Bulletin of the American Physical Society
2020 Annual Meeting of the APS Four Corners Section (Virtual)
Volume 65, Number 16
Friday–Saturday, October 23–24, 2020; Albuquerque, NM (Virtual)
Session E01: Astrophysics IILive
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Chair: Brandon Wiggins, SUU |
Friday, October 23, 2020 2:00PM - 2:24PM Live |
E01.00001: Simulating the First Water in the Universe Invited Speaker: Brandon Wiggins It is now believed that as much as 50\% of the solar system’s water may have predated the Sun, suggesting an ancient heritage for this life-giving substance. This raises questions about the abundance of water throughout the universe, and touches on the question of the cosmic conditions in which this ingredient for the rise of life first appeared. In this talk, I will summarize efforts, now 4 years in the making and spanning 5 institutions, to create the first simulation of the rise of water in the early universe. We couple a fully implicit chemical reaction network, including 50 reactants and now 350 reactions, inline with an Eulerian cosmology code. I’ll present state-of-the-art visualizations of our initial simulation results of water appearing in its first cosmological context in the very early universe and will discuss implications of our results. [Preview Abstract] |
Friday, October 23, 2020 2:24PM - 2:36PM Live |
E01.00002: TeV astrophysics with the HAWC observatory Mora Durocher The High Altitude Water Cherenkov (HAWC) Observatory, located in central Mexico at 4100 m above sea level, is sensitive to gamma rays from 300 GeV to more than 100 TeV and continuously observes a wide field-of-view ($\sim$ 2 sr). With its high energy reach and large area coverage, HAWC is well-suited to perform unbiased surveys of the TeV sky. This had lead to numerous studies: cataloging and classifying TeV gamma-ray sources, setting limits on Dark Matter and the Diffuse Gamma-Ray Background, and investigating galactic and extragalactic extended sources as well as high-energy particle acceleration sites. This presentation will be an overview of HAWC's latest findings on these subjects. [Preview Abstract] |
Friday, October 23, 2020 2:36PM - 2:48PM Live |
E01.00003: Obtaining Dark Matter Distribution from the Milky Way's rotation curve Alec Hewitt, Pearl Sandick Gaia offers a plethora of new data to explore. In this presentation we apply method’s of galkin to a larger data set obtained from Gaia DR2, selecting stars within 100 pc of the galactic plane. This data set is further constrained to select stars with sufficiently circular velocities by requiring radial velocity to be small. The rotation curve is obtained, the baryonic component is subtracted off and modeled using RBR morphology. From this resulting curve we obtain parameters using NFW profile. These results agree with the compilation of 12 data sets called galkin12. [Preview Abstract] |
Friday, October 23, 2020 2:48PM - 3:00PM Live |
E01.00004: Presupernova neutrinos: directional sensitivity and prospects for progenitor identification Mainak Mukhopadhyay, Cecilia Lunardini, Frank Timmes, Kai Zuber We explore the potential of current and future liquid scintillator neutrino detectors of $\mathcal O (10)$ kt mass to localize a pre-supernova neutrino signal in the sky. In the hours preceding the core collapse of a nearby star (at distance $D < 1$ kpc), tens to hundreds of inverse beta decay events will be recorded, and their reconstructed topology in the detector can be used to estimate the direction to the star. Although the directionality of inverse beta decay is weak ($\sim$8 % forward-backward asymmetry for currently available liquid scintillators), we find that for a fiducial signal of $200$ events (which is realistic for Betelgeuse), a positional error of $\sim$60$^\circ$ can be achieved, resulting in the possibility to narrow the list of potential stellar candidates to less than ten, typically. For a configuration with improved forward-backward asymmetry ($\sim$40 %, as expected for a lithium-loaded liquid scintillator), the angular sensitivity improves to $\sim$15$^\circ$, and -- when a distance upper limit is obtained from the overall event rate -- it is in principle possible to uniquely identify the progenitor star. Any localization information accompanying an early supernova alert will be useful to multi-messenger observations and to particle physics tests. [Preview Abstract] |
Friday, October 23, 2020 3:00PM - 3:12PM Live |
E01.00005: G-mode slope estimation from gravitational waves produced by Core Collapse Supernovae Michael Benjamin, Michele Zanolin, Joshua Freed, Marek Szczepanczyk, Manuel David Morales Gravitational wave physics is one of the newest and most unknown fields of physics in the modern day. The analysis of raw interferometric data has specific problems that require new research order to extract and interpret the astrophysical information. In this project, we will be assessing the capacity to characterize vibrational modes of Neutron stars forming at the center of a core collapse supernova, which are called g-modes, and specifically tracking the early slope and the late slope of the g-mode in the presence of noisy interferometric data. The g-mode of a supernova is one of three modes of oscillation that a proton-neutron star experiences when it goes supernova and is the dominant one in the LIGO signature band. The primary tool that will be used is a software package called Adaptive Wavelet Clustering. We will be using this clustering algorithm to find a least square fit to the curve of the g-mode. Adaptive Wavelet Clustering is a novel clustering technique produced by Chen et al. described in the paper "Adaptive Wavelet Clustering for Highly Noisy Data." [Preview Abstract] |
Friday, October 23, 2020 3:12PM - 3:24PM |
E01.00006: Gravitational Wave Calibration Error for Supernovae Core Collapse Brad Ratto In order to detect Gravitational Waves (GWs), laser interferometers measure microscopic deformations in space-time caused by transient GWs. However, it is important to realize that interferometers, like any measurement device, introduce distortion in the recorded signals. The recorded signal is a convolution of the laser intensity with a calibration function, where the calibration function contains amplitude and phase errors at every frequency. The maximum amplitude of these errors is documented, but the relationship between the phase and amplitude errors of neighboring frequencies is not well understood. In order to understand this relationship, a plugin in coherent Wave Burst (cWB), a data analysis tool, was developed that allows for frequency and detector dependent calibration errors to be injected into simulated waveforms. This presentation aims to study the impact of this relationship for GWs from core-collapse supernovae (CCSN) and establish realistic correlations of phase calibration errors with frequency. [Preview Abstract] |
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