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Field", "name": "Scott E. Field", "type": "personal" } }, { "person_or_org": { "family_name": "Chad R. Galley", "name": "Chad R. Galley", "type": "personal" } }, { "person_or_org": { "family_name": "Jan S. Hesthaven", "name": "Jan S. Hesthaven", "type": "personal" } }, { "person_or_org": { "family_name": "Jason Kaye", "name": "Jason Kaye", "type": "personal" } }, { "person_or_org": { "family_name": "Manuel Tiglio", "name": "Manuel Tiglio", "type": "personal" } }, { "person_or_org": { "family_name": "Jonathan Blackman", "name": "Jonathan Blackman", "type": "personal" } }, { "person_or_org": { "family_name": "B\u00e9la Szil\u00e1gyi", "name": "B\u00e9la Szil\u00e1gyi", "type": "personal" } }, { "person_or_org": { "family_name": "Mark A. Scheel", "name": "Mark A. Scheel", "type": "personal" } }, { "person_or_org": { "family_name": "Daniel A. Hemberger", "name": "Daniel A. Hemberger", "type": "personal" } }, { "person_or_org": { "family_name": "Patricia Schmidt", "name": "Patricia Schmidt", "type": "personal" } }, { "person_or_org": { "family_name": "Rory Smith", "name": "Rory Smith", "type": "personal" } }, { "person_or_org": { "family_name": "Christian D. Ott", "name": "Christian D. Ott", "type": "personal" } }, { "person_or_org": { "family_name": "Michael Boyle", "name": "Michael Boyle", "type": "personal" } }, { "person_or_org": { "family_name": "Lawrence E. Kidder", "name": "Lawrence E. Kidder", "type": "personal" } }, { "person_or_org": { "family_name": "Harald P. Pfeiffer", "name": "Harald P. Pfeiffer", "type": "personal" } }, { "person_or_org": { "family_name": "Vijay Varma", "name": "Vijay Varma", "type": "personal" } } ], "description": "
This repository contains all publicly available numerical relativity surrogate data for waveforms\n produced by the\n Spectral Einstein Code\n . The base method for building surrogate models can be found in\n Field et al., PRX 4,\n 031006 (2014)\n .\n
\n\nSeveral numerical relativity surrogate models are currently available in this catalog:\n
\n\nNRSur7dq4.h5 — This is a surrogate model for binary black hole mergers with\n\t generic spins and mass ratios up to 4. A paper describing it can be found at\n Varma et al., arxiv:1905.09300\n . It is evaluated with the gwsurrogate Python package, which can be found on\n PyPI\n . Instructions for evaluating this surrogate can be found at\n this example\n IPython code\n .\n
\nNRHybSur3dq8.h5 — This is a surrogate model for binary black hole systems\n\t with generic mass ratios but restricted to nonprecessing spins. Before constructing\n\t the surrogate, the NR waveforms are hybridized with post-Newtonian waveforms to\n\t include the early inspiral. Therefore this model covers the full stellar mass range\n\t for ground-based detectors. A paper describing it can be found at\n Varma\n et al., PRD 99, 064045 (2019)\n . It is evaluated with the gwsurrogate Python package, which can be\n found on\n PyPI\n . Instructions for evaluating this surrogate can be found this\n example\n IPython code\n .\n
\nNRSur7dq4Remnant — This is a surrogate model for mass, spin, and recoil\n\t kick velocity of the remnant BH left behind in generically precessing binary black\n\t hole mergers, with mass ratios up to 4. A paper describing it can be found at\n Varma et al., arxiv:1905.09300\n . It is evaluated with the surfinBH Python package, which can be found on\n PyPI\n . Installation instructions and an ipython help notebook can be found in the\n same link.\n
\nSpEC_q1_10_NoSpin_nu5thDegPoly_exclude_2_0.h5 — A surrogate model for\n\t binary black hole mergers with non-spinning black holes. This is describedin\n Blackman\n et al., PRL115, 121102 (2015)\n . It is evaluated with the gwsurrogate python package, which can be found on\n PyPI\n . Instructions for evaluating this surrogate can be found in tutorials\n included with the gwsurrogate package and in this\n example\n IPython code\n .\n
\nNRSur4d2s_FDROM_grid12.h5 and NRSur4d2s_TDROM_grid12.h5 — These are fast\n\t frequency-domain and time-domain (respectively) surrogate models for binary black\n\t hole mergers where the black holes may be spinning, but the spins are restricted to\n\t a parameter subspace which includes some but not all precessing\n\t configurations. NRSur4d2s_FDROM_grid12.h5 is the NRSur4d2s_FDROM model described in\n Blackman et al., PRD 95,\n 104023, (2017)\n , and NRSur4d2s_TDROM_grid12.h5 is built from the underlying (slower)\n NRSur4d2s time-domain model in the same way but without the FFTs. These surrogates\n are also evaluated using gwsurrogate, and a tutorial can be found in this\n example\n IPython code\n .\n
\nNRSur7dq2.h5 — This is a surrogate model for binary black hole mergers with\n\t generic spins. A paper describing it can be foundat\n Blackman et al., PRD 96,\n 024058 (2017)\n . This surrogate is evaluated through a standalone python package contained in\n NRSur7dq2.tar.gz, which has simple installation instructions in its README file. A\n tutorial can be found for evaluating this surrogate in this\n example\n IPython code\n .\n
\n\n
\n\n\n
\n\nIf you find these surrogate models useful in your own research please cite the Field et al., PRX\n (2014) paper as well as the relevant paper describing the specific numerical relativity surrogate\n model, if available (e.g., the Blackman et al. 2015 paper for non-spinning binary black hole\n coalescences).\n
\n\nCaveats:\n
\n\nEvaluating surrogate models outside of the ranges they were trained upon may give\n inaccurate results. Please use with caution when extrapolating.\n
\nThe surrogate data available here for non-spinning binary black holes produced in\n Blackman et al. 2015 contains the (2,0) mode. However, this mode was not used in the\n paper. While this surrogate can predict a (2,0) mode, current numerical relativity\n simulations may not yet be able to accumulate (non-oscillatory) Christodoulou memory\n sufficiently. The surrogate (2,0) mode is founded upon basis SpEC waveforms that have been\n hybridized with leading order post-Newtonian waveforms. Therefore, the (2,0) mode can be\n included in the mode’s output but should be used with caution. Currently, the default\n option to evaluate this surrogate (using GWSurrogate) is to exclude all m=0 modes.\n
\nThis community simply collects results published by the SXS collaboration; requests from outside of this collaboration are not accepted.
\r\n", "page": "The SXS project is a collaborative research effort involving multiple institutions. Our goal is the simulation of black holes and other extreme spacetimes to gain a better understanding of Relativity, and the physics of exotic objects in the distant cosmos.
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