Searches for con,nuous gravita,onal waves in LIGO/Virgo data and the post-merger remnant following the binary neutron star merger GW170817

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1 Searches for con,nuous gravita,onal waves in LIGO/Virgo data and the post-merger remnant following the binary neutron star merger GW Evan Goetz for the LIGO Scien,fic Collabora,on and Virgo Collabora,on LIGO Hanford Observatory LIGO-G

2 Transient vs con,nuous gravita,onal wave signals Compact binary coalescence gravita,onal wave signals are strong but transient Cannot perform long dura,on studies of par,cular source Con3nuous gravita,onal wave signals are weak but persistent enabling long term studies of a source 2

3 Con,nuous gravita,onal waves (1) Radia,on generated by,me-varying quadrupolar mass-moment h µ = 2G rc 4 d 2 dt 2 [I µ ] I µ r Quadrupole moment of iner,a tensor Distance to source Rapidly-rota,ng neutron star with equatorial ellip,city (tri-axial ellipsoid) h r 1kpc 1 fgw 1 khz 2 " 10 6 I zz kg m 2 " = I xx I yy I zz Equatorial ellip,city f GW =2f rot P. Jaranowski, A. Królak, B. Schutz, Phys. Rev. D

4 Con,nuous gravita,onal waves (2) Con,nuous GWs are nearly monochroma,c sinusoidal waves Plausible breaking strain of NS ma`er: Normal nuclear ma`er Hybrid (hadron-quark core) Quark star Gravita,onal wave emission strength and frequency depends on mechanism, ex: Tri-axial ellipsoid r-mode fluid oscilla,ons Free-precession " < 10 5 " < 10 3 " < 10 1 f GW =2f rot f GW ' (4/3)f rot f GW = f rot ± f prec N. Johnson-McDaniel and B. Owen, PRD

5 Why we search for con,nuous gravita,onal waves Just one system would provide a rich laboratory! Neutron star equa,on of state? Maximum ellip,city? Does NS have exo,c states of ma`er? Maximum mass of a neutron star? How fast can a neutron star spin? Other tests of General Rela,vity NS dynamics Implica,ons for popula,on models Stochas,c background of GWs from spinning neutron stars Images: h`p:// h`p://sci.esa.int/loi/49338-equa,on-of-state-for-neutron-stars/ 5

6 Recent results: O1 targeted search Strain Sensitivity h O1 sensitivity estimate O1 results spin-down limits surpass spin-down limits Initial detector results Targeted search of 200 known pulsars in first Advanced LIGO observing run Results for 8 pulsars beat the spin-down limit Overall, 2x be`er than ini,al LIGO/Virgo results Crab limit at 0.2% of total energy loss Vela limit at 1% of total energy loss Smallest ellip,city limit: " < One of several targeted analyses Gravitational-wave Frequency (Hz) B. P. Abbo`, et al. ApJ

7 Recent results: O1 searches for Sco X-1 Three different methods: Unmodeled cross-correla,on (radiometer) Hidden Markov model tracking of spin-wandering signal (Viterbi) Model-based crosscorrela,on (CrossCorr) Tightest limits nearly reach the torque-balance limit near 100 Hz An,cipate refined limits with addi,onal data / improved detectors / advancements in methods Abbo`, et al., 2017 ApJ

8 Recent results: O1 all-sky, isolated neutron star search 4 different pipelines: PowerFlux,,me-domain F-sta,s,c, Sky Hough and Frequency Hough Pipelines provide consistent results; confidence nothing has been missed Tightest limits h 0 ' (circular polariza,on) near 170 Hz arxiv: [gr-qc] 8

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sha1_base64="fkbjwep/c4xy5py7dz7ktvrvboi=">aaab/xicbvbns8naen3ur1q/ouljy2irvfgset8oqtglxwrgftpynttju3szcbubqgkf/4oxdype/r/e/ddu2xy09cha470zzuyfcwdko863vvhyxfpeka6w1ty3nrfs7z0hfaesgkdjhstgqbrwjsdtthnojbjifhcob/2bsv8fgfqsfvd6miafka5gianeg6lt77ugrekigi8fvsku85gdn43adtmpobpgeelmpixy1nr2v6st0zqcosknsjvdj9f+rqrmlmoo1eovjit2sreahgosgfkzyfkjfgiudg5jaupopff/t2qkumoybayzirqnzr2x+j/xthv44wdmjkkgqaelwprjhenxfrjdjfdnh4yqkpm5fdmekyrqk1jjhodovjxpvjpkzcw9oy1xr/m0imgfhaaj5kjzvew3qiy8rfggntereroerbfr3fqythasfgyx/yh1+qmwojsh</latexit> <latexit sha1_base64="fkbjwep/c4xy5py7dz7ktvrvboi=">aaab/xicbvbns8naen3ur1q/ouljy2irvfgset8oqtglxwrgftpynttju3szcbubqgkf/4oxdype/r/e/ddu2xy09cha470zzuyfcwdko863vvhyxfpeka6w1ty3nrfs7z0hfaesgkdjhstgqbrwjsdtthnojbjifhcob/2bsv8fgfqsfvd6miafka5gianeg6lt77ugrekigi8fvsku85gdn43adtmpobpgeelmpixy1nr2v6st0zqcosknsjvdj9f+rqrmlmoo1eovjit2sreahgosgfkzyfkjfgiudg5jaupopff/t2qkumoybayzirqnzr2x+j/xthv44wdmjkkgqaelwprjhenxfrjdjfdnh4yqkpm5fdmekyrqk1jjhodovjxpvjpkzcw9oy1xr/m0imgfhaaj5kjzvew3qiy8rfggntereroerbfr3fqythasfgyx/yh1+qmwojsh</latexit> Recent results: O1 all-sky isolated neutron star search reach Ellip,city of a NS at a given distance for which circularly polarized waves could be detected using, e.g. PowerFlux algorithm Ex: at 1 kpc, can exclude sources emisng at f GW > 400 Hz with <latexit sha1_base64="1hm3mmetpochbbl4nuft6na/tvs=">aaacbnicbvdlssnafj3uv62vqetbgkvwiswrgrqrogu7rgbsoqlhmp20qycpzm7egrjz46+4cahi1m9w5984fqjaeudc4zx7ufcep+fmgml+ayw5+yxfpejyawv1bx1d39y6kxeqclvjzgpr8rgknexubgacthjbcehz2vt7f0o/euufzhf0dyoeuihurixgbiosph038bygdydc7lkzn1vn0zn8eer3uaexzyo5gjflrakpowkanv7pdgkshjqcwrgubctmwm2waey4zutokmmcsr93avvrciduutnoj9zyv0rhcgkhkgjjpp6eyhao5sd0vweiosenvah4n9doithxmxylkdcijbcfktcgnoahgb0mkae+uaqtwdstbulhgqmo6eoqbgv65vlih1vok9zvtvw7n6rrrdtodx0gcx2jgqqjbrirqq/ocb2gv+1re9betpdxa0gbzgyjp9a+vge4bzka</latexit> " = 10 6 Tightest constraint " = at arxiv: [gr-qc] f GW = 1975 Hz <latexit 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10 Recent results: O1 all-sky isolated lowfrequency search Powerflux O1 search Time-domain F-stat O1 search Sky Hough O1 search Frequency Hough O1 search Results from this search distributed compu,ng project results Hz, deep search (restricted spindown search compared with other searches) Tightest limits: h 0 ' (marginalized over NS orienta,on); above 55 Hz, can exclude sources with " > 10 5 within 1 kpc of Earth 10 Abbo`, et al., Phys. Rev. D

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12 <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> Plausible signal of post-merger remnant from GW Bar-mode instabili,es? Magnetar like waveforms? r-mode oscilla,ons/instabili,es? First non-detec,on results for signals <500s Challenges for longer-dura,on search: Unknown GW emission frequency and (rapid) signal evolu,on Distance is far for tradi,onal CW searches d = Mpc Abbo`, et al., 2017 ApJL 851 L16 12

13 Bar-mode instabili,es NS becomes deformed into tri-axial ellipsoid Magnetar undergoing secular bar-mode instability might explain plateau in GRB light curves Reich, Nature 468, 15 (2010) Lai & Shapiro 1995 Corsi & Meszaros

14 Bar-mode instability model waveform examples Typical GRB magnetar: 1.4 Msun, 20 km radius, 1e14 G, n = 1 Corsi & Meszaros 2009 Coyne et al

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sha1_base64="fuuuse3g0lkujtnqazvueff7g7i=">aaab6xicbvbns8naej3ur1q/qh69lbbbu0leqb6eohepfy0ttkfsttt26wytdidccf0jxjyoepufefpfug1z0nyha4/3zpizfyzsghtdb6ewsrq2vlhclg1t7+zulfcphk2casz9fstyt0jqubsk+yhq8laioy1cyzvh6gbqn5+4nijwdzhoebdrgrj9wsha6v5d1brlilt1zydlxmtjbxi0uuwvti9macqvmkmnaxtugkfgnqom+atusq1pkbvraw9bqmjetzdntp2qe6v0sd/wthssmfp7iqormemotj0rxafz9kbif147xf5fkamvpmgvmy/qp5jgtkz/k57qnkecw0kzfvzwwozuu4y2nzinwvt8ezn4z9xlqnd3xqlf52ku4qio4rq8qeedbqebpjaywdo8wpsjnrfn3fmytxacfoyq/sd5/ae/zy1o</latexit> <latexit sha1_base64="gnmhxtou6ipho68kve/t2fy3+ao=">aaab8nicbvbns8naej3ur1q/qh69lbbbu0luug9flx4rgftoqtlsp+3szsbsboqs+je8efdx6q/x5r9x2+agrq8ghu/nmdmvsgxxxnw/ndlk6tr6rnmzsrw9s7tx3t941emmgposeylqr1sj4bj9w43adqqqxphavjs6nfqtj1saj/lbjfmmyzqqvm8znvykjakeaq15tm671zpbd2cgy8qrsa0knlvvr6cxscxgazigwnc8nzvhtpxhtockemqau8pgdiadsywnuyf57oyjobfkj/qtzusamln/t+q01nocr7yzpmaof72p+j/xyuz/ksy5tdodks0x9tnbtekmazaev8imgftcmel2vskgvffmbewvg4k3+piy8c/q13xv/qlwucnskmmrhmmpehajdbidjvjaiivneiu3j3nenhfny95acoqzq/gd5/mhtlgraw==</latexit> <latexit sha1_base64="gnmhxtou6ipho68kve/t2fy3+ao=">aaab8nicbvbns8naej3ur1q/qh69lbbbu0luug9flx4rgftoqtlsp+3szsbsboqs+je8efdx6q/x5r9x2+agrq8ghu/nmdmvsgxxxnw/ndlk6tr6rnmzsrw9s7tx3t941emmgposeylqr1sj4bj9w43adqqqxphavjs6nfqtj1saj/lbjfmmyzqqvm8znvykjakeaq15tm671zpbd2cgy8qrsa0knlvvr6cxscxgazigwnc8nzvhtpxhtockemqau8pgdiadsywnuyf57oyjobfkj/qtzusamln/t+q01nocr7yzpmaof72p+j/xyuz/ksy5tdodks0x9tnbtekmazaev8imgftcmel2vskgvffmbewvg4k3+piy8c/q13xv/qlwucnskmmrhmmpehajdbidjvjaiivneiu3j3nenhfny95acoqzq/gd5/mhtlgraw==</latexit> <latexit sha1_base64="gnmhxtou6ipho68kve/t2fy3+ao=">aaab8nicbvbns8naej3ur1q/qh69lbbbu0luug9flx4rgftoqtlsp+3szsbsboqs+je8efdx6q/x5r9x2+agrq8ghu/nmdmvsgxxxnw/ndlk6tr6rnmzsrw9s7tx3t941emmgposeylqr1sj4bj9w43adqqqxphavjs6nfqtj1saj/lbjfmmyzqqvm8znvykjakeaq15tm671zpbd2cgy8qrsa0knlvvr6cxscxgazigwnc8nzvhtpxhtockemqau8pgdiadsywnuyf57oyjobfkj/qtzusamln/t+q01nocr7yzpmaof72p+j/xyuz/ksy5tdodks0x9tnbtekmazaev8imgftcmel2vskgvffmbewvg4k3+piy8c/q13xv/qlwucnskmmrhmmpehajdbidjvjaiivneiu3j3nenhfny95acoqzq/gd5/mhtlgraw==</latexit> <latexit sha1_base64="gnmhxtou6ipho68kve/t2fy3+ao=">aaab8nicbvbns8naej3ur1q/qh69lbbbu0luug9flx4rgftoqtlsp+3szsbsboqs+je8efdx6q/x5r9x2+agrq8ghu/nmdmvsgxxxnw/ndlk6tr6rnmzsrw9s7tx3t941emmgposeylqr1sj4bj9w43adqqqxphavjs6nfqtj1saj/lbjfmmyzqqvm8znvykjakeaq15tm671zpbd2cgy8qrsa0knlvvr6cxscxgazigwnc8nzvhtpxhtockemqau8pgdiadsywnuyf57oyjobfkj/qtzusamln/t+q01nocr7yzpmaof72p+j/xyuz/ksy5tdodks0x9tnbtekmazaev8imgftcmel2vskgvffmbewvg4k3+piy8c/q13xv/qlwucnskmmrhmmpehajdbidjvjaiivneiu3j3nenhfny95acoqzq/gd5/mhtlgraw==</latexit> Spindown Magnetar-like emission GW emission = Dipole EM emission r-mode emission Observed EM spindown k n n =5 n =3 n =7 n. 3 GW frequency f gw (t) =f gw,0 1+ t 1 1 n = 1 0 n k(1 n) <latexit sha1_base64="tguityrynmlfcrpwf4om6rpepmg=">aaacdxicbvdlssnafj34rpuvdelmsbtqoiurqv0irtfurgbsoylhmp20qyetmdmrssgxupfx3lhqcevenx/jtm1cww9c7ugce5m5j0gylcqyvo2fxaxlldxswnl9y3nr29zzvznxkjbxcmxi0qmqjixy4iiqgokkgqaoykqddc/hfvubceljfqtgcfei1oc0pbgplflm1vuohefqdqxcwd29jkgf+dz9ztd5nmfdmu6huw9wriy1azwndkeqoedln7/cxoztihcfgzkya1uj8jikfmwm5gu3lsrbeij6pksprxgrxjy5j4dvrfrggatdxmgj+nsjq5guoyjqkxfsaznrjcx/vg6qwlmvozxjfef4+lcymqhiom4g9qggwlgrjgglqv8k8qdpyjroskxdsgdpnifoueosyd8cv5oxrrolsa8oqa3y4aq0wrvoaqdg8aiewst4m56mf+pd+jiolhjfzh74a+pzb22dmqc=</latexit> Lasky, et al., LIGO-T

16 Magnetar-like emission waveform examples Lasky, et al., LIGO-T

17 <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> <latexit sha1_base64="l12hhcslb936cts1e1tq6ja94fw=">aaacb3icbvdlsgnbejynrxhfqx49obgeqq27ejaehkaxl0ie1wssdzmdtmyq2qczvwjy9ujfx/hiqcwrv+dnv3hyoghiqunr1u13lx8lrscyvo3czozc/ej+sbc0vlk6zq5v3kgokzq5nbkrbphemcfd5gahwrqxzctwbav7vfobx79nuveoviz+znya3iw8wykblxnmdhuf4rj1m+5xmi89tmtz66af7afkkf7gnppmolwyhsdtxb6tihqj5plfrxzek4cfqavrqmlbmbgpkccpyfmhlsgwe9ojd6ypaugcptx0+eigd7xsxp1i6gobd9xfeykjloohvu4mchtvpdcq//oacxqqbsrdoaew0tgitiiwrhiqcm5zysiiviaesq5vxbrljkggsyvoeozjl6ejc1q6kdlx5wl1bjxghm2hhbshbhsmqugc1zcdkhpez+gvvrlpxovxbnymwnpgegyt/yhx+qple5g8</latexit> r-mode oscilla,ons? d = Mpc Toroidal pulsa,ons of NS are unstable most likely some damping reaching a satura,on amplitude r-mode satura,on amplitude depends on NS EOS My,dis, et al ApJ

18 CW search methods adapted Viterbi / Hidden Markov Model previously used for Sco X-1 searches Tuned SkyHough / FrequencyHough / F-stat methods adapted from all-sky searches STAMP-VLT adapted from short dura,on cross-correla,on burst searches 18

19 Conclusions LIGO and Virgo Collabora,ons have set forth a robust program to detect con,nuous gravita,onal waves Detec,ng one source would provide rich laboratory including post-merger remnant searches! Cri,cally important: improved detectors, sensi,ve algorithms, and con,nued collabora,on with EM partners No detec,ons yet, but we are searching hard Non-detec,ons are probing interes,ng astrophysics 19