Upgraded conventional neutrino beams: Neutrino superbeams
The capabilities of greatly upgraded conventional neutrino beams
and the comparison with neutrino factories is under study.
This page collects together some useful working information
and at the bottom you can find links to studies that have already
been done!

MI upgrade limitations
Conf97199, W. Chou

NUMI low energy beam with L = 732 km
uoscillation signals for point IA1 (LMA scenario) but with sin**2 2theta(13) =
0.01, from Steve Geer.

NUMI medium energy beam with L = 2800 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.04,
from Steve Geer.

NUMI medium energy beam with L = 2800 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.01,
from Steve Geer.

NUMI medium energy beam with L = 2800 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
from Steve Geer.

NUMI medium energy beam with L = 2800 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
and negative delta m**2,
from Steve Geer.

NUMI medium energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.04,
from Steve Geer.

NUMI medium energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.01,
from Steve Geer.

NUMI medium energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
from Steve Geer.

NUMI medium energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
negative dm**2,
from Steve Geer.

NUMI high energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.01,
from Steve Geer.

NUMI high energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
from Steve Geer.

NUMI high energy beam with L = 7300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.001,
and negative dm**2,
from Steve Geer.

NUMI high energy beam with L = 9300 km
oscillation signals for point IA1 (LMA scenario) with sin**2 2theta(13) = 0.01,
from Steve Geer.

Event Energy Spectra for L = 2800,7300 km and different angles
This file shows the charged current event energy spectra for different
components of the NUMI Medium Energy beam AND the neutral current
energy spectra,
and on the last page compares the NC visible energy spectra with the nu_mu to
nu_e and nu_e to nu_e charged current energy spectra. These plots were
made with the group 4 background ntuples and Steve Geer's flux histograms
shown in the other links from this page. Finally, the energies shown
are for a perfect detector, perfect acceptance, and NO neutral current
rejection factor. Also, because of limitations in the background ntuples
and the signal histograms, respectively,
these plots have NO ENTRIES in them from neutrinos with energies below 1GeV,
or above 20GeV, but the latter will be remedied soon. This is simply
meant to be a first pass look at what the neutral currents look like.
From Debbie Harris.

Event Energy Spectra for L =7300 km , MINOS High energy beam neutrino
running

Event Energy Spectra for L =7300 km , MINOS High energy beam antineutrino running
WAY PRELIMINARY: These two files compare 3 different scenarios:
sin^22theta_13 = .001 with two different signs for delta m^2,
and sin^2theta_13=.01 with one sign of delta m^2. There is an
assumed hadron energy resolution of 15%/sqrt(e_had) and electron
energy resolution of 5%/sqrt(e_electron), which I think is near
what a liquid argon calorimeter would achieve. The effect of
such a good energy resolution is tiny, and switching the sign of
delta m^2 is a huge effect. Basically for one sign of delta m^2
the signal is much much smaller than the nue contamination, and
for the other sign of delta m^2 the signal is about the same size,
but with a different energy spectrum. For sin^22theta_13=.01,
the signal is at least much bigger than the intrinsic nue background,
and you just have to worry about getting rid of the nc background.
For these plots there are no neutrinos below 1GeV or above 50GeV, but
this effect is probably very small. Also, in nubar running the nu_e
contamination is about 50% as large as the nubar_e contamination and
so it should also be included...(and will be soon). From Debbie Harris
starting with Steve Geer's flux files shown above.

7/19/2000 Background Plots: Include intrinsic nu_e and tau>e
backgrounds at sin^22theta_13=.01 for Low Medium and High Energy beams,
at 732,2800, and 7300km. These plots show backgrounds from
tau decays to electrons in charged current events. The assumptions
made on cross section ratios and tau to electron energy spectra
are shown on the first page, and comparisons on the later pages.
From Debbie Harris starting with Steve Geer's flux files shown above.

Comparison of neutrino vs antineutrino running for Horn Beam
WAY PRELIMINARY:
This file shows the crosssection weighted fluxes (at 732km) for two possible
conventional beam: the solid lines are the minos high energy beam
with the polarity of the horns set to focus positive pions making
neutrino beams, and the dashed lines are the same thing but with the
opposite polarity in the horns, to make a nubar beam. Note that there
are about 34% as many nubar events as nu events: so the beamline is
only 68% as efficient at creating and focusing negative pions vs
positive pions. The nue/nubare event rate is about 50% in
nubar running, compared to
a <10% rate of nubare/nue in neutrino running. From Debbie Harris
and the GEANTbased NUMI beam monte carlo.

Event rates table
NUMI beam x 4 with L = 3000 km and 7200 km, from Heidi Schellman.

Ray Stefanski's talk from July 5, 2000 meeting
This document describes some of the low energy neutrino
physics that is of interest, as well as the salient features
of the PRISM project in Japan.
References about Superbeams:
CP and T violation in long baseline experiments with low energy neutrino
by Joe Sato, hepph/0006127 , June 13, 2000.
A Comparison of the Physics Potential of Future Long Baseline Neutrino
Oscillation Experiments
by K. Dick, M. Freund, P.Huber, M. Lindner, hepph/0008016 ,August 2, 2000.
Masses and Mixings from Neutrino Beams pointing to Neutrino Telescopes
by K. Dick, M. Freund, P.Huber, M. Lindner hepph/0006090 , June 9, 2000.
Last updated July 6, 2000
Suggestions ? Contact sgeer@fnal.gov