Baryonic Antimatter in Cosmic Rays

Transcription

1 Baryonic Antimatter in Cosmic Rays Context & propagation Antiprotons Antideuterons [USINE & CLUMPY ] David Maurin (LPNHE) dmaurin@lpnhe.in2p3.fr PPC 2010 Torino, 15th July 2010

2 (Still) open questions in CR physics 1. Do we understand the standard galactic fluxes? - Sources (SN, pulsars, SB...) - Nucleosynthesis (r and s-process for heavy nuclei) - Acceleration mechanisms (injection, B amplification) - Propagation mechanisms (link to turbulence, spatial dependence, isotropy) - Magneto-cosmico-gaseo properties of the Galaxy (MHD description) i) GCRs here/in the whole Galaxy (linked to diffuse emissions) ii) GCRs now/in the past/future (linked with massive extinctions?) 2. Do we understand Solar Modulation? 3. Are GCRs a good laboratory to search for new physics? - Dark matter/new physics? - Just standard astrophysics? I. Context & propagation

3 ~ Milestones ~ Measurements AMS, CREAM, FERMI, PAMELA, TRACER,... Acceleration 2000 Non-linear magnetic field amplification in diffusive shocks (à la Bell & Lucek) Transport 2000's Necessity to take into account time-dependent effects and local sources? 2010's Inhomogeneous transport, MHD self-consistent approaches? I. Context & propagation

4 Cosmic Ray journey in 3 steps: Requirement: consistent description of all fluxes (electrons, nuclei and gamma) 1. Synthesis and acceleration 2. Transport (diffusion & interactions) 3. Solar modulation+detection HESS 1 FERMI, AMS-γ 2 ν _ d ν ANTARES km3 3 Adapted from Moskalenko et al. (2004) AMS GAPS AMS, CREAM, PAMELA => Search for DM where standard production is rare (secondary) => Use LiBeB to calibrate the transport coefficients I. Context & propagation

5 Basics on transport: diffusion and source slope Steady-state: 1D Diffusion Model vs LeakyBox Model D => Link between LBM and diffusion models Degeneracy: Models with the same D0/L are equivalent (secondary-to-primary production) Simple case: secondary-to-primary ratio High energy: I. Context & propagation

6 Phenomenology of the DM signal Maurin et al., 2006a [arxiv:astro-ph/ ] Maurin et al., 2006b [ arxiv:astro-ph/ ] Taillet & Maurin, A&A 402, 971 (2003) Maurin & Taillet, A&A 404, 949 (2003) 1) Good approximation to neglect: energy losses, spallations 2) In 1D model (only z-dependence): 3) Breaks Do/L degeneracy: 2D => signal uncertainty scales as L => signal not very sensitive to (r) near the GC (if L 10 kpc) [pbar and dbar PBH] Barrau et al., A&A 388, 676 (2002) Barrau et al., A&A 398, 403 (2003) [pbar and dbar SUSY & KK] Donato et al., PRD 69, (2004) Barrau et al., PRD 72, (2005) Donato et al., PRD 78, (2008) N.B.: effect of Vc or Vl (at low energy) can also be addressed I. Context & propagation

7 Transport parameter determination: status => already tricky in a given configuration Automated parameter scan Maurin et al., ApJ 555, 596 (2001) Maurin, Taillet & Donato, A&A 394, 1039 (2002) => δ [ ] Markov Chain Monte Carlo scan [+ local bubble (determination of L)] Donato, Maurin & Taillet, A&A 381, 539 (2002) Putze et al., A&A 497, 991 (2009) Putze, Derome & Maurin, A&A 516, A66 (2010) Systematic uncertainties Maurin, Putze & Derome, A&A 516, A67 (2010) => L [1-50] kpc => ingredients yield Sys.Unc.>Stat.Unc. => But definitively no standard propagation model yet... Bloemen et al. A&A 267, 372 (1993) Erlykin & Wolfendale, J. Phys. G 28, 2329 (2002) Jones et al., ApJ 547, 264 (2001) Ptuskin & Soutoul, A&A 337, 859 (1998) Shibata et al., ApJ 642, 882 (2006) Berezhko et al., A&A 410, 189 (2003) Breitschwerdt et al., A&A 385, 216 (2002) Evoli et al. JCAP 10, 18 (2008) Farahat et al., ApJ 681, 1334 (2008) Strong & Moskalenko, ApJ 509, 212 (1998) => Semi-analytical (homogeneous D, linear wind) => Semi-analytical (use (r), linked to turbulence level) => Semi-analytical (homogeneous D, constant wind) => Semi-analytical (radioactive nuc. and LISM) => Semi-analytical (inhomog. D, no V) => Secondary production in source => Numerical (homog. D, but V(r,z)) => Numerical (inhomogeneous D, no V, no E losses) => Numerical (backward Markov stochastic processes) => Numerical (cst + linear wind) + anisotropic diffusion (e.g., to explain the knee) + time-dependent effects (HE leptons) + MHD couplings of magnetic fields, CRs and gas... I. Context & propagation

8 Context & propagation Antiprotons Antideuterons [USINE & CLUMPY ]

9 Current measurements: interpretation PAMELA, arxiv 1007:0821 BESS, PRD 95, (2005) => Antiprotons: consistent with secondary production => Antideuterons: only upper limit II. Antiprotons

10 Primary signal: boost for antinuclei? Lavalle et al., A&A 479, 427 (2008) Donato et al., PRL 102, (2009) + Via Lactea II simulation ~O (1) [Diemand et al.,nature 454, 735 (2008)] => No boost from substructures => typical constraint on signal enhancement from PAMELA data => high precision measurement of antiprotons helpful => triggered useful multi-messenger analysis of DM candidates... II. Antiprotons

11 Context & propagation Antiprotons Antideuterons [USINE & CLUMPY ]

12 Antideuteron & detection (1) 1997 The Production of Anti-Matter in our Galaxy Chardonnet, Orloff & Salati, Phys.Lett. B 409, 313 (1997) [...] AMS should detect a few cosmic ray anti-deuterons. [...] a single anti-helium would be a smoking gun for the presence of anti-matter in the universe and for the existence of anti-stars and antigalaxies Antideuterons as a Signature of Supersymmetric Dark Matter Donato, Fornengo & Salati, Phys. Rev. D 62, (2000) If a few low energy antideuterons are measured [by the future AMS experiment on board ISSA], this should be seriously taken as a clue for the existence of massive neutralinos in the Milky Way 2002 A Novel Antimatter Detector Based on X-Ray Deexcitation of Exotic Atoms Mori et al. (GAPS collab.), ApJ 566, 604 (2002) We propose a novel antiparticle detector [...].This space-based search for the neutralino is capable of achieving comparable sensitivity to as yet unrealized third-generation, underground DM experiments 2005 Flux of light antimatter nuclei by CRs in the Galaxy and in the atmosphere Duperray et al., Phys. Rev. D 71, (2005) The hadronic production cross section is based on a recent parametrization of a wide set of accelerator data. The non annihilating inelastic scattering process is taken into account for the first time 2005 Search for Cosmic-Ray Antideuterons Fuke et al. (BESS collab.), Phys. Rev. D 95, (2005) We derived, for the first time, an upper limit of (m2s sr GeV/nuc)-1 for the differential flux of CR antideuterons, at the 95% conf. level, between GeV/nuc at the top of the atmosphere. III. Antideuterons

13 Antideuteron & detection (2) 2006 Accelerator testing of the general antiparticle spectrometer; a novel approach to indirect dark matter detection Hailey et al. (GAPS collab.), Phys. Rev. D 01, 007 (2006) GAPS captures antideuterons into a target with the subsequent formation of exotic atoms. The latter decay with the emission of x-rays[...]. This signature uniquely characterizes the antideuterons Antideuteron fluxes from dark matter annihilation in diffusion models Donato, Fornengo & Maurin, Phys. Rev. D 78, (2008) updated calculation of both the secondary and primary dbar fluxes. GAPS and AMS-02 provide exciting perspectives for a positive measurement in the near future 2009 An indirect search for dark matter using antideuterons: the GAPS experiment Hailey et al. (GAPS collab.), New Journal of Physics 11, (2009) GAPS is funded for a prototype flight in 2011, to be followed by a long duration balloon flight to execute its science program Enhanced anti-deuteron Dark Matter signal and the implications of PAMELA Kadastik, Raidal & Strumia, Phys. Lett. B 683, 248 (2010) Jet structure of DM annihilation enhances the dbar production rate by orders of magnitude w.r.t. the spherically symmetric coalescence mode. Searches become sensitive to heavy DM above O(1) GeV scale [my apologies for unquoted studies] III. Antideuterons

14 Antideuteron secondary flux Donato et al., PRD 78, (2008) ph phe Total HeH HeHe -p H -p He => Transport uncertainty (<40%), as for pbar [should decrease soon: PAMELA, AMS] => Nuclear uncertainty ~ factor of 10 [more nuclear data required] III. Antideuterons

15 Primary flux: promising prospects for detection ULDM = Ultra Long Duration Flight ( days) LDB = Long Duration Flight Kadastik et al., PLB 683, 248 (2010) Donato et al., PRD 78, (2008) => Spherical cow or more realistic coalescence scheme (dbar from pbar-nbar pairs), very good perspectives for the near future III. Antideuterons

16 Conclusions 1. Background are mostly under control - propagation uncertainties will further decrease with PAMELA & AMS-02 - nuclear uncertainties still O(1) for antideuterons => production in source expected at some energy, but level unknown 2. Signal still plagued by many uncertain uncertainties - transport in the diffusion halo not really constrained - boost #1 inefficient, boost #2 natural? What's next? => cross-constrained may be helpful, but as well be useless Antideuterons definitely look promising - AMS on ISS in 2010 ( new magnet still OK for dbar?) - GAPS prototype flight in 2011 => Dbar may be one of the most sensitive probe for DM indirect detection

17 Context & propagation Antiprotons Antideuterons [USINE & CLUMPY ]

18 USINE: a propagation code We are working hard to make it public (~September 2010) - V1.0 public release - Online Database (data + weblinks + macros) - Website (simple model online calculation) USINE-core (+ root-like documentation): D.M. (LPNHE) Database: R. Taillet (LAPTh) GUI: F. Barao (LIP) Fit +MCMC tools: A. Putze (KTH), L. Derome (LPSC) and expected for subsequent releases e+/e-: T. Delahaye, F. Donato, J. Lavalle, R. Lineros, P. Salati Fiasson & others Z>30: C. Combet & others More tools (genetic algo. + model comp.): A. Putze & L. Derome N'USINE (N'umerical USINE): B. Coste & others Better Solar modulation: discussions in progress... => to be thought as a toolbox to implement your own models

19 CLUMPY: a code for DM annihilations in the Galaxy Charbonnier, Combet & Maurin (submitted soon) [public code: smooth/dsphs/(sub)clumps, Doxygen documentation] J for a Dsph: 2 2 [core profile + NFW/B01 subclumps] [d=100 kpc, no gal. bkgd] Skymap slice toward = (-120,20) [ (r) + dp/dv(r) + clump profiles = Einasto] res. = 0.1 res. = 0.05 Charbonnier, Combet, Daniel, Hinton, Maurin, Power, Read, Sarkar, Walker, & Wilkinson Dsphs & γ-ray observatories (submitted soon) => 2nd release to include more messengers