Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data
We present a search for gravitational waves from 221 pulsars with rotation frequencies \(\gtrsim 10\) Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target em...
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| creator | Ananyeva, A Areeda, J S Arnaud, N Aston, S M Barayoga, J C Barta, D Bernuzzi, S Bode, N Bossilkov, V Bosveld, J Bouffanais, Y Brinkmann, M Calloni, E Cerretani, G Chao, S Chia, H Y Cho, M Cleva, F Cocchieri, C Costa, C A Daw, E J Degallaix, J Deléglise, S Dent, T Díaz, M C Dietrich, T Dwyer, S E Estelles, H Fairhurst, S Favata, M Fidecaro, F Fyffe, M Gair, J R Giazotto, A Goncharov, B Gruning, P Hall, B R Hannuksela, O A Heidmann, A Heptonstall, A W Hoy, C G Hulko, M Iyer, B R Kang, G Karki, S Keerthana, N V Kijbunchoo, N Kim, W Klika, J H Koehlenbeck, S M Kumar, P Landry, M Lazzarini, A Lecoeuche, Y K Y Ma Malik, A Mandic, V Maros, E Martelli, F Mason, K Mukherjee, Arunava Obergaulinger, M O'Brien, B D Okada, M A O'Reilly, B Pele, A Penn, S Pitkin, M Poggiani, R Prasad, J Privitera, S Punturo, M Rajan, C Reitze, D H Ricci, F Rolland, L Rose, K Saleem, M Sanchez, E J Sanders, J R Schale, P Scheuer, J Shaffer, T Siellez, K Singer, L P Steinmeyer, D Sudhir, V Szczepańczyk, M J Thomas, M Töyrä, D Trovato, A van Heijningen, J V Wade, A R Wang, Y F Ward, R L Weaver, B Wright, J L Yeeles, D W Zhang, J Zucker, M E |
| description | We present a search for gravitational waves from 221 pulsars with rotation frequencies \(\gtrsim 10\) Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the \(l = m = 2\) mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and from the \(l = 2\), \(m = 1\) mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the \(l = m = 2\) mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of \(10^{38}\) kg m\(^2\) for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of \(1.2\!\times\!10^{-8}\). We also place new limits on the emission amplitude at the rotation frequency of the pulsars. |
| doi_str_mv | 10.48550/arxiv.1902.08507 |
| format | Article |
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We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the \(l = m = 2\) mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and from the \(l = 2\), \(m = 1\) mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the \(l = m = 2\) mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of \(10^{38}\) kg m\(^2\) for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of \(1.2\!\times\!10^{-8}\). We also place new limits on the emission amplitude at the rotation frequency of the pulsars.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1902.08507</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Amplitudes ; Crabs ; Ellipticity ; Emissions control ; Gravitation ; Gravitational waves ; Luminosity ; Millisecond pulsars ; Moments of inertia ; Physics - General Relativity and Quantum Cosmology ; Physics - High Energy Astrophysical Phenomena ; Pulsars ; Quadrupoles ; Rotation ; Searching</subject><ispartof>arXiv.org, 2020-07</ispartof><rights>2020. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.1902.08507$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/1538-4357/ab20cb$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Ananyeva, A</creatorcontrib><creatorcontrib>Areeda, J S</creatorcontrib><creatorcontrib>Arnaud, N</creatorcontrib><creatorcontrib>Aston, S M</creatorcontrib><creatorcontrib>Barayoga, J C</creatorcontrib><creatorcontrib>Barta, 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F</creatorcontrib><creatorcontrib>Rolland, L</creatorcontrib><creatorcontrib>Rose, K</creatorcontrib><creatorcontrib>Saleem, M</creatorcontrib><creatorcontrib>Sanchez, E J</creatorcontrib><creatorcontrib>Sanders, J R</creatorcontrib><creatorcontrib>Schale, P</creatorcontrib><creatorcontrib>Scheuer, J</creatorcontrib><creatorcontrib>Shaffer, T</creatorcontrib><creatorcontrib>Siellez, K</creatorcontrib><creatorcontrib>Singer, L P</creatorcontrib><creatorcontrib>Steinmeyer, D</creatorcontrib><creatorcontrib>Sudhir, V</creatorcontrib><creatorcontrib>Szczepańczyk, M J</creatorcontrib><creatorcontrib>Thomas, M</creatorcontrib><creatorcontrib>Töyrä, D</creatorcontrib><creatorcontrib>Trovato, A</creatorcontrib><creatorcontrib>van Heijningen, J V</creatorcontrib><creatorcontrib>Wade, A R</creatorcontrib><creatorcontrib>Wang, Y F</creatorcontrib><creatorcontrib>Ward, R L</creatorcontrib><creatorcontrib>Weaver, B</creatorcontrib><creatorcontrib>Wright, J L</creatorcontrib><creatorcontrib>Yeeles, D W</creatorcontrib><creatorcontrib>Zhang, J</creatorcontrib><creatorcontrib>Zucker, M E</creatorcontrib><title>Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data</title><title>arXiv.org</title><description>We present a search for gravitational waves from 221 pulsars with rotation frequencies \(\gtrsim 10\) Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the \(l = m = 2\) mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and from the \(l = 2\), \(m = 1\) mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the \(l = m = 2\) mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of \(10^{38}\) kg m\(^2\) for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of \(1.2\!\times\!10^{-8}\). We also place new limits on the emission amplitude at the rotation frequency of the pulsars.</description><subject>Amplitudes</subject><subject>Crabs</subject><subject>Ellipticity</subject><subject>Emissions control</subject><subject>Gravitation</subject><subject>Gravitational waves</subject><subject>Luminosity</subject><subject>Millisecond pulsars</subject><subject>Moments of inertia</subject><subject>Physics - General Relativity and Quantum Cosmology</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Pulsars</subject><subject>Quadrupoles</subject><subject>Rotation</subject><subject>Searching</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkEtLA0EQhAdBMMT8AE8OeN7YPTO9j6NETYKBCAY8eFh6H4Mbkp04s0nMvzcPL1VQfBRUCXGHMDQpETyy_212Q8xADSElSK5ET2mNUWqUuhGDEJYAoOJEEeme-Pqo2ZffdZDWeTn2vGs67hrX8kp-8u6Ue7eWb63bt_J9uwrsg-ROLvZOTtivXduUQTatVIAUHSWRs-l4Lp-541txbXkV6sG_98Xi9WUxmkSz-Xg6eppFTEpFVHGMQIWNU6SSVGl1VSBmVaEqY0yNaOLSAqQFa4ucWSAynOisJMgwKXRf3F9qz8vzjW_W7A_56YH8_MCReLgQG-9-tnXo8qXb-uPEkCtMYwCtjdJ_4H9bdg</recordid><startdate>20200728</startdate><enddate>20200728</enddate><creator>Ananyeva, A</creator><creator>Areeda, J S</creator><creator>Arnaud, N</creator><creator>Aston, S 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arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20200728</creationdate><title>Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data</title><author>Ananyeva, A ; Areeda, J S ; Arnaud, N ; Aston, S M ; Barayoga, J C ; Barta, D ; Bernuzzi, S ; Bode, N ; Bossilkov, V ; Bosveld, J ; Bouffanais, Y ; Brinkmann, M ; Calloni, E ; Cerretani, G ; Chao, S ; Chia, H Y ; Cho, M ; Cleva, F ; Cocchieri, C ; Costa, C A ; Daw, E J ; Degallaix, J ; Deléglise, S ; Dent, T ; Díaz, M C ; Dietrich, T ; Dwyer, S E ; Estelles, H ; Fairhurst, S ; Favata, M ; Fidecaro, F ; Fyffe, M ; Gair, J R ; Giazotto, A ; Goncharov, B ; Gruning, P ; Hall, B R ; Hannuksela, O A ; Heidmann, A ; Heptonstall, A W ; Hoy, C G ; Hulko, M ; Iyer, B R ; Kang, G ; Karki, S ; Keerthana, N V ; Kijbunchoo, N ; Kim, W ; Klika, J H ; Koehlenbeck, S M ; Kumar, P ; Landry, M ; Lazzarini, A ; Lecoeuche, Y K ; Y Ma ; Malik, A ; Mandic, V ; Maros, E ; Martelli, F ; Mason, K ; Mukherjee, Arunava ; Obergaulinger, M ; O'Brien, B D ; Okada, M A ; O'Reilly, B ; Pele, A ; Penn, S ; Pitkin, M ; Poggiani, R ; Prasad, J ; Privitera, S ; Punturo, M ; Rajan, C ; Reitze, D H ; Ricci, F ; Rolland, L ; Rose, K ; Saleem, M ; Sanchez, E J ; Sanders, J R ; Schale, P ; Scheuer, J ; Shaffer, T ; Siellez, K ; Singer, L P ; Steinmeyer, D ; Sudhir, V ; Szczepańczyk, M J ; Thomas, M ; Töyrä, D ; Trovato, A ; van Heijningen, J V ; Wade, A R ; Wang, Y F ; Ward, R L ; Weaver, B ; Wright, J L ; Yeeles, D W ; Zhang, J ; Zucker, M E</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a522-5da6105bf6815c52cf3db119db2d444e1146cf008ba3f1a9f0554a739c50917b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Amplitudes</topic><topic>Crabs</topic><topic>Ellipticity</topic><topic>Emissions control</topic><topic>Gravitation</topic><topic>Gravitational waves</topic><topic>Luminosity</topic><topic>Millisecond pulsars</topic><topic>Moments of inertia</topic><topic>Physics - General Relativity and Quantum Cosmology</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Pulsars</topic><topic>Quadrupoles</topic><topic>Rotation</topic><topic>Searching</topic><toplevel>online_resources</toplevel><creatorcontrib>Ananyeva, A</creatorcontrib><creatorcontrib>Areeda, J S</creatorcontrib><creatorcontrib>Arnaud, N</creatorcontrib><creatorcontrib>Aston, S M</creatorcontrib><creatorcontrib>Barayoga, J C</creatorcontrib><creatorcontrib>Barta, D</creatorcontrib><creatorcontrib>Bernuzzi, S</creatorcontrib><creatorcontrib>Bode, N</creatorcontrib><creatorcontrib>Bossilkov, V</creatorcontrib><creatorcontrib>Bosveld, J</creatorcontrib><creatorcontrib>Bouffanais, Y</creatorcontrib><creatorcontrib>Brinkmann, M</creatorcontrib><creatorcontrib>Calloni, E</creatorcontrib><creatorcontrib>Cerretani, G</creatorcontrib><creatorcontrib>Chao, S</creatorcontrib><creatorcontrib>Chia, H Y</creatorcontrib><creatorcontrib>Cho, M</creatorcontrib><creatorcontrib>Cleva, F</creatorcontrib><creatorcontrib>Cocchieri, C</creatorcontrib><creatorcontrib>Costa, C A</creatorcontrib><creatorcontrib>Daw, E J</creatorcontrib><creatorcontrib>Degallaix, J</creatorcontrib><creatorcontrib>Deléglise, S</creatorcontrib><creatorcontrib>Dent, T</creatorcontrib><creatorcontrib>Díaz, M C</creatorcontrib><creatorcontrib>Dietrich, T</creatorcontrib><creatorcontrib>Dwyer, S E</creatorcontrib><creatorcontrib>Estelles, H</creatorcontrib><creatorcontrib>Fairhurst, S</creatorcontrib><creatorcontrib>Favata, M</creatorcontrib><creatorcontrib>Fidecaro, F</creatorcontrib><creatorcontrib>Fyffe, M</creatorcontrib><creatorcontrib>Gair, J R</creatorcontrib><creatorcontrib>Giazotto, A</creatorcontrib><creatorcontrib>Goncharov, B</creatorcontrib><creatorcontrib>Gruning, P</creatorcontrib><creatorcontrib>Hall, B R</creatorcontrib><creatorcontrib>Hannuksela, O A</creatorcontrib><creatorcontrib>Heidmann, A</creatorcontrib><creatorcontrib>Heptonstall, A W</creatorcontrib><creatorcontrib>Hoy, C G</creatorcontrib><creatorcontrib>Hulko, M</creatorcontrib><creatorcontrib>Iyer, B R</creatorcontrib><creatorcontrib>Kang, G</creatorcontrib><creatorcontrib>Karki, S</creatorcontrib><creatorcontrib>Keerthana, N V</creatorcontrib><creatorcontrib>Kijbunchoo, N</creatorcontrib><creatorcontrib>Kim, W</creatorcontrib><creatorcontrib>Klika, J H</creatorcontrib><creatorcontrib>Koehlenbeck, S M</creatorcontrib><creatorcontrib>Kumar, P</creatorcontrib><creatorcontrib>Landry, M</creatorcontrib><creatorcontrib>Lazzarini, A</creatorcontrib><creatorcontrib>Lecoeuche, Y K</creatorcontrib><creatorcontrib>Y Ma</creatorcontrib><creatorcontrib>Malik, A</creatorcontrib><creatorcontrib>Mandic, V</creatorcontrib><creatorcontrib>Maros, E</creatorcontrib><creatorcontrib>Martelli, F</creatorcontrib><creatorcontrib>Mason, K</creatorcontrib><creatorcontrib>Mukherjee, Arunava</creatorcontrib><creatorcontrib>Obergaulinger, M</creatorcontrib><creatorcontrib>O'Brien, B D</creatorcontrib><creatorcontrib>Okada, M A</creatorcontrib><creatorcontrib>O'Reilly, B</creatorcontrib><creatorcontrib>Pele, A</creatorcontrib><creatorcontrib>Penn, S</creatorcontrib><creatorcontrib>Pitkin, M</creatorcontrib><creatorcontrib>Poggiani, R</creatorcontrib><creatorcontrib>Prasad, J</creatorcontrib><creatorcontrib>Privitera, S</creatorcontrib><creatorcontrib>Punturo, M</creatorcontrib><creatorcontrib>Rajan, C</creatorcontrib><creatorcontrib>Reitze, D H</creatorcontrib><creatorcontrib>Ricci, F</creatorcontrib><creatorcontrib>Rolland, L</creatorcontrib><creatorcontrib>Rose, K</creatorcontrib><creatorcontrib>Saleem, M</creatorcontrib><creatorcontrib>Sanchez, E J</creatorcontrib><creatorcontrib>Sanders, J R</creatorcontrib><creatorcontrib>Schale, P</creatorcontrib><creatorcontrib>Scheuer, J</creatorcontrib><creatorcontrib>Shaffer, T</creatorcontrib><creatorcontrib>Siellez, K</creatorcontrib><creatorcontrib>Singer, L P</creatorcontrib><creatorcontrib>Steinmeyer, D</creatorcontrib><creatorcontrib>Sudhir, V</creatorcontrib><creatorcontrib>Szczepańczyk, M J</creatorcontrib><creatorcontrib>Thomas, M</creatorcontrib><creatorcontrib>Töyrä, D</creatorcontrib><creatorcontrib>Trovato, A</creatorcontrib><creatorcontrib>van Heijningen, J V</creatorcontrib><creatorcontrib>Wade, A R</creatorcontrib><creatorcontrib>Wang, Y F</creatorcontrib><creatorcontrib>Ward, R L</creatorcontrib><creatorcontrib>Weaver, B</creatorcontrib><creatorcontrib>Wright, J L</creatorcontrib><creatorcontrib>Yeeles, D W</creatorcontrib><creatorcontrib>Zhang, J</creatorcontrib><creatorcontrib>Zucker, M E</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Ananyeva, A</au><au>Areeda, J S</au><au>Arnaud, N</au><au>Aston, S M</au><au>Barayoga, J C</au><au>Barta, D</au><au>Bernuzzi, S</au><au>Bode, N</au><au>Bossilkov, V</au><au>Bosveld, J</au><au>Bouffanais, Y</au><au>Brinkmann, M</au><au>Calloni, E</au><au>Cerretani, G</au><au>Chao, S</au><au>Chia, H Y</au><au>Cho, M</au><au>Cleva, F</au><au>Cocchieri, C</au><au>Costa, C A</au><au>Daw, E J</au><au>Degallaix, J</au><au>Deléglise, S</au><au>Dent, T</au><au>Díaz, M C</au><au>Dietrich, T</au><au>Dwyer, S E</au><au>Estelles, H</au><au>Fairhurst, S</au><au>Favata, M</au><au>Fidecaro, F</au><au>Fyffe, M</au><au>Gair, J R</au><au>Giazotto, A</au><au>Goncharov, B</au><au>Gruning, P</au><au>Hall, B R</au><au>Hannuksela, O A</au><au>Heidmann, A</au><au>Heptonstall, A W</au><au>Hoy, C G</au><au>Hulko, M</au><au>Iyer, B R</au><au>Kang, G</au><au>Karki, S</au><au>Keerthana, N V</au><au>Kijbunchoo, N</au><au>Kim, W</au><au>Klika, J H</au><au>Koehlenbeck, S M</au><au>Kumar, P</au><au>Landry, M</au><au>Lazzarini, A</au><au>Lecoeuche, Y K</au><au>Y Ma</au><au>Malik, A</au><au>Mandic, V</au><au>Maros, E</au><au>Martelli, F</au><au>Mason, K</au><au>Mukherjee, Arunava</au><au>Obergaulinger, M</au><au>O'Brien, B D</au><au>Okada, M A</au><au>O'Reilly, B</au><au>Pele, A</au><au>Penn, S</au><au>Pitkin, M</au><au>Poggiani, R</au><au>Prasad, J</au><au>Privitera, S</au><au>Punturo, M</au><au>Rajan, C</au><au>Reitze, D H</au><au>Ricci, F</au><au>Rolland, L</au><au>Rose, K</au><au>Saleem, M</au><au>Sanchez, E J</au><au>Sanders, J R</au><au>Schale, P</au><au>Scheuer, J</au><au>Shaffer, T</au><au>Siellez, K</au><au>Singer, L P</au><au>Steinmeyer, D</au><au>Sudhir, V</au><au>Szczepańczyk, M J</au><au>Thomas, M</au><au>Töyrä, D</au><au>Trovato, A</au><au>van Heijningen, J V</au><au>Wade, A R</au><au>Wang, Y F</au><au>Ward, R L</au><au>Weaver, B</au><au>Wright, J L</au><au>Yeeles, D W</au><au>Zhang, J</au><au>Zucker, M E</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data</atitle><jtitle>arXiv.org</jtitle><date>2020-07-28</date><risdate>2020</risdate><eissn>2331-8422</eissn><abstract>We present a search for gravitational waves from 221 pulsars with rotation frequencies \(\gtrsim 10\) Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the \(l = m = 2\) mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and from the \(l = 2\), \(m = 1\) mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the \(l = m = 2\) mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of \(10^{38}\) kg m\(^2\) for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of \(1.2\!\times\!10^{-8}\). We also place new limits on the emission amplitude at the rotation frequency of the pulsars.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1902.08507</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2020-07 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1902_08507 |
| source | arXiv.org; Free E- Journals |
| subjects | Amplitudes Crabs Ellipticity Emissions control Gravitation Gravitational waves Luminosity Millisecond pulsars Moments of inertia Physics - General Relativity and Quantum Cosmology Physics - High Energy Astrophysical Phenomena Pulsars Quadrupoles Rotation Searching |
| title | Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data |
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