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The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behaviour and it is one of only a few FSRQs detected in very-high-energy (VHE, E>100 GeV) gamma rays. The VHE gamma -ray observations with H.E.S.S. and MAGIC in late May and early June 2016 resulted in the detection of an unprecedented flare, which revealed, for the first time, VHE gamma -ray intranight variability for this source. While a common variability timescale of 1.5 h has been found, there is a significant deviation near the end of the flare, with a timescale of similar to 20 min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, a curvature was detected in the VHE gamma -ray spectrum of PKS 1510-089, which can be fully explained by the absorption on the part of the extragalactic background light. Optical R-band observations with ATOM revealed a counterpart of the gamma -ray flare, even though the detailed flux evolution differs from the VHE gamma -ray light curve. Interestingly, a steep flux decrease was observed at the same time as the cessation of the VHE gamma -ray flare. In the high-energy (HE, E> 100 MeV) gamma -ray band, only a moderate flux increase was observed with Fermi-LAT, while the HE gamma -ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the gamma -ray spectrum indicates that the emission region is located outside of the BLR. Radio very-long-baseline interferometry observations reveal a fast-moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located similar to 50 pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this is indeed a true correlation, the VHE gamma rays must have been produced far down in the jet, where turbulent plasma crosses a standing shock.
H.e.s.s. and MAGIC observations of a sudden cessation of a very-high-energy γ -ray flare in PKS 1510-089 in May 2016
H. Abdalla;R. Adam;F. Aharonian;F. Ait Benkhali;E. O. Ang??ner;C. Arcaro;C. Armand;T. Armstrong;H. Ashkar;M. Backes;V. Baghmanyan;V. Barbosa Martins;A. Barnacka;M. Barnard;Y. Becherini;D. Berge;K. Bernl??hr;B. Bi;M. B??ttcher;C. Boisson;J. Bolmont;S. Bonnefoy;M. de Bony de Lavergne;J. Bregeon;M. Breuhaus;F. Brun;P. Brun;M. Bryan;M. B??chele;T. Bulik;T. Bylund;S. Caroff;A. Carosi;S. Casanova;T. Chand;S. Chandra;A. Chen;G. Cotter;M. Cury??o;J. Damascene Mbarubucyeye;I. D. Davids;J. Davies;C. Deil;J. Devin;P. deWilt;L. Dirson;A. Djannati-Ata??;A. Dmytriiev;A. Donath;V. Doroshenko;J. Dyks;K. Egberts;F. Eichhorn;S. Einecke;G. Emery;J. -P. Ernenwein;K. Feijen;S. Fegan;A. Fiasson;G. Fichet de Clairfontaine;M. Filipovic;G. Fontaine;S. Funk;M. F????ling;S. Gabici;Y. A. Gallant;G. Giavitto;L. Giunti;D. Glawion;J. F. Glicenstein;D. Gottschall;M. -H. Grondin;J. Hahn;M. Haupt;G. Hermann;J. A. Hinton;W. Hofmann;C. Hoischen;T. L. Holch;M. Holler;M. H??rbe;D. Horns;D. Huber;M. Jamrozy;D. Jankowsky;F. Jankowsky;A. Jardin-Blicq;V. Joshi;I. Jung-Richardt;M. A. Kastendieck;K. Katarzy??ski;U. Katz;D. Khangulyan;B. Kh??lifi;S. Klepser;W. Klu??niak;Nu. Komin;R. Konno;K. Kosack;D. Kostunin;M. Kreter;G. Lamanna;A. Lemi??re;M. Lemoine-Goumard;J. -P. Lenain;C. Levy;T. Lohse;I. Lypova;J. Mackey;J. Majumdar;D. Malyshev;D. Malyshev;V. Marandon;P. Marchegiani;A. Marcowith;A. Mares;G. Mart??-Devesa;R. Marx;G. Maurin;P. J. Meintjes;M. Meyer;A. M. W. Mitchell;R. Moderski;M. Mohamed;L. Mohrmann;A. Montanari;C. Moore;P. Morris;E. Moulin;J. Muller;T. Murach;K. Nakashima;A. Nayerhoda;M. de Naurois;H. Ndiyavala;F. Niederwanger;J. Niemiec;L. Oakes;P. O???Brien;H. Odaka;S. Ohm;L. Olivera-Nieto;E. de Ona Wilhelmi;M. Ostrowski;M. Panter;S. Panny;R. D. Parsons;G. Peron;B. Peyaud;Q. Piel;S. Pita;V. Poireau;A. Priyana Noel;D. A. Prokhorov;H. Prokoph;G. P??hlhofer;M. Punch;A. Quirrenbach;S. Raab;R. Rauth;P. Reichherzer;A. Reimer;O. Reimer;Q. Remy;M. Renaud;F. Rieger;L. Rinchiuso;C. Romoli;G. Rowell;B. Rudak;E. Ruiz-Velasco;V. Sahakian;S. Sailer;D. A. Sanchez;A. Santangelo;M. Sasaki;M. Scalici;F. Sch??ssler;H. M. Schutte;U. Schwanke;S. Schwemmer;M. Seglar-Arroyo;M. Senniappan;A. S. Seyffert;N. Shafi;K. Shiningayamwe;R. Simoni;A. Sinha;H. Sol;A. Specovius;S. Spencer;M. Spir-Jacob;??. Stawarz;L. Sun;R. Steenkamp;C. Stegmann;S. Steinmassl;C. Steppa;T. Takahashi;T. Tavernier;A. M. Taylor;R. Terrier;D. Tiziani;M. Tluczykont;L. Tomankova;C. Trichard;M. Tsirou;R. Tuffs;Y. Uchiyama;D. J. van der Walt;C. van Eldik;C. van Rensburg;B. van Soelen;G. Vasileiadis;J. Veh;C. Venter;P. Vincent;J. Vink;H. J. V??lk;T. Vuillaume;Z. Wadiasingh;S. J. Wagner;J. Watson;F. Werner;R. White;A. Wierzcholska;Yu. W. Wong;A. Yusafzai;M. Zacharias;R. Zanin;D. Zargaryan;A. A. Zdziarski;A. Zech;S. J. Zhu;J. Zorn;S. Zouari;N. ??ywucka;V. A. Acciari;S. Ansoldi;L. A. Antonelli;A. Arbet Engels;K. Asano;D. Baack;A. Babi??;A. Baquero;U. Barres de Almeida;J. A. Barrio;J. Becerra Gonz??lez;W. Bednarek;L. Bellizzi;E. Bernardini;A. Berti;J. Besenrieder;W. Bhattacharyya;C. Bigongiari;A. Biland;O. Blanch;G. Bonnoli;??. Bo??njak;G. Busetto;R. Carosi;G. Ceribella;M. Cerruti;Y. Chai;A. Chilingarian;S. Cikota;S. M. Colak;U. Colin;E. Colombo;J. L. Contreras;J. Cortina;S. Covino;G. D???Amico;V. D???Elia;P. Da Vela;F. Dazzi;A. De Angelis;B. De Lotto;M. Delfino;J. Delgado;D. Depaoli;F. Di Pierro;L. Di Venere;E. Do Souto Espi??eira;D. Dominis Prester;A. Donini;D. Dorner;M. Doro;D. Elsaesser;V. Fallah Ramazani;A. Fattorini;G. Ferrara;L. Foffano;M. V. Fonseca;L. Font;C. Fruck;S. Fukami;R. J. Garc??a L??pez;M. Garczarczyk;S. Gasparyan;M. Gaug;N. Giglietto;F. Giordano;P. Gliwny;N. Godinovi??;D. Green;D. Hadasch;A. Hahn;L. Heckmann;J. Herrera;J. Hoang;D. Hrupec;M. H??tten;T. Inada;S. Inoue;K. Ishio;Y. Iwamura;L. Jouvin;Y. Kajiwara;M. Karjalainen;D. Kerszberg;Y. Kobayashi;H. Kubo;J. Kushida;A. Lamastra;D. Lelas;F. Leone;E. Lindfors;S. Lombardi;F. Longo;M. L??pez;R. L??pez-Coto;A. L??pez-Oramas;S. Loporchio;B. Machado de Oliveira Fraga;C. Maggio;P. Majumdar;M. Makariev;M. Mallamaci;G. Maneva;M. Manganaro;K. Mannheim;L. Maraschi;M. Mariotti;M. Mart??nez;D. Mazin;S. Mender;S. Mi??anovi??;D. Miceli;T. Miener;M. Minev;J. M. Miranda;R. Mirzoyan;E. Molina;A. Moralejo;D. Morcuende;V. Moreno;E. Moretti;P. Munar-Adrover;V. Neustroev;C. Nigro;K. Nilsson;D. Ninci;K. Nishijima;K. Noda;S. Nozaki;Y. Ohtani;T. Oka;J. Otero-Santos;M. Palatiello;D. Paneque;R. Paoletti;J. M. Paredes;L. Pavleti??;P. Pe??il;C. Perennes;M. Persic;P. G. Prada Moroni;E. Prandini;C. Priyadarshi;I. Puljak;W. Rhode;M. Rib??;J. Rico;C. Righi;A. Rugliancich;L. Saha;N. Sahakyan;T. Saito;S. Sakurai;K. Satalecka;B. Schleicher;K. Schmidt;T. Schweizer;J. Sitarek;I. ??nidari??;D. Sobczynska;A. Spolon;A. Stamerra;D. Strom;M. Strzys;Y. Suda;T. Suri??;M. Takahashi;F. Tavecchio;P. Temnikov;T. Terzi??;M. Teshima;N. Torres-Alb??;L. Tosti;S. Truzzi;J. van Scherpenberg;G. Vanzo;M. Vazquez Acosta;S. Ventura;V. Verguilov;C. F. Vigorito;V. Vitale;I. Vovk;M. Will;D. Zari??;S. G. Jorstad;A. P. Marscher;B. Boccardi;C. Casadio;J. Hodgson;J. -Y. Kim;T. P. Krichbaum;A. L??hteenm??ki;M. Tornikoski;E. Traianou;Z. R. Weaver
2021-01-01
Abstract
The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behaviour and it is one of only a few FSRQs detected in very-high-energy (VHE, E>100 GeV) gamma rays. The VHE gamma -ray observations with H.E.S.S. and MAGIC in late May and early June 2016 resulted in the detection of an unprecedented flare, which revealed, for the first time, VHE gamma -ray intranight variability for this source. While a common variability timescale of 1.5 h has been found, there is a significant deviation near the end of the flare, with a timescale of similar to 20 min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, a curvature was detected in the VHE gamma -ray spectrum of PKS 1510-089, which can be fully explained by the absorption on the part of the extragalactic background light. Optical R-band observations with ATOM revealed a counterpart of the gamma -ray flare, even though the detailed flux evolution differs from the VHE gamma -ray light curve. Interestingly, a steep flux decrease was observed at the same time as the cessation of the VHE gamma -ray flare. In the high-energy (HE, E> 100 MeV) gamma -ray band, only a moderate flux increase was observed with Fermi-LAT, while the HE gamma -ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the gamma -ray spectrum indicates that the emission region is located outside of the BLR. Radio very-long-baseline interferometry observations reveal a fast-moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located similar to 50 pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this is indeed a true correlation, the VHE gamma rays must have been produced far down in the jet, where turbulent plasma crosses a standing shock.
GERMANIA SPAGNA STATI UNITI D'AMERICA ARMENIA AUSTRIA GIAPPONE POLONIA
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H. Abdalla; R. Adam; F. Aharonian; F. Ait Benkhali; E. O. Ang??ner; C. Arcaro; C. Armand; T. Armstrong; H. Ashkar; M. Backes; V. Baghmanyan; V. Barbos...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/1877413
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simulazione ASN
Il report seguente simula gli indicatori relativi alla produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione.
La simulazione si basa sui dati IRIS e presenta gli indicatori calcolati alla data indicata sul report. Si ricorda che in sede di domanda ASN presso il MIUR gli indicatori saranno invece calcolati a partire dal 1° gennaio rispettivamente del quinto/decimo/quindicesimo anno precedente la scadenza del quadrimestre di presentazione della domanda (art 2 del DM 598/2018).
In questa simulazione pertanto il valore degli indicatori potrà differire da quello conteggiato all’atto della domanda ASN effettuata presso il MIUR a seguito di:
Correzioni imputabili a eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori.
Presenza di eventuali errori di catalogazione e/o dati mancanti in IRIS
Variabilità nel tempo dei valori citazionali (per i settori bibliometrici)
Variabilità della finestra temporale considerata in funzione della sessione di domanda ASN a cui si partecipa.
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