ORCID Profile
0000-0002-0005-2631
Current Organisation
The Ohio State University
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Atomic, Molecular, Nuclear, Particle and Plasma Physics | Cosmic Ray Physics | High Energy Astrophysics; Cosmic Rays | Nuclear And Particle Physics | Particle Physics | Nuclear Physics
Expanding Knowledge in the Physical Sciences | Physical sciences |
Publisher: American Astronomical Society
Date: 28-12-2022
Abstract: Using the first epoch of four-band NIRCam observations obtained by the James Webb Space Telescope (JWST) Prime Extragalactic Areas for Reionization and Lensing Science Program in the Spitzer IRAC Dark Field, we search for F150W and F200W dropouts. In 14.2 arcmin 2 , we have found eight F150W dropouts and eight F200W dropouts, all brighter than 27.5 mag (the brightest being ∼24 mag) in the band to the red side of the break. As they are detected in multiple bands, these must be real objects. Their nature, however, is unclear, and characterizing their properties is important for realizing the full potential of JWST. If the observed color decrements are due to the Lyman break, these objects should be at z ≳ 11.7 and z ≳ 15.4, respectively. The color diagnostics show that at least four F150W dropouts are far away from the usual contaminators encountered in dropout searches (red galaxies at much lower redshifts or brown dwarf stars). While the diagnostics of the F200W dropouts are less certain due to the limited number of passbands, at least one of them is likely not a known type of contaminant, and the rest are consistent with either high-redshift galaxies with evolved stellar populations or old galaxies at z ≈ 3–8. If a significant fraction of our dropouts are indeed at z ≳ 12, we have to face the severe problem of explaining their high luminosities and number densities. Spectroscopic identifications of such objects are urgently needed.
Publisher: Elsevier BV
Date: 06-2012
Publisher: American Association for the Advancement of Science (AAAS)
Date: 11-07-2018
Abstract: Previous detections of in idual astrophysical sources of neutrinos are limited to the Sun and the supernova 1987A, whereas the origins of the diffuse flux of high-energy cosmic neutrinos remain unidentified. On 22 September 2017, we detected a high-energy neutrino, IceCube-170922A, with an energy of ~290 tera-electron volts. Its arrival direction was consistent with the location of a known γ-ray blazar, TXS 0506+056, observed to be in a flaring state. An extensive multiwavelength c aign followed, ranging from radio frequencies to γ-rays. These observations characterize the variability and energetics of the blazar and include the detection of TXS 0506+056 in very-high-energy γ-rays. This observation of a neutrino in spatial coincidence with a γ-ray-emitting blazar during an active phase suggests that blazars may be a source of high-energy neutrinos.
Publisher: American Physical Society (APS)
Date: 11-11-2003
Publisher: IOP Publishing
Date: 02-2017
Publisher: American Physical Society (APS)
Date: 24-06-2002
Publisher: American Physical Society (APS)
Date: 05-01-2004
Publisher: American Astronomical Society
Date: 14-12-2022
Abstract: We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST “Prime Extragalactic Areas for Reionization and Lensing Science” (PEARLS) project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP) seven gravitationally lensing clusters two high redshift protoclusters and the iconic backlit VV 191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, active galactic nucleus (AGN) growth, and First Light. Five fields—the JWST NEP Time-Domain Field (TDF), IRAC Dark Field, and three lensing clusters—will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9–4.5 μ m galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9–4.5 μ m. PEARLS is designed to be of lasting benefit to the community.
Publisher: American Physical Society (APS)
Date: 26-09-2008
Publisher: American Physical Society (APS)
Date: 29-06-2017
Publisher: American Astronomical Society
Date: 29-10-2018
Publisher: American Physical Society (APS)
Date: 05-05-2005
Publisher: American Physical Society (APS)
Date: 09-05-2003
Publisher: American Astronomical Society
Date: 09-05-2012
Publisher: American Astronomical Society
Date: 06-07-2020
Publisher: American Physical Society (APS)
Date: 16-09-2004
Publisher: American Physical Society (APS)
Date: 18-07-2018
Publisher: American Physical Society (APS)
Date: 05-12-2007
Publisher: American Physical Society (APS)
Date: 30-01-2004
Publisher: American Physical Society (APS)
Date: 29-07-2002
Publisher: IOP Publishing
Date: 20-01-2023
Abstract: High energy collisions at the High-Luminosity Large Hadron Collider (LHC) produce a large number of particles along the beam collision axis, outside of the acceptance of existing LHC experiments. The proposed Forward Physics Facility (FPF), to be located several hundred meters from the ATLAS interaction point and shielded by concrete and rock, will host a suite of experiments to probe standard model (SM) processes and search for physics beyond the standard model (BSM). In this report, we review the status of the civil engineering plans and the experiments to explore the erse physics signals that can be uniquely probed in the forward region. FPF experiments will be sensitive to a broad range of BSM physics through searches for new particle scattering or decay signatures and deviations from SM expectations in high statistics analyses with TeV neutrinos in this low-background environment. High statistics neutrino detection will also provide valuable data for fundamental topics in perturbative and non-perturbative QCD and in weak interactions. Experiments at the FPF will enable synergies between forward particle production at the LHC and astroparticle physics to be exploited. We report here on these physics topics, on infrastructure, detector, and simulation studies, and on future directions to realize the FPF’s physics potential.
Publisher: American Astronomical Society
Date: 22-01-2019
Location: United States of America
Location: United States of America
Start Date: 07-2022
End Date: 06-2025
Amount: $432,195.00
Funder: Australian Research Council
View Funded ActivityStart Date: 2010
End Date: 12-2014
Amount: $180,000.00
Funder: Australian Research Council
View Funded Activity