Bulletin of the American Physical Society
APS New England Section 2018 Fall Meeting
Volume 63, Number 21
Friday–Saturday, November 2–3, 2018; University of Massachusetts Dartmouth, Dartmouth, Massachusetts
Session C02: Gravity I |
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Room: CCB Building 248 |
Saturday, November 3, 2018 10:00AM - 10:12AM |
C02.00001: Characterization of low-significance gravitational-wave compact binary sources Yiwen Huang, Hannah Middleton, Ken K. Y. Ng, Salvatore Vitale, John Veitch Advanced LIGO and Advanced Virgo will start their third observing run early 2019. Given our current rate estimates, we expect the detection of a binary black hole signal every week. The majority of these sources will be far away, and thus have low signal-to-noise ratios (SNRs). In this talk we show if, and to which extent, the physical parameters of neutron stars and black holes in binaries can be measured at low SNRs. We find that sub-threshold binary neutron stars, with SNRs below 12 (10), yield uncertainties in their sky position larger than 400 (700) deg2 (90% credible interval), making electromagnetic follow-ups difficult in bands other than radio. The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for binary neutron stars and neutron star black hole mergers. We will also show that we may be able to recover some information for intrinsic parameters, masses and spins, at SNRs as low as 6, but multimodality is not uncommon and can significantly broaden the posteriors. For spins, in particular, the uncertainty is higher for systems with comparable component masses or lack of spin precession. |
Saturday, November 3, 2018 10:12AM - 10:24AM |
C02.00002: Neutron Star Equation of State Constrained by Gravitational Waves William Spinella, Fridolin Weber A little over one year ago gravitational (GW170817) and electromagnetic waves emitted by a binary neutron star (BNS) merger were first observed. Analyses of these observations have led to new estimates of the maximum mass and canonical radius of neutron stars, placing strict constraints on the equation of state of dense matter. In this short talk we discuss the composition of neutron star matter in light of these new constraints, focusing on the possible presence of hyperons. We use an equation of state modeled using the relativistic mean-field approximation and parameterized for consistency with constraints from theoretical and experimental nuclear physics and neutron star observations. We find that hyperonic neutron star matter is not ruled out by analyses of the BNS merger, but that the presence and abundance of hyperons depend on the choice of the vector meson-hyperon coupling constants. |
Saturday, November 3, 2018 10:24AM - 10:36AM |
C02.00003: Exploring Convolutional Neural Networks for Gravitational Wave data analysis Dwyer S S Deighan Gravitational wave astronomy can benefit from the rapid classification of gravitational wave signals buried deep in instrumentation noise. In 2017, George and Heurata (and since then other researchers) have considered Convolutional Neural Networks to detect gravitational waves signals and estimate some of the corresponding binary's parameters (i.e. distance, total mass, mass ratio and orientation in the sky). In this talk I will summarize efforts to extend this classification and prediction strategy. In particular, we discuss strategies to optimize the hyper parameters of our network, in an attempt to make our networks as compact and effective as possible. Preliminary results will be discussed for some simple setups. |
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