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In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid- and high- frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.","external_url":"https://arxiv.org/abs/1411.4547","cited_by_count":null,"metadata_source":"pith","metadata_fetched_at":"2026-07-04T19:40:06.484660+00:00","pith_arxiv_id":"1411.4547","created_at":"2026-05-09T02:57:49.756266+00:00","updated_at":"2026-07-04T19:40:06.484660+00:00","title_quality_ok":false,"display_title":"Advanced LIGO","render_title":"Advanced LIGO"},"hub":{"state":{"work_id":"b93186e6-8d0a-440a-aa48-9de6dbff57b9","tier":"super_hub","tier_reason":"100+ Pith inbound or 10,000+ external citations","pith_inbound_count":138,"external_cited_by_count":null,"distinct_field_count":9,"first_pith_cited_at":"2019-03-11T17:43:43+00:00","last_pith_cited_at":"2026-07-01T18:34:19+00:00","author_build_status":"needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-08-20T20:59:19.700738+00:00","tier_text":"super_hub"},"tier":"super_hub","role_counts":[{"context_role":"background","n":50},{"context_role":"method","n":4},{"context_role":"other","n":1}],"polarity_counts":[{"context_polarity":"background","n":47},{"context_polarity":"use_method","n":4},{"context_polarity":"unclear","n":3},{"context_polarity":"support","n":1}],"runs":{"ask_index":{"job_type":"ask_index","status":"succeeded","result":{"title":"Advanced LIGO","claims":[{"claim_text":"The Advanced LIGO gravitational wave detectors are second generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA. 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These considerations should be useful to inform the development of the XG detector network. I. INTRODUCTION In the past decade, the observation of the gravitational- wave (GW) signal emitted by compact binary coalescences (CBCs) gave us a new tool to study the Universe. With more than 200 event candidates observed by the LIGO [1], Virgo [2], and KAGRA [3] (LVK) detectors, the GWs give us insight into the demography of masses, redshifts, and spins of compac","claim_type":"background","confidence":0.95,"evidence_strength":"citation_context"},{"claim_text":"Space Antenna (LISA) and TianQin may be sensitive to 0.1-100 mHz GWs, while next-generation Earth-based missions such as Cosmic Explorer (CE) and Einstein Telescope (ET) will push the lower limit of ground-based sensitivity to a few Hz [21-24]. Still, seismic and grav- ity gradient noises severely limit ground-based detector sensitivity below∼1 Hz [2, 25, 26]. 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Capano, Astrophys. J.946, 59 (2023), arXiv:2112.06878 [astro-ph.HE]. [6] R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]. [7] B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]. [8] J. Aasiet al.(LIGO Scientific), Class. Quant. Grav.32, 074001 (2015), arXiv:1411.4547 [gr-qc]. [9] F. Acerneseet al.(VIRGO), Class. Quant. Grav.32","claim_type":"background","confidence":0.9,"evidence_strength":"citation_context"},{"claim_text":"improved sensitivity will allow the detection of additional subdominant modes. To address these challenges, we adopt the semiana- lytic method based on orthonormalized QNMs, which reduces parameter degeneracies and accelerates compu- tations [76]. In this paper, we apply this approach to the event GW250114 082203, henceforth GW250114 [15]. 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