Explore DM Blind Spots with Gravitational Wave

Transcription

1 Explore DM Blind Spots with Gravitational Wave University of Massachusetts Amherst F. P. Huang, JHY, BLV 017 May 16, 017

2 Motivation Higgs & GW discoveries, evidence of Dark Matter, connection among them? Higgs El Hedri s talk Higgs portal DM Electroweak baryogenesis Ramsey-Musolf s talk DM EWPT Kuhnel s talk Primordial black hole DM GW PT GW detection Mertens s talk Long s talk

3 Inert Scalar Dark Matter A simplified model rules them all Higgs DM Inert Scalar EWPT GW See also Wagner s and Guo s talk 3

4 Outline Review general inert scalar dark matter models How to realize strong first order phase transition, while avoiding other constraints? Motivate the mixed dark matter which has strong first order phase transition, viable dark matter candidate, GWs, etc 4

5 General Inert Scalar DM Minimal Dark Matter: scalar multiplet DM Higgs H H H n n Scalar DM H n = 0 +j. j 1 C A (j +1,Y) Direct detection bound SI ' f N Cirelli, Fornengo, Strumia 007 Hambye, Ling, Honorez, Rocher 009 H 4 Thermal relic cross section: constraint on DM mass m N m m h! H small! DM: neutral component h vi ' n4 4n +3 n g 4 18 M + 1 n H 16 M ' n4 4n +3 n g 4 18 M 5

6 Strong EW Phase Transition Thermal barrier in effective potential V (H, T) =m (T )H ETH 3 + (T )H 4 Strongly first order phase transition condition (sphaleron decoupling) v c T c E sph (T c ) ' 1.16 New scalar needs to be light (< 00 GeV) to be in thermal plasma during EW phase transition Scalar multiplet DM case E ' 1 v 3 0 m 3 W + m 3 Z + n 3/ H v 0 Large scalar d.o.f enhances size of PT M (H, T) ' H H +(n 1)g T Large screening reduces size of PT 6

7 Strong EWPT in Inert DM Tension between strong FOPT and Direct Detection E ' 1 v 3 0 m 3 W + m 3 Z + n 3/ H v 0 SI H 4! H small! h vi(! W W/ZZ)! m > 0.54 TeV(n > 1) not in plasma during EWPT Higgs resonance region usually not good because small coupling needed for relic abundance Lesson I: strong FOPT strength is related to direct detection rate Lesson : thermal relic is fully determined by gauge interactions, typically heavy dark matter Hard to realize strong FOPT in scalar multiplet models Need to avoid the above general relations Break relations or Higgs resonance region 7

8 Strong PT in Singlet DM Light WIMP DM possible due to SU()L singlet Direct Detection rules out large region h vi! m > 10 GeV(n = 1) Higgs resonance region: Need larger coupling to realize strong FOPT De Simone, Giudice, Strumia 014 Beniwal, et.al

9 Strong PT in Inert Doublet DM No direct correlation between strong PT and direct detection m + = µ v Different parameter dependence: m N SI ' fn m m h E v 3 ' 6m3 W +3m3 Z v / = / / m A = µ + 1 ( )v m H = µ + 1 ( 345)v Region: lambda3, lambda4 and lambda5 large (non-degenerate mass) But Lambda345 small due to cancellation among them And inert scalar should be lighter than 00 GeV 9

10 Inert Doublet DM Two regions allowed by WIMP DM + Higgs data + Oblique ST Belyaev, et.al

11 Inert Doublet DM Non-degenerate mass pattern allowed Near Higgs funnel region with small lambda345 Belyaev, et.al. 016 Benchmark point µ = 60 GeV, 3 =.8, 4 = 5 = 1.4, 345 =0.01 m + = m A >m H ' 60 GeV 11

12 Inert Doublet DM WIMP DM, Strong PT and Gravitational Wave Huang, JHY, 017 CEPC: 0.4% with 10 ab-1 data 1

13 Inert Higher Multiplet DM Usually tension between direct detection and sfopt Relic density (VV channel) usually needs heavy scalar Higgs resonance region usually won t help, except inert HDM Also high multiplets encounter other tight collider constraints Strength of first order phase transition decreases for higher multiplet Large screening effects Usually large multiplicity not good. possible for special potential setup AbdusSalam, Chowdhury, 014 How about increasing number of scalar multiplet? 13

14 Mixed Scalar Dark Matter Mixed dark matter: singlet-doublet, singlet-triplet models Need singlet to decrease the DM mass (relic density consideration) Should avoid higher multiplet (otherwise mostly singlet) H Higgs H H H n n + HS H HS Scalar singlet + doublet or triplet Cohen, Kearney, Pierce, Tucker-Smith 011 Cheung, Sanford 013 Advantage 1: blind spot region for direct detection!!! Advantage : large coupling for strong FOPT is still possible Advantage 3: Singlet component of DM helps reduce the DM mass (keep in thermal plasma) 14

15 Mixed Singlet-Doublet DM Real singlet plus complex doublet V = MD + 3 H H + 4 H + 5 [( H) + h.c.] + 1 M SS + 1 S S H + A S H + h.c. Mixed dark matter candidate = cos S sin 0, s =sin S + cos 0. Blind spot region: direct detection OK Blind spot Conditions: L ( S v sin v cos A sin )h L ( S v cos v sin + A sin )hss For small (large), 345 ( S ) approaches to zero! For moderate, cancellation among three terms! When minimize hdm coupling, hss coupling maximized (good for sfopt)! 15

16 Mixed Singlet-Doublet DM Relic density induces small mixing angle Gauge contribution dominant Small mixing angle for light DM (< 00 GeV) Large thermal barrier if small mixing and small lambda345 E v 3 ' 6m3 W +3m3 Z v / / +( h ) 3/ +( hss) 3/ 16

17 Mixed Singlet-Doublet DM Large parameter region with broad DM mass range 3 =3.006, 4 = 1.5, 5 = 1.5, S =4.006, A = 91 GeV M D = M S = GeV 17

18 Mixed Singlet-Triplet DM Real singlet plus Y = 0 real triplet V = 1 M SS + M Tr( )+apple H HTr( ) + apple H S + SH H. Mixed dark matter candidate = cos S sin 0, s =sin S + cos 0. Small mixing angle for light DM (< 00 GeV) Blind spot region and sfopt L (applev sin + apple v cos v sin )h L (applev cos + apple v sin + v sin )hss sfopt E v 3 ' 6m3 W +3m3 Z v 3 +( h ) 3/ +( hss ) 3/ +(apple /) 3/ 18

19 Mixed Singlet-Triplet DM Benchmark point apple =0.01, apple =3.0, = , M = 50 GeV, M S = GeV 19

20 Conclusion Study strongly first order phase transition and gravitational wave in classified general scalar multiplet DM model Typically hard to realize due to tension among strong FOPT and direct detection, relic density requirement. Inert HDM: small parameter region allowed (near Higgs resonance region) Mixed scalar dark matter could produce strong FOPT and GW Large parameter region (broad DM mass range) due to singlet-non-singlet mixing Blind spot region could avoid direct detection constraints and obtain viable WIMP DM, strong FOPT and GW Thank You! 0

21 Backup Bubble nucleation rate Latent heat release inverse time of PT 1