Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo

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. With...

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Veröffentlicht in:	Astrophys.J 2021-11, Vol.921 (1), p.80
Hauptverfasser:	Abraham, S., Baird, J., Barker, D., Barone, F., Barsotti, L., Bécsy, B., Bentley, J. D., Bertolini, A., Bondu, F., Brunett, S., Cain III, H. W., Callaghan, J. D., Cesarini, E., Chu, H., Coughlin, M. W., Dana, A., D’Angelo, B., De Pietri, R., Ding, B., D’Onofrio, L., Edo, T. B., Effler, A., Enomoto, Y., Farah, A. M., Fays, M., Fittipaldi, R., Fornal, B., Fukushima, M., Ganapathy, D., Garaventa, B., George, J., Gibson, D. R., Goetz, E., Grimes, E., Guimaraes, A. R., Hanson, J., Howell, E. J., Hui, D. C. Y., Ide, S., JaberianHamedan, V., Janthalur, N. N., Kaihotsu, K., Kamai, B., Kanda, N., Kapasi, D. P., Knee, A. M., Koper, N., Kuo, C., Lartaux-Vollard, A., Lin, C-Y., Liu, K., Mastrogiovanni, S., Merilh, E. L., Michimura, Y., Middleton, H., Mitselmakher, G., Mohite, S. R., Ng, K. Y., Ni, W.-T., Ohishi, N., Okada, M. A., Osthelder, C., Page, M. A., Paolone, A., Pham, K. A., Pilo, F., Powell, J., Prestegard, T., Puosi, F., Radkins, H., Ricker, P. M., Rizzo, M., Rollins, J. G., Romero, A., Romero-Shaw, I. M., Rose, C. A., Salemi, F., Sarin, N., Sato, T., Schaetzl, D., Sekiguchi, Y., Spagnuolo, V., Steer, D. A., Tacca, M., Tanaka, Takahiro, Tapia, A., Tolley, A. E., Tsang, T., Ushiba, T., Vander-Hyde, D. C., Vecchio, A., Vedovato, G., Washimi, T., Weinstein, A. J., Winkler, W., Yamamoto, Kohei, Yang, Yi, Ying, M., Yokogawa, K., Zhan, M.
Format:	Artikel
Sprache:	eng
Schlagworte:	1108 1667 Amplitudes Artifact identification Astrophysics Astrophysics - High Energy Astrophysical Phenomena Aérospatiale, astronomie & astrophysique Confidence intervals Ellipticity Ephemerides Frequencies Gamma rays Gravitational wave astronomy Gravitational waves Identification methods Neutron stars Physical, chemical, mathematical & earth Sciences Physics Physique, chimie, mathématiques & sciences de la terre Radiation Searching Space science, astronomy & astrophysics Space telescopes Supernova Supernova remnants Supernovae
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creator	Abraham, S. Baird, J. Barker, D. Barone, F. Barsotti, L. Bécsy, B. Bentley, J. D. Bertolini, A. Bondu, F. Brunett, S. Cain III, H. W. Callaghan, J. D. Cesarini, E. Chu, H. Coughlin, M. W. Dana, A. D’Angelo, B. De Pietri, R. Ding, B. D’Onofrio, L. Edo, T. B. Effler, A. Enomoto, Y. Farah, A. M. Fays, M. Fittipaldi, R. Fornal, B. Fukushima, M. Ganapathy, D. Garaventa, B. George, J. Gibson, D. R. Goetz, E. Grimes, E. Guimaraes, A. R. Hanson, J. Howell, E. J. Hui, D. C. Y. Ide, S. JaberianHamedan, V. Janthalur, N. N. Kaihotsu, K. Kamai, B. Kanda, N. Kapasi, D. P. Knee, A. M. Koper, N. Kuo, C. Lartaux-Vollard, A. Lin, C-Y. Liu, K. Mastrogiovanni, S. Merilh, E. L. Michimura, Y. Middleton, H. Mitselmakher, G. Mohite, S. R. Ng, K. Y. Ni, W.-T. Ohishi, N. Okada, M. A. Osthelder, C. Page, M. A. Paolone, A. Pham, K. A. Pilo, F. Powell, J. Prestegard, T. Puosi, F. Radkins, H. Ricker, P. M. Rizzo, M. Rollins, J. G. Romero, A. Romero-Shaw, I. M. Rose, C. A. Salemi, F. Sarin, N. Sato, T. Schaetzl, D. Sekiguchi, Y. Spagnuolo, V. Steer, D. A. Tacca, M. Tanaka, Takahiro Tapia, A. Tolley, A. E. Tsang, T. Ushiba, T. Vander-Hyde, D. C. Vecchio, A. Vedovato, G. Washimi, T. Weinstein, A. J. Winkler, W. Yamamoto, Kohei Yang, Yi Ying, M. Yokogawa, K. Zhan, M.
description	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 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 subbands, 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 7.7 × 10 −26 and 7.8 × 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 ≲10 −7 and ≲ 10 −5 , respectively, at frequencies above ∼400 Hz for the closest supernova remnant G266.2–1.2/Vela Jr.
doi_str_mv	10.3847/1538-4357/ac17ea
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D. ; Bertolini, A. ; Bondu, F. ; Brunett, S. ; Cain III, H. W. ; Callaghan, J. D. ; Cesarini, E. ; Chu, H. ; Coughlin, M. W. ; Dana, A. ; D’Angelo, B. ; De Pietri, R. ; Ding, B. ; D’Onofrio, L. ; Edo, T. B. ; Effler, A. ; Enomoto, Y. ; Farah, A. M. ; Fays, M. ; Fittipaldi, R. ; Fornal, B. ; Fukushima, M. ; Ganapathy, D. ; Garaventa, B. ; George, J. ; Gibson, D. R. ; Goetz, E. ; Grimes, E. ; Guimaraes, A. R. ; Hanson, J. ; Howell, E. J. ; Hui, D. C. Y. ; Ide, S. ; JaberianHamedan, V. ; Janthalur, N. N. ; Kaihotsu, K. ; Kamai, B. ; Kanda, N. ; Kapasi, D. P. ; Knee, A. M. ; Koper, N. ; Kuo, C. ; Lartaux-Vollard, A. ; Lin, C-Y. ; Liu, K. ; Mastrogiovanni, S. ; Merilh, E. L. ; Michimura, Y. ; Middleton, H. ; Mitselmakher, G. ; Mohite, S. R. ; Ng, K. Y. ; Ni, W.-T. ; Ohishi, N. ; Okada, M. A. ; Osthelder, C. ; Page, M. A. ; Paolone, A. ; Pham, K. A. ; Pilo, F. ; Powell, J. ; Prestegard, T. ; Puosi, F. ; Radkins, H. ; Ricker, P. M. ; Rizzo, M. ; Rollins, J. G. ; Romero, A. ; Romero-Shaw, I. M. ; Rose, C. A. ; Salemi, F. ; Sarin, N. ; Sato, T. ; Schaetzl, D. ; Sekiguchi, Y. ; Spagnuolo, V. ; Steer, D. A. ; Tacca, M. ; Tanaka, Takahiro ; Tapia, A. ; Tolley, A. E. ; Tsang, T. ; Ushiba, T. ; Vander-Hyde, D. C. ; Vecchio, A. ; Vedovato, G. ; Washimi, T. ; Weinstein, A. J. ; Winkler, W. ; Yamamoto, Kohei ; Yang, Yi ; Ying, M. ; Yokogawa, K. ; Zhan, M.</creator><creatorcontrib>Abraham, S. ; Baird, J. ; Barker, D. ; Barone, F. ; Barsotti, L. ; Bécsy, B. ; Bentley, J. D. ; Bertolini, A. ; Bondu, F. ; Brunett, S. ; Cain III, H. W. ; Callaghan, J. D. ; Cesarini, E. ; Chu, H. ; Coughlin, M. W. ; Dana, A. ; D’Angelo, B. ; De Pietri, R. ; Ding, B. ; D’Onofrio, L. ; Edo, T. B. ; Effler, A. ; Enomoto, Y. ; Farah, A. M. ; Fays, M. ; Fittipaldi, R. ; Fornal, B. ; Fukushima, M. ; Ganapathy, D. ; Garaventa, B. ; George, J. ; Gibson, D. R. ; Goetz, E. ; Grimes, E. ; Guimaraes, A. R. ; Hanson, J. ; Howell, E. J. ; Hui, D. C. Y. ; Ide, S. ; JaberianHamedan, V. ; Janthalur, N. N. ; Kaihotsu, K. ; Kamai, B. ; Kanda, N. ; Kapasi, D. P. ; Knee, A. M. ; Koper, N. ; Kuo, C. ; Lartaux-Vollard, A. ; Lin, C-Y. ; Liu, K. ; Mastrogiovanni, S. ; Merilh, E. L. ; Michimura, Y. ; Middleton, H. ; Mitselmakher, G. ; Mohite, S. R. ; Ng, K. Y. ; Ni, W.-T. ; Ohishi, N. ; Okada, M. A. ; Osthelder, C. ; Page, M. A. ; Paolone, A. ; Pham, K. A. ; Pilo, F. ; Powell, J. ; Prestegard, T. ; Puosi, F. ; Radkins, H. ; Ricker, P. M. ; Rizzo, M. ; Rollins, J. G. ; Romero, A. ; Romero-Shaw, I. M. ; Rose, C. A. ; Salemi, F. ; Sarin, N. ; Sato, T. ; Schaetzl, D. ; Sekiguchi, Y. ; Spagnuolo, V. ; Steer, D. A. ; Tacca, M. ; Tanaka, Takahiro ; Tapia, A. ; Tolley, A. E. ; Tsang, T. ; Ushiba, T. ; Vander-Hyde, D. C. ; Vecchio, A. ; Vedovato, G. ; Washimi, T. ; Weinstein, A. J. ; Winkler, W. ; Yamamoto, Kohei ; Yang, Yi ; Ying, M. ; Yokogawa, K. ; Zhan, M.</creatorcontrib><description>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 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 subbands, 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 7.7 × 10 −26 and 7.8 × 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 ≲10 −7 and ≲ 10 −5 , respectively, at frequencies above ∼400 Hz for the closest supernova remnant G266.2–1.2/Vela Jr.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ac17ea</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>1108 ; 1667 ; Amplitudes ; Artifact identification ; Astrophysics ; Astrophysics - High Energy Astrophysical Phenomena ; Aérospatiale, astronomie & astrophysique ; Confidence intervals ; Ellipticity ; Ephemerides ; Frequencies ; Gamma rays ; Gravitational wave astronomy ; Gravitational waves ; Identification methods ; Neutron stars ; Physical, chemical, mathematical & earth Sciences ; Physics ; Physique, chimie, mathématiques & sciences de la terre ; Radiation ; Searching ; Space science, astronomy & astrophysics ; Space telescopes ; Supernova ; Supernova remnants ; Supernovae</subject><ispartof>Astrophys.J, 2021-11, Vol.921 (1), p.80</ispartof><rights>2021. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Nov 01, 2021</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c494t-6847d69473d7c4cb88e8b7d4b1c200cced51c484cbf784d883ca81d2853547663</citedby><cites>FETCH-LOGICAL-c494t-6847d69473d7c4cb88e8b7d4b1c200cced51c484cbf784d883ca81d2853547663</cites><orcidid>0000-0001-5852-2301 ; 0000-0002-4341-2860 ; 0000-0003-2572-3101 ; 0000-0001-6487-5197 ; 0000-0002-1180-4050 ; 0000-0001-7469-4250 ; 0000-0003-3762-6958 ; 0000-0003-0589-9687 ; 0000-0002-7686-3334 ; 0000-0001-6589-8673 ; 0000-0003-1714-365X ; 0000-0002-0685-8310 ; 0000-0002-4991-8213 ; 0000-0002-1019-6911</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ac17ea/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ac17ea$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-03261149$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Abraham, S.</creatorcontrib><creatorcontrib>Baird, J.</creatorcontrib><creatorcontrib>Barker, D.</creatorcontrib><creatorcontrib>Barone, F.</creatorcontrib><creatorcontrib>Barsotti, L.</creatorcontrib><creatorcontrib>Bécsy, B.</creatorcontrib><creatorcontrib>Bentley, J. D.</creatorcontrib><creatorcontrib>Bertolini, A.</creatorcontrib><creatorcontrib>Bondu, F.</creatorcontrib><creatorcontrib>Brunett, S.</creatorcontrib><creatorcontrib>Cain III, H. W.</creatorcontrib><creatorcontrib>Callaghan, J. D.</creatorcontrib><creatorcontrib>Cesarini, E.</creatorcontrib><creatorcontrib>Chu, H.</creatorcontrib><creatorcontrib>Coughlin, M. W.</creatorcontrib><creatorcontrib>Dana, A.</creatorcontrib><creatorcontrib>D’Angelo, B.</creatorcontrib><creatorcontrib>De Pietri, R.</creatorcontrib><creatorcontrib>Ding, B.</creatorcontrib><creatorcontrib>D’Onofrio, L.</creatorcontrib><creatorcontrib>Edo, T. B.</creatorcontrib><creatorcontrib>Effler, A.</creatorcontrib><creatorcontrib>Enomoto, Y.</creatorcontrib><creatorcontrib>Farah, A. 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M.</creatorcontrib><creatorcontrib>Koper, N.</creatorcontrib><creatorcontrib>Kuo, C.</creatorcontrib><creatorcontrib>Lartaux-Vollard, A.</creatorcontrib><creatorcontrib>Lin, C-Y.</creatorcontrib><creatorcontrib>Liu, K.</creatorcontrib><creatorcontrib>Mastrogiovanni, S.</creatorcontrib><creatorcontrib>Merilh, E. L.</creatorcontrib><creatorcontrib>Michimura, Y.</creatorcontrib><creatorcontrib>Middleton, H.</creatorcontrib><creatorcontrib>Mitselmakher, G.</creatorcontrib><creatorcontrib>Mohite, S. R.</creatorcontrib><creatorcontrib>Ng, K. Y.</creatorcontrib><creatorcontrib>Ni, W.-T.</creatorcontrib><creatorcontrib>Ohishi, N.</creatorcontrib><creatorcontrib>Okada, M. A.</creatorcontrib><creatorcontrib>Osthelder, C.</creatorcontrib><creatorcontrib>Page, M. A.</creatorcontrib><creatorcontrib>Paolone, A.</creatorcontrib><creatorcontrib>Pham, K. A.</creatorcontrib><creatorcontrib>Pilo, F.</creatorcontrib><creatorcontrib>Powell, J.</creatorcontrib><creatorcontrib>Prestegard, T.</creatorcontrib><creatorcontrib>Puosi, F.</creatorcontrib><creatorcontrib>Radkins, H.</creatorcontrib><creatorcontrib>Ricker, P. M.</creatorcontrib><creatorcontrib>Rizzo, M.</creatorcontrib><creatorcontrib>Rollins, J. G.</creatorcontrib><creatorcontrib>Romero, A.</creatorcontrib><creatorcontrib>Romero-Shaw, I. M.</creatorcontrib><creatorcontrib>Rose, C. A.</creatorcontrib><creatorcontrib>Salemi, F.</creatorcontrib><creatorcontrib>Sarin, N.</creatorcontrib><creatorcontrib>Sato, T.</creatorcontrib><creatorcontrib>Schaetzl, D.</creatorcontrib><creatorcontrib>Sekiguchi, Y.</creatorcontrib><creatorcontrib>Spagnuolo, V.</creatorcontrib><creatorcontrib>Steer, D. A.</creatorcontrib><creatorcontrib>Tacca, M.</creatorcontrib><creatorcontrib>Tanaka, Takahiro</creatorcontrib><creatorcontrib>Tapia, A.</creatorcontrib><creatorcontrib>Tolley, A. E.</creatorcontrib><creatorcontrib>Tsang, T.</creatorcontrib><creatorcontrib>Ushiba, T.</creatorcontrib><creatorcontrib>Vander-Hyde, D. C.</creatorcontrib><creatorcontrib>Vecchio, A.</creatorcontrib><creatorcontrib>Vedovato, G.</creatorcontrib><creatorcontrib>Washimi, T.</creatorcontrib><creatorcontrib>Weinstein, A. J.</creatorcontrib><creatorcontrib>Winkler, W.</creatorcontrib><creatorcontrib>Yamamoto, Kohei</creatorcontrib><creatorcontrib>Yang, Yi</creatorcontrib><creatorcontrib>Ying, M.</creatorcontrib><creatorcontrib>Yokogawa, K.</creatorcontrib><creatorcontrib>Zhan, M.</creatorcontrib><title>Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo</title><title>Astrophys.J</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>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 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 subbands, 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 7.7 × 10 −26 and 7.8 × 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 ≲10 −7 and ≲ 10 −5 , respectively, at frequencies above ∼400 Hz for the closest supernova remnant G266.2–1.2/Vela Jr.</description><subject>1108</subject><subject>1667</subject><subject>Amplitudes</subject><subject>Artifact identification</subject><subject>Astrophysics</subject><subject>Astrophysics - High Energy Astrophysical Phenomena</subject><subject>Aérospatiale, astronomie & astrophysique</subject><subject>Confidence intervals</subject><subject>Ellipticity</subject><subject>Ephemerides</subject><subject>Frequencies</subject><subject>Gamma rays</subject><subject>Gravitational wave astronomy</subject><subject>Gravitational waves</subject><subject>Identification methods</subject><subject>Neutron stars</subject><subject>Physical, chemical, mathematical & earth Sciences</subject><subject>Physics</subject><subject>Physique, chimie, mathématiques & sciences de la terre</subject><subject>Radiation</subject><subject>Searching</subject><subject>Space science, astronomy & astrophysics</subject><subject>Space telescopes</subject><subject>Supernova</subject><subject>Supernova remnants</subject><subject>Supernovae</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp1kc1q3DAUhUVpodO0-y4FXRXqxvqxJC-HIZkEBgaS9G8lriV5RsEjTSXbkAfoe9euS7rqStLV9x2QDkLvSfmZKS4vScVUwVklL8EQ6eAFWj2PXqJVWZa8EEx-f43e5Pw4H2ldr9CvewfJHF3GbUx4E0PvwxCHjLcJRt9D72OADn-DcUZSPOEfcQgHfD-cXQpxBHznTgFCn7EPuD86fAWpe8IPR58s3jfZpdFP_N0QcGzx2o4QjLN4d7vdYwgWf_XpEN-iVy102b37u16gL9dXD5ubYrff3m7Wu8LwmveFmB5qRc0ls9Jw0yjlVCMtb4ihZWmm3IoYrqabVipulWIGFLFUVaziUgh2gdiS23l3cDqmxuuR6gh-2Q_dQYPRjdOUCqWpkJSqyfq4WEfo9Dn5E6SnP87NeqfnWcmoIITXI5nYDwt7TvHn4HKvH-OQpi_MmlZ1RSrKxJxYLpRJMefk2udYUuq5Tj13p-fu9FLnpHxaFB_P_zL_i_8GlUqgtg</recordid><startdate>20211101</startdate><enddate>20211101</enddate><creator>Abraham, S.</creator><creator>Baird, J.</creator><creator>Barker, D.</creator><creator>Barone, F.</creator><creator>Barsotti, L.</creator><creator>Bécsy, B.</creator><creator>Bentley, J. 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Y.</creator><creator>Ide, S.</creator><creator>JaberianHamedan, V.</creator><creator>Janthalur, N. N.</creator><creator>Kaihotsu, K.</creator><creator>Kamai, B.</creator><creator>Kanda, N.</creator><creator>Kapasi, D. P.</creator><creator>Knee, A. M.</creator><creator>Koper, N.</creator><creator>Kuo, C.</creator><creator>Lartaux-Vollard, A.</creator><creator>Lin, C-Y.</creator><creator>Liu, K.</creator><creator>Mastrogiovanni, S.</creator><creator>Merilh, E. L.</creator><creator>Michimura, Y.</creator><creator>Middleton, H.</creator><creator>Mitselmakher, G.</creator><creator>Mohite, S. R.</creator><creator>Ng, K. Y.</creator><creator>Ni, W.-T.</creator><creator>Ohishi, N.</creator><creator>Okada, M. A.</creator><creator>Osthelder, C.</creator><creator>Page, M. A.</creator><creator>Paolone, A.</creator><creator>Pham, K. 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J.</creator><creator>Winkler, W.</creator><creator>Yamamoto, Kohei</creator><creator>Yang, Yi</creator><creator>Ying, M.</creator><creator>Yokogawa, K.</creator><creator>Zhan, M.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>University of Chicago Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>Q33</scope><orcidid>https://orcid.org/0000-0001-5852-2301</orcidid><orcidid>https://orcid.org/0000-0002-4341-2860</orcidid><orcidid>https://orcid.org/0000-0003-2572-3101</orcidid><orcidid>https://orcid.org/0000-0001-6487-5197</orcidid><orcidid>https://orcid.org/0000-0002-1180-4050</orcidid><orcidid>https://orcid.org/0000-0001-7469-4250</orcidid><orcidid>https://orcid.org/0000-0003-3762-6958</orcidid><orcidid>https://orcid.org/0000-0003-0589-9687</orcidid><orcidid>https://orcid.org/0000-0002-7686-3334</orcidid><orcidid>https://orcid.org/0000-0001-6589-8673</orcidid><orcidid>https://orcid.org/0000-0003-1714-365X</orcidid><orcidid>https://orcid.org/0000-0002-0685-8310</orcidid><orcidid>https://orcid.org/0000-0002-4991-8213</orcidid><orcidid>https://orcid.org/0000-0002-1019-6911</orcidid></search><sort><creationdate>20211101</creationdate><title>Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo</title><author>Abraham, S. ; Baird, J. ; Barker, D. ; Barone, F. ; Barsotti, L. ; Bécsy, B. ; Bentley, J. D. ; Bertolini, A. ; Bondu, F. ; Brunett, S. ; Cain III, H. W. ; Callaghan, J. D. ; Cesarini, E. ; Chu, H. ; Coughlin, M. W. ; Dana, A. ; D’Angelo, B. ; De Pietri, R. ; Ding, B. ; D’Onofrio, L. ; Edo, T. B. ; Effler, A. ; Enomoto, Y. ; Farah, A. M. ; Fays, M. ; Fittipaldi, R. ; Fornal, B. ; Fukushima, M. ; Ganapathy, D. ; Garaventa, B. ; George, J. ; Gibson, D. R. ; Goetz, E. ; Grimes, E. ; Guimaraes, A. R. ; Hanson, J. ; Howell, E. J. ; Hui, D. C. Y. ; Ide, S. ; JaberianHamedan, V. ; Janthalur, N. N. ; Kaihotsu, K. ; Kamai, B. ; Kanda, N. ; Kapasi, D. P. ; Knee, A. M. ; Koper, N. ; Kuo, C. ; Lartaux-Vollard, A. ; Lin, C-Y. ; Liu, K. ; Mastrogiovanni, S. ; Merilh, E. L. ; Michimura, Y. ; Middleton, H. ; Mitselmakher, G. ; Mohite, S. R. ; Ng, K. Y. ; Ni, W.-T. ; Ohishi, N. ; Okada, M. A. ; Osthelder, C. ; Page, M. A. ; Paolone, A. ; Pham, K. A. ; Pilo, F. ; Powell, J. ; Prestegard, T. ; Puosi, F. ; Radkins, H. ; Ricker, P. M. ; Rizzo, M. ; Rollins, J. G. ; Romero, A. ; Romero-Shaw, I. M. ; Rose, C. A. ; Salemi, F. ; Sarin, N. ; Sato, T. ; Schaetzl, D. ; Sekiguchi, Y. ; Spagnuolo, V. ; Steer, D. A. ; Tacca, M. ; Tanaka, Takahiro ; Tapia, A. ; Tolley, A. E. ; Tsang, T. ; Ushiba, T. ; Vander-Hyde, D. C. ; Vecchio, A. ; Vedovato, G. ; Washimi, T. ; Weinstein, A. J. ; Winkler, W. ; Yamamoto, Kohei ; Yang, Yi ; Ying, M. ; Yokogawa, K. ; Zhan, M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c494t-6847d69473d7c4cb88e8b7d4b1c200cced51c484cbf784d883ca81d2853547663</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>1108</topic><topic>1667</topic><topic>Amplitudes</topic><topic>Artifact identification</topic><topic>Astrophysics</topic><topic>Astrophysics - High Energy Astrophysical Phenomena</topic><topic>Aérospatiale, astronomie & astrophysique</topic><topic>Confidence intervals</topic><topic>Ellipticity</topic><topic>Ephemerides</topic><topic>Frequencies</topic><topic>Gamma rays</topic><topic>Gravitational wave astronomy</topic><topic>Gravitational waves</topic><topic>Identification methods</topic><topic>Neutron stars</topic><topic>Physical, chemical, mathematical & earth Sciences</topic><topic>Physics</topic><topic>Physique, chimie, mathématiques & sciences de la terre</topic><topic>Radiation</topic><topic>Searching</topic><topic>Space science, astronomy & astrophysics</topic><topic>Space telescopes</topic><topic>Supernova</topic><topic>Supernova remnants</topic><topic>Supernovae</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Abraham, S.</creatorcontrib><creatorcontrib>Baird, J.</creatorcontrib><creatorcontrib>Barker, D.</creatorcontrib><creatorcontrib>Barone, F.</creatorcontrib><creatorcontrib>Barsotti, L.</creatorcontrib><creatorcontrib>Bécsy, B.</creatorcontrib><creatorcontrib>Bentley, J. D.</creatorcontrib><creatorcontrib>Bertolini, A.</creatorcontrib><creatorcontrib>Bondu, F.</creatorcontrib><creatorcontrib>Brunett, S.</creatorcontrib><creatorcontrib>Cain III, H. W.</creatorcontrib><creatorcontrib>Callaghan, J. D.</creatorcontrib><creatorcontrib>Cesarini, E.</creatorcontrib><creatorcontrib>Chu, H.</creatorcontrib><creatorcontrib>Coughlin, M. W.</creatorcontrib><creatorcontrib>Dana, A.</creatorcontrib><creatorcontrib>D’Angelo, B.</creatorcontrib><creatorcontrib>De Pietri, R.</creatorcontrib><creatorcontrib>Ding, B.</creatorcontrib><creatorcontrib>D’Onofrio, L.</creatorcontrib><creatorcontrib>Edo, T. B.</creatorcontrib><creatorcontrib>Effler, A.</creatorcontrib><creatorcontrib>Enomoto, Y.</creatorcontrib><creatorcontrib>Farah, A. 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J.</creatorcontrib><creatorcontrib>Winkler, W.</creatorcontrib><creatorcontrib>Yamamoto, Kohei</creatorcontrib><creatorcontrib>Yang, Yi</creatorcontrib><creatorcontrib>Ying, M.</creatorcontrib><creatorcontrib>Yokogawa, K.</creatorcontrib><creatorcontrib>Zhan, M.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Université de Liège - Open Repository and Bibliography (ORBI)</collection><jtitle>Astrophys.J</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Abraham, S.</au><au>Baird, J.</au><au>Barker, D.</au><au>Barone, F.</au><au>Barsotti, L.</au><au>Bécsy, B.</au><au>Bentley, J. D.</au><au>Bertolini, A.</au><au>Bondu, F.</au><au>Brunett, S.</au><au>Cain III, H. W.</au><au>Callaghan, J. D.</au><au>Cesarini, E.</au><au>Chu, H.</au><au>Coughlin, M. W.</au><au>Dana, A.</au><au>D’Angelo, B.</au><au>De Pietri, R.</au><au>Ding, B.</au><au>D’Onofrio, L.</au><au>Edo, T. B.</au><au>Effler, A.</au><au>Enomoto, Y.</au><au>Farah, A. M.</au><au>Fays, M.</au><au>Fittipaldi, R.</au><au>Fornal, B.</au><au>Fukushima, M.</au><au>Ganapathy, D.</au><au>Garaventa, B.</au><au>George, J.</au><au>Gibson, D. R.</au><au>Goetz, E.</au><au>Grimes, E.</au><au>Guimaraes, A. R.</au><au>Hanson, J.</au><au>Howell, E. J.</au><au>Hui, D. C. Y.</au><au>Ide, S.</au><au>JaberianHamedan, V.</au><au>Janthalur, N. N.</au><au>Kaihotsu, K.</au><au>Kamai, B.</au><au>Kanda, N.</au><au>Kapasi, D. P.</au><au>Knee, A. M.</au><au>Koper, N.</au><au>Kuo, C.</au><au>Lartaux-Vollard, A.</au><au>Lin, C-Y.</au><au>Liu, K.</au><au>Mastrogiovanni, S.</au><au>Merilh, E. L.</au><au>Michimura, Y.</au><au>Middleton, H.</au><au>Mitselmakher, G.</au><au>Mohite, S. R.</au><au>Ng, K. Y.</au><au>Ni, W.-T.</au><au>Ohishi, N.</au><au>Okada, M. A.</au><au>Osthelder, C.</au><au>Page, M. A.</au><au>Paolone, A.</au><au>Pham, K. A.</au><au>Pilo, F.</au><au>Powell, J.</au><au>Prestegard, T.</au><au>Puosi, F.</au><au>Radkins, H.</au><au>Ricker, P. M.</au><au>Rizzo, M.</au><au>Rollins, J. G.</au><au>Romero, A.</au><au>Romero-Shaw, I. M.</au><au>Rose, C. A.</au><au>Salemi, F.</au><au>Sarin, N.</au><au>Sato, T.</au><au>Schaetzl, D.</au><au>Sekiguchi, Y.</au><au>Spagnuolo, V.</au><au>Steer, D. A.</au><au>Tacca, M.</au><au>Tanaka, Takahiro</au><au>Tapia, A.</au><au>Tolley, A. E.</au><au>Tsang, T.</au><au>Ushiba, T.</au><au>Vander-Hyde, D. C.</au><au>Vecchio, A.</au><au>Vedovato, G.</au><au>Washimi, T.</au><au>Weinstein, A. J.</au><au>Winkler, W.</au><au>Yamamoto, Kohei</au><au>Yang, Yi</au><au>Ying, M.</au><au>Yokogawa, K.</au><au>Zhan, M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo</atitle><jtitle>Astrophys.J</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2021-11-01</date><risdate>2021</risdate><volume>921</volume><issue>1</issue><spage>80</spage><pages>80-</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>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 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 subbands, 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 7.7 × 10 −26 and 7.8 × 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 ≲10 −7 and ≲ 10 −5 , respectively, at frequencies above ∼400 Hz for the closest supernova remnant G266.2–1.2/Vela Jr.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ac17ea</doi><tpages>29</tpages><orcidid>https://orcid.org/0000-0001-5852-2301</orcidid><orcidid>https://orcid.org/0000-0002-4341-2860</orcidid><orcidid>https://orcid.org/0000-0003-2572-3101</orcidid><orcidid>https://orcid.org/0000-0001-6487-5197</orcidid><orcidid>https://orcid.org/0000-0002-1180-4050</orcidid><orcidid>https://orcid.org/0000-0001-7469-4250</orcidid><orcidid>https://orcid.org/0000-0003-3762-6958</orcidid><orcidid>https://orcid.org/0000-0003-0589-9687</orcidid><orcidid>https://orcid.org/0000-0002-7686-3334</orcidid><orcidid>https://orcid.org/0000-0001-6589-8673</orcidid><orcidid>https://orcid.org/0000-0003-1714-365X</orcidid><orcidid>https://orcid.org/0000-0002-0685-8310</orcidid><orcidid>https://orcid.org/0000-0002-4991-8213</orcidid><orcidid>https://orcid.org/0000-0002-1019-6911</orcidid><oa>free_for_read</oa></addata></record>
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subjects	1108 1667 Amplitudes Artifact identification Astrophysics Astrophysics - High Energy Astrophysical Phenomena Aérospatiale, astronomie & astrophysique Confidence intervals Ellipticity Ephemerides Frequencies Gamma rays Gravitational wave astronomy Gravitational waves Identification methods Neutron stars Physical, chemical, mathematical & earth Sciences Physics Physique, chimie, mathématiques & sciences de la terre Radiation Searching Space science, astronomy & astrophysics Space telescopes Supernova Supernova remnants Supernovae
title	Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo
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