1
|
Marcelli L, Bolmgren K, Barghini D, Battisti M, Blaksley C, Blin S, Belov A, Bertaina M, Bianciotto M, Bisconti F, Cambiè G, Capel F, Casolino M, Churilo I, Crisconio M, Taille CDL, Ebisuzaki T, Eser J, Fenu F, Franceschi M, Fuglesang C, Golzio A, Gorodetzky P, Kasuga H, Kajino F, Klimov P, Kuznetsov V, Manfrin M, Mascetti G, Marszal W, Miyamoto H, Murashov A, Napolitano T, Ohmori H, Olinto A, Parizot E, Picozza P, Piotrowski L, Plebaniak Z, Prevot G, Reali E, Romoli G, Ricci M, Sakaki N, Shinozaki K, Szabelski J, Takizawa Y, Vagelli V, Valentini G, Vrabel M, Wiencke L. Dataset of night-time emissions of the Earth in the near UV range (290-430 nm), with 6.3 km resolution in the latitude range -51.6<L<+51.6 degrees, acquired on board the International Space Station with the Mini-EUSO detector. Data Brief 2023; 48:109105. [PMID: 37095754 PMCID: PMC10121388 DOI: 10.1016/j.dib.2023.109105] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/06/2023] [Revised: 03/21/2023] [Accepted: 03/24/2023] [Indexed: 04/03/2023] Open
Abstract
The data presented in this article are related to the research paper entitled "Observation of night-time emissions of the Earth in the near UV range from the International Space Station with the Mini-EUSO detector" (Remote Sensing of Environment, Volume 284, January 2023, 113336, https://doi.org/10.1016/j.rse.2022.113336). The data have been acquired with the Mini-EUSO detector, an UV telescope operating in the range 290-430 nm and located inside the International Space Station. The detector was launched in August 2019, and it has started operations from the nadir-facing UV-transparent window in the Russian Zvezda module in October 2019. The data presented here refer to 32 sessions acquired between 2019-11-19 and 2021-05-06. The instrument consists of a Fresnel-lens optical system and a focal surface composed of 36 multi-anode photomultiplier tubes, each with 64 channels, for a total of 2304 channels with single photon counting sensitivity. The telescope, with a square field-of-view of 44°, has a spatial resolution on the Earth surface of 6.3 km and saves triggered transient phenomena with a temporal resolution of 2.5 µs and 320 µs. The telescope also operates in continuous acquisition at a 40.96 ms scale. In this article, large-area night-time UV maps obtained processing the 40.96 ms data, taking averages over regions of some specific geographical areas (e.g., Europe, North America) and over the entire globe, are presented. Data are binned into 0.1° × 0.1° or 0.05° × 0.05° cells (depending on the scale of the map) over the Earth's surface. Raw data are made available in the form of tables (latitude, longitude, counts) and .kmz files (containing the .png images). These are - to the best of our knowledge - the highest sensitivity data in this wavelength range and can be of use to various disciplines.
Collapse
|
2
|
Adams JH, Ahmad S, Allard D, Anzalone A, Bacholle S, Barrillon P, Bayer J, Bertaina M, Bisconti F, Blaksley C, Blin-Bondil S, Bobík P, Cafagna F, Campana D, Capel F, Casolino M, Cassardo C, Catalano C, Cremonini R, Dagoret-Campagne S, Danto P, del Peral L, de la Taille C, Díaz Damian A, Dupieux M, Ebersoldt A, Ebisuzaki T, Eser J, Evrard J, Fenu F, Ferrarese S, Fornaro C, Fouka M, Gorodetzky P, Guarino F, Guzman A, Hachisu Y, Haungs A, Judd E, Jung A, Karczmarczyk J, Kawasaki Y, Klimov PA, Kuznetsov E, Mackovjak S, Manfrin M, Marcelli L, Medina-Tanco G, Mercier K, Merino A, Mernik T, Miyamoto H, Morales de los Ríos JA, Moretto C, Mot B, Neronov A, Ohmori H, Olinto AV, Osteria G, Panico B, Parizot E, Paul T, Picozza P, Piotrowski LW, Plebaniak Z, Pliego S, Prat P, Prévôt G, Prieto H, Putis M, Rabanal J, Ricci M, Rojas J, Rodríguez Frías MD, Roudil G, Sáez Cano G, Sahnoun Z, Sakaki N, Sanchez JC, Santangelo A, Sarazin F, Scotti V, Shinozaki K, Silva H, Soriano JF, Suino G, Szabelski J, Toscano S, Tabone I, Takizawa Y, von Ballmoos P, Wiencke L, Wille M, Zotov M. A Review of the EUSO-Balloon Pathfinder for the JEM-EUSO Program. Space Sci Rev 2022; 218:3. [PMID: 35153338 PMCID: PMC8807436 DOI: 10.1007/s11214-022-00870-x] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/24/2021] [Accepted: 12/31/2021] [Indexed: 06/14/2023]
Abstract
EUSO-Balloon is a pathfinder for JEM-EUSO, the mission concept of a spaceborne observatory which is designed to observe Ultra-High Energy Cosmic Ray (UHECR)-induced Extensive Air Showers (EAS) by detecting their UltraViolet (UV) light tracks "from above." On August 25, 2014, EUSO-Balloon was launched from Timmins Stratospheric Balloon Base (Ontario, Canada) by the balloon division of the French Space Agency CNES. After reaching a floating altitude of 38 km, EUSO-Balloon imaged the UV light in the wavelength range ∼290-500 nm for more than 5 hours using the key technologies of JEM-EUSO. The flight allowed a good understanding of the performance of the detector to be developed, giving insights into possible improvements to be applied to future missions. A detailed measurement of the photoelectron counts in different atmospheric and ground conditions was achieved. By means of the simulation of the instrument response and by assuming atmospheric models, the absolute intensity of diffuse light was estimated. The instrument detected hundreds of laser tracks with similar characteristics to EASs shot by a helicopter flying underneath. These are the first recorded laser tracks measured from a fluorescence detector looking down on the atmosphere. The reconstruction of the direction of the laser tracks was performed. In this work, a review of the main results obtained by EUSO-Balloon is presented as well as implications for future space-based observations of UHECRs.
Collapse
Affiliation(s)
- J. H. Adams
- University of Alabama in Huntsville, Huntsville, USA
| | - S. Ahmad
- Omega, Ecole Polytechnique, CNRS/IN2P3, Palaiseau, France
| | - D. Allard
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - A. Anzalone
- INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Palermo, Italy
- Istituto Nazionale di Fisica Nucleare - Sezione di Catania, Catania, Italy
| | - S. Bacholle
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - P. Barrillon
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay, France
| | - J. Bayer
- Institute for Astronomy and Astrophysics, University of Tübingen, Tübingen, Germany
| | - M. Bertaina
- Istituto Nazionale di Fisica Nucleare - Sezione di Torino, Torino, Italy
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | - F. Bisconti
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
- Karlsruhe Institute of Technology, Karlsruhe, Germany
| | - C. Blaksley
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - S. Blin-Bondil
- Omega, Ecole Polytechnique, CNRS/IN2P3, Palaiseau, France
| | - P. Bobík
- Institute of Experimental Physics, Slovak Academy of Sciences, Košice, Slovakia
| | - F. Cafagna
- Istituto Nazionale di Fisica Nucleare - Sezione di Bari, Bari, Italy
| | - D. Campana
- Istituto Nazionale di Fisica Nucleare - Sezione di Napoli, Naples, Italy
| | - F. Capel
- KTH Royal Institute of Technology, Stockholm, Sweden
| | - M. Casolino
- RIKEN, 2-1 Hirosawa, Wako, Saitama Japan
- Istituto Nazionale di Fisica Nucleare - Sezione di Roma Tor Vergata, Roma, Italy
| | - C. Cassardo
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | - C. Catalano
- IRAP, Université de Toulouse, CNRS, Toulouse, France
| | - R. Cremonini
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | | | - P. Danto
- CNES, 18 avenue Edouard Belin, Toulouse, France
| | | | | | | | - M. Dupieux
- IRAP, Université de Toulouse, CNRS, Toulouse, France
| | - A. Ebersoldt
- Karlsruhe Institute of Technology, Karlsruhe, Germany
| | | | - J. Eser
- Colorado School of Mines, Golden, USA
| | - J. Evrard
- CNES, 18 avenue Edouard Belin, Toulouse, France
| | - F. Fenu
- Istituto Nazionale di Fisica Nucleare - Sezione di Torino, Torino, Italy
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | - S. Ferrarese
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | | | - M. Fouka
- Center of Research in Astronomy, Astrophysics, and Geophysics, Algiers, Algeria
| | - P. Gorodetzky
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - F. Guarino
- Istituto Nazionale di Fisica Nucleare - Sezione di Napoli, Naples, Italy
- Dipartimento di Scienze Fisiche, Universitá di Napoli Federico II, Naples, Italy
| | - A. Guzman
- Institute for Astronomy and Astrophysics, University of Tübingen, Tübingen, Germany
| | - Y. Hachisu
- RIKEN, 2-1 Hirosawa, Wako, Saitama Japan
| | - A. Haungs
- Karlsruhe Institute of Technology, Karlsruhe, Germany
| | - E. Judd
- Space Sciences Laboratory, University of California, Berkeley, CA USA
| | - A. Jung
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | | | | | - P. A. Klimov
- Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia
| | - E. Kuznetsov
- University of Alabama in Huntsville, Huntsville, USA
| | - S. Mackovjak
- Institute of Experimental Physics, Slovak Academy of Sciences, Košice, Slovakia
| | - M. Manfrin
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | - L. Marcelli
- Istituto Nazionale di Fisica Nucleare - Sezione di Roma Tor Vergata, Roma, Italy
| | - G. Medina-Tanco
- Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - K. Mercier
- CNES, 18 avenue Edouard Belin, Toulouse, France
| | | | - T. Mernik
- Institute for Astronomy and Astrophysics, University of Tübingen, Tübingen, Germany
| | - H. Miyamoto
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay, France
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | | | - C. Moretto
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay, France
| | - B. Mot
- IRAP, Université de Toulouse, CNRS, Toulouse, France
| | - A. Neronov
- ISDC Data Centre for Astrophysics, Versoix, Switzerland
| | - H. Ohmori
- RIKEN, 2-1 Hirosawa, Wako, Saitama Japan
| | | | - G. Osteria
- Istituto Nazionale di Fisica Nucleare - Sezione di Napoli, Naples, Italy
| | - B. Panico
- Istituto Nazionale di Fisica Nucleare - Sezione di Napoli, Naples, Italy
- Dipartimento di Scienze Fisiche, Universitá di Napoli Federico II, Naples, Italy
| | - E. Parizot
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - T. Paul
- Lehman College, City University of New York, New York, USA
| | - P. Picozza
- RIKEN, 2-1 Hirosawa, Wako, Saitama Japan
- Istituto Nazionale di Fisica Nucleare - Sezione di Roma Tor Vergata, Roma, Italy
- Dipartimento di Fisica, Universitá di Roma Tor Vergata, Roma, Italy
| | | | - Z. Plebaniak
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
- National Centre for Nuclear Research, Lodz, Poland
| | - S. Pliego
- Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - P. Prat
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - G. Prévôt
- APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Paris, France
| | - H. Prieto
- Universidad de Alcalá, Madrid, Spain
| | - M. Putis
- Institute of Experimental Physics, Slovak Academy of Sciences, Košice, Slovakia
| | - J. Rabanal
- Université Paris-Saclay, CNRS/IN2P3, IJCLab, Orsay, France
| | - M. Ricci
- Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali di Frascati, Frascati, Italy
| | - J. Rojas
- Universidad Nacional Autónoma de México, Mexico City, Mexico
| | | | - G. Roudil
- IRAP, Université de Toulouse, CNRS, Toulouse, France
| | | | - Z. Sahnoun
- Center of Research in Astronomy, Astrophysics, and Geophysics, Algiers, Algeria
| | - N. Sakaki
- RIKEN, 2-1 Hirosawa, Wako, Saitama Japan
| | - J. C. Sanchez
- Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - A. Santangelo
- Institute for Astronomy and Astrophysics, University of Tübingen, Tübingen, Germany
| | | | - V. Scotti
- Istituto Nazionale di Fisica Nucleare - Sezione di Napoli, Naples, Italy
- Dipartimento di Scienze Fisiche, Universitá di Napoli Federico II, Naples, Italy
| | - K. Shinozaki
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
- National Centre for Nuclear Research, Lodz, Poland
| | - H. Silva
- Universidad Nacional Autónoma de México, Mexico City, Mexico
| | | | - G. Suino
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | - J. Szabelski
- National Centre for Nuclear Research, Lodz, Poland
| | - S. Toscano
- ISDC Data Centre for Astrophysics, Versoix, Switzerland
| | - I. Tabone
- Dipartimento di Fisica, Universitá di Torino, Torino, Italy
| | | | | | | | - M. Wille
- ECAP, University of Erlangen-Nuremberg, Erlangen, Germany
| | - M. Zotov
- Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia
| |
Collapse
|