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 C13: Multimessenger Astronomy II |
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Sponsoring Units: DAP Chair: Justin Vandenbroucke, University of Wisconsin - Madison Room: Marquette IV - 2nd Floor |
Saturday, April 15, 2023 1:30PM - 1:42PM |
C13.00001: Searching for GRB Counterparts to Gravitational-wave Events from the Third Gravitational Wave Observing Run with Fermi-GBM and Swift-BAT Joshua R Wood We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) observations of gravitational-wave (GW) events detected during the third LIGO/Virgo/KAGRA Collaboration observing run (O3). Using Fermi-GBM on-board triggers as well as sub-threshold searches in both Fermi-GBM and Swift-BAT ground data, we search for coincident gamma-ray transients associated with the GW events. No new joint events were found. We therefore calculate flux upper limits for the associated gamma-ray luminosity of each GW event. Using the lack of electromagnetic (EM) emission from binary black hole (BBH) mergers, we begin to constrain theoretical models of any such emission. |
Saturday, April 15, 2023 1:42PM - 1:54PM |
C13.00002: bajes-mma: Joint Bayesian Inference Framework for Multi-Messenger Astronomy with Binary Neutron Star Coalescences Ssohrab Borhanian, Matteo Breschi, Gregorio Carullo, Giacomo Ricigliano, Lukas Lippold, Albino Perego, Sebastiano Bernuzzi The coincident observation of three events GW170817, GRB170817A, and AT2017gfo---a gravitational-wave signal with associated electromagnetic counterpart observed via a short gamma-ray burst, kilonova, and successive long-term afterglow emission---marked the onset of multi-messenger astronomy using gravitational and electromagnetic waves. The consequent analyses of these transient events provided a treasure trove of data shedding light onto the dense matter regime, cosmological measurements, and the accuracy of general relativity itself. In expectation of further multi-messenger events during upcoming observing runs by the LIGO, Virgo, and KAGRA observatories we developed a data analysis pipeline to jointly examine the observational data associated with a multi-messenger event. The pipeline is built on the Bayesian inference framework bajes and leverages its strength to incorporate any data channel, i.e. for binary neutron star mergers the gravitational waves signal and associated electromagnetic transients---including klionovae, short gamma-ray bursts, and synchrotron from the fast-tail of the ejecta. Using this pipeline we analyzed the events associated to GW170817 simultaneously to improve the parameter constraints of prior studies.
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Saturday, April 15, 2023 1:54PM - 2:06PM Withdrawn |
C13.00003: Joint Bayesian inference of gravitational-wave and NICER data Chaitanya Afle, Duncan A Brown, Ingo Tews, Collin Capano, Rahul Somasundaram We perform a joint, multi-messenger analysis of the neutron star equation of state by combining the gravitational-wave measurements of GW170817 with the measurements made by the Neutron Star Interior Composition Explorer (NICER) of PSR J0030+0451 and PSR J0740+6620. We develop a joint likelihood function that can simultaneously sample in the parameter space of the gravitational-wave and X-ray measurements. We incorporate models of the equation of state generated using chiral effective field theory into the joint GW/X-ray analysis. We sample the likelihood in equation of state and mass, which provides a direct measurement of chiral field theory equation of state. |
Saturday, April 15, 2023 2:06PM - 2:18PM |
C13.00004: Extracting the Neutron Star Equation of State from Theoretical and Observational Constraints Using Modified Gaussian Processes Debora Mroczek, Michael C Miller, Jacquelyn Noronha-Hostler, Nicolas Yunes Functional forms of the neutron star Equation of State (EoS) are required to extract the viable EoS band from neutron star observations. Typically, one of three methods are used-- spectral functions, piecewise polytropes, or gaussian processes. However, realistic nuclear EoS, containing deconfined quarks or hyperons, present nontrivial features in the speed of sound such as bumps, kinks and plateaus. These features in the speed of sound are difficult to capture using previous methods [1]. We modify gaussian processes by introducing spikes and plateaus in the speed of sound and check how those features impact the posterior distribution obtained using constraints from NICER, gravitational-wave observations, and perturbative QCD. We find that introducing modifications to the EoS plays a role in understanding the possible phase structure of neutron stars at densities around twice saturation density. |
Saturday, April 15, 2023 2:18PM - 2:30PM |
C13.00005: Neutron star merger ejecta estimation with kilonova light curve surrogates Atul Kedia, Marko Ristic, Richard O'Shaughnessy, Ryan Wollaeger, Anjali Balasaheb Yelikar, Oleg Korobkin, Eve Chase, Chris L Fryer, Christopher J Fontes The observation of GW170817 sparked the era of multi-messenger astrophysics when a merger of two neutron stars was observed by both gravitational wave detection and its electromagnetic counterpart, the kilonova emission. Such neutron star mergers enrich the environment with neutron rich material. The mass and velocity of the ejecta material can be inferred independently from both the kilonova emission and the gravitational wave observation, however, those inferred from the kilonova AT2017gfo has been in tension with the properties inferred based on the gravitational wave signal GW170817. In this talk, we will present the newly developed surrogate models for light curves resulting from 2-D kilonova simulations (SuperNu) made for a large set of ejecta outflow morphologies and compositions. We use these models to then calculate the inferred ejecta properties, which helps identify the effect of morphologies and composition in this tension. We find that due to these additional ejecta models the tension is alleviated to some extent but there still remains significant disagreement. We will also show the capabilities of our surrogate models that can produce LCs for a range of ejecta component velocities, viewing angles, and at any broadband filter within a range of wavelengths. |
Saturday, April 15, 2023 2:30PM - 2:42PM |
C13.00006: Multi-Messenger Diagnostics of the Supernova Engine Chris L Fryer, Eric Burns, Aimee Hungerford Core-collapse supernovae play important roles in a wide range of astrophysics including transient outbursts that probe stellar evolution, the formation of compact remnants and the production and injection of heavy elements into the galaxy. Understanding these roles requires an understanding of the supernova engine. In this talk, I will review the current status of the theories behind supernova explosions and the observational constraints (both past and future) that can be used to confirm these engines and probe the extreme physics behind them. A broad range of observations exist from direct (but difficult to obtain) probes to indirect probes for which we can obtain much more data. We will discuss these different probes and the physics modeling required to apply them to our understanding of the physics behind the supernova engine. |
Saturday, April 15, 2023 2:42PM - 2:54PM |
C13.00007: GW170817: Is its Host Galaxy an Interloper? David Wright, Shivani Shah, Stephen Eikenberry, Paul Torrey, Anthony Gonzalez Observation of the GW170817 NS-NS merger presented the first opportunity to measure H0 using gravitational waves; furthermore, it offered a method for resolving the Hubble tension. However, in order to break the tension we must first develop a robust understanding of the errors and uncertainties inherent to such measurements. The error on H0 measurements using gravitational wave events is comprised of two components: (i) rigorously-modeled statistical and systematic errors in the standard siren distance and (ii) error in the Hubble velocity measurement. Because the Hubble velocity cannot be directly observed, it must instead be estimated by indirect means. If this estimation is not done carefully, it is easy to introduce unaccounted systematic biases in the Hubble velocity and therefore H0. One possible source of such error is the incorrect association of galaxies with a host group, which could severely impact peculiar velocity corrections to the Hubble velocity measurement. By applying the grouping algorithm used in the 2MASS Redshift Survey (2MRS) group catalog to cosmological simulations, we investigate the possibility that NGC4993, the host galaxy of GW170817, is incorrectly associated with its group in the 2MRS group catalog. For groups of similar mass to the NGC4993 group, we find that the probability for incorrect association of group members is significant. We present our methods in detail and discuss techniques to obtain realistic Hubble velocities for future H0 measurements. |
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