LIGO Detector Characterization in the Second and Third Observing Runs. (arXiv:2101.11673v2 [astro-ph.IM] UPDATED)

LIGO Detector Characterization in the Second and Third Observing Runs. (arXiv:2101.11673v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Davis_D/0/1/0/all/0/1">D. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Areeda_J/0/1/0/all/0/1">J. S. Areeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_B/0/1/0/all/0/1">B. K. Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruntz_R/0/1/0/all/0/1">R. Bruntz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Effler_A/0/1/0/all/0/1">A. Effler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Essick_R/0/1/0/all/0/1">R. C. Essick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fisher_R/0/1/0/all/0/1">R. P. Fisher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Godwin_P/0/1/0/all/0/1">P. Godwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goetz_E/0/1/0/all/0/1">E. Goetz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Helmling_Cornell_A/0/1/0/all/0/1">A. F. Helmling-Cornell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughey_B/0/1/0/all/0/1">B. Hughey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katsavounidis_E/0/1/0/all/0/1">E. Katsavounidis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lundgren_A/0/1/0/all/0/1">A. P. Lundgren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macleod_D/0/1/0/all/0/1">D. M. Macleod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marka_Z/0/1/0/all/0/1">Z. Márka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massinger_T/0/1/0/all/0/1">T. J. Massinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matas_A/0/1/0/all/0/1">A. Matas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McIver_J/0/1/0/all/0/1">J. McIver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mo_G/0/1/0/all/0/1">G. Mo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mogushi_K/0/1/0/all/0/1">K. Mogushi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nguyen_P/0/1/0/all/0/1">P. Nguyen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nuttall_L/0/1/0/all/0/1">L. K. Nuttall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schofield_R/0/1/0/all/0/1">R. M. S. Schofield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shoemaker_D/0/1/0/all/0/1">D. H. Shoemaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soni_S/0/1/0/all/0/1">S. Soni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stuver_A/0/1/0/all/0/1">A. L. Stuver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urban_A/0/1/0/all/0/1">A. L. Urban</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valdes_G/0/1/0/all/0/1">G. Valdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walker_M/0/1/0/all/0/1">M. Walker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_R/0/1/0/all/0/1">R. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_R/0/1/0/all/0/1">R. X. Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ananyeva_A/0/1/0/all/0/1">A. Ananyeva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Appert_S/0/1/0/all/0/1">S. Appert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arai_K/0/1/0/all/0/1">K. Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asali_Y/0/1/0/all/0/1">Y. Asali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aston_S/0/1/0/all/0/1">S. M. Aston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austin_C/0/1/0/all/0/1">C. Austin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baer_A/0/1/0/all/0/1">A. M. Baer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ball_M/0/1/0/all/0/1">M. Ball</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballmer_S/0/1/0/all/0/1">S. W. Ballmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banagiri_S/0/1/0/all/0/1">S. Banagiri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barker_D/0/1/0/all/0/1">D. Barker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barschaw_C/0/1/0/all/0/1">C. Barschaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barsotti_L/0/1/0/all/0/1">L. Barsotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartlett_J/0/1/0/all/0/1">J. Bartlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Betzwieser_J/0/1/0/all/0/1">J. Betzwieser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beda_R/0/1/0/all/0/1">R. Beda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharjee_D/0/1/0/all/0/1">D. Bhattacharjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bidler_J/0/1/0/all/0/1">J. Bidler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Billingsley_G/0/1/0/all/0/1">G. Billingsley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biscans_S/0/1/0/all/0/1">S. Biscans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blair_C/0/1/0/all/0/1">C. D. Blair</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blair_R/0/1/0/all/0/1">R. M. Blair</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bode_N/0/1/0/all/0/1">N. Bode</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Booker_P/0/1/0/all/0/1">P. Booker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bork_R/0/1/0/all/0/1">R. Bork</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bramley_A/0/1/0/all/0/1">A. Bramley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_A/0/1/0/all/0/1">A. F. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_D/0/1/0/all/0/1">D. D. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buikema_A/0/1/0/all/0/1">A. Buikema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cahillane_C/0/1/0/all/0/1">C. Cahillane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Callister_T/0/1/0/all/0/1">T. A. Callister</a>, et al. (224 additional authors not shown)

The characterization of the Advanced LIGO detectors in the second and third
observing runs has increased the sensitivity of the instruments, allowing for a
higher number of detectable gravitational-wave signals, and provided
confirmation of all observed gravitational-wave events. In this work, we
present the methods used to characterize the LIGO detectors and curate the
publicly available datasets, including the LIGO strain data and data quality
products. We describe the essential role of these datasets in LIGO-Virgo
Collaboration analyses of gravitational-waves from both transient and
persistent sources and include details on the provenance of these datasets in
order to support analyses of LIGO data by the broader community. Finally, we
explain anticipated changes in the role of detector characterization and
current efforts to prepare for the high rate of gravitational-wave alerts and
events in future observing runs.

http://arxiv.org/icons/sfx.gif