| Observation point . | Mt. Sierra Negra . |
|---|---|
| Altitude | 4580 m |
| Vertical atmospheric pressure | 575 g cm−2 |
| Geophysical coordinates | N|$19^{\circ}0'$|, W|$97^{\circ}3'$| |
| Sensor surface area | 4.0 m2 |
| Sensor thickness | 30 cm |
| Interaction probability for n | 0.307 |
| Pair-creation probability for γ | 0.208 |
| Counting rate C1 (min−1) | 173000 (> 30 MeV) |
| Counting rate C2 | 77600 (> 60 MeV) |
| Counting rate C3 | 30100 (> 90 MeV) |
| Counting rate C4 | 14600 (> 120 MeV) |
| Counting rate N1 (min−1) | 86400 (> 30 MeV) |
| Counting rate N2 | 32500 (> 60 MeV) |
| Counting rate N3 | 10080 (> 90 MeV) |
| Counting rate N4 | 4880 (> 120 MeV) |
| Counting rate L1 (min−1) | 27500 |
| Counting rate L2 | 16130 |
| Counting rate L3 | 12400 |
| Counting rate L4 | 9240 |
| Observation point . | Mt. Sierra Negra . |
|---|---|
| Altitude | 4580 m |
| Vertical atmospheric pressure | 575 g cm−2 |
| Geophysical coordinates | N|$19^{\circ}0'$|, W|$97^{\circ}3'$| |
| Sensor surface area | 4.0 m2 |
| Sensor thickness | 30 cm |
| Interaction probability for n | 0.307 |
| Pair-creation probability for γ | 0.208 |
| Counting rate C1 (min−1) | 173000 (> 30 MeV) |
| Counting rate C2 | 77600 (> 60 MeV) |
| Counting rate C3 | 30100 (> 90 MeV) |
| Counting rate C4 | 14600 (> 120 MeV) |
| Counting rate N1 (min−1) | 86400 (> 30 MeV) |
| Counting rate N2 | 32500 (> 60 MeV) |
| Counting rate N3 | 10080 (> 90 MeV) |
| Counting rate N4 | 4880 (> 120 MeV) |
| Counting rate L1 (min−1) | 27500 |
| Counting rate L2 | 16130 |
| Counting rate L3 | 12400 |
| Counting rate L4 | 9240 |
*Parameters and typical counting rates of the neutron telescopes of Mt. Sierra Negra. In the table, the interaction probabilities for n and pair creation for γ do not include the threshold effect due to the discriminator. The interaction probability is given for neutrons with an energy of ∼20 GeV. In the case of solar neutron detection at about ∼500 MeV, the value would be slightly higher than this value at ∼0.46.
| Observation point . | Mt. Sierra Negra . |
|---|---|
| Altitude | 4580 m |
| Vertical atmospheric pressure | 575 g cm−2 |
| Geophysical coordinates | N|$19^{\circ}0'$|, W|$97^{\circ}3'$| |
| Sensor surface area | 4.0 m2 |
| Sensor thickness | 30 cm |
| Interaction probability for n | 0.307 |
| Pair-creation probability for γ | 0.208 |
| Counting rate C1 (min−1) | 173000 (> 30 MeV) |
| Counting rate C2 | 77600 (> 60 MeV) |
| Counting rate C3 | 30100 (> 90 MeV) |
| Counting rate C4 | 14600 (> 120 MeV) |
| Counting rate N1 (min−1) | 86400 (> 30 MeV) |
| Counting rate N2 | 32500 (> 60 MeV) |
| Counting rate N3 | 10080 (> 90 MeV) |
| Counting rate N4 | 4880 (> 120 MeV) |
| Counting rate L1 (min−1) | 27500 |
| Counting rate L2 | 16130 |
| Counting rate L3 | 12400 |
| Counting rate L4 | 9240 |
| Observation point . | Mt. Sierra Negra . |
|---|---|
| Altitude | 4580 m |
| Vertical atmospheric pressure | 575 g cm−2 |
| Geophysical coordinates | N|$19^{\circ}0'$|, W|$97^{\circ}3'$| |
| Sensor surface area | 4.0 m2 |
| Sensor thickness | 30 cm |
| Interaction probability for n | 0.307 |
| Pair-creation probability for γ | 0.208 |
| Counting rate C1 (min−1) | 173000 (> 30 MeV) |
| Counting rate C2 | 77600 (> 60 MeV) |
| Counting rate C3 | 30100 (> 90 MeV) |
| Counting rate C4 | 14600 (> 120 MeV) |
| Counting rate N1 (min−1) | 86400 (> 30 MeV) |
| Counting rate N2 | 32500 (> 60 MeV) |
| Counting rate N3 | 10080 (> 90 MeV) |
| Counting rate N4 | 4880 (> 120 MeV) |
| Counting rate L1 (min−1) | 27500 |
| Counting rate L2 | 16130 |
| Counting rate L3 | 12400 |
| Counting rate L4 | 9240 |
*Parameters and typical counting rates of the neutron telescopes of Mt. Sierra Negra. In the table, the interaction probabilities for n and pair creation for γ do not include the threshold effect due to the discriminator. The interaction probability is given for neutrons with an energy of ∼20 GeV. In the case of solar neutron detection at about ∼500 MeV, the value would be slightly higher than this value at ∼0.46.
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