Searches for continuous gravitational waves from young supernova remnants in the early third observing run of Advanced LIGO and Virgo. (arXiv:2105.11641v2 [astro-ph.HE] UPDATED)

Searches for continuous gravitational waves from young supernova remnants in the early third observing run of Advanced LIGO and Virgo. (arXiv:2105.11641v2 [astro-ph.HE] UPDATED)
The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_LIGO_Scientific/0/1/0/all/0/1">LIGO Scientific Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Virgo/0/1/0/all/0/1">Virgo Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_KAGRA/0/1/0/all/0/1">KAGRA Collaboration</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:+Abbott_T/0/1/0/all/0/1">T. D. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_S/0/1/0/all/0/1">S. Abraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acernese_F/0/1/0/all/0/1">F. Acernese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackley_K/0/1/0/all/0/1">K. Ackley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_A/0/1/0/all/0/1">A. Adams</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:+Adya_V/0/1/0/all/0/1">V. B. Adya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Affeldt_C/0/1/0/all/0/1">C. Affeldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agarwal_D/0/1/0/all/0/1">D. Agarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agathos_M/0/1/0/all/0/1">M. Agathos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agatsuma_K/0/1/0/all/0/1">K. Agatsuma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aggarwal_N/0/1/0/all/0/1">N. Aggarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguiar_O/0/1/0/all/0/1">O. D. Aguiar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiello_L/0/1/0/all/0/1">L. Aiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ain_A/0/1/0/all/0/1">A. Ain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajith_P/0/1/0/all/0/1">P. Ajith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akutsu_T/0/1/0/all/0/1">T. Akutsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aleman_K/0/1/0/all/0/1">K. M. Aleman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_G/0/1/0/all/0/1">G. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allocca_A/0/1/0/all/0/1">A. Allocca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altin_P/0/1/0/all/0/1">P. A. Altin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amato_A/0/1/0/all/0/1">A. Amato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anand_S/0/1/0/all/0/1">S. Anand</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:+Anderson_S/0/1/0/all/0/1">S. B. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_W/0/1/0/all/0/1">W. G. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ando_M/0/1/0/all/0/1">M. Ando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angelova_S/0/1/0/all/0/1">S. V. Angelova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansoldi_S/0/1/0/all/0/1">S. Ansoldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antelis_J/0/1/0/all/0/1">J. M. Antelis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antier_S/0/1/0/all/0/1">S. Antier</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">Koya Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arai_K/0/1/0/all/0/1">Koji Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arai_Y/0/1/0/all/0/1">Y. Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araki_S/0/1/0/all/0/1">S. Araki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araya_A/0/1/0/all/0/1">A. Araya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araya_M/0/1/0/all/0/1">M. C. Araya</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:+Arene_M/0/1/0/all/0/1">M. Arène</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aritomi_N/0/1/0/all/0/1">N. Aritomi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_N/0/1/0/all/0/1">N. Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aronson_S/0/1/0/all/0/1">S. M. Aronson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arun_K/0/1/0/all/0/1">K. G. Arun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asada_H/0/1/0/all/0/1">H. Asada</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:+Ashton_G/0/1/0/all/0/1">G. Ashton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aso_Y/0/1/0/all/0/1">Y. Aso</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:+Astone_P/0/1/0/all/0/1">P. Astone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aubin_F/0/1/0/all/0/1">F. Aubin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aufmuth_P/0/1/0/all/0/1">P. Aufmuth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+AultONeal_K/0/1/0/all/0/1">K. AultONeal</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:+Babak_S/0/1/0/all/0/1">S. Babak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badaracco_F/0/1/0/all/0/1">F. Badaracco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bader_M/0/1/0/all/0/1">M. K. M. Bader</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bae_S/0/1/0/all/0/1">S. Bae</a>, et al. (1529 additional authors not shown)

We present results of three wide-band directed searches for continuous
gravitational waves from 15 young supernova remnants in the first half of the
third Advanced LIGO and Virgo observing run. We use three search pipelines with
distinct signal models and methods of identifying noise artifacts. Without
ephemerides of these sources, the searches are conducted over a frequency band
spanning from 10~Hz to 2~kHz. We find no evidence of continuous gravitational
radiation from these sources. We set upper limits on the intrinsic signal
strain at 95% confidence level in sample sub-bands, estimate the sensitivity
in the full band, and derive the corresponding constraints on the fiducial
neutron star ellipticity and $r$-mode amplitude. The best 95% confidence
constraints placed on the signal strain are $7.7times 10^{-26}$ and $7.8times
10^{-26}$ near 200~Hz for the supernova remnants G39.2–0.3 and G65.7+1.2,
respectively. The most stringent constraints on the ellipticity and $r$-mode
amplitude reach $lesssim 10^{-7}$ and $ lesssim 10^{-5}$, respectively, at
frequencies above $sim 400$~Hz for the closest supernova remnant
G266.2–1.2/Vela Jr.

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