first results of galactic observations with magic javier rico institut de física d’altes energies...
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First results of Galactic First results of Galactic observations with MAGICobservations with MAGIC
Javier RicoJavier RicoInstitut de Física d’Altes EnergiesInstitut de Física d’Altes Energies
Barcelona, SpainBarcelona, Spain
XII International Workshop on “Neutrino Telescopes”Twenty years after the Supernova 1987A neutrino bursts discovery
March 6-9, 2007“Istituto Veneto di Scienze, Lettere ed Arti”, Palazzo Franchetti - S. Stefano
Venice (Italy)
J. Rico (IFAE)First results of Galactic observations with MAGIC
Su
mm
ary
Su
mm
ary
1. TeV gamma-ray astronomy with Cherenkov telescopes
2. MAGIC Technical features Results
3. LS I +61 303
4. MAGIC as a neutrino telecope
5. Conclusions
Gamma-ray
~ 10 kmParticleshower
~ 1o
Che
renk
ov L
ight
~ 120 m
Cherenkov telescopesCherenkov telescopes
Collection area:~ 105 m2
Important sincegamma-rays at theseenergies are rare(1/m2 month)
GLAST(slightly magnified)
Image intensityPrimary energy
Image orientation Prim. direction
Image shape Primary nature
Imaging Imaging
techniquetechnique
StereoscopyStereoscopy
Better determinationPrimary energyPrimary natureBetter signal/backgrounddiscrimination
First results of Galactic observations with MAGIC J. Rico (IFAE)
Get
tin
g r
id o
f th
e b
ackg
rou
nd
(C
R)
Get
tin
g r
id o
f th
e b
ackg
rou
nd
(C
R)
(2) Orientation: -rays point to the source: excess at small alpha
ON: Pointing to source
OFF: Pointing somewhere else
Crab Nebula
Image parameterization
CR
(1) Shape: –rays are narrowerthan cosmic rays.
Cherenkov images are parameterized by the light distribution (shape, position and orientation)
First results of Galactic observations with MAGIC J. Rico (IFAE)
The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:
• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
17 m
Th
e M
AG
IC t
eles
cop
eT
he
MA
GIC
tel
esco
pe The existing technology has been carried to the limit to improve sensitiity and lower the
energy threshold:• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:
• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:
• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:
• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
The existing technology has been carried to the limit to improve sensitiity and lower the energy threshold:
• The largest reflector, 17 m diameter → lowest energy threshold (100 GeV)• A 3.5 FOV camera with 577 PMTs (QE=30%)• An ultra-light structure (carbon-fiber) that allows for fast repositioning (40s)• Signal transmition through optical fiber to reduce noise• Dinamical mirror position correction thanks to a laser system
MAGIC is located at La Palma, Canary Islands (Northern Hemisphere)
First results of Galactic observations with MAGIC J. Rico (IFAE)
Active Mirror Control
Jupiter before and after focusing
Super-light structure (65 t), to catch GRBs
AM
C a
nd
fas
t m
ove
men
tA
MC
an
d f
ast
mo
vem
ent
First results of Galactic observations with MAGIC J. Rico (IFAE)
MA
GIC
nea
r fu
ture
MA
GIC
nea
r fu
ture
MAGIC-II:• Second telescope, completion in 2007• Stereo high purity gamma samples better physics (lower threshold and better sensitivity)
MAGIC-1.5:• Running since February’07. • 2 GHz readout• Power of timing information under study
First results of Galactic observations with MAGIC J. Rico (IFAE)
Ph
ysic
s w
ith
100
GeV
-10
TeV
P
hys
ics
wit
h 1
00 G
eV-1
0 Te
V
-ray
s-r
ays
SNRsSNRs
Cold Cold Dark Dark
MatterMatter
PWNPWNPulsarsPulsars
GRBsGRBs
Quantum Quantum Gravity effectsGravity effects
cosmologiccosmologicalal-Ray -Ray HorizonHorizon
AGNsAGNs
Origin of Origin of CRsCRs
Astrophysics
Fundamental Physics
BinariesBinariesQSRsQSRs
First results of Galactic observations with MAGIC J. Rico (IFAE)
VH
E
VH
E
con
nec
tio
n c
on
nec
tio
n
VHE fluxes → upper limits to fluxes (unless strong absorption)
km3 detectors sensitivity: F(>1TeV) = 10-11 /cm2s → Crab nebula -ray flux
Shell type supernova remnants with ~1 Crab flux in -rays: RAJ1713.7-3946 and RAJ0852.0-4622 best explained by hadronic interactions (extension, morphology, hard spectrum up to 100 TeV)
PWN: well explained by leptonic models but room for ions accelerated in the pulsar relativistic wind: Vela-X, Crab
Compact binary systems: LS5039 and LSI+61303. Lower flux F(>1TeV) = 10-12 /cm2s or more depending on -ray production region
VHE ’s messengers of non-thermal processes involving hadronic interactions
Ultimate proof of Galactic CR origin
p
p±
0
+ photo-meson interaction in high magnetic fields
(TeV-PeV)
First results of Galactic observations with MAGIC J. Rico (IFAE)
Ob
serv
atio
n c
ycle
IO
bse
rvat
ion
cyc
le I
Observations from November 2004 to May 2006
About 25% total observation time for Galactic targets (apart from Crab Nebula)
Targets include: SNR:
Intense EGRET sources HESS galactic scan sources (HESS J1834, HESS
J1813) PWN Pulsars: limits to Crab, PSR B1957, PSR B1951 Binaries/microquasars (low and high mass)
LS I +61 303 variable source Galactic Center HEGRA Unidentified TeV2032 Cataclysmic variable (AE Aquari)
HESS J1834
PSR B1951+32
J. Rico (IFAE)First results of Galactic observations with MAGIC
LS
I +
61 3
03L
S I
+61
303
LS I +61 303: High Mass x-ray binary at a distance of 2 kpc Optical companion is a B0 Ve star of 10.7 mag with a circumstellar disc Compact object probably a neutron star High eccentricity or the orbit (0.7) Modulation of the emission from radio to x-rays with period 26.5 days attributed to orbital period Secondary modulation of period 4 years attributed to changes in the Be star equatorial disc
0.20.1
0.3
0.5
0.9
0.70.4 AU
To observer
J. Rico (IFAE)First results of Galactic observations with MAGIC
• LSI was temptatively associated to an EGRET source (<10 GeV)
EG
RE
T s
ou
rces
EG
RE
T s
ou
rces
LS5039Detected by HESS
Hartman et al. 1999
LSI +61 303Detected by MAGIC
J. Rico (IFAE)First results of Galactic observations with MAGIC
LS
I +
61 3
03 b
y M
AG
ICL
S I
+61
303
by
MA
GIC
Albert et al. 2006
• We observed LS I +61 303 with MAGIC for 54 horas between November 2005 and March 2006 (6 orbital cycles)
• LS I +61 303 is a VHE gamma-ray emitter:• The flux is variable• It is modulated by the orbital motion (first indication of periodicity) • The peak of intensity is far from periastron
• Results from another 4 orbital cycles obs. during fall 2006 published soon
J. Rico (IFAE)First results of Galactic observations with MAGIC
Flu
x ti
me
vari
abili
tyF
lux
tim
e va
riab
ility
Albert et al. 2006
MAGIC has observed LSI during 6 orbital cycles A variable flux above 400 GeV (probability of statistical fluctuation 310-5) detected Marginal detections at phases 0.2-0.4 Maximum flux detected at phase 0.6 with a 16% of the Crab Nebula flux More luminous at these energies than at x-rays Energy spectrum from 200 GeV to 4 TeV is well fitted by a power law with spectral index = -2.6, no cutoff seen
J. Rico (IFAE)First results of Galactic observations with MAGIC
• The broad-band experimental data on LSI may be explained both as produced by
• relativistic jets (microquasar) • interaction of the winds of a young pulsar with that of the companion star.
• In both cases the responsible may be accelerated electrons (Inverse Compton) or protons (pp interaction) → neutrinos!
Em
issi
on
mo
del
sE
mis
sio
n m
od
els
J. Rico (IFAE)First results of Galactic observations with MAGIC
MA
GIC
as
a n
eutr
ino
tel
esco
pe
MA
GIC
as
a n
eutr
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• Ultra-high energy neutrinos (PeV energies or more) can be looked for using MAGIC (Fargion 2002)• lifetime is 50 m at 1 PeV (1015eV) and hundreds of km for 1 EeV (1018eV)• 83% of the times the decay produces air showers observable by MAGIC
• Feasibility studies in MAGIC started this observation cycle• Data taking → background studies (scattered light)• Preliminary Sensitivity studies:
MAGIC not competitive for diffuse neutrinos Identified best source candidates:
LS I +61 303 1ES1959 1ES2344
• No “normal” observation time is lost since it is done when clouds do not allow them
J. Rico (IFAE)First results of Galactic observations with MAGIC
Co
ncl
usi
on
sC
on
clu
sio
ns
New generation of Cherenkov telescopes are main actors of the recent burst of VHE astronomy
MAGIC has a major role with already 5 new discoveries and other interesting results
The compact binary system LS I +61 303 has been detected at TeV energies The emission is variable Possible hint of periodicity The maximum of the emission happens 1/3 of
the orbit away from periastron The possibility of using MAGIC as a
telescope for UHE neutrinos is under study