Table 1
Summary of the efforts to observe PSR B1706−44 in the VHE γ-ray domain.
| Observation dates | Instrument | Test position | Extension | Integral flux (ph cm-2 s-1) | Reference |
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| 1992 | CANGAROO-I | PSR B1706−44 | n/a | F(> 1 TeV) ~ 1 × 10-11 | Ogio et al. (1993) |
| 1993 | CANGAROO-I | PSR B1706−44 | n/a | F(> 3.2 ± 1.6 TeV) < 8.0 × 10-13 | Yoshikoshi et al. (2009) |
| 1993–1994 | CANGAROO-I | PSR B1706−44 | n/a | F(> 3.2 ± 1.6 TeV) < 6.1 × 10-13 | Yoshikoshi et al. (2009) |
| 1995 | CANGAROO-I | PSR B1706−44 | n/a | F(> 3.2 ± 1.6 TeV) < 8.9 × 10-13 | Yoshikoshi et al. (2009) |
| 1997 | CANGAROO-I | PSR B1706−44 | n/a | F(> 1.8 ± 0.9 TeV) < 4.1 × 10-12 | Yoshikoshi et al. (2009) |
| 1998 | CANGAROO-I | PSR B1706−44 | n/a | F(> 2.7 ± 1.4 TeV) < 1.3 × 10-12 | Yoshikoshi et al. (2009) |
| 1993–1994 | BIGRAT | PSR B1706−44 | n/a | F(> 0.5 TeV) < (7.0 ± 0.7) × 10-11 | Rowell et al. (1998) |
| 1996 | Durham Mark 6 | PSR B1706−44 | n/a | F(> 0.3 TeV) = (3.9 ± 0.7) × 10-11 | Chadwick et al. (1998) |
| 2000–2001 | CANGAROO-II | PSR B1706−44 | n/a | n/a | Kushida et al. (2003) |
| 2003 | H.E.S.S. | G 343.1−2.3 center | 0.6° | F(> 0.50 TeV) < 7.6 × 10-12 | Appendix A |
| 2003 | H.E.S.S. | G 343.1−2.3 center | 0.6° | F(> 0.60 TeV) < 6.3 × 10-12 | Appendix A |
| 2004–2007 | CANGAROO-III | PSR B1706−44 | 0.26° | F(> 1 TeV) = (3.0 ± 0.6) × 10-12 | Enomoto et al. (2009) |
| 2004–2007 | CANGAROO-III | PSR B1706−44 | 1.0° | F(> 1 TeV) ≈ 2.2 × 10-11 | Enomoto et al. (2009) |
| 2007 | H.E.S.S. | PSR B1706−44 | 0.1° | F(> 0.6 TeV) < 3.3 × 10-13 | Sect. 3 |
| 2007 | H.E.S.S. | G 343.1−2.3 center | 0.6° | F(> 0.6 TeV) ≈ 6.5 × 10-12 | Sect. 3 |
Notes. The CANGAROO upper limits (ULs) are at a 95% confidence level (CL), the BIGRAT UL is at 3σ (99.7% CL), and the H.E.S.S. ULs are at a 99% CL. The CANGAROO-I integral flux based on the 1992 dataset (Ogio et al. 1993) likely suffered from systematics similar to those that affected the 1993 data, which has since been re-analysed along with an analysis of the previously unreleased 1994–1998 CANGAROO-I data; the ULs assume a Crab-like spectral index Γ = −2.5 (Yoshikoshi et al. 2009). Only the latest, revised results are shown in this table; see Sect. 1 for further discussion. The BIGRAT UL is subject to an additional ± 50% systematic uncertainty (Rowell et al. 1998). The integral flux from the 2000–2001 CANGAROO-II data analysis was not disclosed but was claimed to confirm previous results (Kushida et al. 2003). The 2003 H.E.S.S. ULs are based on the re-analysis presented in Appendix A; the first UL (row 10) assumes Γ = −2.5 for comparison to the CANGAROO ULs, while the second UL (row 11) assumes Γ = −2.0 for comparison to the 2007 H.E.S.S. detection. The CANGAROO-III fluxes are from the ON-OFF analysis presented in Enomoto et al. (2009). The 2007 H.E.S.S. results are described in Sect. 3, where the center of G 343.1−2.3 is also defined; the point-source UL assumes Γ = −2.5.
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