The point source analysis optimizes the selection
criteria on hard spectra (differential energy spectra proportionally
to E^{2}), although it has reasonable sensitivity to
softer spectra. The critical features of the point source analysis:
demonstrate good angular resolution and absolute pointing and
maintain good effective size for as much of the sky as possible.
The AMANDAB10 detector achieves 10,000 m2 for declinations
greater than 30 degrees if the muon energy at the detector is
greater than 1 TeV.
This figure shows the
space angle resolution and the deduced point spread function.
The angular resolution and absolute pointing were checked
by using events that struck both the SPASE air shower array
and AMANDAB10 array. The point spread function is
fit well by a function composed of the sum of two gaussians.
The tail is partially due to high energy muons that are
not well reconstructed. 
This is the effective
area of the detector for muons that have energies of 1,
10, and 100 TeV. This shows that AMANDA B10 reaches
an effective area of 10,000 m2 for 1 TeV muons. 
This figure
provides the average muon flux limit as a function of
declination. The solid black line includes the impact
of systematic uncertainty in the calculations (as illustrated
by the various symbols in the legend), and represents
the final result of the B10 analysis using data from 1997. 
This figure compares the
B10 muon flux limits as a function of declination (based
on only 1 year of data collected during 1997, which corresponds
to less than 1/3 of a year of live time due to delays
associated with commissioning) with limits presented by
MACRO and Super Kamiokanda collaborations. The solid
red line is the same as the solid black line of the left
figure. The dashed curves correspond azimuthal variation
in the flux limits due to the bintobin statistical variation
for the same declination band. 
The next figure shows the neutrino
flux limits from the 1997 data analysis and compares to a representative
set of models (selected to illustrate the variety of spectral
shapes). Also, the expected sensitivity of AMANDAII and
IceCube are shown.
The AMANDAB10 result is shown for declinations greater than
+40 degrees and includes the impact of systematic uncertainty.
The expected sensitivity for AMANDAII is shown assuming that
the complete data for several years is analyzed. Please note
that this type of plot is misleading for predicted differential
energy spectra not proportional to E^(2). In particular, only
those parameters of models that predict spectra close to E2
and absolute fluxes above the AMANDA limit can be excluded.
