Fundamental Physics / Dark Matter - NASA · 2015-08-12 · Fundamental Physics / Dark Matter. R....
Transcript of Fundamental Physics / Dark Matter - NASA · 2015-08-12 · Fundamental Physics / Dark Matter. R....
![Page 1: Fundamental Physics / Dark Matter - NASA · 2015-08-12 · Fundamental Physics / Dark Matter. R. Caputo, UCSC Overview •Mission Assumptions – MeV/GeV Space-Based •Dark Matter](https://reader036.fdocuments.us/reader036/viewer/2022062602/5ed2f8baa9caa7002f55bc51/html5/thumbnails/1.jpg)
R. CaputoUCSC
29 June 2015GammaSIG Session
HEAD meeting - Chicago
Fundamental Physics / Dark
Matter
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R. Caputo, UCSC
Overview
•Mission Assumptions – MeV/GeV Space-Based
•Dark Matter – MeV and Light GeV range Dark Matter
• The WIMP (and not exactly a WIMP) story • Axion-like particles
– GeV range Dark Matter • WIMPs
•New/Fundamental Physics – Complementary detections, multi-wavelength/messenger
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R. Caputo, UCSC
MeV Mission Assumptions
•An idea of mission capabilities (typically MIDEX class)
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***An attempt to get common parameters among missions*** Not meant to be exhaustive list - only to define parameter
space for new physics searches
Benchmark: 1 MeV-1 GeV, E Res best at 1 MeV Large FOV, Flux sensitivity ~10-6 MeV cm-2s-1
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R. Caputo, UCSC
GeV Mission Assumptions
•An idea of mission capabilities (Probe class)
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***An attempt to get common parameters among missions*** Not meant to be exhaustive list - only to define parameter
space for new physics searches
~1B$ instrument, 3mx5m scintillating fiber tracker, 3.5 times the mass of Fermi, 50 tracker layers, 5.5 radiation length calorimeter in LEO launched by a Falcon 9.
0.1 0.5 1.0 5.0 10.0 50.0 100.0
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E HGeVL
DEêE
0.1 0.5 1.0 5.0 10.0 50.0 100.0
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1.0
2.0
5.0
E HGeVL
sHdegL
Ang. Res. E Res.
APT2
Goal: DM Dwarf sensitivity improved by x10
0.1 1 10 1001¥10-13
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E HGeVL
nFnHerg
s-1 cm-2 L — Fermi-LAT
— APT2
Sensitivity
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R. Caputo, UCSC
A brief history of Dark Matter
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Particle Physics Astrophysics
Cosmology
Particle Dark Matter
Weakly Interacting Massive Particles
Axions
See J. McEnery’s Talk from earlier today…
DM is there, it’s likely a particle it could be many
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R. Caputo, UCSC
Dark Matter Detections
6Slide from Y. Mambrini, 2nd AstroGAM workshop
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R. Caputo, UCSC
Dark Matter Detections
6Slide from Y. Mambrini, 2nd AstroGAM workshop
No Detections
… No
Instrument
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R. Caputo, UCSC
MeV Dark Matter
•Why MeV (WIMP-ish) Dark Matter? – Lee-Weinberg: Cosmological lower bound on heavy neutrino mass
(1977)
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𝛀h2
m𝛘
Thermal relic ~0.1
Too Light? Over produce!
~√10 GeV
𝛀h2∝<σv> = GF2m𝛘2 > 10-9 GeV-2
1. GF2m𝛘2⟹G’F2m𝛘2
Non-SM interaction (not strictly Weakly Interacting)
2. Or not strictly a thermal relic (bound by BBN ~1 MeV)
Two Scenarios:
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R. Caputo, UCSC
MeV Dark Matter
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RC, E. Carlson, F. D’Eramo, and S. Profumo: in preparation
Scan new MeV DM
parameter space to
develop a gamma-ray spectrum
Complement current parameter space…
gamma-rays ~order(-1) DM mass
E𝛄 [GeV]
dN/d
E [G
eV-1
]
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R. Caputo, UCSC
MeV Dark Matter
•Axions in neutron stars (hep-ph/0505090) – emission process for axions with mass up to a few MeV – production in Gamma Ray Bursts
•Axions produced in supernovae (arXiv:1410.3747) – core collapse supernova (SN1987A)
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massless ALP (ma~10−11 eV) with gaγ = 10−10 GeV−1
18 Msol progenitor
timing of photons between (25-100 MeV) with gaγ = 10−10 GeV−1
18 Msol progenitor
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R. Caputo, UCSC
GeV Dark Matter
•GeV DM candidate is standard WIMP picture – Theoretically Motivated
•To cover thermal relic OM sensitivity needed
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R. Caputo, UCSC
GeV Dark Matter
•GeV DM candidate is standard WIMP picture – Theoretically Motivated
•To cover thermal relic OM sensitivity needed
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R. Caputo, UCSC
New/Fundamental Physics
•Complementary detections with other messengers •Gravitational wave detectors
– 2nd generation coming online 2016-ish (LIGO, VIRGO) – GRBs are a GW signal (~50 SHB/year) (E. Chassande-Mottin)
•Neutrino detectors – Complementary: sources of particle acceleration
•Understanding the Galactic Center – Point sources and pulsars
• good angular resolution
• diffuse from ICS (more isotropic), less from 𝛑0
•Open to ideas for physics to add •Discussion
11http://astrogam.iaps.inaf.it/Program_Astrogam2.html
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R. Caputo, UCSC
Backups
12Shamelessly stolen from Elizabeth Ferrara
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R. Caputo, UCSC
What Happens at the MeV scale?
•Fluxes shown as a function of total kinetic energy of particles
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Backgrounds: protons (green filled triangles up), He (purple filled triangles up), electrons (filled red squares), positrons (light blue squares), Earth albedo neutrons (black squares), and Earth albedo γ-rays (dark blue filled triangles down).
1GeV
1GeV
Gamma-Ray production: below 100 MeV gammas from 𝛑0 decay drops