Table 2: Flux upper limits at 99% confidence level for the pulsar position in ${\rm s}^{-1}~{\rm cm}^{-2}$ . The upper limits from Method A were calculated assuming a photon index of $\Gamma = 2.5$ . The numbers in parentheses are the energy thresholds (in TeV) for which the upper limits were determined.
Method A Method B

Standard $1.4\times 10^{-12}$ (0.35) $1.3\times 10^{-12}$ (0.50)

CANGAROO $6.4\times 10^{-13}$ (1.00) $7.7\times 10^{-13}$ (1.00)

Radio arc $5.8\times 10^{-12}$ (0.35) $3.5\times 10^{-12}$ (0.50)

**Table 2:** Flux upper limits at 99% confidence level for the pulsar position in ${\rm s}^{-1}~{\rm cm}^{-2}$ . The upper limits from Method A were calculated assuming a photon index of $\Gamma = 2.5$ . The numbers in parentheses are the energy thresholds (in TeV) for which the upper limits were determined.
	Method A	Method B
Standard	$1.4\times 10^{-12}$	(0.35)	$1.3\times 10^{-12}$	(0.50)
CANGAROO	$6.4\times 10^{-13}$	(1.00)	$7.7\times 10^{-13}$	(1.00)
Radio arc	$5.8\times 10^{-12}$	(0.35)	$3.5\times 10^{-12}$	(0.50)

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data analysis
	3 Results
	4 Discussion and conclusions
	References