{"work":{"id":"9f5dc319-2492-4e65-b851-c5fa7e4e3b44","openalex_id":null,"doi":null,"arxiv_id":"1311.0420","raw_key":null,"title":"TIGER: A data analysis pipeline for testing the strong-field dynamics of general relativity with gravitational wave signals from coalescing compact binaries","authors":null,"authors_text":"M","year":2013,"venue":"gr-qc","abstract":"The direct detection of gravitational waves with upcoming second-generation gravitational wave detectors such as Advanced LIGO and Virgo will allow us to probe the genuinely strong-field dynamics of general relativity (GR) for the first time. We present a data analysis pipeline called TIGER (Test Infrastructure for GEneral Relativity), which is designed to utilize detections of compact binary coalescences to test GR in this regime. TIGER is a model-independent test of GR itself, in that it is not necessary to compare with any specific alternative theory. It performs Bayesian inference on two hypotheses: the GR hypothesis $\\mathcal{H}_{\\rm GR}$, and $\\mathcal{H}_{\\rm modGR}$, which states that one or more of the post-Newtonian coefficients in the waveform are not as predicted by GR. By the use of multiple sub-hypotheses of $\\mathcal{H}_{\\rm modGR}$, in each of which a different number of parameterized deformations of the GR phase are allowed, an arbitrarily large number of 'testing parameters' can be used without having to worry about a model being insufficiently parsimonious if the true number of extra parameters is in fact small. TIGER is well-suited to the regime where most sources have low signal-to-noise ratios, again through the use of these sub-hypotheses. Information from multiple sources can trivially be combined, leading to a stronger test. We focus on binary neutron star coalescences, for which sufficiently accurate waveform models are available that can be generated fast enough on a computer to be fit for use in Bayesian inference. We show that the pipeline is robust against a number of fundamental, astrophysical, and instrumental effects, such as differences between waveform approximants, a limited number of post-Newtonian phase contributions being known, the effects of neutron star spins and tidal deformability on the orbital motion, and instrumental calibration errors.","external_url":"https://arxiv.org/abs/1311.0420","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-05-23T23:58:38.593071+00:00","pith_arxiv_id":"1311.0420","created_at":"2026-05-09T06:19:14.415245+00:00","updated_at":"2026-05-23T23:58:38.593071+00:00","title_quality_ok":true,"display_title":"Agathos, W","render_title":"Agathos, W"},"hub":{"state":{"work_id":"9f5dc319-2492-4e65-b851-c5fa7e4e3b44","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":13,"external_cited_by_count":null,"distinct_field_count":1,"first_pith_cited_at":"2019-03-11T17:43:43+00:00","last_pith_cited_at":"2026-05-12T07:58:35+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-01T12:53:30.174939+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"background","n":7},{"context_role":"method","n":1}],"polarity_counts":[{"context_polarity":"background","n":6},{"context_polarity":"unclear","n":1},{"context_polarity":"use_method","n":1}],"runs":{},"summary":{},"graph":{},"authors":[]}}