Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants
Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants
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DOI：
10.1016/j.astropartphys.2023.102850
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发表时间：
2023-03
影响因子：
3.5
通讯作者：
The Cherenkov Telescope Array Consortium;F. Acero;A. Acharyya;R. Adam;A. Aguasca-Cabot;I. Agudo;A. Aguirre-Santaella;J. Alfaro;R. Aloisio;N. Crespo;R. A. Batista;L. Amati;E. Amato;G. Ambrosi;E. Anguner;C. Aramo;C. Arcaro;T. Armstrong;K. Asano;Y. Ascasibar;J. Aschersleben;Michael Backes;A. Baktash;C. Balázs;M. Balbo;J. Ballet;A. B. Larriva;V. B. Martins;U. D. Almeida;J. Barrio;D. Bastieri;J. Baxter;J. Tjus;W. Benbow;M. I. Bernardos-Mart'in;J. Bernete;A. Berti;B. Bertucci;V. Beshley;P. Bhattacharjee;S. Bhattacharyya;A. Biland;E. Bissaldi;J. Biteau;O. Blanch;P. Bordas;E. Bottacini;J. Bregeon;R. Brose;N. Bucciantini;A. Bulgarelli;M. Capasso;R. Dolcetta;P. Caraveo;M. Cardillo;R. Carosi;S. Casanova;E. Cascone;F. Cassol;F. Catalani;M. Cerruti;P. Chadwick;S. Chaty;A. Chen;M. Chernyakova;A. Chiavassa;J. Chudoba;C. Coimbra-Araújo;V. Conforti;J. Contreras;A. Costa;H. Costantini;P. Cristofari;R. Crocker;Giacomo D’Amico;F. D’Ammando;A. Angelis;V. D. Caprio;E. M. G. D. Pino;E. O. Wilhelmi;V. Souza;C. Delgado;D. Volpe;D. Depaoli;T. D. Girolamo;F. D. Pierro;R. D. Tria;L. Venere;S. Diebold;J. Djuvsland;A. Donini;M. Doro;R. C. Anjos;V. Dwarkadas;S. Einecke;D. Elsasser;G. Emery;Carmelo Evoli;D. Falceta-Gonçalves;E. Fedorova;S. Fegan;G. Ferrand;E. Fiandrini;M. Filipović;V. Fioretti;M. Fiori;L. Foffano;G. Fontaine;S. Fukami;G. Galanti;G. Galaz;V. Gammaldi;C. Gasbarra;A. Ghalumyan;G. Ghirlanda;M. Giarrusso;G. Giavitto;N. Giglietto;F. Giordano;M. Giroletti;A. Giuliani;L. Giunti;N. Godinovic;J. G. Coelho;L. Gr'eaux;D. Green;M. Grondin;O. Gueta;S. Gunji;T. Hassan;M. Heller;S. Hern'andez-Cadena;J. Hinton;B. Hnatyk;R. Hnatyk;D. Hoffmann;W. Hofmann;J. Holder;D. Horan;P. Horváth;M. Hrabovsky;D. Hrupec;T. Inada;F. Incardona;S. Inoue;K. Ishio;M. Jamrozy;P. Janeček;I. Mart'inez;W. Jin;I. Jung-Richardt;J. Juryšek;P. Kaaret;V. Karas;U. Katz;D. Kerszberg;B. Kh'elifi;D. Kieda;R. Kissmann;T. Kleiner;G. Kluge;W. Kluźniak;J. Knodlseder;Y. Kobayashi;K. Kohri;N. Komin;P. Kornecki;H. Kubo;N. Palombara;M. L'ainez;A. Lamastra;J. Lapington;M. Lemoine-Goumard;J. Lenain;F. Leone;G. Leto;F. Leuschner;E. Lindfors;I. Liodakis;T. Lohse;S. Lombardi;F. Longo;R. L'opez-Coto;M. L'opez-Moya;A. L'opez-Oramas;S. Loporchio;P. Luque-Escamilla;O. Macias;J. Mackey;P. Majumdar;D. Mandát;M. Manganaro;G. Manicó;M. Marconi;J. Mart'i;G. Mart'inez;Miguel Ángel Martínez;O. Martínez;A. Mello;S. Menchiari;D. Meyer;S. Micanovic;D. Miceli;M. Miceli;J. Michałowski;T. Miener;J. Miranda;A. Mitchell;B. Mode;R. Moderski;L. Mohrmann;E. Molina;T. Montaruli;D. Morcuende;G. Morlino;A. Morselli;M. Mose;E. Moulin;R. Mukherjee;K. Munari;T. Murach;A. Nagai;S. Nagataki;R. Nemmen;J. Niemiec;D. Nieto;M. N. Rosillo;M. Nikołajuk;K. Nishijima;K. Noda;B. Novosyadlyj;S. Nozaki;M. Ohishi;S. Ohm;Y. Ohtani;A. Okumura;B. Olmi;R. Ong;M. Orienti;R. Orito;M. Orlandini;E. Orlando;S. Orlando;M. Ostrowski;I. Oya;F. Pantaleo;J. Paredes;B. Patricelli;M. Pecimotika;Michele Peresano;J. P'erez-Romero;M. Persic;O. Petruk;G. Piano;E. Pietropaolo;G. Pirola;C. Pittori;M. Pohl;G. Ponti;E. Prandini;G. Principe;C. Priyadarshi;E. Pueschel;G. Puhlhofer;M. L. Pumo;A. Quirrenbach;R. Rando;S. Razzaque;P. Reichherzer;A. Reimer;O. Reimer;M. Renaud;T. Reposeur;M. Rib'o;T. Richtler;J. Rico;F. Rieger;M. Rigoselli;L. Riitano;V. Rizi;E. Roache;P. Romano;G. Romeo;J. Rosado;G. Rowell;B. Rudak;I. Sadeh;S. Safi-Harb;L. Saha;S. Sailer;M. S'anchez-Conde;S. Sarkar;K. Satalecka;F. G. Saturni;A. Scherer;P. Schov'anek;F. Schussler;U. Schwanke;S. Scuderi;M. Seglar-Arroyo;O. Sergijenko;M. Servillat;R. Shang;P. Sharma;H. Siejkowski;V. Sliusar;A. Słowikowska;H. Sol;A. Specovius;S. Spencer;G. Spengler;A. Stamerra;S. Stanivc;T. Starecki;R. Starling;T. Stolarczyk;L. Pereira;Y. Suda;T. Suomijarvi;I. Sushch;H. Tajima;P. Tam;S. Tanaka;F. Tavecchio;V. Testa;W. Tian;L. Tibaldo;D. Torres;N. Tothill;B. Vallage;P. Vallania;C. Eldik;J. Scherpenberg;J. Vandenbroucke;M. V. Acosta;M. Vecchi;S. Vercellone;G. Verna;A. Viana;J. Vignatti;V. Vitale;V. Vodeb;S. Vorobiov;T. Vuillaume;S. Wagner;R. Walter;M. White;A. Wierzcholska;M. Will;D. Williams;L. Yang;T. Yoshida;T. Yoshikoshi;G. Zaharijas;L. Zampieri;D. Zavrtanik;M. Zavrtanik;V. Zhdanov;M. vZivec
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文献类型：
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作者：
The Cherenkov Telescope Array Consortium;F. Acero;A. Acharyya;R. Adam;A. Aguasca-Cabot;I. Agudo;A. Aguirre-Santaella;J. Alfaro;R. Aloisio;N. Crespo;R. A. Batista;L. Amati;E. Amato;G. Ambrosi;E. Anguner;C. Aramo;C. Arcaro;T. Armstrong;K. Asano;Y. Ascasibar;J. Aschersleben;Michael Backes;A. Baktash;C. Balázs;M. Balbo;J. Ballet;A. B. Larriva;V. B. Martins;U. D. Almeida;J. Barrio;D. Bastieri;J. Baxter;J. Tjus;W. Benbow;M. I. Bernardos-Mart'in;J. Bernete;A. Berti;B. Bertucci;V. Beshley;P. Bhattacharjee;S. Bhattacharyya;A. Biland;E. Bissaldi;J. Biteau;O. Blanch;P. Bordas;E. Bottacini;J. Bregeon;R. Brose;N. Bucciantini;A. Bulgarelli;M. Capasso;R. Dolcetta;P. Caraveo;M. Cardillo;R. Carosi;S. Casanova;E. Cascone;F. Cassol;F. Catalani;M. Cerruti;P. Chadwick;S. Chaty;A. Chen;M. Chernyakova;A. Chiavassa;J. Chudoba;C. Coimbra-Araújo;V. Conforti;J. Contreras;A. Costa;H. Costantini;P. Cristofari;R. Crocker;Giacomo D’Amico;F. D’Ammando;A. Angelis;V. D. Caprio;E. M. G. D. Pino;E. O. Wilhelmi;V. Souza;C. Delgado;D. Volpe;D. Depaoli;T. D. Girolamo;F. D. Pierro;R. D. Tria;L. Venere;S. Diebold;J. Djuvsland;A. Donini;M. Doro;R. C. Anjos;V. Dwarkadas;S. Einecke;D. Elsasser;G. Emery;Carmelo Evoli;D. Falceta-Gonçalves;E. Fedorova;S. Fegan;G. Ferrand;E. Fiandrini;M. Filipović;V. Fioretti;M. Fiori;L. Foffano;G. Fontaine;S. Fukami;G. Galanti;G. Galaz;V. Gammaldi;C. Gasbarra;A. Ghalumyan;G. Ghirlanda;M. Giarrusso;G. Giavitto;N. Giglietto;F. Giordano;M. Giroletti;A. Giuliani;L. Giunti;N. Godinovic;J. G. Coelho;L. Gr'eaux;D. Green;M. Grondin;O. Gueta;S. Gunji;T. Hassan;M. Heller;S. Hern'andez-Cadena;J. Hinton;B. Hnatyk;R. Hnatyk;D. Hoffmann;W. Hofmann;J. Holder;D. Horan;P. Horváth;M. Hrabovsky;D. Hrupec;T. Inada;F. Incardona;S. Inoue;K. Ishio;M. Jamrozy;P. Janeček;I. Mart'inez;W. Jin;I. Jung-Richardt;J. Juryšek;P. Kaaret;V. Karas;U. Katz;D. Kerszberg;B. Kh'elifi;D. Kieda;R. Kissmann;T. Kleiner;G. Kluge;W. Kluźniak;J. Knodlseder;Y. Kobayashi;K. Kohri;N. Komin;P. Kornecki;H. Kubo;N. Palombara;M. L'ainez;A. Lamastra;J. Lapington;M. Lemoine-Goumard;J. Lenain;F. Leone;G. Leto;F. Leuschner;E. Lindfors;I. Liodakis;T. Lohse;S. Lombardi;F. Longo;R. L'opez-Coto;M. L'opez-Moya;A. L'opez-Oramas;S. Loporchio;P. Luque-Escamilla;O. Macias;J. Mackey;P. Majumdar;D. Mandát;M. Manganaro;G. Manicó;M. Marconi;J. Mart'i;G. Mart'inez;Miguel Ángel Martínez;O. Martínez;A. Mello;S. Menchiari;D. Meyer;S. Micanovic;D. Miceli;M. Miceli;J. Michałowski;T. Miener;J. Miranda;A. Mitchell;B. Mode;R. Moderski;L. Mohrmann;E. Molina;T. Montaruli;D. Morcuende;G. Morlino;A. Morselli;M. Mose;E. Moulin;R. Mukherjee;K. Munari;T. Murach;A. Nagai;S. Nagataki;R. Nemmen;J. Niemiec;D. Nieto;M. N. Rosillo;M. Nikołajuk;K. Nishijima;K. Noda;B. Novosyadlyj;S. Nozaki;M. Ohishi;S. Ohm;Y. Ohtani;A. Okumura;B. Olmi;R. Ong;M. Orienti;R. Orito;M. Orlandini;E. Orlando;S. Orlando;M. Ostrowski;I. Oya;F. Pantaleo;J. Paredes;B. Patricelli;M. Pecimotika;Michele Peresano;J. P'erez-Romero;M. Persic;O. Petruk;G. Piano;E. Pietropaolo;G. Pirola;C. Pittori;M. Pohl;G. Ponti;E. Prandini;G. Principe;C. Priyadarshi;E. Pueschel;G. Puhlhofer;M. L. Pumo;A. Quirrenbach;R. Rando;S. Razzaque;P. Reichherzer;A. Reimer;O. Reimer;M. Renaud;T. Reposeur;M. Rib'o;T. Richtler;J. Rico;F. Rieger;M. Rigoselli;L. Riitano;V. Rizi;E. Roache;P. Romano;G. Romeo;J. Rosado;G. Rowell;B. Rudak;I. Sadeh;S. Safi-Harb;L. Saha;S. Sailer;M. S'anchez-Conde;S. Sarkar;K. Satalecka;F. G. Saturni;A. Scherer;P. Schov'anek;F. Schussler;U. Schwanke;S. Scuderi;M. Seglar-Arroyo;O. Sergijenko;M. Servillat;R. Shang;P. Sharma;H. Siejkowski;V. Sliusar;A. Słowikowska;H. Sol;A. Specovius;S. Spencer;G. Spengler;A. Stamerra;S. Stanivc;T. Starecki;R. Starling;T. Stolarczyk;L. Pereira;Y. Suda;T. Suomijarvi;I. Sushch;H. Tajima;P. Tam;S. Tanaka;F. Tavecchio;V. Testa;W. Tian;L. Tibaldo;D. Torres;N. Tothill;B. Vallage;P. Vallania;C. Eldik;J. Scherpenberg;J. Vandenbroucke;M. V. Acosta;M. Vecchi;S. Vercellone;G. Verna;A. Viana;J. Vignatti;V. Vitale;V. Vodeb;S. Vorobiov;T. Vuillaume;S. Wagner;R. Walter;M. White;A. Wierzcholska;M. Will;D. Williams;L. Yang;T. Yoshida;T. Yoshikoshi;G. Zaharijas;L. Zampieri;D. Zavrtanik;M. Zavrtanik;V. Zhdanov;M. vZivec
局域宇宙线(CR)能谱在3~PeV能量附近表现出光谱软化现象。能够将强子加速到这种能量的源被称为强子PeVatrons。然而，在银河系中还没有确定强子PeVatrons的存在。包括银河系超新星残留物(SNR)在内的几个源类已经被提议作为PeVatron的候选者。评估了使用切伦科夫望远镜阵列(CTA)搜索强子PeVatrons的可能性。重点是使用非常高的能量射线光谱特征来识别PeVatrons。假设信噪比可以将CRS加速到膝部能量，在信噪比演化模型中估计可被识别为PeVatrons的银河系信噪比数目。此外，还研究了在月光条件下进行PeVatron搜索的后续观测策略的可能性。介绍了识别PeVatrons的统计方法，并对CTA观测站对强子PeVatrons发射光谱的响应进行了真实的蒙特卡罗模拟。根据对SNR演化的简化模型的模拟，平均9个银河系PeVatron SNR的a射线信号的探测预计将在曝光10小时后用CTA扫描银河面。CTA也被证明具有极好的潜力，在每个源暴露数小时的深度观测中确认这些源是PeVatrons。
The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte--Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 hours of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations withhours of exposure per source.