Milky Way Satellites: Probes of Dark Matter Microphysics Ethan Nadler 8/7/19 Small Halos as DM Probes CDM WDM Lovell et al. 2011 Faint Galaxies as DM Probes CDM WDM Milky Way Satellites Boo III CVn II Com Classical CVn I Boo I Boo II Leo II SDSS +60◦ Vir I Wil 1 Leo V PS1 Boo IV Leo IV Seg 1 UMa I Leo I DES UMi Dra II Crt II Sex DECam Her I +30 UMa II Dra HSC ◦ Hyd II ATLAS Gaia Ant II 0◦ CMa Car III Sgr Car II Tri II Sgr II Car LMC Pic II Col I 30◦ Hyi I − Ind II Pic I Seg 2 Peg III SMC Psc II Ret III Tuc I I Tuc V Ret II Gru II Hor I Eri II Aqr II Tuc IV Gru I Hor II 60 Cet III Tuc I I I ◦ Phe II Eri III − For Cet II Scl Credit: Sidney Mau 1. Resimulate Milky Way- like halos from large cosmological volume. ↵<latexit sha1_base64="+wSBPeL8nxBdvzPXA2qswhGhfpg=">AAAB7XicbVBNS8NAEJ3Ur1q/qh69LBbBU0mqoMeiF48V7Ae0oUy2m3btZhN2N0IJ/Q9ePCji1f/jzX/jts1BWx8MPN6bYWZekAiujet+O4W19Y3NreJ2aWd3b/+gfHjU0nGqKGvSWMSqE6BmgkvWNNwI1kkUwygQrB2Mb2d++4kpzWP5YCYJ8yMcSh5yisZKrR6KZIT9csWtunOQVeLlpAI5Gv3yV28Q0zRi0lCBWnc9NzF+hspwKti01Es1S5COcci6lkqMmPaz+bVTcmaVAQljZUsaMld/T2QYaT2JAtsZoRnpZW8m/ud1UxNe+xmXSWqYpItFYSqIicnsdTLgilEjJpYgVdzeSugIFVJjAyrZELzll1dJq1b1Lqq1+8tK/SaPowgncArn4MEV1OEOGtAECo/wDK/w5sTOi/PufCxaC04+cwx/4Hz+AIzPjxw=</latexit> 2. Paint satellite galaxies σ <latexit sha1_base64="P99ez1bWyq6CFJ3tVJiBTJPQvlE=">AAAB/HicbVBNS8NAEN3Ur1q/oj16CRbBU0mqoMeiF48V7Ae0IWy2m3TpbhJ2J2II8a948aCIV3+IN/+N2zYHbX0w8Hhvhpl5fsKZAtv+Nipr6xubW9Xt2s7u3v6BeXjUU3EqCe2SmMdy4GNFOYtoFxhwOkgkxcLntO9Pb2Z+/4FKxeLoHrKEugKHEQsYwaAlz6yPFAsF9vIR0EfIQ8yLwjMbdtOew1olTkkaqETHM79G45ikgkZAOFZq6NgJuDmWwAinRW2UKppgMsUhHWoaYUGVm8+PL6xTrYytIJa6IrDm6u+JHAulMuHrToFhopa9mfifN0whuHJzFiUp0IgsFgUptyC2ZklYYyYpAZ5pgolk+laLTLDEBHReNR2Cs/zyKum1ms55s3V30Whfl3FU0TE6QWfIQZeojW5RB3URQRl6Rq/ozXgyXox342PRWjHKmTr6A+PzB8RalX4=</latexit> gal onto subhalos using B<latexit sha1_base64="rCx6YZKyFarkehd6/kmCVau7Ixc=">AAAB8nicbVDLSgMxFM3UV62vqks3wSK4KjNV0GWpG5cV7AOmQ8mkmTY0kwzJHaEM/Qw3LhRx69e482/MtLPQ1gOBwzn3knNPmAhuwHW/ndLG5tb2Tnm3srd/cHhUPT7pGpVqyjpUCaX7ITFMcMk6wEGwfqIZiUPBeuH0Lvd7T0wbruQjzBIWxGQsecQpASv5g5jAhBKRtebDas2tuwvgdeIVpIYKtIfVr8FI0TRmEqggxviem0CQEQ2cCjavDFLDEkKnZMx8SyWJmQmyReQ5vrDKCEdK2ycBL9TfGxmJjZnFoZ3MI5pVLxf/8/wUotsg4zJJgUm6/ChKBQaF8/vxiGtGQcwsIVRzmxXTCdGEgm2pYkvwVk9eJ91G3buqNx6ua81WUUcZnaFzdIk8dIOa6B61UQdRpNAzekVvDjgvzrvzsRwtOcXOKfoD5/MHcyGRXA==</latexit> <latexit sha1_base64="gV1REod6INZYF0m2I1PcPtZcxYU=">AAAB+XicbVDLSsNAFL2pr1pfUZduBovgqiRV0WXRjRuhgn1AG8JkOm2HTiZhZlIoIX/ixoUibv0Td/6NkzYLbT0wcDjnXu6ZE8ScKe0431ZpbX1jc6u8XdnZ3ds/sA+P2ipKJKEtEvFIdgOsKGeCtjTTnHZjSXEYcNoJJne535lSqVgknvQspl6IR4INGcHaSL5t90OsxwTz9CHz0ysn8+2qU3PmQKvELUgVCjR9+6s/iEgSUqEJx0r1XCfWXoqlZoTTrNJPFI0xmeAR7RkqcEiVl86TZ+jMKAM0jKR5QqO5+nsjxaFSszAwk3lOtezl4n9eL9HDGy9lIk40FWRxaJhwpCOU14AGTFKi+cwQTCQzWREZY4mJNmVVTAnu8pdXSbtecy9q9cfLauO2qKMMJ3AK5+DCNTTgHprQAgJTeIZXeLNS68V6tz4WoyWr2DmGP7A+fwBvspOG</latexit> 50 galaxy—halo model. M σ<latexit sha1_base64="w6kf9ugSeuomJ3tKQ5nBZFNm7MY=">AAAB73icbVDLSgNBEOz1GeMr6tHLYBA8hd0o6DHoxYsQwTwgWcLsZDYZMo91ZlYIS37CiwdFvPo73vwbJ8keNLGgoajqprsrSjgz1ve/vZXVtfWNzcJWcXtnd2+/dHDYNCrVhDaI4kq3I2woZ5I2LLOcthNNsYg4bUWjm6nfeqLaMCUf7DihocADyWJGsHVSu2vYQODeXa9U9iv+DGiZBDkpQ456r/TV7SuSCiot4diYTuAnNsywtoxwOil2U0MTTEZ4QDuOSiyoCbPZvRN06pQ+ipV2JS2aqb8nMiyMGYvIdQpsh2bRm4r/eZ3UxldhxmSSWirJfFGccmQVmj6P+kxTYvnYEUw0c7ciMsQaE+siKroQgsWXl0mzWgnOK9X7i3LtOo+jAMdwAmcQwCXU4Bbq0AACHJ7hFd68R+/Fe/c+5q0rXj5zBH/gff4A8YOP5w==</latexit> M 3. Apply observational selection functions based on imaging data. Markov Chain Monte Carlo 4. Calculate likelihood of observed satellites given galaxy—halo connection parameters. Satellite Galaxy-Subhalo Model Nadler et al. 2019 Baryonic Subhalo Disruption CDM CDM + BARYONS Garrison-Kimmel et al. 2017 Observational Selection Function • Run search algorithms on simulated satellites injected into DES and PS1 data • Trained model predicts satellite detection probability (publicly available soon!) Preliminary DES MWWG in prep. Mock Satellite Observations Mock Satellite Observations Mock Satellite Observations Mock Satellite Observations simulated “LMC” Minimum Halo Mass Constraints Classical+SDSS+DES Classical+SDSS Preliminary 1.8 M 1.2 σ 0.6 8.5 min M 8.0 1.8 1.2 B 0.6 1.44 1.36 1.28 0.6 1.2 1.8 8.0 8.5 0.6 1.2 1.8 − − − ↵ σM min M B Nadler et al. in prep Minimum Halo Mass Constraints DM-Baryon Scattering Constraints • Early-time DM-baryon scattering M [M ] suppresses small-scale power 1016 1014 1012 1010 108 1.0 • Mass of the smallest halo allowed to form corresponds to the size of the horizon when 0.75 CDM /P 0.5 mWDM =0.3 keV mWDM =1.2 keV m =4.7 keV collisional WDM • Minimum inferred subhalo mass P 27 2 0.25 σ0 = 10− cm 28 2 yields cross section limit: σ0 = 10− cm 29 2 σ0 = 10− cm 0.05 0.1 1 5 10 30 50 1 k [h Mpc− ] Nadler et al. 2019 DM-Baryon Scattering Constraints 24 10− CMB Lyman-↵ XQC ] 26 2 10− MiniBoone CR [cm 0 28 σ 10− XENON1T CR 30 10− Direct Detection cross section 32 10− 34 10− 5 4 3 2 1 0 1 2 10− 10− 10− 10− 10− 10 10 10 dark matter mass mχ [GeV] Nadler et al. 2019 DM-Baryon Scattering Constraints 24 10− CMB Lyman-↵ XQC ] ] 26 XQC 2 2 10− MiniBoone CR [cm [cm 0 0 28 Milky Way Satellites σ σ 10− XENON1T CR 30 10− Direct Detection cross section cross section 32 10− Analytic Estimate Population Analysis 34 10− 5 4 3 2 1 0 1 2 10− 10− 10− 10− 10− 10 10 10 dark matter mass mχ [GeV] Nadler et al. 2019 Warm DM Constraints • Smallest detected halo directly 24 constrains WDM mass assuming 10− mχ = 10 GeV 1 thermal production: mχ = 10− GeV 25 3 10− mχ = 10− GeV ] 2 5 M 0.3 mχ = 10− GeV hm − [cm 26 10− mWDM =2.3 keV 0 109 M σ <latexit sha1_base64="bfpkQqx8y7tCSoLpEbTcEWOFBNU=">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</latexit> 27 ⇣ ⌘ 10− • Mapping between WDM and 28 10− DM-baryon scattering implies cross section 29 constraints on any “thermal” DM 10− model: 30 10− 0 2 4 6 8 10 T (σ ,m ) m mWDM [keV] dec 1 χ = WDM,1 T (σ ,m ) m <latexit sha1_base64="l49tPnaQxw1QjcWFVTZInKsn8Rk=">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</latexit> dec 2 χ WDM,2 m > 3.3 keV (95% C.L.) <latexit sha1_base64="CM4FRvfXe8rx3ZZBzUiWMe1yyPc=">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</latexit> WDM DM Formation Redshift Constraints • Excess radiation transitioning to DM after BBN (late-forming DM) suppresses small-scale power • Universal relation between size of horizon at DM formation and half- mode scale: k 1.4 k <latexit sha1_base64="WUXC2YY1wzfWoFnZkSFNB9wm1mM=">AAACBXicbVDLSsNAFJ3UV62vqEtdDBbBVUhqQZdFNy4r2Ac0IUymk3bITBJmJmIJ2bjxV9y4UMSt/+DOv3HaZqGtBy4czrmXe+8JUkalsu1vo7Kyura+Ud2sbW3v7O6Z+wddmWQCkw5OWCL6AZKE0Zh0FFWM9FNBEA8Y6QXR9dTv3RMhaRLfqUlKPI5GMQ0pRkpLvnkc+bkreD7mRQFdlKYieYCO1XRh5Ie+Wbctewa4TJyS1EGJtm9+ucMEZ5zECjMk5cCxU+XlSCiKGSlqbiZJinCERmSgaYw4kV4++6KAp1oZwjARumIFZ+rviRxxKSc80J0cqbFc9Kbif94gU+Gll9M4zRSJ8XxRmDGoEjiNBA6pIFixiSYIC6pvhXiMBMJKB1fTITiLLy+TbsNyzq3GbbPeuirjqIIjcALOgAMuQAvcgDboAAwewTN4BW/Gk/FivBsf89aKUc4cgj8wPn8Ar36YBg==</latexit> hm ⇡ f • Satellites give order-of-magnitude improvement over Lyman-alpha forest constraints: z > 7.8 106 (95% C.L.) <latexit sha1_base64="Q+y+msQm/l+TXLuFg5CnVHC/oyM=">AAACEHicbVC7TgJBFJ3FF+Jr1dJmIiFis9nFB9gYIo2FBSbySNiVzA6zMGH2kZlZE9zwCTb+io2Fxtha2vk3DrCFoie5yck59+bee9yIUSFN80vLLCwuLa9kV3Nr6xubW/r2TlOEMcekgUMW8raLBGE0IA1JJSPtiBPku4y03GFt4rfuCBc0DG7kKCKOj/oB9ShGUkld/eC+68FzWDYqtqQ+EdAyb09tWDw7sQs2tLmf1IwrY3zY1fOmYU4B/xIrJXmQot7VP+1eiGOfBBIzJETHMiPpJIhLihkZ5+xYkAjhIeqTjqIBUsudZPrQGBaU0oNeyFUFEk7VnxMJ8oUY+a7q9JEciHlvIv7ndWLpVZyEBlEsSYBni7yYQRnCSTqwRznBko0UQZhTdSvEA8QRlirDnArBmn/5L2mWDOvIKF0f56sXaRxZsAf2QRFYoAyq4BLUQQNg8ACewAt41R61Z+1Ne5+1ZrR0Zhf8gvbxDRYfmXg=</latexit> f ⇥ Das & Nadler in prep Generalized DM Constraints • Universal transfer function parameterization captures half- mode scale, large and small- scale slopes: Murgia et al. 2018 • Half-mode constraints translate into generalized DM constraints: MW Satellite Forecast Fuzzy DM Constraints • Fuzzy DM constraints are limits on curvature and scale of V(Φ): Armengaud et al. 2017 0.7 21 Mhm − m =1.3 10− eV φ 109 M <latexit 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