Gravitational-wave physics with Cosmic Explorer: limits to low-frequency sensitivity. (arXiv:2012.03608v3 [gr-qc] UPDATED)

Gravitational-wave physics with Cosmic Explorer: limits to low-frequency sensitivity. (arXiv:2012.03608v3 [gr-qc] UPDATED)
<a href="http://arxiv.org/find/gr-qc/1/au:+Hall_E/0/1/0/all/0/1">Evan D. Hall</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kuns_K/0/1/0/all/0/1">Kevin Kuns</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Smith_J/0/1/0/all/0/1">Joshua R. Smith</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bai_Y/0/1/0/all/0/1">Yuntao Bai</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Wipf_C/0/1/0/all/0/1">Christopher Wipf</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Biscans_S/0/1/0/all/0/1">Sebastien Biscans</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Adhikari_R/0/1/0/all/0/1">Rana X Adhikari</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Arai_K/0/1/0/all/0/1">Koji Arai</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Ballmer_S/0/1/0/all/0/1">Stefan Ballmer</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Barsotti_L/0/1/0/all/0/1">Lisa Barsotti</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Chen_Y/0/1/0/all/0/1">Yanbei Chen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Evans_M/0/1/0/all/0/1">Matthew Evans</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Fritschel_P/0/1/0/all/0/1">Peter Fritschel</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Harms_J/0/1/0/all/0/1">Jan Harms</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Kamai_B/0/1/0/all/0/1">Brittany Kamai</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Rollins_J/0/1/0/all/0/1">Jameson Graef Rollins</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Shoemaker_D/0/1/0/all/0/1">David Shoemaker</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Slagmolen_B/0/1/0/all/0/1">Bram Slagmolen</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Weiss_R/0/1/0/all/0/1">Rainer Weiss</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Yamamoto_H/0/1/0/all/0/1">Hiro Yamamoto</a>

Cosmic Explorer (CE) is a next-generation ground-based gravitational-wave
observatory concept, envisioned to begin operation in the 2030s, and expected
to be capable of observing binary neutron star and black hole mergers back to
the time of the first stars. Cosmic Explorer’s sensitive band will extend below
10 Hz, where the design is predominantly limited by geophysical, thermal, and
quantum noises. In this work, thermal, seismic, gravity-gradient, quantum,
residual gas, scattered-light, and servo-control noises are analyzed in order
to motivate facility and vacuum system design requirements, potential test mass
suspensions, Newtonian noise reduction strategies, improved inertial sensors,
and cryogenic control requirements. Our analysis shows that with improved
technologies, Cosmic Explorer can deliver a strain sensitivity better than
$10^{-23}/mathrm{Hz}^{1/2}$ down to 5 Hz. Our work refines and extends
previous analysis of the Cosmic Explorer concept and outlines the key research
areas needed to make this observatory a reality.

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