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Search for Point Sources using AMANDA-B10

 

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 AMANDA-B10 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 AMANDA-B10 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.angular resolution of AMANDA-B10 Effective area of Am-B10 detector
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. 

 
 
flux limits of muons induced by neutrinos using pt source analysis

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.

comparison of B10 results with other detectors
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 bin-to-bin 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 AMANDA-II and IceCube are shown.


neutrino flux limits for point sources
The AMANDA-B10 result is shown for declinations greater than +40 degrees and includes the impact of systematic uncertainty.  The expected sensitivity for AMANDA-II 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 E-2 and absolute fluxes above the AMANDA limit can be excluded.

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UCI Anteater

Barwick Group
School of Physical Sciences
University of California Irvine