department of physics, university of udine, italydeangeli/fismod/vhegamma.pdf · 2012. 12. 4. · 3...
TRANSCRIPT
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Cluster of very bright stars, Omega Centauri,
as observed from the space:
60,000 K
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μ
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~ parsecs
Accretion Disk 3- 10 rs Black Hole Diameter = 2rs ~ 4 AU
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E2 d
N/d
E
energy E
e- (TeV) Synchrotron (eV-keV)
(TeV) Inverse Compton (eV)
B
e.m. processes
0decay
-
0
+
(TeV)
p+ (>>TeV)
matter
hadronic cascades
VHE
In the VHE region, dN/dE ~ E- ( : spectral index)
To distinguish between had/leptonic origin study Spectral Energy Distribution (SED): (differential flux) . E2
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Radio 408 Mhz
Infrared 1-3 μm
Visible Light
Gamma Rays
Centre of Galaxy in Different Photon Wavelengths
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New instruments often give unexpected results:
With future new detector can again hope for completely new discoveries
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De Angelis, Galanti, Roncadelli 2011
with Franceschini EBL modeling
30 G
eV
100 G
eV
red
shif
t z
ray energy (TeV)
= 1 (GRH)
> 1
region of opacity
VHE bck e+e-
( ) ~
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• The earth atmosphere (28 X0 at
sea level) is opaque to X/ Thus
only a satellite-based detector
can detect primary X/
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Atmospheric
Sat
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17 Unfolding is a nice mathematical problem !
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e+ e-
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Incoming
-ray
~ 10 km
~ 1o
Che
renk
ov li
ght
~ 120 m
Image intensity
Shower energy
Image orientation
Shower direction
Image shape
Primary particle
The Cherenkov technique
c ~ 1º
e Threshold @
sl: 21 MeV
Maximum of a 1 TeV
shower
~ 8 Km asl
~ 200 photons/m2 in
the visible
Angular spread ~ 0.5º
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Crab
10% Crab
1% Crab
Fermi
Magic-II
E*F
(>E
) [
TeV
/cm
2s]
Agile
, F
erm
i, A
rgo,
Haw
k:
1 y
ear
Magic
, H
ess,
Verita
s,
CTA
: 50h
Agile
Argo
Hess/Veritas
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24 Marvel 1961
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= ln
=
/( )+( )
(> )
=/( )
+( )
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R 10 km, B 10 T E 10 TeV
Large Hadron Collider
Tycho SuperNova Remnant
E BR
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μ
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μ
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extremely difficult
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dN
dE
dNp
dE p
D x =E
E p
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Fermi,
Egret
Magic,
Veritas
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[Albert et al. ApJ 664L 87A 2007
W51: gamma rays come from a
molecular cloud separated from the
pulsar
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VHE
nucleus
Peak flux
nucleus
X-ray
Radio
HST-1
Core
Knot D Knot A
Colours: 0.2 - 6 keV (Chandra) Contours: 8 GHz radio (VLA)
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Chandra
jet37
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dN
dE
1
2
dN
dE
Very accurate input for
neutrino detectors
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x
x x
Measurement of spectral features permits to constrain EBL models
VHE bck e+e-
Heitler 1960
( ) ~
Mean free path
e+
e-
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Selection bias? New physics ?
~ E-2
Alessandro De Angelis
De Angelis, Galanti, Roncadelli 2011
with Franceschini EBL modeling
red
shif
t z
ray energy (TeV)
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*
a
*
*
…
*
a a
La = ga
E
B ( )a
P a NP1
P1
ga2 BT
2s2
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DARMA
3C279
Note: if conversion “a la
Simet-Hooper-Serpico”,
=> the effect could be directional
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EP = hcG 1.2 1019
H 2= m2
+ p2 H 2= m2
+ p2 1+E
EP
+…
Hp>> p 1+
m2
2p2 +p
2EP
+…
v =H
p1
m2
2p2 +p
EP
v 1+E
EP
t T EEP
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c 2 p2= E 2 1
E
Es
+ OE
Es
2
= -1
= 1
v =H
p1
m2
2p2 +p
EP
1. If <0 => ce < c => decay -> e+e- kinematically allowed for gamma with
energies above
2. If >0 => ce > c => electrons become superluminal for energies larger than
Emax/sqrt(2) => Vacuum Cherenkov Radiation.
- E > 100 TeV => abs( ) < 5 x 10-17
Emax = me sqrt(2/abs( ))
- Ee > 2 TeV from cosmic electron radiation => abs( ) < 2 x 10-14
- Modification of -> e+e- threshold. Using Mkn 501 and Mkn 421
spectra observations up to Eg > 20 TeV
=> abs( ) < 1.3 x 10-15
From MAGIC Mkn501 (taken as a LIV signal): | | ~ 2 10-15
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v 1+E
EP
t T EEP
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HESS PKS 2155 z = 0.116
July 2006 Peak flux ~15 x Crab ~50 x average Doubling times 1-3 min
RBH/c ~ 1...2.104 s
H.E.S.S. arXiV:0706.0797
MAGIC, Mkn 501 Doubling time ~ 2 min
astro-ph/0702008 arXiv:0708.2889
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0.15-0.25 TeV
0.25-0.6 TeV
0.6-1.2 TeV
1.2-10 TeV 4 min lag
1st order
> 1 GeV
< 5 MeV
( t)obs
E
Es1
H0
1 dz'(1+ z')
M (1+ z')3+
0
z
MAGIC Mkn 501, PLB08 (with J. Ellis et al.) Es1 ~ 0.04 MP ( ~ -25) Es1 > 0.02 MP
HESS PKS 2155, PRL08
Es1 > 0.06 MP
GRB X-ray limits: Es1 > 0.11 MP (Fermi, but…)
v c 1+E
MP
+ 22 E
MP2 + ...
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K(z)~z
~ -12
( t)obs
E
Es1
H0
1 dz'(1+ z')
M (1+ z')3+
0
z
t
E MP
H0
1K(z)
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• z = 1.8 ± 0.4
• one of the brightest GRBs
observed by LAT
• after prompt phase, power-low
emission persists in the LAT data as
late as 1 ks post trigger:
highest E photon so far detected:
33.4 GeV, 82 s after GBM trigger
[expected from Ellis & al. (26 ± 13) s]
• much weaker constraints on LIV Es
• z = 0.903 ± 0.003
• prompt spectrum detected,
significant deviation from Band
function at high E
• High energy photon detected:
31 GeV at To + 0.83 s
[expected from Ellis & al. (12 ± 5) s]
• tight constraint on Lorentz
Invariance Violation:
– Es1 = MQG > several MPlanck
=> Fermi rules, and 1st order violations appear unlikely
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Es2 > 6 1010 GeV (~10-9 MP) (HESS, MAGIC)
( t)obs
3
2
E
Es2
2
H01 dz'
(1+ z')2
M (1+ z')3+
0
z
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GRH depends on the –ray path and there the Hubble constant and
the cosmological densities enter => if EBL density and intrinsic
spectra are known, the GRH might be used as a distance estimator
GRH behaves differently than other observables already used for cosmology measurements.
Blanch & Martinez 2004
Simulated measurements
Mkn 421 Mkn 501
1ES1959+650 Mkn 180
1ES 2344+514
PKS2005-489
1ES1218+304
1ES1101-232
H2356-309 PKS 2155-304 H1426+428
EBL constraints are paving
the way for the use of AGN
to fit M and …
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Using the foreseen precision on the
GRH (distance at which (E,z)=1)
measurements of 20 extrapolated
AGN at z>0.2, cosmological
parameters can be fitted.
=> The 2=2.3 2-parameter
contour might improve by a
factor 2 the 2004’ Supernovae
combined result !
E,z( ) = d z dl
d z 0
z
dxx
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d n , z ( ) 2xE 1+ z( )2[ ]
2m 2c 2
Ex 1+z( )2
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Begelman/
Navarro
=( )
( ) ~
r
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los
2dl
from particle physics
from
ast
rophysi
cs
Look to the closest point with M <<L
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All-sky map of simulated gamma ray
signal from DM annihilation
(Pieri et al 2006)
Satellites
Low background and good source id,
but low statistics, astrophysical background
Galactic Center
Good statistics but source
confusion/diffuse background
Milky Way Halo
Large statistics but diffuse background
Spectral Features
Lines, endpoint Bremsstrahlung,…
No astrophysical uncertainties, good source Id, but low sensitivity because of expected small BR
Extra-galactic
Large statistics, but astrophysics, galactic
diffuse backgrounds
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Chandra GC survey
NASA/UMass/D.Wang et al.
CANGAROO (80%)
Whipple (95%)
H.E.S.S.
from W.Hofmann, Heidelberg 2004
detection of -rays from GC by Cangaroo,
Whipple, HESS, MAGIC
hard E-2.2 spectrum
fit to -annihilation continuum
spectrum leads to: M > 14 TeV
other interpretations possible (probable)
Galactic Center: very crowded sky region, strong exp.
evidence against cuspy profile
no real indication of DM…
The spectrum is featurless!!!
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FORNAX
BOOTES
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MAGIC ICRC 2011
Preliminary
all e+e-
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probe e+/e- ratio at 300-700 GeV
?
MAGIC
e+/e
++
e-
Alessandro De Angelis
• LHC may find candidates but cannot prove that
they are the observed Dark Matter, nor localize it
• Direct searches (nuclear recoil) may recognize
local halo WIMPs but cannot prove the nature and
composition of Dark Matter in the sky
• LHC reach limited to some 200-600 GeV; IACT
sensitivity starts at some ~200 GeV (should
improve)
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• extend E range beyond 50 TeV
• better angular resolution
• larger FOV
• monitor many objects simult.
• extend E range under 50 GeV
•10x sources
• better flux sensitivity
• lower threshold
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low energy section
Ethresh ~ 10 GeV
4 23 m telescopes
core array
100 GeV-10 TeV
~ 23 12 m telescopes
high energy section
~35 tel.
on 10 km2 area
2 arrays: north+south
all-sky coverage
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Very deep field
Deep field
~1/3 of telescopes
Monitoring
4 telescopes
Survey mode:
Full sky at current
sensitivity in ~1 year
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Crab
10% Crab
1% Crab
Fermi
Magic-II
E*F
(>E
) [
TeV
/cm
2s]
Agile
, F
erm
i, A
rgo,
Haw
k:
1 y
ear
Magic
, H
ess,
Verita
s,
CTA
: 50h
Agile
C T A
Argo
Hawc
Hess/Veritas
Far universe
Pulsars Fundamental physics
Cosmic rays
at the knee
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Results from HESS, MAGIC and VERITAS
Over 350 publications in high-impact journals:
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Chandra Hubble
Alessandro De Angelis
The future in
VHE gamma ray
astronomy:
World-wide Collaboration
25 countries
132 institutes
>800 scientists
10 fold sensitivity of current instruments
10 fold energy range
improved angular resolution
two sites (North / South)
operated as observatory
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Design study phase concluded in Fall 2010
Design Concepts for the Cherenkov Telescope Array
(arXiv:1008.3703)
FP7-supported Preparatory Phase: Fall 2010 – Fall 2013
Technical design, sites, construction and operation cost
Legal, governance and finance schemes
Small + medium-sized telescope prototypes
Aim for
start of deployment in early 2014
first data in 2016/17
base arrays complete in late 2018
expanded mid-energy array driven by US
total cost below 200 M
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Carbon-fibre
structure
400 m2 dish area
1.5 m sandwich
mirror facets
On (GRB) target
in < 20 sec.
27.8 m focal length
4.5o field of view
0.1o pixels
16 m focal length
7-8o field of view
0.18o pixels
100 m2 dish area
1.2 m mirror
facets
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Under study:
dual-mirror optics with compact photo sensor arrays
single-mirror optics
PMT-based and silicon-based sensors
Not yet conclusive which solution is most cost-effective
One of four
options for
telescope
structure
Multi-Anode PMT camera option
Wavelenght range
300 – 600 nm
Mirror PSF
O(1’) on axis, worse off axis
Pixel size
0.1o – 0.2o
Source localization
5” – 10” for source centroid
Image rate
kHz
Exposure time
single image: O(10 ns)
typical source: 10 – 50 h
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-30
Warning: map not quite accurate
proposals for sites due 6/2011 (S) and 12/2011 (N)
evaluation and downselection to few sites
final selection
Hardware key elements:
- O(100) Telescope structures/drives: very resistant, reliable,
accurate, light-weight (LST)
- O(10.000) m2 Mirrors: good quality, stable in extreme
conditions, cheap, light-weight
- O(2-3 x10.000) camera channels:
* Photosensors: PMT (and eventually SiPMs)
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* Readout Electronics: fast, low dissipation, compact,
reliable, cheap
- Timing/Synchronization: comparable to LHC machine
requirements
- Trigger/Data: comparable to LHC experiments
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Fermi
HESS
CTA
MILAGRO HAWC
factor 3
improvement
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HESS map of the Gal.plane, total exp ~500 hours
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2008 2009 2010 2011 2012 2013 2014 2015
Alessandro De Angelis