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We present ${tt bajes}$, a parallel and lightweight framework for Bayesian inference of multimessenger transients. ${tt bajes}$ is a Python modular package with minimal dependencies on external libraries adaptable to the majority of the Bayesian models and to various sampling methods. We describe the general workflow and the parameter estimation pipeline for compact-binary-coalescence gravitational-wave transients. The latter is validated against injections of binary black hole and binary neutron star waveforms, including confidence interval tests that demonstrates the inference is well-calibrated. Binary neutron star postmerger injections are also studied using a network of five detectors made of LIGO, Virgo, KAGRA and Einstein Telescope. Postmerger signals will be detectable for sources at ${lesssim}80,$Mpc, with Einstein Telescope contributing over 90% of the total signal-to-noise ratio. As a full scale application, we re-analyze the GWTC-1 black hole transients using the effective-one-body ${tt TEOBResumS}$ approximant, and reproduce selected results with other approximants. ${tt bajes}$ inferences are consistent with previous results; the direct comparison of ${tt bajes}$ and ${tt bilby}$ analyses of GW150914 shows a maximum Jensen-Shannon divergence of $5.2{times}10^{-4}$. GW170817 is re-analyzed using ${tt TaylorF2}$ with 5.5PN point-mass and 7.5PN tides, ${tt TEOBResumSPA}$, and ${tt IMRPhenomPv2_NRTidal}$ with different cutoff-frequencies of $1024,$Hz and $2048,$Hz. We find that the former choice minimizes systematics on the reduced tidal parameter, while a larger amount of tidal information is gained with the latter choice. ${tt bajes}$ can perform these analyses in about 1~day using 128 CPUs.
Third-generation (3G) gravitational-wave detectors will observe thousands of coalescing neutron star binaries with unprecedented fidelity. Extracting the highest precision science from these signals is expected to be challenging owing to both high si
A central challenge in Gravitational Wave Astronomy is identifying weak signals in the presence of non-stationary and non-Gaussian noise. The separation of gravitational wave signals from noise requires good models for both. When accurate signal mode
The Neutron Star Interior Composition Explorer (NICER) recently measured the mass and equatorial radius of the isolated neutron star PSR J0030+0451. We use these measurements to infer the moment of inertia, the quadrupole moment, and the surface ecce
Gravitational wave data from ground-based detectors is dominated by instrument noise. Signals will be comparatively weak, and our understanding of the noise will influence detection confidence and signal characterization. Mis-modeled noise can produc
The RIT numerical relativity group is releasing the second public catalog of black-hole-binary waveforms url{http://ccrg.rit.edu/~RITCatalog}. This release consists of 320 accurate simulations that include 46 precessing and 274 nonprecessing binary s