CMB Constraints on Dark Matter Annihilation. Neelima Sehgal Stony Brook University

Transcription

1 CMB Constraints on Dark Matter Annihilation Neelima Sehgal Stony Brook University

2 Outline The CMB in a Nutshell Current Dark Matter Annihilation Bounds from the CMB

3 Outline The CMB in a Nutshell Current Dark Matter Annihilation Bounds from the CMB

4 Cosmic Microwave Background From Lambda website

5 New Generation of Microwave Observations COBE WMAP PLANCK degree 0.1 ACT+SPT We are entering a new regime in CMB physics 0.02

6 New Generation of Microwave Observations COBE WMAP PLANCK degree 0.1 ACT+SPT We are entering a new regime in CMB physics 0.02

7 COBE Satellite 1994

8 WMAP Satellite 2003

9 Planck Satellite 2013

10 Other CMB Experiments ACTpol SPTpol Have broad science range ABS Polarbear SPIDER BICEP Dedicated to r

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12 ACTpol / AdvACTpol ACTpol - Observes from ~4000 sq deg (10% of sky) 4 x better sensitivity than Planck 5 x better resolution than Planck AdvACTpol ~20,000 sq deg (50% of sky) 4 x better sensitivity than Planck 5 x better resolution than Planck

13 Made by Clem Pryke

14 Planck Power Spectrum Planck Results 2013, Paper 1

15 Parameters Change CMB Power Credit: Wayne Hu

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17 CMB Polarization From Lambda website

18 CMB Polarization Temp Temp x E pol E pol B pol

19 First Results from ACTpol Best High-ell EE Power Spectrum Measured to Date! Naess et al. 2014,

20 Outline The CMB in a Nutshell Current Dark Matter Annihilation Bounds from the CMB

21 Dark Matter Annihilation During Recombination e + e Image Credit: William Kinney

22 Energy Deposition in Pre- and Post-Recombination Gas/Plasma Ionization Excitation Heating

23 Effect of Dark Matter Annihilation on CMB Suppression of temperature peaks Enhancement of polarization peaks Suppression of polarization peaks Galli et al ( )

24 Universal Energy Deposition Curve 2.0 w/o Sys. Corrections w/ Sys. Corrections f(z) = 41 X i f i (z) 1.5 i=1 e(z) f(z) = 41 X i=1 ie i (z) Redshift z gives 99.9% of CMB power spectrum variance Padmanabhan & Finkbeiner; Slatyer, Padmanabhan, Finkbeiner; Finkbeiner, Galli, Lin, Slatyer

25 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 Fermi Inner Galaxy l 2 DM candidates favored by direct and indirect searches AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] p ann / f e h vi M This cross section gives right amount of dark matter today if perfect energy absorption (feff=1) Madhavacheril, NS, Slatyer 2014, PRD, ( )

26 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 Fermi Inner Galaxy l 2 DM candidates favored by direct and indirect searches AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] p ann / f e h vi M This cross section gives right amount of dark matter today if expected energy absorption (feff ~ 0.2) Madhavacheril, NS, Slatyer 2014, PRD, ( )

27 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Latest constraint using WMAP9+Planck+ACT +SPT+BAO+HST+SN Madhavacheril, NS, Slatyer 2014, PRD, ( )

28 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Latest constraint using WMAP9+Planck+ACT +SPT+BAO+HST+SN *from CMB Madhavacheril, NS, Slatyer 2014, PRD, ( )

29 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Latest constraint using WMAP9+Planck+ACT +SPT+BAO+HST+SN *from low-redshift data Madhavacheril, NS, Slatyer 2014, PRD, ( )

30 Current Constraints feff <σ v> [cm 3 s 1 ] Planck forecast Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 cosmic variance limit WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Madhavacheril, NS, Slatyer 2014, PRD, ( )

31 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] AdvACTpol Madhavacheril, NS, Slatyer 2014, PRD, ( )

32 feff <σ v> [cm 3 s 1 ] e.g. PAMELA/Fermi/AMS DM + DM! A 0 A 0, Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 cosmic variance limit WMAP 9 + Planck + ACT + SPT + BAO + HST + SN A 0! e + e, µ + µ, + Arkani-Hamed et.al., Pospelov & Ritz (based on fit by Cholis & Hooper, ) standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Madhavacheril, NS, Slatyer 2014, PRD, ( )

33 Alpha Magnetic Spectrometer AMS-02

34 AMS-02/PAMELA/Fermi Dark Matter? electrons plus positrons are flat to 1 TeV Rise in positron fraction Pulsars? AMS-02/PAMELA Fermi AMS-02/PAMELA Fermi Cholis & Hooper, 2013, ( )

35 Fermi Inner Galaxy Hooper & various collaborators DM + DM! hadrons/leptons feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 cosmic variance limit WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Madhavacheril, NS, Slatyer 2014, PRD, ( )

36 Figure Credit: Tim Linden

37 Fermi Inner Galaxy Millisecond Pulsars? Seen away from center also Hooper et al., 2013, ( ) Hooper & Slatyer, 2013, ( )

38 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] 5 AdvACTpol discovery line AdvACTpol Madhavacheril, NS, Slatyer 2014, PRD, ( )

39 Current Constraints feff <σ v> [cm 3 s 1 ] Currently Excluded by Cosmology AdvACT full Planck (temp and pol) / CMB stage 4 WMAP 9 + Planck + ACT + SPT + BAO + HST + SN standard thermal dark matter = 3 x10-26 cm 3 s -1 l 50 cosmic variance limit = 1 = 0.2 DM candidates favored by direct and indirect searches Fermi Inner Galaxy l 2 AMS-02/PAMELA/Fermi Direct Detection: CDMS, CoGeNT, CRESST, and DAMA M χ [GeV] Cosmic Variance Limit Madhavacheril, NS, Slatyer 2014, PRD, ( )

40 Conclusions Dark matter annihilation constraints from CMB and Low-z data have been updated New limits are a factor of 2 better than before Constraints are probing interesting regimes Future reach of Planck and Advanced ACTpol is exciting- may find/confirm a DM signal with CMB