Environmental seismic disturbances limit the sensitivity of LIGO gravitational wave detectors. Trains near the LIGO Livingston detector produce low frequency (0.5–
We demonstrate how to quantify the frequencydomain amplitude and phase accuracy of waveform models,
 Award ID(s):
 2110441
 NSFPAR ID:
 10415585
 Publisher / Repository:
 IOP Publishing
 Date Published:
 Journal Name:
 Classical and Quantum Gravity
 Volume:
 40
 Issue:
 13
 ISSN:
 02649381
 Page Range / eLocation ID:
 Article No. 135002
 Format(s):
 Medium: X
 Sponsoring Org:
 National Science Foundation
More Like this

Abstract ) ground noise that couples into the gravitational wave sensitive frequency band (10– $10\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ ) through light reflected in mirrors and other surfaces. We investigate the effect of trains during the Advanced LIGO third observing run, and propose a method to search for narrow band seismic frequencies responsible for contributing to increases in scattered light. Through the use of the linear regression tool Lasso (least absolute shrinkage and selection operator) and glitch correlations, we identify the most common seismic frequencies that correlate with increases in detector noise as 0.6– $100\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ , 1.7– $0.8\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ , 1.8– $1.9\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ , and 2.3– $2.0\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ in the LIGO Livingston corner station. $2.5\text{\hspace{0.17em}}\mathrm{H}\mathrm{z}$ 
Abstract We present the second data release of gravitational waveforms from binary neutron star (BNS) merger simulations performed by the Computational Relativity (
CoRe ) collaboration. The current database consists of 254 different BNS configurations and a total of 590 individual numericalrelativity simulations using various grid resolutions. The released waveform data contain the strain and the Weyl curvature multipoles up to . They span a significant portion of the mass, massratio, spin and eccentricity parameter space and include targeted configurations to the events GW170817 and GW190425. $\ell =m=4$CoRe simulations are performed with 18 different equations of state, seven of which are finite temperature models, and three of which account for nonhadronic degrees of freedom. About half of the released data are computed with highorder hydrodynamics schemes for tens of orbits to merger; the other half is computed with advanced microphysics. We showcase a standard waveform error analysis and discuss the accuracy of the database in terms of faithfulness. We present readytouse fitting formulas for equation of stateinsensitive relations at merger (e.g. merger frequency), luminosity peak, and postmerger spectrum. 
Abstract We present a measurement of the Hubble Constant
H _{0}using the gravitational wave event GW190412, an asymmetric binary black hole merger detected by LIGO/Virgo, as a dark standard siren. This event does not have an electromagnetic counterpart, so we use the statistical standard siren method and marginalize over potential host galaxies from the Dark Energy Spectroscopic Instrument (DESI) survey. GW190412 is welllocalized to 12 deg^{2}(90% credible interval), so it is promising for a dark siren analysis. The dark siren value for km s^{−1} Mpc^{−1}, with a posterior shape that is consistent with redshift overdensities. When combined with the bright standard siren measurement from GW170817 we recover ${H}_{0}={85.4}_{33.9}^{+29.1}$ km s^{−1} Mpc^{−1}, consistent with both early and latetime Universe measurements of ${H}_{0}={77.96}_{5.03}^{+23.0}$H _{0}. This work represents the first standard siren analysis performed with DESI data, and includes the most complete spectroscopic sample used in a dark siren analysis to date. 
An advanced LIGO and Virgo’s third observing run brought another binary neutron star merger (BNS) and the first neutronstar black hole mergers. While no confirmed kilonovae were identified in conjunction with any of these events, continued improvements of analyses surrounding GW170817 allow us to project constraints on the Hubble Constant (more » « less
H _{0}), the Galactic enrichment fromr process nucleosynthesis, and ultradense matter possible from forthcoming events. Here, we describe the expected constraints based on the latest expected event rates from the international gravitationalwave network and analyses of GW170817. We show the expected detection rate of gravitational waves and their counterparts, as well as how sensitive potential constraints are to the observed numbers of counterparts. We intend this analysis as support for the community when creating scientifically driven electromagnetic followup proposals. During the next observing run O4, we predict an annual detection rate of electromagnetic counterparts from BNS of ( ${0.43}_{0.26}^{+0.58}$ ) for the Zwicky Transient Facility (Rubin Observatory). ${1.97}_{1.2}^{+2.68}$ 
Abstract The best upper limit for the electron electric dipole moment was recently set by the ACME collaboration. This experiment measures an electron spinprecession in a cold beam of ThO molecules in their metastable
state. Improvement in the statistical and systematic uncertainties is possible with more efficient use of molecules from the source and better magnetometry in the experiment, respectively. Here, we report measurements of several relevant properties of the longlived $H\phantom{\rule{0.50em}{0ex}}{(}^{3}{\mathrm{\Delta}}_{1})$ state of ThO, and show that this state is a very useful resource for both these purposes. The $Q\phantom{\rule{0.50em}{0ex}}{(}^{3}{\mathrm{\Delta}}_{2})$Q state lifetime is long enough that its decay during the time of flight in the ACME beam experiment is negligible. The large electric dipole moment measured for theQ state, giving rise to a large linear Stark shift, is ideal for an electrostatic lens that increases the fraction of molecules detected downstream. The measured magnetic moment of theQ state is also large enough to be used as a sensitive comagnetometer in ACME. Finally, we show that theQ state has a large transition dipole moment to the state, which allows for efficient population transfer between the ground state $C\phantom{\rule{0.50em}{0ex}}{(}^{1}{\mathrm{\Pi}}_{1})$ and the $X\phantom{\rule{0.50em}{0ex}}{(}^{1}{\mathrm{\Sigma}}^{+})$Q state via Stimulated Raman Adiabatic Passage (STIRAP). We demonstrate 90 % STIRAP transfer efficiency. In the course of these measurements, we also determine the magnetic moment of $XCQ$C state, the transition dipole moment, and branching ratios of decays from the $X\to C$C state.