Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session V14: Missions, Instruments, and Surveys |
Hide Abstracts |
Sponsoring Units: DAP Chair: Panayiotis Tzanavaris, American Physical Society Room: Marquette V - 2nd Floor |
Tuesday, April 18, 2023 3:45PM - 3:57PM |
V14.00001: GECCO: a Compton Telescope with Coded Aperture Mask Gabriella Carini The Galactic Explorer with a Coded Aperture Mask Compton Telescope (GECCO) is a novel Explorer-class concept for a next-generation telescope covering the poorly explored hard X-ray and soft gamma-ray energies. This concept builds upon the heritage of past and current missions, improving sensitivity and, very importantly, angular resolution. GECCO uses the combined Coded Aperture Mask and Compton telescope techniques to employ the benefits of both: superior angular resolution provided by the Coded Aperture, and good background rejection and wide field-of-view provided by the Compton telescope. It is being developed at NASA/GSFC in collaboration with BNL and other US and foreign institutions. GECCO observations will extend arcminute angular resolution to high-energy images of the Galactic plane, combining the spectral capabilities of INTEGRAL/IBIS and the x-ray imaging of NuSTAR and eROSITA, and will make a bridge to the Fermi-LAT observations, enabling a broad potential for discoveries in the MeV γ-ray sky. GECCO will operate in the 100 keV - 10 MeV energy range, with energy resolution of ~ 1% from 0.5 - 5 MeV. With the unprecedented angular resolution (∼1 arcmin) of the coded mask telescope combined with the sensitive Compton telescope, GECCO will be able to disentangle discrete sources from truly diffuse emission, contributing to understanding the gamma-ray Galactic Centre excess and the Fermi Bubbles, and to tracing low-energy cosmic rays and their propagation in the Galaxy. |
Tuesday, April 18, 2023 3:57PM - 4:09PM |
V14.00002: CCAT-prime: Science Goals & First Light 280 GHz Instrumentation Cody J Duell The CCAT-prime Collaboration's Fred Young Submillimeter Telescope (FYST) is a six-meter aperture telescope currently being built to observe at millimeter and submillimeter wavelengths in Chile's Atacama desert on Cerro Chajnantor and expected to begin science observations in 2024. Prime-Cam, the primary first generation science instrument, will house up to seven total instrument modules, including both polarimetric broadband and imaging spectrometer modules, to simultaneously observe the sky from 210-850 GHz using kinetic inductance detectors. By capitalizing on FYST's extraordinary site at an elevation of 5600 meters, Prime-Cam will enable a more than 10 times improvement in mapping speed over current and near-term submillimeter facilities. CCAT-prime will serve as a complement to upcoming CMB surveys and pursue a broad range of science goals, including tracing galaxy formation during the Epoch of Reionization, probing star formation within the Milky Way, and studying time-domain variability at submillimeter wavelengths. We present the science goals, instrument designs, and status for Prime-Cam on FYST, with a particular emphasis on the detectors and readout for the first light 280 GHz Instrument Module. |
Tuesday, April 18, 2023 4:09PM - 4:21PM |
V14.00003: The Trans-Iron Galactic Element Recorder for the International Space Station (TIGERISS) Brian F Rauch, Wolfgang Zober, Michaela Amoo, Roberto F Borda, Richard G Bose, Nicholas W Cannady, Stephane Coutu, Priyarshini Ghosh, John F Krizmanic, J. Vanderlei Martins, Eileen Meyer, John W W Mitchell, John G Mitchell, Isaac Mognet, Scott Nutter, Kenichi Sakai, Makoto Sasaki, Sonya Smith, Liam P Williams, Alexander A Moiseev, Georgia A de Nolfo, Michael Mcpherson, Harrell A Tolentino, Regina M Caputo TIGERISS is an Ultra-Heavy Galactic Cosmic Ray (UHGCR) detector awarded under the second round of the NASA Astrophysics Pioneers program. It will measure the abundances of every element from 5B to 82Pb relative to 26Fe with kinetic energies over 350 MeV/nucleon. TIGERISS is an evolution of the TIGER and SuperTIGER long-duration balloon instruments incorporating detector improvements from our previous Heavy-Nuclei Explorer SMEX, including silicon strip detectors in place of both scintiallator radiators and scintillating fibers. The performance of these new detector components was demonstrated at CERN/SPS beam tests and will provide TIGERISS with high fidelity charge assignment with σZ <0.25. All available ISS external attachment accommodations are currently under study, including those for the JAXA JEM-EF, the ESA Columbus Laboratory, and the NASA ELC. The TIGERISS geometry factor depends on attachment location (~1 to 1.6 m2 sr), but in one year the baseline instrument would obtain statistics comparable to the current SuperTIGER data set and expand measurements to higher and lower atomic numbers. TIGERISS measurements will be cleaner than SuperTIGER’s as they will not require corrections for atmospheric interactions and scintillator saturation effects. They will also give the first single-element resolution measurements of elements above 56Ba that with extended observations would test models for cosmic-ray origins and acceleration. The SuperTIGER UHGCR measurements through 40Zr have supported a model of CR origins in OB Associations with preferential acceleration of refractory elements more likely found in dust grains than volatiles superposed on Z dependence from grain sputtering injection in SN shocks, but more recent results from 41Nb to 56Ba are inconsistent with that model and require a difference in the acceleration mechanism and/or an additional r-process source. These UHGCR observations will cover elements produced in s-process and r-process neutron capture nucleosynthesis, adding to the multi-messenger effort to determine the relative contributions of supernovae (SN) and Neutron Star Merger (NSM) events to r-process nucleosynthesis. |
Tuesday, April 18, 2023 4:21PM - 4:33PM |
V14.00004: Status and Science Goals of EUSO-SPB2: An ULDB Experiment to Measure VHE- and UHE-Cosmic Rays and Search for VHE Cosmic Neutrinos John F Krizmanic, Angela V Olinto, Lawrence R Wiencke Scheduled to be launched in April-May 2023 from Wanaka, New Zealand, the Extreme Universe Space Observatory on a Super Pressure Balloon, 2nd generation (EUSO-SPB2) is constructed to observe extensive air showers (EAS) initiated by cosmic rays and cosmic neutrinos by measuring the EAS fluorescence or beamed, optical Cherenkov signals. These measurements are made by two custom wide-field of view, 1-meter diameter aperture telescopes: a nadir-pointing Fluorescence Telescope (FT) and an Earth-limb viewing Cherenkov Telescope (CT). The FT records the longitudinal evolution of UHECR EAS with 1 us sampling for E_CR > ~1 EeV, while also searching for fast (<<1 us) upward-moving optical EAS signals. The CT uses novel bifocal optics and is designed to measure the fast, 10 ns-scale Cherenkov signals from EAS with E > ~10 PeV generated either by VHECRs viewed above the Earth's limb or by tau neutrinos that interact in the Earth yielding EAS viewed below the limb. EUSO-SB2 has the capability to slew and tilt the CT to search for tau-neutrinos from target-of-opportunity, i.e. transient sources. Both telescopes are configured to measure and study the potential backgrounds to the science signals. The goals, status, test results, and capability of EUSO-SPB2 to make pioneering astroparticle physics measurements will be presented. |
Tuesday, April 18, 2023 4:33PM - 4:45PM |
V14.00005: Detector Performance of the Moon Burst Energetics All-sky Monitor Sarah J Dalessi Moon Burst Energetics All-sky Monitor (MoonBEAM) is a gamma-ray mission in a cislunar orbit to observe the entire sky instantaneously for relativistic astrophysical explosions. It is designed to explore the behavior of matter and energy under extreme conditions by observing the prompt emission from gamma-ray bursts, identifying the conditions capable of launching transient relativistic jets and the origins of high-energy radiation from the relativistic outflows. MoonBEAM utilizes a set of 6 phoswhich detectors to achieve all-sky nearly continuous coverage. The phoswich design allows for dual mode observations, for localization and a wide spectral coverage. In this talk I will discuss the initial calibration and lab validation on the detectors utilizing different radioactive sources. |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700