHs), we find that FRB hosts have a median stellar mass of ≈10 9.9 M ⊙ , mass-weighted age ≈5.1 Gyr, and ongoing star formation rate ≈1.3 M ⊙ yr −1 but span wide ranges in all properties. Classifying the hosts by degree of star formation, we find that 87% (20 of 23 hosts) are star-forming, two are transitioning, and one is quiescent. The majority trace the star-forming main sequence of galaxies, but at least three FRBs in our s le originate in less-active environments (two nonrepeaters and one repeater). Across all modeled properties, we find no statistically significant distinction between the hosts of repeaters and nonrepeaters. However, the hosts of repeating FRBs generally extend to lower stellar masses, and the hosts of nonrepeaters arise in more optically luminous galaxies. While four of the galaxies with the clearest and most prolonged rises in their SFHs all host repeating FRBs, demonstrating heightened star formation activity in the last ≲100 Myr, one nonrepeating host shows this SFH as well. Our results support progenitor models with short delay channels (i.e., magnetars formed via core-collapse supernova) for most FRBs, but the presence of some FRBs in less-active environments suggests a fraction form through more delayed channels.
THE PROPER MOTION OF THE GALACTIC CENTER PULSAR RELATIVE TO SAGITTARIUS A*
Publisher: American Astronomical Society
Date: 08-01-2015
VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. VII. MONOCEROS R2
Publisher: American Astronomical Society
Date: 08-2016
Evolution of the low-frequency pulse profile of PSR B2217+47
Publisher: Cambridge University Press (CUP)
Date: 09-2017
DOI: 10.1017/S1743921317010006
Abstract: An evolution of the low-frequency pulse profile of PSR B2217+47 is observed during a six-year observing c aign with the LOFAR telescope at 150 MHz. The evolution is manifested as a new component in the profile trailing the main peak. The leading part of the profile, including a newly-observed weak component, is steady during the c aign. The transient component is not visible in simultaneous observations at 1500 MHz using the Lovell telescope, implying a chromatic effect. A variation in the dispersion measure of the source is detected in the same timespan. Precession of the pulsar and changes in the magnetosphere are investigated to explain the profile evolution. However, the listed properties favour a model based on turbulence in the interstellar medium (ISM). This interpretation is confirmed by a strong correlation between the intensity of the transient component and main peak in single pulses. Since PSR B2217+47 is the fourth brightest pulsar visible to LOFAR, we speculate that ISM-induced pulse profile evolution might be relatively common but subtle and that SKA-Low will detect many similar ex les. In this scenario, similar studies of pulse profile evolution could be used in parallel with scintillation arcs to characterize the properties of the ISM.
Angular Analysis of the
B + →
Publisher:
American Physical Society (APS)
Date:
22-04-2021
Publisher: American Physical Society (APS)
Date: 22-04-2021
Study of charmonium and charmonium-like contributions in B+ → J/ψηK+ decays
Publisher: Springer Science and Business Media LLC
Date: 08-04-2022
Abstract: A study of B + → J / ψηK + decays, followed by J / ψ → μ + μ − and η → γγ, is performed using a dataset collected with the LHCb detector in proton-proton collisions at centre-of-mass energies of 7, 8 and 13 TeV, corresponding to an integrated luminosity of 9 fb − 1 . The J / ψη mass spectrum is investigated for contributions from charmonia and charmonium-like states. Evidence is found for the B + → (ψ 2 (3823) → J / ψη)K + and B + → (ψ(4040) → J / ψη)K + decays with significance of 3.4 and 4.7 standard deviations, respectively. This constitutes the first evidence for the ψ 2 (3823) → J / ψη decay.
The LOFAR Two-metre Sky Survey
Publisher: EDP Sciences
Date: 02-2017
Wide-field observations in the SDSS Stripe 82 with the European VLBI Network
Publisher: Cambridge University Press (CUP)
Date: 10-2013
DOI: 10.1017/S174392131400386X
Abstract: We observed an area of sky located within the SDSS Stripe 82 field at 1.6 GHz with the European VLBI Network (EVN). There are fifteen mJy/sub-mJy radio sources within the primary beam of a typical 30-m class EVN radio telescope. Our aim was to obtain information on compact radio structures of all VLBI-detectable sources within this primary beam area. The source of particular interest is the recently identified radio quasar J222843.54+011032.2 (J2228+0110) at z = 5.95. The data correlation was performed at the EVN software correlator at JIVE (SFXC). Three targets (J2228+0110, J222851.45+011203.4, J222941.76+011428.5) were detected, all three with position offsets not exceeding the 3σ accuracy of the original low-resolution radio surveys. The detection rate of 20% is consistent with other wide-field VLBI experiments carried out recently (e.g. Middelberg et al . 2013). The project presented here demonstrates the ability of EVN in multiple-phase-centre experiments and paves the way for future large-scale EVN surveys of compact structures in extragalactic radio sources using the multiple-phase-centre VLBI technique.
The faint radio sky: VLBA observations of the COSMOS field
Publisher: EDP Sciences
Date: 11-2017
Nowhere to Hide: Radio-faint AGN in GOODS-N field: I. Initial catalogue and radio properties
Publisher: EDP Sciences
Date: 11-2018
DOI: 10.1051/0004-6361/201833399
Abstract: Context . The occurrence of active galactic nuclei (AGN) is critical to our understanding of galaxy evolution and formation. Radio observations provide a crucial, dust-independent tool to study the role of AGN. However, conventional radio surveys of deep fields ordinarily have arc-second scale resolutions often insufficient to reliably separate radio emission in distant galaxies originating from star-formation and AGN-related activity. Very long baseline interferometry (VLBI) can offer a solution by identifying only the most compact radio emitting regions in galaxies at cosmological distances where the high brightness temperatures (in excess of 10 5 K) can only be reliably attributed to AGN activity. Aims . We present the first in a series of papers exploring the faint compact radio population using a new wide-field VLBI survey of the GOODS-N field. This will expand upon previous surveys, permitting the characterisation of the faint, compact radio source population in the GOODS-N field. The unparalleled sensitivity of the European VLBI Network (EVN) will probe a luminosity range rarely seen in deep wide-field VLBI observations, thus providing insights into the role of AGN to radio luminosities of the order 10 22 WHz −1 across cosmic time. Methods . The newest VLBI techniques are used to completely cover an entire 7′̣5 radius area to milliarcsecond resolutions, while bright radio sources ( S 0.1 mJy) are targeted up to 25′ from the pointing centre. Multi-source self-calibration, and a primary beam model for the EVN array are used to correct for residual phase errors and primary beam attenuation respectively. Results . This paper presents the largest catalogue of VLBI detected sources in GOODS-N comprising of 31 compact radio sources across a redshift range of 0.11–3.44, almost three times more than previous VLBI surveys in this field. We provide a machine-readable catalogue and introduce the radio properties of the detected sources using complementary data from the e-MERLIN Galaxy Evolution survey (eMERGE).
Geodetic VLBI correlation in software
Publisher: Springer Science and Business Media LLC
Date: 10-06-2009
The radio/X-ray correlation in Swift J1753.5-0127
Publisher: Wiley
Date: 05-2016
Abstract: Great effort has gone into trying to explain the two observed radio/X‐ray correlation tracks seen in the low/hard state of black hole X‐ray binaries in recent years. The original, “standard” correlation of the form L R ∝ L b X , where b = 0.7 ± 0.1, is paired with a separate, lower correlation track with a steeper slope of ∼ 1–1.4, at least at high luminosities. These outlier sources seem to show fainter radio emission than expected for a given X‐ray luminosity, thus acquiring the term “radio‐quiet”. While most sources seem to maintain their intrinsic correlation slopes over decades in luminosity, a growing s le of sources have recently been reported to move from one correlation to the other. We present preliminary results from a coordinated radio/X‐ray monitoring c aign of the radio‐quiet black hole binary Swift J1753.5–0127, spanning nearly two years in time. Our observations add lower‐luminosity coverage to an existing s le of observations, and we observe the radio‐quiet track to proceed horizontally towards the standard correlation as the X‐ray luminosity slowly starts to decrease. The source stays on the transition track for ∼ 60 days, during which its X‐ray luminosity is observed to drop by more than an order of magnitude while its radio luminosity stays constant. Time‐averaged X‐ray energy spectra show very little change during this phase, leaving no obvious parameters to explain the observed transition behaviour. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Precise determination of the $$B_{\mathrm{s}}^0$$–$$\overline B_{\mathrm{s}}^0$$ oscillation frequency
Publisher: Springer Science and Business Media LLC
Date: 2022
DOI: 10.1038/S41567-021-01394-X
Abstract: Mesons comprising a beauty quark and strange quark can oscillate between particle ( $${B}_{\\mathrm{s}}^{0}$$ B s 0 ) and antiparticle ( $${\\overline{B}}_{\\mathrm{s}}^{0}$$ B ¯ s 0 ) flavour eigenstates, with a frequency given by the mass difference between heavy and light mass eigenstates, Δ m s . Here we present a measurement of Δ m s using $${B}_{\\mathrm{s}}^{0}\\to {D}_{\\mathrm{s}}^{-}$$ B s 0 → D s − π + decays produced in proton–proton collisions collected with the LHCb detector at the Large Hadron Collider. The oscillation frequency is found to be Δ m s = 17.7683 ± 0.0051 ± 0.0032 ps −1 , where the first uncertainty is statistical and the second is systematic. This measurement improves on the current Δ m s precision by a factor of two. We combine this result with previous LHCb measurements to determine Δ m s = 17.7656 ± 0.0057 ps −1 , which is the legacy measurement of the original LHCb detector.
Measurement of J/ψ production cross-sections in pp collisions at $$ \sqrt{s} $$ = 5 TeV
Publisher: Springer Science and Business Media LLC
Date: 11-2021
Abstract: The production cross-sections of J/ψ mesons in proton-proton collisions at a centre-of-mass energy of $$ \\sqrt{s} $$ s = 5 TeV are measured using a data s le corresponding to an integrated luminosity of 9 . 13 ± 0 . 18 pb − 1 , collected by the LHCb experiment. The cross-sections are measured differentially as a function of transverse momentum, p T , and rapidity, y , and separately for J/ψ mesons produced promptly and from beauty hadron decays (nonprompt). With the assumption of unpolarised J/ψ mesons, the production cross-sections integrated over the kinematic range 0 p T 20 GeV/ c and 2 . 0 y 4 . 5 are $$ {\\displaystyle \\begin{array}{c}{\\sigma}_{\\mathrm{prompt}}\\ J/\\psi =8.154\\pm 0.010\\pm 0.283\\ \\upmu \\mathrm{b},\\\\ {}{\\sigma}_{\\mathrm{nonprompt}}\\ J/\\psi =0.820\\pm 0.003\\pm 0.034\\ \\upmu \\mathrm{b},\\end{array}} $$ σ prompt J / ψ = 8.154 ± 0.010 ± 0.283 μb , σ nonprompt J / ψ = 0.820 ± 0.003 ± 0.034 μb , where the first uncertainties are statistical and the second systematic. These cross-sections are compared with those at $$ \\sqrt{s} $$ s = 8 TeV and 13 TeV, and are used to update the measurement of the nuclear modification factor in proton-lead collisions for J/ψ mesons at a centre-of-mass energy per nucleon pair of $$ \\sqrt{s_{\\mathrm{NN}}} $$ s NN = 5 TeV. The results are compared with theoretical predictions.
Jet quenching in the neutron star low-mass X-ray binary 1RXS J180408.9-342058
Publisher: Oxford University Press (OUP)
Date: 19-05-2017
The UTMOST survey for magnetars, intermittent pulsars, RRATs, and FRBs – I. System description and overview
Publisher: Oxford University Press (OUP)
Date: 15-01-2020
Abstract: We describe the ongoing ‘survey for magnetars, intermittent pulsars, rotating radio transients, and fast radio bursts’ (SMIRF), performed using the newly refurbished UTMOST telescope. SMIRF repeatedly sweeps the southern Galactic plane performing real-time periodicity and single pulse searches, and is the first survey of its kind carried out with an interferometer. SMIRF is facilitated by a robotic scheduler which is capable of fully autonomous commensal operations. We report on the SMIRF observational parameters, the data analysis methods, the survey’s sensitivity to pulsars, techniques to mitigate radio frequency interference, and present some early survey results. UTMOST’s wide field of view permits a full sweep of the Galactic plane to be performed every fortnight, two orders of magnitude faster than previous surveys. In six months of operations from 2018 January to June, we have performed ∼10 sweeps of the Galactic plane with SMIRF. Notable blind redetections include the magnetar PSR J1622−4950, the RRAT PSR J0941−3942 and the eclipsing pulsar PSR J1748−2446A. We also report the discovery of a new pulsar, PSR J1659−54. Our follow-up of this pulsar at an average flux limit of ≤20 mJy, categorizes this as an intermittent pulsar with a high nulling fraction of & .002.
Detection of compact radio emission from Circinus X-1 with the first Southern hemisphere e-VLBI experiment
Publisher: Oxford University Press (OUP)
Date: 09-2007
RADIOASTRONSTUDIES OF THE NEARBY, TURBULENT INTERSTELLAR PLASMA WITH THE LONGEST SPACE-GROUND INTERFEROMETER BASELINE
Publisher: American Astronomical Society
Date: 24-04-2014
The unseen host galaxy and high dispersion measure of a precisely localized fast radio burst suggests a high-redshift origin
Publisher: Oxford University Press (OUP)
Date: 04-08-2023
Abstract: FRB 20210912A is a fast radio burst (FRB), detected and localized to subarcsecond precision by the Australian Square Kilometre Array Pathfinder. No host galaxy has been identified for this burst despite the high precision of its localization and deep optical and infrared follow-up, to 5σ limits of R = 26.7 mag and Ks = 24.9 mag with the Very Large Telescope. The combination of precise radio localization and deep optical imaging has almost always resulted in the secure identification of a host galaxy, and this is the first case in which the line of sight is not obscured by the Galactic disc. The dispersion measure of this burst, DMFRB = 1233.696 ± 0.006 pc cm−3, allows for a large source redshift of z & 1 according to the Macquart relation. It could thus be that the host galaxy is consistent with the known population of FRB hosts, but is too distant to detect in our observations (z & 0.7 for a host like that of the first repeating FRB source, FRB 20121102A) that it is more nearby with a significant excess in DMhost, and thus dimmer than any known FRB host or, least likely, that the FRB is truly hostless. We consider each possibility, making use of the population of known FRB hosts to frame each scenario. The fact of the missing host has ramifications for the FRB field: even with high-precision localization and deep follow-up, some FRB hosts may be difficult to detect, with more distant hosts being the less likely to be found. This has implications for FRB cosmology, in which high-redshift detections are valuable.
Precision Southern Hemisphere pulsar vlbi astrometry: Techniques and results for PSR J1559-4438
Publisher: American Astronomical Society
Date: 12-2009
Tests of Lepton Universality Using
B 0 →
Publisher:
American Physical Society (APS)
Date:
11-05-2022
Publisher: American Physical Society (APS)
Date: 11-05-2022
Measurement of the
B s 0
Publisher: American Physical Society (APS)
Date: 25-01-2022
Five new real-time detections of fast radio bursts with UTMOST
Publisher: Oxford University Press (OUP)
Date: 04-07-2019
Abstract: We detail a new fast radio burst (FRB) survey with the Molonglo Radio Telescope, in which six FRBs were detected between 2017 June and 2018 December. By using a real-time FRB detection system, we captured raw voltages for five of the six events, which allowed for coherent dedispersion and very high time resolution (10.24 $\\mu$s) studies of the bursts. Five of the FRBs show temporal broadening consistent with interstellar and/or intergalactic scattering, with scattering time-scales ranging from 0.16 to 29.1 ms. One burst, FRB181017, shows remarkable temporal structure, with three peaks each separated by 1 ms. We searched for phase-coherence between the leading and trailing peaks and found none, ruling out lensing scenarios. Based on this survey, we calculate an all-sky rate at 843 MHz of $98^{+59}_{-39}$ events sky−1 d−1 to a fluence limit of 8 Jy ms: a factor of 7 below the rates estimated from the Parkes and ASKAP telescopes at 1.4 GHz assuming the ASKAP-derived spectral index α = −1.6 (Fν ∝ να). Our results suggest that FRB spectra may turn over below 1 GHz. Optical, radio, and X-ray follow-up has been made for most of the reported bursts, with no associated transients found. No repeat bursts were found in the survey.
The Orbital-decay Test of General Relativity to the 2% Level with 6 yr VLBA Astrometry of the Double Neutron Star PSR J1537+1155
Publisher: American Astronomical Society
Date: 11-2021
Observation of the $$ {B}_s^0 $$ → D*+D*− decay
Publisher: Springer Science and Business Media LLC
Date: 13-07-2023
Abstract: The first observation of the $$ {B}_s^0 $$ B s 0 → D ∗+ D ∗ − decay and the measurement of its branching ratio relative to the B 0 → D ∗+ D ∗ − decay are presented. The data s le used corresponds to an integrated luminosity of 9 fb − 1 of proton-proton collisions recorded by the LHCb experiment at centre-of-mass energies of 7, 8 and 13 TeV between 2011 and 2018. The decay is observed with more than 10 standard deviations and the time-integrated ratio of branching fractions is determined to be $$ \\frac{\\mathcal{B}\\left({B}_s^0\\to {D}^{\\ast +}{D}^{\\ast -}\\right)}{\\mathcal{B}\\left({B}^0\\to {D}^{\\ast +}{D}^{\\ast -}\\right)}=0.269\\pm 0.032\\pm 0.011\\pm 0.008, $$ B B s 0 → D ∗ + D ∗ − B B 0 → D ∗ + D ∗ − = 0.269 ± 0.032 ± 0.011 ± 0.008 , where the first uncertainty is statistical, the second systematic and the third due to the uncertainty of the fragmentation fraction ratio f s /f d . The $$ {B}_s^0 $$ B s 0 → D *+ D * − branching fraction is calculated to be $$ \\mathcal{B}\\left({B}_s^0\\to {D}^{\\ast +}{D}^{\\ast -}\\right)=\\left(2.15\\pm 0.26\\pm 0.09\\pm 0.06\\pm 0.16\\right)\\times {10}^{-4}, $$ B B s 0 → D ∗ + D ∗ − = 2.15 ± 0.26 ± 0.09 ± 0.06 ± 0.16 × 10 − 4 , where the fourth uncertainty is due to the B 0 → D * + D *− branching fraction. These results are calculated using the average $$ {B}_s^0 $$ B s 0 meson lifetime in simulation. Correction factors are reported for scenarios where either a purely heavy or a purely light $$ {B}_s^0 $$ B s 0 eigenstate is considered.
Mosaiced wide-field VLBI observations of the Lockman Hole/XMM
Publisher: EDP Sciences
Date: 03-2013
Chronicling the Host Galaxy Properties of the Remarkable Repeating FRB 20201124A
Publisher: American Astronomical Society
Date: 30-09-2021
Extremely band-limited repetition from a fast radio burst source
Publisher: Oxford University Press (OUP)
Date: 05-11-2020
Abstract: The fast radio burst (FRB) population is observationally ided into sources that have been observed to repeat and those that have not. There is tentative evidence that the bursts from repeating sources have different properties than the non-repeating ones. In order to determine the occurrence rate of repeating sources and characterize the nature of repeat emission, we have been conducting sensitive searches for repetitions from bursts detected with the Australian Square Kilometre Array Pathfinder (ASKAP) with the 64-m Parkes radio telescope, using the recently commissioned Ultra-wideband Low (UWL) receiver system, over a band spanning 0.7–4.0 GHz. We report the detection of a repeat burst from the source of FRB 20190711A. The detected burst is 1 ms wide and has a bandwidth of just 65 MHz. We find no evidence of any emission in the remaining part of the 3.3 GHz UWL band. While the emission bandwidths of the ASKAP and UWL bursts show ν−4 scaling consistent with a propagation effect, the spectral occupancy is inconsistent with diffractive scintillation. This detection rules out models predicting broad-band emission from the FRB 20190711A source and puts stringent constraints on the emission mechanism. The low spectral occupancy highlights the importance of sub-banded search methods in detecting FRBs.
Potential cooling of an accretion-heated neutron star crust in the low-mass X-ray binary 1RXS J180408.9−342058
Publisher: Oxford University Press (OUP)
Date: 07-01-2017
A 1.05M☉COMPANION TO PSR J2222–0137: THE COOLEST KNOWN WHITE DWARF?
Publisher: American Astronomical Society
Date: 20-06-2014
Spiral density waves in a young protoplanetary disk
Publisher: American Association for the Advancement of Science (AAAS)
Date: 30-09-2016
Abstract: Gravitational forces are expected to excite spiral density waves in protoplanetary disks, disks of gas and dust orbiting young stars. However, previous observations that showed spiral structure were not able to probe disk midplanes, where most of the mass is concentrated and where planet formation takes place. Using the Atacama Large Millimeter/submillimeter Array, we detected a pair of trailing symmetric spiral arms in the protoplanetary disk surrounding the young star Elias 2-27. The arms extend to the disk outer regions and can be traced down to the midplane. These millimeter-wave observations also reveal an emission gap closer to the star than the spiral arms. We argue that the observed spirals trace shocks of spiral density waves in the midplane of this young disk.
A High-resolution View of Fast Radio Burst Host Environments
Publisher: American Astronomical Society
Date: 08-2021
The MSPSRπ catalogue: VLBA astrometry of 18 millisecond pulsars
Publisher: Oxford University Press (OUP)
Date: 20-12-2022
Abstract: With unparalleled rotational stability, millisecond pulsars (MSPs) serve as ideal laboratories for numerous astrophysical studies, many of which require precise knowledge of the distance and/or velocity of the MSP. Here, we present the astrometric results for 18 MSPs of the ‘MSPSR$\\pi$’ project focusing exclusively on astrometry of MSPs, which includes the re-analysis of three previously published sources. On top of a standardized data reduction protocol, more complex strategies (i.e. normal and inverse-referenced 1D interpolation) were employed where possible to further improve astrometric precision. We derived astrometric parameters using sterne, a new Bayesian astrometry inference package that allows the incorporation of prior information based on pulsar timing where applicable. We measured significant (${& }3\\, \\sigma$) parallax-based distances for 15 MSPs, including 0.81 ± 0.02 kpc for PSR J1518+4904 – the most significant model-independent distance ever measured for a double neutron star system. For each MSP with a well-constrained distance, we estimated its transverse space velocity and radial acceleration. Among the estimated radial accelerations, the updated ones of PSR J1012+5307 and PSR J1738+0333 impose new constraints on dipole gravitational radiation and the time derivative of Newton’s gravitational constant. Additionally, significant angular broadening was detected for PSR J1643−1224, which offers an independent check of the postulated association between the HII region Sh 2-27 and the main scattering screen of PSR J1643−1224. Finally, the upper limit of the death line of γ-ray-emitting pulsars is refined with the new radial acceleration of the hitherto least energetic γ-ray pulsar PSR J1730−2304.
A study of $$C\!P$$ violation in the decays $${{B} ^\pm } \rightarrow [{{K} ^+} {{K} ^-} {{\uppi } ^+} {{\uppi } ^-} ]_{D} h^{\pm }$$ ($$h = K, \pi $$) and $${{B} ^\pm } \rightarrow [{{\uppi } ^+} {{\
Publisher: Springer Science and Business Media LLC
Date: 29-06-2023
DOI: 10.1140/EPJC/S10052-023-11560-5
Abstract: The first study of $$C\\!P$$ C P violation in the decay mode $${{B} ^\\pm } \\rightarrow [{{K} ^+} {{K} ^-} {{\\uppi } ^+} {{\\uppi } ^-} ]_{D} h^\\pm $$ B ± → [ K + K - π + π - ] D h ± , with $$h=K,\\pi $$ h = K , π , is presented, exploiting a data s le of proton–proton collisions collected by the LHCb experiment that corresponds to an integrated luminosity of $$9\\text {\\,fb} ^{-1} $$ 9 \\,fb - 1 . The analysis is performed in bins of phase space, which are optimised for sensitivity to local $$C\\!P$$ C P asymmetries. $$C\\!P$$ C P -violating observables that are sensitive to the angle $$\\gamma $$ γ of the Unitarity Triangle are determined. The analysis requires external information on charm-decay parameters, which are currently taken from an litude analysis of LHCb data, but can be updated in the future when direct measurements become available. Measurements are also performed of phase-space integrated observables for $${{B} ^\\pm } \\rightarrow [{{K} ^+} {{K} ^-} {{\\uppi } ^+} {{\\uppi } ^-} ]_{D} h^\\pm $$ B ± → [ K + K - π + π - ] D h ± and $${{B} ^\\pm } \\rightarrow [{{\\uppi } ^+} {{\\uppi } ^-} {{\\uppi } ^+} {{\\uppi } ^-} ]_{D} h^\\pm $$ B ± → [ π + π - π + π - ] D h ± decays.
DiFX: A software correlator for very long baseline interferometry using multiprocessor computing environments
Publisher: IOP Publishing
Date: 03-2007
DOI: 10.1086/513572
New Discoveries from the GBT 350-MHz Drift-Scan Survey
Publisher: AIP
Date: 2011
DOI: 10.1063/1.3615070
The Radio Parallax of the Crab Pulsar: A First VLBI Measurement Calibrated with Giant Pulses
Publisher: American Astronomical Society
Date: 27-07-2023
Abstract: We use four observations with the European very long baseline interferometry (VLBI) network to measure the first precise radio parallax of the Crab Pulsar. We found two in-beam extragalactic sources just outside the Crab Nebula, with one bright enough to use as a background reference source in our data. We use the Crab Pulsar’s giant pulses to determine fringe and bandpass calibration solutions, which greatly improved the sensitivity and reliability of our images and allowed us to determine precise positional offsets between the pulsar and the background source. From those offsets, we determine a parallax of π = 0.53 ± 0.06 mas and proper motion of ( μ α , μ δ ) = (−11.34 ± 0.06, 2.65 ± 0.14) mas yr −1 , yielding a distance of d = 1.90 − 0.18 + 0.22 kpc and transverse velocity of v ⊥ = 104 − 11 + 13 km s − 1 . These results are consistent with the Gaia 3 measurements, and open up the possibility of far more accurate astrometry with further VLBI observations.
A VLBI Distance and Transverse Velocity for PSR B1913+16
Publisher: American Astronomical Society
Date: 08-2018
Shock location and CME 3D reconstruction of a solar type II radio burst with LOFAR
Publisher: EDP Sciences
Date: 07-2018
DOI: 10.1051/0004-6361/201732308
Abstract: Context. Type II radio bursts are evidence of shocks in the solar atmosphere and inner heliosphere that emit radio waves ranging from sub-meter to kilometer lengths. These shocks may be associated with coronal mass ejections (CMEs) and reach speeds higher than the local magnetosonic speed. Radio imaging of decameter wavelengths (20–90 MHz) is now possible with the Low Frequency Array (LOFAR), opening a new radio window in which to study coronal shocks that leave the inner solar corona and enter the interplanetary medium and to understand their association with CMEs. Aims. To this end, we study a coronal shock associated with a CME and type II radio burst to determine the locations at which the radio emission is generated, and we investigate the origin of the band-splitting phenomenon. Methods. Thetype II shock source-positions and spectra were obtained using 91 simultaneous tied-array beams of LOFAR, and the CME was observed by the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) and by the COR2A coronagraph of the SECCHI instruments on board the Solar Terrestrial Relation Observatory(STEREO). The 3D structure was inferred using triangulation of the coronographic observations. Coronal magnetic fields were obtained from a 3D magnetohydrodynamics (MHD) polytropic model using the photospheric fields measured by the Heliospheric Imager (HMI) on board the Solar Dynamic Observatory (SDO) as lower boundary. Results. The type II radio source of the coronal shock observed between 50 and 70 MHz was found to be located at the expanding flank of the CME, where the shock geometry is quasi-perpendicular with θ Bn ~ 70°. The type II radio burst showed first and second harmonic emission the second harmonic source was cospatial with the first harmonic source to within the observational uncertainty. This suggests that radio wave propagation does not alter the apparent location of the harmonic source. The sources of the two split bands were also found to be cospatial within the observational uncertainty, in agreement with the interpretation that split bands are simultaneous radio emission from upstream and downstream of the shock front. The fast magnetosonic Mach number derived from this interpretation was found to lie in the range 1.3–1.5. The fast magnetosonic Mach numbers derived from modelling the CME and the coronal magnetic field around the type II source were found to lie in the range 1.4–1.6.
A Radio Frequency Study of the Accreting Millisecond X-ray Pulsar, IGR J16597–3704, in the Globular Cluster NGC 6256
Publisher: American Astronomical Society
Date: 20-02-2018
Measurement of the prompt-production cross-section ratio
σ ( χ <
Publisher: American Physical Society (APS)
Date: 09-06-2021
FRB microstructure revealed by the real-time detection of FRB170827
Publisher: Oxford University Press (OUP)
Date: 03-05-2018
ERRATUM: “THE PROPER MOTION OF THE GALACTIC CENTER PULSAR RELATIVE TO SAGITTARIUS A*” (2015, ApJ, 798, 120)
Publisher: American Astronomical Society
Date: 22-04-2016
Radio AGN in spiral galaxies
Publisher: Oxford University Press (OUP)
Date: 06-10-2015
Pulsar lensing geometry
Publisher: Oxford University Press (OUP)
Date: 10-02-2016
DOI: 10.1093/MNRAS/STW314
Constraints on the CKM angle γ from B± → Dh± decays using D → h±h′∓π0 final states
Publisher: Springer Science and Business Media LLC
Date: 07-2022
Abstract: A data s le collected with the LHCb detector corresponding to an integrated luminosity of 9 fb − 1 is used to measure eleven CP violation observables in B ± → Dh ± decays, where h is either a kaon or a pion. The neutral D meson decay is reconstructed in the three-body final states: K ± π ∓ π 0 π + π − π 0 K + K − π 0 and the suppressed π ± K ∓ π 0 combination. The mode where a large CP asymmetry is expected, B ± → [ π ± K ∓ π 0 ] D K ± , is observed with a significance greater than seven standard deviations. The ratio of the partial width of this mode relative to that of the favoured mode, B ± → [ K ± π ∓ π 0 ] D K ± , is R ADS( K ) = (1 . 27 ± 0 . 16 ± 0 . 02) × 10 − 2 . Evidence for a large CP asymmetry is also seen: A ADS( K ) = −0 . 38 ± 0 . 12 ± 0 . 02. Constraints on the CKM angle γ are calculated from the eleven reported observables.
Evidence for Modification of
b
Publisher:
American Physical Society (APS)
Date:
10-08-2023
Publisher: American Physical Society (APS)
Date: 10-08-2023
PARSEC-SCALE RADIO EMISSION FROM THE LOW-LUMINOSITY ACTIVE GALACTIC NUCLEUS IN THE DWARF STARBURST GALAXY HENIZE 2-10
Publisher: American Astronomical Society
Date: 16-04-2012
Estimating fast transient detection pipeline efficiencies at UTMOST via real-time injection of mock FRBs
Publisher: Oxford University Press (OUP)
Date: 02-12-2021
Abstract: Dedicated surveys using different detection pipelines are being carried out at multiple observatories to find more fast radio bursts (FRBs). Understanding the efficiency of detection algorithms and the survey completeness function is important to enable unbiased estimation of the underlying FRB population properties. One method to achieve end-to-end testing of the system is by injecting mock FRBs in the live data stream and searching for them blindly. Mock FRB injection is particularly effective for machine-learning-based classifiers, for which analytic characterization is impractical. We describe a first-of-its-kind implementation of a real-time mock FRB injection system at the upgraded Molonglo Observatory Synthesis Telescope (UTMOST) and present our results for a set of 20 000 mock FRB injections. The injections have yielded clear insight into the detection efficiencies and have provided a survey completeness function for pulse width, fluence, and dispersion measure (DM). Mock FRBs are recovered with uniform efficiency over the full range of injected DMs however, the recovery fraction is found to be a strong function of the width and signal-to-noise ratio (SNR). For low widths (≲20 ms) and high SNR (≳9) the recovery is highly effective with recovery fractions exceeding 90 per cent. We find that the presence of radio-frequency interference causes the recovered SNR values to be systematically lower by up to 20 per cent compared to the injected values. We find that wider FRBs become increasingly hard to recover for the machine-learning-based classifier employed at UTMOST. We encourage other observatories to implement live injection set-ups for similar testing of their surveys.
Radio and X-ray monitoring of the accreting millisecond X-ray pulsar IGR J17591−2342 in outburst
Publisher: Oxford University Press (OUP)
Date: 12-12-2019
Abstract: IGR J17591−2342 is a new accreting millisecond X-ray pulsar that was recently discovered in outburst in 2018. Early observations revealed that the source’s radio emission is brighter than that of any other known neutron star low-mass X-ray binary (NS–LMXB) at comparable X-ray luminosity, and assuming its likely ≳6 kpc distance. It is comparably radio bright to black hole LMXBs at similar X-ray luminosities. In this work, we present the results of our extensive radio and X-ray monitoring c aign of the 2018 outburst of IGR J17591−2342. In total, we collected 10 quasi-simultaneous radio (VLA, ATCA) and X-ray (Swift–XRT) observations, which make IGR J17591−2342 one of the best-s led NS–LMXBs. We use these to fit a power-law correlation index $\\beta = 0.37^{+0.42}_{-0.40}$ between observed radio and X-ray luminosities (LR ∝ LXβ). However, our monitoring revealed a large scatter in IGR J17591−2342’s radio luminosity (at a similar X-ray luminosity, LX ∼1036 erg s−1, and spectral state), with LR ∼ 4 × 1029 erg s−1 during the first three reported observations, and up to a factor of 4 lower LR during later radio observations. None the less, the average radio luminosity of IGR J17591−2342 is still one of the highest among NS–LMXBs, and we discuss possible reasons for the wide range of radio luminosities observed in such systems during outburst. We found no evidence for radio pulsations from IGR J17591−2342 in our Green Bank Telescope observations performed shortly after the source returned to quiescence. None the less, we cannot rule out that IGR J17591−2342 becomes a radio millisecond pulsar during quiescence.
Search for the doubly heavy baryon decaying to *
Publisher: IOP Publishing
Date: 09-2023
Abstract: A first search for the decay is performed by the LHCb experiment with a data s le of proton-proton collisions, corresponding to an integrated luminosity of 9 fb −1 recorded at centre-of-mass energies of 7, 8, and 13 TeV. Two peaking structures are seen with a local (global) significance of and standard deviations at masses of 6571 and 6694 MeV/ , respectively. Upper limits are set on the baryon production cross-section times the branching fraction relative to that of the decay at centre-of-mass energies of 8 and 13 TeV, in the and in the rapidity and transverse-momentum ranges from 2.0 to 4.5 and 0 to , respectively. Upper limits are presented as a function of the mass and lifetime.
Reconciling Optical and Radio Observations of the Binary Millisecond Pulsar PSR J1640+2224
Publisher: American Astronomical Society
Date: 14-03-2018
VLBI ASTROMETRY OF PSR J2222-0137: A PULSAR DISTANCE MEASURED TO 0.4% ACCURACY
Publisher: American Astronomical Society
Date: 05-06-2013
Numerical modeling of dusty debris disks
Publisher: American Astronomical Society
Date: 20-05-2005
DOI: 10.1086/429365
Corrigendum: Nowhere to Hide: Radio-faint AGN in GOODS-N field I. Initial catalogue and radio properties (Physics of Fluids 473 (2018) DOI: 10.1051/0004-6361/201833399)
Publisher: EDP Sciences
Date: 05-2019
Study of the doubly charmed tetraquark $${{{{{{\rm{T}}}}}}}_{{{{{{\rm{c}}}}}}{{{{{\rm{c}}}}}}}^{+}$$
Publisher: Springer Science and Business Media LLC
Date: 16-06-2022
DOI: 10.1038/S41467-022-30206-W
Abstract: Quantum chromodynamics, the theory of the strong force, describes interactions of coloured quarks and gluons and the formation of hadronic matter. Conventional hadronic matter consists of baryons and mesons made of three quarks and quark-antiquark pairs, respectively. Particles with an alternative quark content are known as exotic states. Here a study is reported of an exotic narrow state in the D 0 D 0 π + mass spectrum just below the D *+ D 0 mass threshold produced in proton-proton collisions collected with the LHCb detector at the Large Hadron Collider. The state is consistent with the ground isoscalar $${{{{{{\\rm{T}}}}}}}_{{{{{{\\rm{c}}}}}}{{{{{\\rm{c}}}}}}}^{+}$$ T c c + tetraquark with a quark content of $${{{{{\\rm{c}}}}}}{{{{{\\rm{c}}}}}}\\overline{{{{{{\\rm{u}}}}}}}\\overline{{{{{{\\rm{d}}}}}}}$$ c c u ¯ d ¯ and spin-parity quantum numbers J P = 1 + . Study of the DD mass spectra disfavours interpretation of the resonance as the isovector state. The decay structure via intermediate off-shell D *+ mesons is consistent with the observed D 0 π + mass distribution. To analyse the mass of the resonance and its coupling to the D * D system, a dedicated model is developed under the assumption of an isoscalar axial-vector $${{{{{{\\rm{T}}}}}}}_{{{{{{\\rm{c}}}}}}{{{{{\\rm{c}}}}}}}^{+}$$ T c c + state decaying to the D * D channel. Using this model, resonance parameters including the pole position, scattering length, effective range and compositeness are determined to reveal important information about the nature of the $${{{{{{\\rm{T}}}}}}}_{{{{{{\\rm{c}}}}}}{{{{{\\rm{c}}}}}}}^{+}$$ T c c + state. In addition, an unexpected dependence of the production rate on track multiplicity is observed.
Observation of excited
Ω c 0
Publisher: American Physical Society (APS)
Date: 24-11-2021
Observation of $$ {\Lambda}_b^0 $$ → D+pπ−π− and $$ {\Lambda}_b^0 $$ → D*+pπ−π− decays
Publisher: Springer Science and Business Media LLC
Date: 03-2022
Abstract: The multihadron decays $$ {\\Lambda}_b^0 $$ Λ b 0 → D + pπ−π− and $$ {\\Lambda}_b^0 $$ Λ b 0 → D * + pπ−π− are observed in data corresponding to an integrated luminosity of 3 fb − 1 , collected in proton-proton collisions at centre-of-mass energies of 7 and 8 TeV by the LHCb detector. Using the decay $$ {\\Lambda}_b^0 $$ Λ b 0 → $$ {\\Lambda}_c^{+} $$ Λ c + π + π − π − as a normalisation channel, the ratio of branching fractions is measured to be $$ \\frac{\\mathcal{B}\\left({\\Lambda}_b^0\\to {D}^{+}p{\\pi}^{-}{\\pi}^{-}\\right)}{\\mathcal{B}\\left({\\Lambda}_b^0\\to {\\Lambda}_c^0{\\pi}^{+}{\\pi}^{-}{\\pi}^{-}\\right)}\\times \\frac{\\mathcal{B}\\left({D}^{+}\\to {K}^{-}{\\pi}^{+}{\\pi}^{+}\\right)}{\\mathcal{B}\\left({\\Lambda}_c^0\\to {pK}^{-}{\\pi}^{-}\\right)}=\\left(5.35\\pm 0.21\\pm 0.16\\right)\\%, $$ B Λ b 0 → D + p π − π − B Λ b 0 → Λ c 0 π + π − π − × B D + → K − π + π + B Λ c 0 → pK − π − = 5.35 ± 0.21 ± 0.16 % , where the first uncertainty is statistical and the second systematic. The ratio of branching fractions for the $$ {\\Lambda}_b^0 $$ Λ b 0 → D *+ pπ − π − and $$ {\\Lambda}_b^0 $$ Λ b 0 → D + pπ − π − decays is found to be $$ \\frac{\\mathcal{B}\\left({\\Lambda}_b^0\\to {D}^{\\ast +}p{\\pi}^{-}{\\pi}^{-}\\right)}{\\mathcal{B}\\left({\\Lambda}_b^0\\to {D}^{+}p{\\pi}^{-}{\\pi}^{-}\\right)}\\times \\left(\\mathcal{B}\\left({D}^{\\ast +}\\to {D}^{+}{\\pi}^0\\right)+\\mathcal{B}\\left({D}^{\\ast +}\\to {D}^{+}\\gamma \\right)\\right)=\\left(61.3\\pm 4.3\\pm 4.0\\right)\\%. $$ B Λ b 0 → D ∗ + p π − π − B Λ b 0 → D + p π − π − × B D ∗ + → D + π 0 + B D ∗ + → D + γ = 61.3 ± 4.3 ± 4.0 % .
Measurement of antiproton production from antihyperon decays in $${p} \textrm{He}$$ collisions at $$\sqrt{s_{\scriptscriptstyle \mathrm NN}} =110$$ $$\,\text {Ge\hspace{-1.00006pt}V}$$
Publisher: Springer Science and Business Media LLC
Date: 27-06-2023
DOI: 10.1140/EPJC/S10052-023-11673-X
Abstract: The interpretation of cosmic antiproton flux measurements from space-borne experiments is currently limited by the knowledge of the antiproton production cross-section in collisions between primary cosmic rays and the interstellar medium. Using collisions of protons with an energy of 6.5 $$\\,\\text {Te\\hspace{-1.00006pt}V}$$ Te V incident on helium nuclei at rest in the proximity of the interaction region of the LHCb experiment, the ratio of antiprotons originating from antihyperon decays to prompt production is measured for antiproton momenta between 12 and $$110\\,\\text {Ge\\hspace{-1.00006pt}V\\!/}c $$ 110 Ge V\\!/ c . The dominant antihyperon contribution, namely $${\\overline{\\varLambda }} \\rightarrow {\\overline{{p}}} {{\\pi } ^+} $$ Λ ¯ → p ¯ π + decays from promptly produced $$\\overline{\\varLambda }$$ Λ ¯ particles, is also exclusively measured. The results complement the measurement of prompt antiproton production obtained from the same data s le. At the energy scale of this measurement, the antihyperon contributions to antiproton production are observed to be significantly larger than predictions of commonly used hadronic production models.
Observation of the Mass Difference between Neutral Charm-Meson Eigenstates
Publisher: American Physical Society (APS)
Date: 07-09-2021
Observation of the decay $$ {\Lambda}_{\mathrm{b}}^0 $$ → χc1pπ−
Publisher: Springer Science and Business Media LLC
Date: 05-2021
Abstract: The Cabibbo-suppressed decay $$ {\\Lambda}_{\\mathrm{b}}^0 $$ Λ b 0 → χ c1 pπ − is observed for the first time using data from proton-proton collisions corresponding to an integrated luminosity of 6 fb − 1 , collected with the LHCb detector at a centre-of-mass energy of 13 TeV. Evidence for the $$ {\\Lambda}_{\\mathrm{b}}^0 $$ Λ b 0 → χ c2 pπ − decay is also found. Using the $$ {\\Lambda}_{\\mathrm{b}}^0 $$ Λ b 0 → χ c1 pK − decay as normalisation channel, the ratios of branching fractions are measured to be $$ {\\displaystyle \\begin{array}{c}\\frac{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}1}{\\mathrm{p}\\uppi}^{-}\\right)}{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}1}{\\mathrm{p}\\mathrm{K}}^{-}\\right)}=\\left(6.59\\pm 1.01\\pm 0.22\\right)\\times {10}^{-2},\\\\ {}\\frac{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}2}{\\mathrm{p}\\uppi}^{-}\\right)}{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}1}{\\mathrm{p}\\uppi}^{-}\\right)}=0.95\\pm 0.30\\pm 0.04\\pm 0.04,\\\\ {}\\frac{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}2}{\\mathrm{p}\\mathrm{K}}^{-}\\right)}{\\mathcal{B}\\left({\\Lambda}_{\\mathrm{b}}^0\\to {\\upchi}_{\\mathrm{c}1}{\\mathrm{p}\\mathrm{K}}^{-}\\right)}=1.06\\pm 0.05\\pm 0.04\\pm 0.04,\\end{array}} $$ B Λ b 0 → χ c 1 pπ − B Λ b 0 → χ c 1 pK − = 6.59 ± 1.01 ± 0.22 × 10 − 2 , B Λ b 0 → χ c 2 pπ − B Λ b 0 → χ c 1 pπ − = 0.95 ± 0.30 ± 0.04 ± 0.04 , B Λ b 0 → χ c 2 pK − B Λ b 0 → χ c 1 pK − = 1.06 ± 0.05 ± 0.04 ± 0.04 , where the first uncertainty is statistical, the second is systematic and the third is due to the uncertainties in the branching fractions of χ c1 , 2 → J / ψγ decays.
Velocity selection of Rydberg positronium using a curved electrostatic guide
Publisher: American Physical Society (APS)
Date: 19-05-2017
Search for massive long-lived particles decaying semileptonically at $${\sqrt{s}}=13\,\hbox {TeV}$$
Publisher: Springer Science and Business Media LLC
Date: 04-2022
DOI: 10.1140/EPJC/S10052-022-10186-3
Abstract: A search is performed for massive long-lived particles (LLPs) decaying semileptonically into a muon and two quarks. Two kinds of LLP production processes were considered. In the first, a Higgs-like boson with mass from 30 to 200 $$\\text {\\,GeV\\!/}c^2$$ \\,GeV\\!/ c 2 is produced by gluon fusion and decays into two LLPs. The analysis covers LLP mass values from 10 $$\\text {\\,GeV\\!/}c^2$$ \\,GeV\\!/ c 2 up to about one half the Higgs-like boson mass. The second LLP production mode is directly from quark interactions, with LLP masses from 10 to 90 $$\\text {\\,GeV\\!/}c^2$$ \\,GeV\\!/ c 2 . The LLP lifetimes considered range from 5 to 200 ps. This study uses LHCb data collected from proton-proton collisions at $$\\sqrt{s} = 13\\text {\\,TeV} $$ s = 13 \\,TeV , corresponding to an integrated luminosity of 5.4 $$\\text {\\,fb} ^{-1}$$ \\,fb - 1 . No evidence of these long-lived states has been observed, and upper limits on the production cross-section times branching ratio have been set for each model considered.
100 μas RESOLUTION VLBI IMAGING OF ANISOTROPIC INTERSTELLAR SCATTERING TOWARD PULSAR B0834+06
Publisher: American Astronomical Society
Date: 09-12-2009
Search for the lepton-flavour violating decays B$^{0}$→ K$^{*0}$μ$^{±}$e$^{∓}$ and $ {B}_s^0 $→ ϕμ$^{±}$e$^{∓}$
Publisher: Springer Science and Business Media LLC
Date: 14-06-2023
Abstract: A search for the lepton-flavour violating decays B 0 → K *0 μ ± e ∓ and $$ {B}_s^0 $$ B s 0 → ϕμ ± e ∓ is presented, using proton-proton collision data collected by the LHCb detector at the LHC, corresponding to an integrated luminosity of 9 fb − 1 . No significant signals are observed and upper limits of $$ {\\displaystyle \\begin{array}{c}\\mathcal{B}\\left({B}^0\\to {K}^{\\ast 0}{\\mu}^{+}{e}^{-}\\right) .7\\times {10}^{-9}\\left(6.9\\times {10}^{-9}\\right),\\\\ {}\\mathcal{B}\\left({B}^0\\to {K}^{\\ast 0}{\\mu}^{-}{e}^{+}\\right) .8\\times {10}^{-9}\\left(7.9\\times {10}^{-9}\\right),\\\\ {}\\mathcal{B}\\left({B}^0\\to {K}^{\\ast 0}{\\mu}^{\\pm }{e}^{\\mp}\\right) .1\\times {10}^{-9}\\left(11.7\\times {10}^{-9}\\right),\\\\ {}\\mathcal{B}\\left({B}_s^0\\to \\phi {\\mu}^{\\pm }{e}^{\\mp}\\right) .0\\times {10}^{-9}\\left(19.8\\times {10}^{-9}\\right)\\end{array}} $$ B B 0 → K ∗ 0 μ + e − 5.7 × 10 − 9 6.9 × 10 − 9 , B B 0 → K ∗ 0 μ − e + 6.8 × 10 − 9 7.9 × 10 − 9 , B B 0 → K ∗ 0 μ ± e ∓ 10.1 × 10 − 9 11.7 × 10 − 9 , B B s 0 → ϕ μ ± e ∓ 16.0 × 10 − 9 19.8 × 10 − 9 are set at 90% (95%) confidence level. These results constitute the world’s most stringent limits to date, with the limit on the decay $$ {B}_s^0 $$ B s 0 → ϕμ ± e ∓ the first being set. In addition, limits are reported for scalar and left-handed lepton-flavour violating New Physics scenarios.
Charmonium production in pNe collisions at $$\sqrt{s_{\scriptscriptstyle \text {NN}}} =68.5$$ GeV
Publisher: Springer Science and Business Media LLC
Date: 17-07-2023
DOI: 10.1140/EPJC/S10052-023-11608-6
Abstract: The measurement of charmonium states produced in proton-neon ( $$p\\text {Ne}$$ p Ne ) collisions by the LHCb experiment in its fixed-target configuration is presented. The production of $${{J} \\hspace{-1.66656pt}/\\hspace{-1.111pt}\\psi }$$ J / ψ and $$\\psi {(2S)}$$ ψ ( 2 S ) mesons is studied with a beam of 2.5 $$\\mathrm{\\,Te\\hspace{-1.00006pt}V}$$ Te V protons colliding on gaseous neon targets at rest, corresponding to a nucleon-nucleon centre-of-mass energy $$\\sqrt{s_{\\scriptscriptstyle \\text {NN}}} =68.5\\mathrm{\\,Ge\\hspace{-1.00006pt}V} $$ s NN = 68.5 Ge V . The data s le corresponds to an integrated luminosity of $$21.7\\pm 1.4 $$ 21.7 ± 1.4 nb $$^{-1}$$ - 1 . The $${{J} \\hspace{-1.66656pt}/\\hspace{-1.111pt}\\psi }$$ J / ψ and $$\\psi {(2S)}$$ ψ ( 2 S ) hadrons are reconstructed in $$\\mu ^+$$ μ + $$\\mu ^-$$ μ - final states. The $${{J} \\hspace{-1.66656pt}/\\hspace{-1.111pt}\\psi }$$ J / ψ production cross-section per target nucleon in the centre-of-mass rapidity range $$y^\\star \\in [-2.29, 0]$$ y ⋆ ∈ [ - 2.29 , 0 ] is found to be $$506 \\pm 8 \\pm 46 \\text { nb/nucleon}$$ 506 ± 8 ± 46 nb/nucleon . The ratio of $${{J} \\hspace{-1.66656pt}/\\hspace{-1.111pt}\\psi }$$ J / ψ and $$D^0$$ D 0 cross-sections is evaluated to $$(1.06 \\pm 0.02 \\pm 0.09)\\%$$ ( 1.06 ± 0.02 ± 0.09 ) % . The $$\\psi {(2S)}$$ ψ ( 2 S ) to $${{J} \\hspace{-1.66656pt}/\\hspace{-1.111pt}\\psi }$$ J / ψ relative production rate is found to be $$(1.67 \\pm 0.27\\pm 0.10)\\%$$ ( 1.67 ± 0.27 ± 0.10 ) % in good agreement with other measurements involving beam and target nuclei of similar sizes.
Asymmetric structure in Sgr A* at 3 mm from closure phase measurements with VLBA, GBT and LMT
Publisher: Oxford University Press (OUP)
Date: 19-07-2016
The peculiar radio galaxy 4C 35.06: a case for recurrent AGN activity?
Publisher: EDP Sciences
Date: 22-06-2015
V-FASTR: The VLBA fast radio transients experiment
Publisher: American Astronomical Society
Date: 22-06-2011
Detection of fast radio transients with multiple stations: A case study using the very long baseline array
Publisher: American Astronomical Society
Date: 22-06-2011
Cold-gas outflows in typical low-redshift galaxies are driven by star formation, not AGN
Publisher: Oxford University Press (OUP)
Date: 22-11-2015
Search for the doubly heavy baryons and decaying to and *
Publisher: IOP Publishing
Date: 09-2021
Abstract: The first search for the doubly heavy baryon and a search for the baryon are performed using collision data collected via the experiment from 2016 to 2018 at a centre-of-mass energy of , corresponding to an integrated luminosity of 5.2 . The baryons are reconstructed via their decays to and . No significant excess is found for invariant masses between 6700 and 7300 , in a rapidity range from 2.0 to 4.5 and a transverse momentum range from 2 to 20 . Upper limits are set on the ratio of the and production cross-section times the branching fraction to ( ) relative to that of the ( ) baryon, for different lifetime hypotheses, at 95% confidence level. The upper limits range from to for the ( ) decay, and from to for the ( ) decay, depending on the considered mass and lifetime of the ( ) baryon.
Author Correction: Superluminal motion of a relativistic jet in the neutron-star merger GW170817 (Nature, (2018), 561, 7723, (355-359), 10.1038/s41586-018-0486-3)
Publisher: Springer Science and Business Media LLC
Date: 17-12-2019
DOI: 10.1038/S41586-019-1860-5
Abstract: An Amendment to this paper has been published and can be accessed via a link at the top of the paper.
First Measurement of the
Z → μ
Publisher:
American Physical Society (APS)
Date:
24-08-2022
Publisher: American Physical Society (APS)
Date: 24-08-2022
Search for the doubly charmed baryon $$ {\varXi}_{cc}^{+} $$ in the $$ {\varXi}_c^{+}{\pi}^{-}{\pi}^{+} $$ final state
Publisher: Springer Science and Business Media LLC
Date: 12-2021
Abstract: A search for the doubly charmed baryon $$ {\\varXi}_{cc}^{+} $$ Ξ cc + is performed in the $$ {\\varXi}_c^{+}{\\pi}^{-}{\\pi}^{+} $$ Ξ c + π − π + invariant-mass spectrum, where the $$ {\\varXi}_c^{+} $$ Ξ c + baryon is reconstructed in the pK − π + final state. The study uses proton-proton collision data collected with the LHCb detector at a centre- of-mass energy of 13 TeV, corresponding to a total integrated luminosity of 5.4 fb − 1 . No significant signal is observed in the invariant-mass range of 3.4–3.8 GeV/ c 2 . Upper limits are set on the ratio of branching fractions multiplied by the production cross-section with respect to the $$ {\\varXi}_{cc}^{++} $$ Ξ cc + + → ( $$ {\\varXi}_c^{+} $$ Ξ c + → pK − π + ) π + decay for different $$ {\\varXi}_{cc}^{+} $$ Ξ cc + mass and lifetime hypotheses in the rapidity range from 2.0 to 4.5 and the transverse momentum range from 2.5 to 25 GeV/ c . The results from this search are combined with a previously published search for the $$ {\\varXi}_{cc}^{+} $$ Ξ cc + → $$ {\\varLambda}_c^{+} $$ Λ c + K − π + decay mode, yielding a maximum local significance of 4.0 standard deviations around the mass of 3620 MeV/ c 2 , including systematic uncertainties. Taking into account the look-elsewhere effect in the 3.5–3.7 GeV/ c 2 mass window, the combined global significance is 2.9 standard deviations including systematic uncertainties.
Superluminal motion of a relativistic jet in the neutron-star merger GW170817
Publisher: Springer Science and Business Media LLC
Date: 09-2018
DOI: 10.1038/S41586-018-0486-3
Abstract: The binary neutron-star merger GW170817
ACCRETION-POWERED PULSATIONS IN AN APPARENTLY QUIESCENT NEUTRON STAR BINARY
Publisher: American Astronomical Society
Date: 07-2015
Active Galactic nuclei cores in infrared-faint radio sources
Publisher: EDP Sciences
Date: 06-2015
High time resolution and polarization properties of ASKAP-localized fast radio bursts
Publisher: Oxford University Press (OUP)
Date: 24-07-2020
Abstract: Combining high time and frequency resolution full-polarization spectra of fast radio bursts (FRBs) with knowledge of their host galaxy properties provides an opportunity to study both the emission mechanism generating them and the impact of their propagation through their local environment, host galaxy, and the intergalactic medium. The Australian Square Kilometre Array Pathfinder (ASKAP) telescope has provided the first ensemble of bursts with this information. In this paper, we present the high time and spectral resolution, full polarization observations of five localized FRBs to complement the results published for the previously studied ASKAP FRB 181112. We find that every FRB is highly polarized, with polarization fractions ranging from 80 to 100 per cent, and that they are generally dominated by linear polarization. While some FRBs in our s le exhibit properties associated with an emerging archetype (i.e. repeating or apparently non-repeating), others exhibit characteristic features of both, implying the existence of a continuum of FRB properties. When examined at high time resolution, we find that all FRBs in our s le have evidence for multiple subcomponents and for scattering at a level greater than expected from the Milky Way. We find no correlation between the erse range of FRB properties (e.g. scattering time, intrinsic width, and rotation measure) and any global property of their host galaxy. The most heavily scattered bursts reside in the outskirts of their host galaxies, suggesting that the source-local environment rather than the host interstellar medium is likely the dominant origin of the scattering in our s le.
Gaia EDR3 parallaxes of type I X-ray bursters and their implications on the models of type I X-ray bursts: A generic approach to the Gaia parallax zero point and its uncertainty
Publisher: Cambridge University Press (CUP)
Date: 2021
DOI: 10.1017/PASA.2021.37
Abstract: Light curves of photospheric radius expansion (PRE) bursts, a subset of type I X-ray bursts, have been used as standard candles to estimate the ‘nominal PRE distances’ for 63% of PRE bursters (bursters), assuming PRE burst emission is spherically symmetric. Model-independent geometric parallaxes of bursters provide a valuable chance to test models of PRE bursts (PRE models) and can be provided in some cases by Gaia astrometry of the donor stars in bursters. We searched for counterparts to 115 known bursters in the Gaia Early Data Release 3 and confirmed 4 bursters with Gaia counterparts that have detected ( $\\gt\\!3\\,\\sigma$ , prior to zero-point correction) parallaxes. We describe a generic approach to the Gaia parallax zero point as well as its uncertainty using an ensemble of Gaia quasars in idually determined for each target. Assuming the spherically symmetric PRE model is correct, we refined the resultant nominal PRE distances of three bursters (i.e. Cen $\\textrm{X}-4$ , Cyg $\\textrm{X}-2$ , and $4\\textrm{U}\\,0919-54$ ) and put constraints on their compositions of the nuclear fuel powering the bursts. Finally, we describe a method for testing the correctness of the spherically symmetric PRE model using parallax measurements and provide preliminary results.
THE ANGULAR BROADENING OF THE GALACTIC CENTER PULSAR SGR J1745-29: A NEW CONSTRAINT ON THE SCATTERING MEDIUM
Publisher: American Astronomical Society
Date: 10-12-2013
Real-time adaptive event detection in astronomical data streams
Publisher: Institute of Electrical and Electronics Engineers (IEEE)
Date: 2014
DOI: 10.1109/MIS.2013.10
A measurement of Hubble’s Constant using Fast Radio Bursts
Publisher: Oxford University Press (OUP)
Date: 08-09-2022
Abstract: We constrain the Hubble constant H0 using Fast Radio Burst (FRB) observations from the Australian Square Kilometre Array Pathfinder (ASKAP) and Murriyang (Parkes) radio telescopes. We use the redshift-dispersion measure (‘Macquart’) relationship, accounting for the intrinsic luminosity function, cosmological gas distribution, population evolution, host galaxy contributions to the dispersion measure (DMhost), and observational biases due to burst duration and telescope beamshape. Using an updated s le of 16 ASKAP FRBs detected by the Commensal Real-time ASKAP Fast Transients (CRAFT) Survey and localized to their host galaxies, and 60 unlocalized FRBs from Parkes and ASKAP, our best-fitting value of H0 is calculated to be $73_{-8}^{+12}$ km s−1 Mpc−1. Uncertainties in FRB energetics and DMhost produce larger uncertainties in the inferred value of H0 compared to previous FRB-based estimates. Using a prior on H0 covering the 67–74 km s−1 Mpc−1 range, we estimate a median ${\\rm DM}_{\\rm host}= 186_{-48}^{+59}\\,{\\rm pc \\, cm^{-3}}$, exceeding previous estimates. We confirm that the FRB population evolves with redshift similarly to the star-formation rate. We use a Schechter luminosity function to constrain the maximum FRB energy to be log10Emax$=41.26_{-0.22}^{+0.27}$ erg assuming a characteristic FRB emission bandwidth of 1 GHz at 1.3 GHz, and the cumulative luminosity index to be $\\gamma =-0.95_{-0.15}^{+0.18}$. We demonstrate with a s le of 100 mock FRBs that H0 can be measured with an uncertainty of ±2.5 km s−1 Mpc−1, demonstrating the potential for clarifying the Hubble tension with an upgraded ASKAP FRB search system. Last, we explore a range of s le and selection biases that affect FRB analyses.
Extremely high precision VLBI astrometry of PSR J0437-4715 and implications for theories of gravity
Publisher: American Astronomical Society
Date: 26-08-2008
DOI: 10.1086/592401
A very long baseline interferometry detection of the class I protostar IRS 5 in Corona Australis
Publisher: EDP Sciences
Date: 21-03-2013
Observation of a $$ {\varLambda}_b^0 $$ − $$ {\overline{\varLambda}}_b^0 $$ production asymmetry in proton-proton collisions at $$ \sqrt{s} $$ = 7 and 8 TeV
Publisher: Springer Science and Business Media LLC
Date: 10-2021
Abstract: This article presents differential measurements of the asymmetry between $$ {\\varLambda}_b^0 $$ Λ b 0 and $$ {\\overline{\\varLambda}}_b^0 $$ Λ ¯ b 0 baryon production rates in proton-proton collisions at centre-of-mass energies of $$ \\sqrt{s} $$ s = 7 and 8 TeV collected with the LHCb experiment, corresponding to an integrated luminosity of 3 fb − 1 . The $$ {\\varLambda}_b^0 $$ Λ b 0 baryons are reconstructed through the inclusive semileptonic decay $$ {\\varLambda}_b^0 $$ Λ b 0 → $$ {\\varLambda}_c^{+} $$ Λ c + μ − $$ \\overline{\\nu} $$ ν ¯ μ X . The production asymmetry is measured both in intervals of rapidity in the range 2 . 15 y 4 . 10 and transverse momentum in 2 p T 27 GeV/ c . The results are found to be incompatible with symmetric production with a significance of 5.8 standard deviations for both $$ \\sqrt{s} $$ s = 7 and 8 TeV data, assuming no CP violation in the decay. There is evidence for a trend as a function of rapidity with a significance of 4 standard deviations. Comparisons to predictions from hadronisation models in P ythia and heavy-quark recombination are provided. This result constitutes the first observation of a particle-antiparticle asymmetry in b -hadron production at LHC energies.
Strong-Field Gravity Tests with the Double Pulsar
Publisher: American Physical Society (APS)
Date: 13-12-2021
On the structure of the transition disk around TW Hydrae
Publisher: EDP Sciences
Date: 04-2014
Constraining properties of neutron star merger outflows with radio observations
Publisher: Oxford University Press (OUP)
Date: 17-04-2020
Abstract: The jet opening angle and inclination of GW170817 – the first detected binary neutron star merger – were vital to understand its energetics, relation to short gamma-ray bursts, and refinement of the standard siren-based determination of the Hubble constant, H0. These basic quantities were determined through a combination of the radio light curve and Very Long Baseline Interferometry (VLBI) measurements of proper motion. In this paper, we discuss and quantify the prospects for the use of radio VLBI observations and observations of scintillation-induced variability to measure the source size and proper motion of merger afterglows, and thereby infer properties of the merger including inclination angle, opening angle, and energetics. We show that these techniques are complementary as they probe different parts of the circum-merger density/inclination angle parameter space and different periods of the temporal evolution of the afterglow. We also find that while VLBI observations will be limited to the very closest events it will be possible to detect scintillation for a large fraction of events beyond the range of current gravitational wave detectors. Scintillation will also be detectable with next-generation telescopes such as the Square Kilometre Array, 2000 antenna Deep Synoptic Array, and the next-generation Very Large Array, for a large fraction of events detected with third-generation gravitational wave detectors. Finally, we discuss prospects for the measurement of the H0 with VLBI observations of neutron star mergers and compare this technique to other standard siren methods.
Precision southern hemisphere vlbi pulsar astrometry. ii. measurement of seven parallaxes
Publisher: American Astronomical Society
Date: 30-07-2009
Measurement of the Nuclear Modification Factor and Prompt Charged Particle Production in
p
Publisher: American Physical Society (APS)
Date: 07-04-2022
RESOLVED MULTIFREQUENCY RADIO OBSERVATIONS OF GG Tau
Publisher: American Astronomical Society
Date: 13-05-2014
Single Pulses from the Galactic Center Magnetar with the Very Large Array
Publisher: Cambridge University Press (CUP)
Date: 09-2017
DOI: 10.1017/S1743921317009358
Abstract: Phased VLA observations of the Galactic center magnetar J1745-2900 over 8-12 GHz reveal rich single pulse behavior. The average profile is comprised of several distinct components and is fairly stable over day timescales and GHz frequencies. The average profile is dominated by the jitter of relatively narrow pulses. The pulses in each of the four profile components are uncorrelated in phase and litude, although the occurrence of pulse components 1 and 2 appear to be correlated. Using a collection of the brightest in idual pulses, we verify that the index of the dispersion law is consistent with the expected cold plasma value of 2. The scattering time is weakly constrained, but consistent with previous measurements, while the dispersion measure DM = 1763 +3 −10 pc cm −3 is lower than previous measurements, which could be a result of time variability in the line-of-sight column density or changing pulse profile shape over time or frequency.
Wide-field vlbi observations of M31: A unique probe of the ionized interstellar medium of a nearby Galaxy
Publisher: American Astronomical Society
Date: 09-04-2013
Search for
C P
Publisher:
American Physical Society (APS)
Date:
20-09-2021
Publisher: American Physical Society (APS)
Date: 20-09-2021
Erratum: FRB microstructure revealed by the real-time detection of FRB170827
Publisher: Oxford University Press (OUP)
Date: 17-12-2018
Study of the Bose-Einstein correlations of same-sign pions in proton-lead collisions
Publisher: Springer Science and Business Media LLC
Date: 26-09-2023
Observation of the suppressed
Λ b 0
Publisher:
American Physical Society (APS)
Date:
27-12-2021
Publisher: American Physical Society (APS)
Date: 27-12-2021
Related Organisations
National Radio Astronomy Observatory
Location: United States of America
ASTRON, The Netherlands Institute For Radio Astronomy
Location: Netherlands
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