Residual flux and angular distribution of high-energy cosmic muons have been measured in two underground locations at the Canfranc Underground Laboratory (LSC) using a dedicated Muon Monitor. The instrument consists of three layers of fast scintillation detector modules operating as 352 independent pixels. The monitor has a flux-defining area of $$1~\hbox {m}^{2}$$ and covers all azimuth angles, and zenith angles up to $$80^{\circ }$$ . The measured integrated muon flux is $$(5.26 \pm 0.21) \times 10^{-3}~\hbox {m}^{-2}\hbox {s}^{-1}$$ in the Hall A of the LAB2400 and $$(4.29 \,\pm \, 0.17) \times 10^{-3}~\hbox {m}^{-2}\hbox {s}^{-1}$$ in LAB2500. The angular dependence is consistent with the known profile and rock density of the surrounding mountains. In particular, there is a clear maximum in the flux coming from the direction of the Rioseta valley.
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"value": "Residual flux and angular distribution of high-energy cosmic muons have been measured in two underground locations at the Canfranc Underground Laboratory (LSC) using a dedicated Muon Monitor. The instrument consists of three layers of fast scintillation detector modules operating as 352 independent pixels. The monitor has a flux-defining area of $$1~\\hbox {m}^{2}$$ <math><mrow><mn>1</mn><mspace width=\"3.33333pt\"></mspace><msup><mtext>m</mtext><mn>2</mn></msup></mrow></math> and covers all azimuth angles, and zenith angles up to $$80^{\\circ }$$ <math><msup><mn>80</mn><mo>\u2218</mo></msup></math> . The measured integrated muon flux is $$(5.26 \\pm 0.21) \\times 10^{-3}~\\hbox {m}^{-2}\\hbox {s}^{-1}$$ <math><mrow><mrow><mo>(</mo><mn>5.26</mn><mo>\u00b1</mo><mn>0.21</mn><mo>)</mo></mrow><mo>\u00d7</mo><msup><mn>10</mn><mrow><mo>-</mo><mn>3</mn></mrow></msup><mspace width=\"3.33333pt\"></mspace><msup><mtext>m</mtext><mrow><mo>-</mo><mn>2</mn></mrow></msup><msup><mtext>s</mtext><mrow><mo>-</mo><mn>1</mn></mrow></msup></mrow></math> in the Hall A of the LAB2400 and $$(4.29 \\,\\pm \\, 0.17) \\times 10^{-3}~\\hbox {m}^{-2}\\hbox {s}^{-1}$$ <math><mrow><mrow><mo>(</mo><mn>4.29</mn><mspace width=\"0.166667em\"></mspace><mo>\u00b1</mo><mspace width=\"0.166667em\"></mspace><mn>0.17</mn><mo>)</mo></mrow><mo>\u00d7</mo><msup><mn>10</mn><mrow><mo>-</mo><mn>3</mn></mrow></msup><mspace width=\"3.33333pt\"></mspace><msup><mtext>m</mtext><mrow><mo>-</mo><mn>2</mn></mrow></msup><msup><mtext>s</mtext><mrow><mo>-</mo><mn>1</mn></mrow></msup></mrow></math> in LAB2500. The angular dependence is consistent with the known profile and rock density of the surrounding mountains. In particular, there is a clear maximum in the flux coming from the direction of the Rioseta valley."
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