search results and prospects from atmospheric cherenkov ...search results and prospects from...
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![Page 1: Search Results and Prospects from Atmospheric Cherenkov ...Search Results and Prospects from Atmospheric Cherenkov Telescopes Andrew W Smith University of Marland, College Park / NASA](https://reader030.vdocuments.mx/reader030/viewer/2022040412/5f06977b7e708231d418c0ed/html5/thumbnails/1.jpg)
Search Results and Prospects from Atmospheric Cherenkov
Telescopes
Andrew W Smith University of Marland, College Park / NASA GSFC
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From P5 report (Cosmic Frontier) Arrenberg et al.
Indirect Detection probes a wide range of theory space in DM
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In an ideal situation, DM
should produce a
very recognizable
signal in gamma rays
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Imaging Atmospheric Cherenkov Technique:
Primary gamma rays initiate EM showers w
particle v>c: Cherenkov pulses
HESS (Prague WG) Arrenberg et al.
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Current TeV Experiments
VERITAS Southern AZ, USA 4x12m
MAGIC-II Canary Islands 2 x 17m
HESS-II Namibia
4x12.5, 1x 28
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* Energy range: ~80 GeV to >30 TeV
* Energy resolution: 15% at 1 TeV * observation time per year: ~1200
hours * point source sensitivity: 1% Crab
in <30h, 10% in <30 min
Rough Performance Valuesfor Current Generation IACTs
Instrumental PSF
= ~600 ɣ/hr (0.1-50 TeV) in footprint of array
Current IACTs can detect (5σ) sources producing 6 ɣ/hr in 25 hrs
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Indirect Detection of DM w/IACTs
Assume all the 𝛾s you didnt see is
this:Constrain this
Choose some ppp model to tell
you what you should have seen
Find an real astronomer to model this for
you
M𝜒
σv
Constraint s= Discrete SUSY parameter scan results.
Above curve = disallowed model
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Indirect Detection of DM w/IACTs
This term is very sensitive to
fluctuations in methods progress?
Significant progress
M𝜒
σv
Constraint s= Discrete SUSY parameter scan results.
Above curve = disallowed model
What have we learned about this
equation?
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Target Advantages Disadvantages
Galactic Center Close by, lots of DM Large 𝛾 BG
Galactic Substructure
Possibly local, Fermi-LAT sources Unknown distance, nature
Galaxy Clusters-Largest DM
concentrations in universe
-very distant (weak signal) -very extended -possible 𝛾 BG
Dwarf Galaxies -High Mass/Light -No likely 𝛾 BG
DM distribution can be very uncertain
IACT DM Targets
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Target Advantages Disadvantages
Galactic Center Close by, lots of DM Large 𝛾 BG
Galactic Substructure
Possibly local, Fermi-LAT sources Unknown distance, nature
Galaxy Clusters-Largest DM
concentrations in universe
-very distant (weak signal) -very extended -possible 𝛾 BG
Dwarf Galaxies -High Mass/Light -No likely 𝛾 BG
DM distribution can be very uncertain
IACT DM Targets
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Galactic Center
HESS >300 GeV
Peak of DM profile
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2011 Abramowski et al. 112 Hours of H.E.S.S. Data
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254 Hours of H.E.S.S. data 2015 Le Franc et al (ICRC)
HESS II
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VERITAS Galactic Center (> 2 TeV)
VERITAS Observations will constrain multi-Tev
parameter space
VERITAS 100 hr estimate
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Dwarf Spheroidal Searches
from Drlica-Wagner 2014/Ackermann et al 2015 and
source therein
J ~ (DM density profile)2 along line of sight
NFW Profile, 0.50 integration radiusSagittarius
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from Drlica-Wagner 2014/Ackermann et al 2015 and
source therein
Sagittarius
HESSMAGIC
VERITAS
Dwarf Spheroidal Searches
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Dwarf Spheroidal Searches
from Drlica-Wagner 2014/Ackermann et al 2015 and
source therein
Sagittarius
All 3 IACTs have accrued ~150-200 hrs
on dSphs.
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MAGIC (165 hrs on Segue I) (Aleksic et al 2015)
VERITAS 215 hours on 4 dSphs Zitzer et al 2015)
HESS Combined Limits: 140 hours on 5 targets
(Abramowski et al 2014)
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MAGIC (165 hrs on Segue I) (Aleksic et al 2015)
VERITAS 215 hours on 4 dSphs Zitzer et al 2015)
HESS Combined Limits: 140 hours on 5 targets
(Abramowski et al 2014)
Aleksic et al 2014
Likelihood methods improve limits by 2-3
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MAGIC (Einasto)
VERITAS HESS
NATURAL CROSS SECTION
IACT Dwarf Spheroidal Limits
𝝌 𝝌 -> 𝜏+ 𝜏-
NFW
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MAGIC (EInasto)
VERITASHESS dSph
NATURAL CROSS SECTION
HESS GC
𝝌 𝝌 -> 𝜏+ 𝜏-
NFW
IACT Dwarf Spheroidal Limits
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Limits on 𝞆 𝞆 -> ɣ ɣ
HESS GC
VERITAS dSPHs
MAGIC Segue I
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Where can we go from here?
MOU in preparation between IACTs
to combine data, joint likelihood methods may
improve limits on full data set
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Where can we go from here?
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CTA Design (S array)
Low energies Energy threshold 20-30 GeV 23 m diameter 4 telescopes (LST’s)
Medium energies 100 GeV – 10 TeV
9.5 to 12 m diameter 25 single-mirror telescopes
up to 24 dual-mirror telescopes (MST’s/SCTs)
High energies 10 km2 area at few TeV
3 to 4m diameter 70 telescopes
(SST’s)
Science Optimization under budget constraints
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Hinton & Funk arXiv:1205.0832
HESS / VERITAS 100 hrs
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Hinton & Funk arXiv:1205.0832
HESS / VERITAS 100 hrs
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300 h
Galactic Plane Survey
525 h
300 h Fermi bubbles
Galactic PlaneSurvey
In the first 3 years of
observations, CTA will
observe the GC for >500
hours
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Thermal DM
CTA
con
sorti
um, i
n pr
epar
atio
n
CTA GC Limits
CTA will probe deep into natural cross section within 3 years of operation
Silverwood, et al., JCAP 03, 055 (2015) Lefranc, et al., PRD 91, 12 (2015)
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Summary-Current Generation of IACTs have developed and executed a multi-year DM search program (still in
progress)
-These programs (significant) have set deep limits, although still mostly separate from the natural cross section. Progress on combining limits.
-These programs have paved the way for upcoming searches with CTA, this search will
probe deep into the natural cross section within the first few years of operation