Upload
colton
View
32
Download
2
Tags:
Embed Size (px)
DESCRIPTION
Expected Performance of a Neutrino Telescope for Seeing AGN/GC Behind a Mountain. Abstract We study the expected performance of building a neutrino telescope, which targets at energy greater than - PowerPoint PPT Presentation
Citation preview
George W.S. Hou & M.A. HuangCenter for Cosmology and Particle Astrophysics
Department of Physics, National Taiwan University, 1, Sec. 4, Roosevelt Rd.,Taipei, 106,TAIWAN
http://[email protected] & [email protected]
?
Window of new techniques for observing Neutrinos
Conventional detectors such as SK have difficulty to expand target volume, maximum energy ~ 1015 eV.
UHECR detector such as Auger array also detect , energy threshold is high ~ 1018 eV.
Alternative approachUse mountain as target and shield. Use atmosphere as calorimeter, measured air shower initiated by the decay of .
appearance Only can be
seen, observation such event prove to
oscillation seen by SK.
VHE Neutrino Telescope Workshop Mar. 21-23, 2002, Taipei, Taiwan, http://hep1.phys.nt
u.edu.tw/VHENTW
Potential site: Hawaii Big IslandGood weather & Less artificial lightMt. Hualalai provide a good view of Mt. Loa and situated in the dryer west side of island.Mt. Loa provide long base line, ~ 90 km wide and 4 km high.
Slice along this line
: Conversion efficiency
Blue : No dE/dX Red: dE/dX
AbstractWe study the expected performance of building a neutrino telescope, which targets at energy greater than
10^14 eV utilizing a mountain to interact with neutrinos. The telescope's efficiency in converting neutrinos into leptons is first examined. Then using a potential site on the Big Island of Hawaii, we estimate the
acceptance of the proposed detector. The neutrino flux limit at event rate 0.3/year/half decade of energy is estimated to be comparable to that of AMANDA neutrino flux limit at above 10^16 eV.
astro-ph/0204145
Detection mechanism similar to -ray imaging Chrenkov telescope.
Cherenkov light image on a 8x8 MAPMT
EUSO type compact detector (Fresnel lens + MAPMT)
Tentative international collaboration:
NTU, TaiwanU. Paris, FrenchU. Palermo, ItalyU. Hawaii, USARIKEN, Japan Euso prototype 40cm diameter Fresn
el lens, assembled in RIKEN, Japan(Kawasaki et al., 2001, 27th ICRC, 893)
)(/)(
1)(
11
3
/2
/1
0 32
1total
max
0
1
dxdE
rockin y probabilit survival τ
yprobabilitn interactio
rockin y probabilit survival
atmospherein y probabilit survival
)()(
Errd
ExLE
x
x
L
d
eP
E
E
eP
dx
eP
eP
dxxLPxP
PP
atm
Field of view of telescope
Azimuth angle: from south to east.Zenith angle: from 86.9º to 91.5º
Acceptance•Select field of view, count mountain-passing events only!•Effective solid angle is Cerenkov light cone, c ~ 5 º.•Effective area: area where tau decay and initiate shower.
•Consider conversion efficiency
Over 1 km2 sr!
Assuming sensitivity is the flux which produce 0.3 events/year* per half decade of energy.* Calendar year, consider 10% duty cycle.
Sky coverage
• From field of view and operation from 12/2003 to 12/2007; 20% duty time •Optical detector operate in moonless and cloudless night, typical duty cycle 10%.
Galactic center is visible!
Conclusions:Hualalai site provide acceptance > 1km2 sr and good weather condition.Chance to explore MPR limits and set similar upper limit as AMANDA-B10 at higher energy.Nearby point source could be detected, AGN and galactic center could be good candidate for such point source.Earth skimming and Near Horizon shower are being studied. Acceptance will be updated.