Detecting Dark Matter in the LISA era: Gravitational Waves from Intermediate Mass Ratio Inspirals Bradley J Kavanagh GRAPPA, University of Amsterdam SLAP2019, 27th September 2019 b.j.kavanagh@uva.nl @BradleyKavanagh Powered by
Preliminary work in collaboration with: Gianfranco Bertone David Nichols Daniele Gaggero [GRAPPA] [University of Virginia, [IFT Madrid, formerly GRAPPA] formerly GRAPPA] but working closely with everyone at GRAPPA. 2 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
GW probes of DM Current Interferometers Future Interferometers Axion Pulsar Timing Arrays EMRI/IMRI dephasing forces QCD Axion DM production (GW/Radio) by bubble collisions Axion DM Rolling Rolling axions axions Dark blobs Hidden sector Dark Photon DM PBH scalars mergers BH-Boson condensate BH spin distribution PBH/sub-halo transits Boson star 1 M � binaries 10 − 20 10 − 10 10 20 10 30 10 40 10 50 10 60 10 70 1 10 Dark Matter Candidate Mass [eV] [1907.10610] 3 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
GW probes of DM Current Interferometers Future Interferometers Axion Pulsar Timing Arrays EMRI/IMRI dephasing forces QCD Axion DM production (GW/Radio) by bubble collisions Axion DM Rolling Rolling axions axions Dark blobs Hidden sector Dark Photon DM PBH scalars mergers BH-Boson condensate BH spin distribution PBH/sub-halo transits Boson star 1 M � binaries 10 − 20 10 − 10 10 20 10 30 10 40 10 50 10 60 10 70 1 10 Dark Matter Candidate Mass [eV] [1907.10610] 4 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
<latexit sha1_base64="xtYoklD0DgP9ExdiuADxze+xE=">ACE3icbVDLSgMxFM3UV62vUZdugkUQ0TLTKrqSopu6KFSwD+jUknTNjSZDElGKEP/wY2/4saFIm7duPNvzLRdaOuFkM53LvPX7IqNKO82lFhaXlfSq5m19Y3NLXt7p6ZEJDGpYsGEbPhIEUYDUtVUM9IJUHcZ6TuD64Tvf5ApKIiuNPDkLQ46gW0SzHShmrbR+W2x5HuSx7flK9KI+gpyqHr3BfgSfKdQe/YWERH6LadXLOuOA8cKcgC6ZVadtfXkfgiJNAY4aUarpOqFsxkpiRkYZL1IkRHiAeqRpYIA4Ua14fNMIHhimA7tCmhdoOGZ/d8SIKzXkvnEm+6tZLSH/05qR7l60YhqEkSYBngzqRgxqAZOAYIdKgjUbGoCwpGZXiPtIqxNjBkTgjt78jyo5XNuIZe/Pc0WL6dxpMEe2AeHwAXnoAhKoAKqAINH8AxewZv1ZL1Y79bHxJqypj274E9Znz/YTpuW</latexit> <latexit sha1_base64="I1iPuIAVula+v38DpNpD8tcZc=">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</latexit> Intermediate Mass Ratio Inspiral (IMRI) Stellar mass compact object (NS/BH) inspirals towards intermediate mass black hole (IMBH) NS/ M IMBH ∼ 10 3 − 10 5 M � IMBH BH GW emission causes long, slow inspiral: E GW ≈ 32 G 4 M IMBH3 M NS2 ˙ ∝ ( f GW ) 10 / 3 5 c 5 r 5 LISA should detect ~ 3 - 10 IMRIs per year [1711.00483] 5 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
<latexit sha1_base64="pGlmVhrL8UY8eNX0uqnmQAX2c28=">ACF3icbZDLSgMxFIYz9VbrbdSlm2ARXGiZaQu6koIbN0IFe4FOWzKZTBuaTIYkI5Rh3sKNr+LGhSJudefbmF4W2vpD4OM/5Bzfj9mVGnH+bZyK6tr6xv5zcLW9s7unr1/0FQikZg0sGBCtn2kCKMRaWiqGWnHkiDuM9LyR9eTeuBSEVFdK/HMelyNIhoSDHSxurbJU8OBfQU5dB1em5mkHv7LbviUBoQx5Heih5GuOsl5Xsr5dErOVHAZ3DkUwVz1v3lBQInEQaM6RUx3Vi3U2R1BQzkhW8RJEY4REakI7BCHGiun0rgyeGCeAoZDmRpO3d8TKeJKjblvOid7qsXaxPyv1kl0eNlNaRQnmkR49lGYMKgFnIQEAyoJ1mxsAGFJza4QD5FEWJsoCyYEd/HkZWiWS26lVL6rFmtX8zjy4Agcg1PgtQAzegDhoAg0fwDF7Bm/VkvVjv1sesNWfNZw7BH1mfP/fLnpI=</latexit> <latexit sha1_base64="JzDoBpUpSXK2ZRb1vHl5Gdy540=">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</latexit> <latexit sha1_base64="Yuz9Y2pb3x/SsUJgkjBWtIJHp0=">ACAXicbVDLSsNAFJ3UV62vqBvBzWARXNWkFepGKbhxWcE+oAlhMp2Q2cmYWYilFA3/obF4q49S/c+TdO2iy09cCFwzn3cu89Ycyo0o7zbRVWVtfWN4qbpa3tnd09e/+graJEYtLCEYtkN0SKMCpIS1PNSDeWBPGQkU4vsn8zgORikbiXk9i4nM0FHRAMdJGCuwjb4g4R4HkR5Jnqp4Cq9g/bwW2GWn4swAl4mbkzLI0QzsL68f4YQToTFDSvVcJ9Z+iqSmJFpyUsUiREeoyHpGSoQJ8pPZx9M4alR+nAQSVNCw5n6eyJFXKkJD01ndqha9DLxP6+X6MGln1IRJ5oIPF80SBjUEczigH0qCdZsYgjCkpbIR4hibA2oZVMCO7iy8ukXa24tUr17qLcuM7jKIJjcALOgAvqoAFuQRO0AaP4Bm8gjfryXqx3q2PeWvBymcOwR9Ynz9pqpYv</latexit> Dark Matter ‘Mini-spikes’ Depending on the formation mechanism of the IMBH, expect an over-density of DM: � γ sp � r sp ρ DM ( r ) = ρ sp DM r IMBH For BH forming in an NFW halo, from adiabatic growth expect: γ sp = 7 / 3 ρ ∼ 10 24 M � pc � 3 Density can reach (~10 24 times larger than local density) [astro-ph/9906391, astro-ph/0501555, astro-ph/0501625, astro-ph/0509565, 0902.3665, 1305.2619] 6 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
<latexit sha1_base64="59PJBAiNQ9zZ3ZESeKxzTuDlI=">AB9XicbVDLSgMxFL1TX7W+qi7dBIvgqsxUQZdFNy4r2Ae0Y8mkmTY0yQxJRi1D/8ONC0Xc+i/u/Bsz7Sy09UDgcM693JMTxJxp47rfTmFldW19o7hZ2tre2d0r7x+0dJQoQpsk4pHqBFhTziRtGmY47cSKYhFw2g7G15nfqBKs0jemUlMfYGHkoWMYGOl+6DfE9iMlEgFfpr2yxW36s6AlomXkwrkaPTLX71BRBJBpSEca9313Nj4KVaGEU6npV6iaYzJGA9p1KJBdV+Oks9RSdWGaAwUvZJg2bq740UC60nIrCTWUa96GXif143MeGlnzIZJ4ZKMj8UJhyZCGUVoAFTlBg+sQTxWxWREZYWJsUSVbgrf45WXSqlW9s2rt9rxSv8rKMIRHMpeHABdbiBjSBgIJneIU359F5cd6dj/lowcl3DuEPnM8fJMuS7g=</latexit> <latexit sha1_base64="Bhm8L5IXQ9ez0fX/yaDiqXbxs0=">AB6nicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Qe0oWy2k3bpZhN2N0IJ/QlePCji1V/kzX/jts1BWx8MPN6bYWZekAiujet+O4W19Y3NreJ2aWd3b/+gfHjU0nGqGDZLGLVCahGwSU2DTcCO4lCGgUC28H4dua3n1BpHstHM0nQj+hQ8pAzaqz0oPpuv1xq+4cZJV4OalAjka/NUbxCyNUBomqNZdz02Mn1FlOBM4LfVSjQlYzrErqWSRqj9bH7qlJxZUDCWNmShszV3xMZjbSeRIHtjKgZ6WVvJv7ndVMTXvsZl0lqULFojAVxMRk9jcZcIXMiIklClubyVsRBVlxqZTsiF4y+vklat6l1Ua/eXlfpNHkcRTuAUzsGDK6jDHTSgCQyG8Ayv8OYI58V5dz4WrQUnzmGP3A+fwACVo2d</latexit> <latexit sha1_base64="vyRPgFdY1QFczRQXBU8cvTwyo=">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</latexit> Dynamical Friction [Chandrasekhar, 1943] NS/BH b max r 0 E DF ∼ 4 π G 2 N M 2 NS ρ DM ( r ) 2 ˙ 3 γ − 3 ln Λ ∝ ( f GW ) v NS IMBH 7 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
IMRI + Dark Matter DM makes the compact object spiral in faster, NS/ primarily due to dynamical friction IMBH BH This can be seen in the rate at which the GW signal accumulates phase ‘De-phasing’ 8 Bradley J. Kavanagh (GRAPPA, Amsterdam) Detecting DM in the LISA era: GWs from IMRIs
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