# Performance of the MAGIC telescopes under moonlight

**Authors:** MAGIC Collaboration: M. L. Ahnen (1), S. Ansoldi (2,24), L. A., Antonelli (3), C. Arcaro (4), A. Babi\'c (5), B. Banerjee (6), P. Bangale, (7), U. Barres de Almeida (7,25), J. A. Barrio (8), J. Becerra Gonz\'alez, (9), W. Bednarek (10), E. Bernardini (11,28), A. Berti (2,29), W., Bhattacharyya (11), B. Biasuzzi (2), A. Biland (1), O. Blanch (12), S., Bonnefoy (8), G. Bonnoli (13), R. Carosi (13), A. Carosi (3), A. Chatterjee, (6), P. Colin (7), E. Colombo (9), J. L. Contreras (8), J. Cortina (12), S., Covino (3), P. Cumani (12), P. Da Vela (13), F. Dazzi (3), A. De Angelis (4),, B. De Lotto (2), E. de O\~na Wilhelmi (14), F. Di Pierro (4), M. Doert (15),, A. Dom\'inguez (8), D. Dominis Prester (5), D. Dorner (16), M. Doro (4), S., Einecke (15), D. Eisenacher Glawion (16), D. Elsaesser (15), M. Engelkemeier, (15), V. Fallah Ramazani (17), A. Fern\'andez-Barral (12), D. Fidalgo (8), M., V. Fonseca (8), L. Font (18), C. Fruck (7), D. Galindo (19), R. J. Garc\'ia, L\'opez (9), M. Garczarczyk (11), M. Gaug (18), P. Giammaria (3), N., Godinovi\'c (5), D. Gora (11), S. Griffiths (12), D. Guberman (12), D., Hadasch (20), A. Hahn (7), T. Hassan (12), M. Hayashida (20), J. Herrera (9),, J. Hose (7), D. Hrupec (5), G. Hughes (1), K. Ishio (7), Y. Konno (20), H., Kubo (20), J. Kushida (20), D. Kuve\v{z}di\'c (5), D. Lelas (5), E. Lindfors, (17), S. Lombardi (3), F. Longo (2,29), M. L\'opez (8), C. Maggio (18), P., Majumdar (6), M. Makariev (21), G. Maneva (21), M. Manganaro (9), K. Mannheim, (16), L. Maraschi (3), M. Mariotti (4), M. Mart\'inez (12), D. Mazin (7,24),, U. Menzel (7), M. Minev (21), R. Mirzoyan (7), A. Moralejo (12), V. Moreno, (18), E. Moretti (7), V. Neustroev (17), A. Niedzwiecki (10), M. Nievas, Rosillo (8), K. Nilsson (17,31), D. Ninci (12), K. Nishijima (20), K. Noda, (12), L. Nogu\'es (12), S. Paiano (4), J. Palacio (12), D. Paneque (7), R., Paoletti (13), J. M. Paredes (19), X. Paredes-Fortuny (19), G. Pedaletti, (11), M. Peresano (2), L. Perri (3), M. Persic (2,3), P. G. Prada Moroni, (22), E. Prandini (4), I. Puljak (5), J. R. Garcia (7), I. Reichardt (4), W., Rhode (15), M. Rib\'o (19), J. Rico (12), A. Rugliancich (13), T. Saito (20),, K. Satalecka (11), S. Schroeder (15), T. Schweizer (7), A. Sillanp\"a\"a, (17), J. Sitarek (10), I. \v{S}nidari\'c (5), D. Sobczynska (10), A. Stamerra, (3), M. Strzys (7), T. Suri\'c (5), L. Takalo (17), F. Tavecchio (3), P., Temnikov (21), T. Terzi\'c (5), D. Tescaro (4), M. Teshima (7,24), D. F., Torres (23), N. Torres-Alb\`a (19), A. Treves (2), G. Vanzo (9), M. Vazquez, Acosta (9), I. Vovk (7), J. E. Ward (12), M. Will (9), D. Zari\'c (5) ((1), ETH Zurich, Institute for Particle Physics, Zurich, Switzerland, (2), Universit\`a di Udine, INFN, sezione di Trieste, Italy, Udine, Italy, (3), INAF - National Institute for Astrophysics, Roma, Italy, (4) Dipartimento di, Fisica ed Astronomia, Universit\`a di Padova, INFN sez. di Padova, Padova,, Italy, (5) Croatian MAGIC Consortium: Rudjer Boskovic Institute, University, of Rijeka, University of Split - FESB, University of Zagreb-FER, University, of Osijek, Split, Croatia, (6) Saha Institute of Nuclear Physics, HBNI,, Kolkata, India, (7) Max-Planck-Institut f\"ur Physik, M\"unchen, Germany, (8), Grupo de Altas Energias, Universidad Complutense, Madrid, Madrid, Spain, (9), Instituto de Astrofisica de Canarias, La Laguna (Tenerife), Spain, (10), Division of Astrophysics, University of Lodz, Lodz, Poland, (11) Deutsches, Elektronen-Synchrotron (DESY) Zeuthen, Zeuthen, Germany, (12) Institut de, Fisica d'Altes Energies (IFAE), The Barcelona Institute of Science and, Technology, Bellaterra (Barcelona), Spain, (13) Dipartimento di Fisica,, Universit\`a di Siena, INFN sez. di Pisa, Siena, Italy, (14) Institut de, Ciencies de l'Espai (IEEC-CSIC), Bellaterra, Spain, (15) Technische, Universit\"at Dortmund, Dortmund, Germany, (16) Institut f\"ur Theoretische, Physik und Astrophysik - Fakult\"at f\"ur Physik und Astronomie -, Universit\"at W\"urzburg, W\"urzburg, Germany, (17) Finnish MAGIC Consortium,, Tuorla Observatory, University of Turku, Astronomy Division, University of, Oulu, Finland, Piikki\"o, Finland, (18) Universitat Aut\`onoma de Barcelona,, Barcelona, Spain, (19) Universitat de Barcelona, Barcelona, Spain, (20), Japanese MAGIC Consortium, Kyoto, Japan, (21) Institute for Nuclear Research, and Nuclear Energy, Sofia, Bulgaria, (22) Universita di Pisa, and INFN Pisa,, Pisa, Italy, (23) ICREA, Institut de Ciencies de l'Espai (IEEC-CSIC),, Bellaterra, Spain, (24) Japanese MAGIC Consortium, Kyoto, Japan (25) Centro, Brasileiro de Pesquisas F\'isicas (CBPF/MCTI), Rio de Janeiro, Brazil, (28), Humboldt University of Berlin, Institut f\"ur Physik, Berlin, Germany, (29), University of Trieste, (31) Finnish Centre for Astronomy with ESO (FINCA),, Turku, Finland)

arXiv: 1704.00906 · 2020-01-27

## TL;DR

This study evaluates how MAGIC telescopes perform under moonlight, showing that observations during moonlight can significantly increase duty cycle with manageable sensitivity loss, enabling more continuous gamma-ray observations.

## Contribution

The paper introduces a Moon-adapted analysis method and assesses performance under various moonlight conditions, including hardware modifications, to extend observational duty cycle.

## Key findings

- Crab Nebula spectrum accurately reconstructed under moonlight
- Sensitivity degradation remains below 10-80% depending on conditions
- Duty cycle increased from 18% to 40% with moderate performance impact

## Abstract

MAGIC, a system of two imaging atmospheric Cherenkov telescopes, achieves its best performance under dark conditions, i.e. in absence of moonlight or twilight. Since operating the telescopes only during dark time would severely limit the duty cycle, observations are also performed when the Moon is present in the sky. Here we develop a dedicated Moon-adapted analysis to characterize the performance of MAGIC under moonlight. We evaluate energy threshold, angular resolution and sensitivity of MAGIC under different background light levels, based on Crab Nebula observations and tuned Monte Carlo simulations. This study includes observations taken under non-standard hardware configurations, such as reducing the camera photomultiplier tubes gain by a factor ~1.7 (Reduced HV settings) with respect to standard settings (Nominal HV) or using UV-pass filters to strongly reduce the amount of moonlight reaching the cameras of the telescopes. The Crab Nebula spectrum is correctly reconstructed in all the studied illumination levels, that reach up to 30 times brighter than under dark conditions. The main effect of moonlight is an increase in the analysis energy threshold and in the systematic uncertainties on the flux normalization. The sensitivity degradation is constrained to be below 10%, within 15-30% and between 60 and 80% for Nominal HV, Reduced HV and UV-pass filter observations, respectively. No worsening of the angular resolution was found. Thanks to observations during moonlight, the maximal duty cycle of MAGIC can be increased from ~18%, under dark nights only, to up to ~40% in total with only moderate performance degradation.

## Full text

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## Figures

26 figures with captions in the complete paper: https://tomesphere.com/paper/1704.00906/full.md

## References

45 references — full list in the complete paper: https://tomesphere.com/paper/1704.00906/full.md

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Source: https://tomesphere.com/paper/1704.00906