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Related papers: Latest view of CTA 1 with VERITAS

200 papers

CTA 1 (G119.5+10.2) is a composite supernova remnant (SNR) with a shell-type structure, visible in the radio band, surrounding a smaller pulsar wind nebula. Fermi detected a radio-quiet pulsar PSR J0007+7303 within the radio shell. 26.5…

High Energy Astrophysical Phenomena · Physics 2019-08-13 Nahee Park

CTA 1 (G119.5+10.2) is a composite supernova remnant (SNR) with a shell-type structure in the radio band and a center filled morphology at X-ray energies. Fermi has detected a radio-quiet pulsar PSR J0007+7303 within the radio shell of CTA…

High Energy Astrophysical Phenomena · Physics 2019-08-13 Steven McArthur

We report the discovery of TeV gamma-ray emission coincident with the shell-type radio supernova remnant (SNR) CTA 1 using the VERITAS gamma-ray observatory. The source, VER J0006+729, was detected as a 6.5 standard deviation excess over…

CTA~1 is a composite supernova remnant featuring a shell structure and an inner Pulsar Wind Nebula. The shell is visible in the radio band, while Fermi has detected the radio-quiet pulsar PSR J0007+7303 at its core. Gamma-ray detectors such…

High Energy Astrophysical Phenomena · Physics 2025-10-01 Bastien Lacave

We present deep Chandra observations of the pulsar wind nebula (PWN) powered by PSR J0007+7303 in the composite supernova remnant CTA 1. The merged ACIS image shows a $\sim20''$ jet extending south of the pulsar and bending toward the…

High Energy Astrophysical Phenomena · Physics 2026-05-21 Seth Gagnon , Oleg Kargaltsev , Jason Alford , Joseph Gelfand , Alexander Lange

We estimate the molecular mass around CTA 1 using data from Planck and the Harvard CO survey. We observe that the molecular mass in the vicinity of the complex is not enough to explain the TeV emission observed by VERITAS, even under…

High Energy Astrophysical Phenomena · Physics 2016-04-20 Jonatan Martín , Diego F. Torres , Giovanna Pedaletti

Supernova remnants (SNRs) are among the strongest candidates to explain the flux of cosmic rays below the knee around 10^15 eV. Pulsar wind nebulae (PWNe), synchrotron nebulae powered by the spin-down of energetic young pulsars, comprise…

Astrophysics of Galaxies · Physics 2019-08-13 Thomas Brian Humensky

We present evidence that the very-high-energy (VHE, E > 100 GeV) gamma-ray emission coincident with the supernova remnant IC 443 is extended. IC 443 contains one of the best-studied sites of supernova remnant/molecular cloud interaction and…

The study of supernova remnants and pulsar wind nebulae was one of the Key Science Projects for the first two years of VERITAS observations. VERITAS is an array of four imaging Cherenkov telescopes located at the Whipple Observatory in…

Astrophysics of Galaxies · Physics 2019-08-13 Brian Humensky

Shell-type supernova remnants (SNRs) accelerate particles at the shock front between the expanding remnant and the swept-up interstellar medium. If these particles include protons and nuclei, very-high-energy gamma-ray emission may result…

Astrophysics · Physics 2007-09-28 VERITAS Collaboration , T. B. Humensky

The Cherenkov Telescope Array (CTA) is planned to serve as a ground-based observatory for (very-)high-energy gamma-ray astronomy, open to a wide astrophysics community, providing a deep insight into the non-thermal high-energy universe. It…

High Energy Astrophysical Phenomena · Physics 2019-08-15 M. Renaud

We report on an 105 ks Suzaku observation of the supernova remnant CTA 1 (G119.5+10.2). The Suzaku soft X-ray observation was carried out with both timing mode and imaging mode. A ~ 10' extended feature, which is interpreted as a bow-shock…

We report a detection of GeV $\gamma$-ray emission potentially originating from the pulsar wind nebula in CTA 1 by analyzing about 15 yr of Fermi Large Area Telescope data. By selecting an energy range from 50 GeV to 1 TeV to remove…

High Energy Astrophysical Phenomena · Physics 2024-03-12 Liancheng Zhou , Keyao Wu , Yunlu Gong , Jun Fang

Energetic young pulsars and expanding blast waves (supernova remnants, SNRs) are the most visible remains after massive stars, ending their lives, explode in core-collapse supernovae. The Fermi Gamma-Ray Space Telescope has unveiled a radio…

Astrophysics · Physics 2012-08-27 Fermi LAT Collaboration

We present new radio images of the supernova remnant (SNR) CTA 1 at 1420 and 408 MHz, and in the 21 cm line of H I observed with the Dominion Radio Astrophysical Observatory Synthesis Telescope and at 1420 MHz observed with the Effelsberg…

High Energy Astrophysical Phenomena · Physics 2024-12-20 Tam Do , Roland Kothes , Alex S. Hill , Andrew Gray , Patricia Reich , Wolfgang Reich

The last few years have seen a revolution in very-high gamma-ray astronomy (VHE; E>100 GeV) driven largely by a new generation of Cherenkov telescopes (namely the H.E.S.S. telescope array, the MAGIC and MAGIC-II large telescopes and the…

Instrumentation and Methods for Astrophysics · Physics 2019-08-13 E. de Ona Wilhelmi , B. Rudak , J. A. Barrio , J. L. Contreras , Y. Gallant , D. Hadasch , T. Hassan , M. Lopez , D. Mazin , N. Mirabal , G. Pedaletti , M. Renaud , R. de los Reyes , D. F. Torres

Pulsar wind nebulae (PWNe) studies with the Chandra X-ray Observatory have opened a new window to address the physics of pulsar winds, zoom on their interaction with their hosting supernova remnant (SNR) and interstellar medium, and…

High Energy Astrophysical Phenomena · Physics 2015-06-16 H. Matheson , S. Safi-Harb , R. Kothes

We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX~J1713.7$-$3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very-high-energy (VHE) gamma rays. Special attention is…

High Energy Astrophysical Phenomena · Physics 2020-01-30 The CTA Consortium , : , F. Acero , R. Aloisio , J. Amans , E. Amato , L. A. Antonelli , C. Aramo , T. Armstrong , F. Arqueros , K. Asano , M. Ashley , M. Backes , C. Balazs , A. Balzer , A. Bamba , M. Barkov , J. A. Barrio , W. Benbow , K. Bernlöhr , V. Beshley , C. Bigongiari , A. Biland , A. Bilinsky , E. Bissaldi , J. Biteau , O. Blanch , P. Blasi , J. Blazek , C. Boisson , G. Bonanno , A. Bonardi , C. Bonavolontà , G. Bonnoli , C. Braiding , S. Brau-Nogué , J. Bregeon , A. M. Brown , V. Bugaev , A. Bulgarelli , T. Bulik , M. Burton , A. Burtovoi , G. Busetto , M. Böttcher , R. Cameron , M. Capalbi , A. Caproni , P. Caraveo , R. Carosi , E. Cascone , M. Cerruti , S. Chaty , A. Chen , X. Chen , M. Chernyakova , M. Chikawa , J. Chudoba , J. Cohen-Tanugi , S. Colafrancesco , V. Conforti , J. L. Contreras , A. Costa , G. Cotter , S. Covino , G. Covone , P. Cumani , G. Cusumano , F. D'Ammando , D. D'Urso , M. Daniel , F. Dazzi , A. De Angelis , G. De Cesare , A. De Franco , F. De Frondat , E. M. de Gouveia Dal Pino , C. De Lisio , R. de los Reyes Lopez , B. De Lotto , M. de Naurois , F. De Palma , M. Del Santo , C. Delgado , D. della Volpe , T. Di Girolamo , C. Di Giulio , F. Di Pierro , L. Di Venere , M. Doro , J. Dournaux , D. Dumas , V. Dwarkadas , C. Díaz , J. Ebr , K. Egberts , S. Einecke , D. Elsässer , S. Eschbach , D. Falceta-Goncalves , G. Fasola , E. Fedorova , A. Fernández-Barral , G. Ferrand , M. Fesquet , E. Fiandrini , A. Fiasson , M. D. Filipovíc , V. Fioretti , L. Font , G. Fontaine , F. J. Franco , L. Freixas Coromina , Y. Fujita , Y. Fukui , S. Funk , A. Förster , A. Gadola , R. Garcia López , M. Garczarczyk , N. Giglietto , F. Giordano , A. Giuliani , J. Glicenstein , R. Gnatyk , P. Goldoni , T. Grabarczyk , R. Graciani , J. Graham , P. Grandi , J. Granot , A. J. Green , S. Griffiths , S. Gunji , H. Hakobyan , S. Hara , T. Hassan , M. Hayashida , M. Heller , J. C. Helo , J. Hinton , B. Hnatyk , J. Huet , M. Huetten , T. B. Humensky , M. Hussein , J. Hörandel , Y. Ikeno , T. Inada , Y. Inome , S. Inoue , T. Inoue , Y. Inoue , K. Ioka , M. Iori , J. Jacquemier , P. Janecek , D. Jankowsky , I. Jung , P. Kaaret , H. Katagiri , S. Kimeswenger , S. Kimura , J. Knödlseder , B. Koch , J. Kocot , K. Kohri , N. Komin , Y. Konno , K. Kosack , S. Koyama , M. Kraus , H. Kubo , G. Kukec Mezek , J. Kushida , N. La Palombara , K. Lalik , G. Lamanna , H. Landt , J. Lapington , P. Laporte , S. Lee , J. Lees , J. Lefaucheur , J. -P. Lenain , G. Leto , E. Lindfors , T. Lohse , S. Lombardi , F. Longo , M. Lopez , F. Lucarelli , P. L. Luque-Escamilla , R. López-Coto , M. C. Maccarone , G. Maier , G. Malaguti , D. Mandat , G. Maneva , S. Mangano , A. Marcowith , J. Martí , M. Martínez , G. Martínez , S. Masuda , G. Maurin , N. Maxted , C. Melioli , T. Mineo , N. Mirabal , T. Mizuno , R. Moderski , M. Mohammed , T. Montaruli , A. Moralejo , K. Mori , G. Morlino , A. Morselli , E. Moulin , R. Mukherjee , C. Mundell , H. Muraishi , K. Murase , S. Nagataki , T. Nagayoshi , T. Naito , D. Nakajima , T. Nakamori , R. Nemmen , J. Niemiec , D. Nieto , M. Nievas-Rosillo , M. Nikołajuk , K. Nishijima , K. Noda , L. Nogues , D. Nosek , B. Novosyadlyj , S. Nozaki , Y. Ohira , M. Ohishi , S. Ohm , A. Okumura , R. A. Ong , R. Orito , A. Orlati , M. Ostrowski , I. Oya , M. Padovani , J. Palacio , M. Palatka , J. M. Paredes , S. Pavy , A. Pe'er , M. Persic , P. Petrucci , O. Petruk , A. Pisarski , M. Pohl , A. Porcelli , E. Prandini , J. Prast , G. Principe , M. Prouza , E. Pueschel , G. Pühlhofer , A. Quirrenbach , M. Rameez , O. Reimer , M. Renaud , M. Ribó , J. Rico , V. Rizi , J. Rodriguez , G. Rodriguez Fernandez , J. J. Rodríguez Vázquez , P. Romano , G. Romeo , J. Rosado , J. Rousselle , G. Rowell , B. Rudak , I. Sadeh , S. Safi-Harb , T. Saito , N. Sakaki , D. Sanchez , P. Sangiorgi , H. Sano , M. Santander , S. Sarkar , M. Sawada , E. J. Schioppa , H. Schoorlemmer , P. Schovanek , F. Schussler , O. Sergijenko , M. Servillat , A. Shalchi , R. C. Shellard , H. Siejkowski , A. Sillanpää , D. Simone , V. Sliusar , H. Sol , S. Stanič , R. Starling , Ł. Stawarz , S. Stefanik , M. Stephan , T. Stolarczyk , M. Szanecki , T. Szepieniec , G. Tagliaferri , H. Tajima , M. Takahashi , J. Takeda , M. Tanaka , S. Tanaka , L. A. Tejedor , I. Telezhinsky , P. Temnikov , Y. Terada , D. Tescaro , M. Teshima , V. Testa , S. Thoudam , F. Tokanai , D. F. Torres , E. Torresi , G. Tosti , C. Townsley , P. Travnicek , C. Trichard , M. Trifoglio , S. Tsujimoto , V. Vagelli , P. Vallania , L. Valore , W. van Driel , C. van Eldik , J. Vandenbroucke , V. Vassiliev , M. Vecchi , S. Vercellone , S. Vergani , C. Vigorito , S. Vorobiov , M. Vrastil , M. L. Vázquez Acosta , S. J. Wagner , R. Wagner , S. P. Wakely , R. Walter , J. E. Ward , J. J. Watson , A. Weinstein , M. White , R. White , A. Wierzcholska , P. Wilcox , D. A. Williams , R. Wischnewski , P. Wojcik , T. Yamamoto , H. Yamamoto , R. Yamazaki , S. Yanagita , L. Yang , T. Yoshida , M. Yoshida , S. Yoshiike , T. Yoshikoshi , M. Zacharias , L. Zampieri , R. Zanin , M. Zavrtanik , D. Zavrtanik , A. Zdziarski , A. Zech , H. Zechlin , V. Zhdanov , A. Ziegler , J. Zorn

SNR G0.9+0.1 is a well known source in the direction of the Galactic Center composed by a Supernova Remnant (SNR) and a Pulsar Wind Nebula (PWN) in the core. We investigate the potential of the future Cherenkov Telescope Array (CTA),…

High Energy Astrophysical Phenomena · Physics 2020-10-07 M. Fiori , L. Zampieri , A. Burtovoi , P. Caraveo , L. Tibaldo
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