The$ASTRI/CTAmini.array$of$Small$Size$Telescopes ...Proceeding2013.![5] New$surprises Limiting flux...
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Limiting flux a factor 2 better than H.E.S.S. above a few TeV for an array composed by 7 telescopes Angular resolution a few (4-5) arcmin Energy resolution of the order of 10-15 % The ASTRI/CTA miniarray of Small Size Telescopes as a precursor of the Cherenkov Telescope Array G. Pareschi 1 , G. Agne1a 2 , E. Antolini 3 , L.A. Antonelli 4 , D. Bas<eri 5 , G. Bellassai 6 , C. Bigongiari 7 , S. Billo1a 6 , B. Biondo 2 , M. Boe1cher 8 , G. Bonanno 6 , G. Bonnoli 1 , P. Bruno 6 , A. Bulgarelli 9 , R. Canestrari 1 , M. Capalbi 2 , G. Capobianco 7 , P. Caraveo 10 , A. Carosi 4 , E. Cascone 11 , O. Catalano 2 , P. Conconi 1 , V. Confor< 9 , G. Cusumano 2 , V. De Caprio 11 , A. De Luca 10 , E. M. de Gouveia Dal Pino 12 , A. Di Paola 4 , F. Di Pierro 7 , D. Fan<nel 13 , M. Fiorini 10 , D. Fugazza 1 , D. Gardiol 7 , C. Gargano 2 , S. Garozzo 6 , F. GianoR 9 , S. Giarrusso 2 , E. Giro 13 , A. Grillo 6 , D. Impiombato 2 , S. Incorvaia 10 , A. La Barbera 2 , N. La Palombara 10 , V. La Parola 2 , G. La Rosa 2 , L. Lessio 13 , G. Leto 6 , S. Lombardi 4 , F. Lucarelli 4 , M.C. Maccarone 2 , G. Malaspina 1 , D. Marano 6 , E. Mar<neR 6 , C. Melioli 12 , R. Millul 1 , T. Mineo 2 , G. Morlino 4 , R. Nemmen 15 , L. Perri 1 , G. Rodeghiero 5 , P. Romano 2 , G. Romeo 6 , F. Russo 2 , B. Sacco 2 , J. Schwarz 1 , A. Segreto 2 , D. Selvestrel 13 , G. Sironi 1 , G. SoRle 2 , A. Stamerra 7 , E. Strazzeri 2 , L. StringheR 10 , G. Tagliaferri 1 , C. Tanci 3 , V. Testa 4 , M.C. Timpanaro 6 , G. Toso 10 , G. Tos< 3 , M. Trifoglio 9 , P. Vallania 7 , S. Vercellone 2 , A. Volpicelli 7 , V. Zitelli 14 for the CTA Consor<um and the ASTRI collabora<on (1) INAF – Osservatorio Astronomico di Brera, Milano/Merate, Italy – (2) INAF Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Italy – (3) Università di Perugia, Italy (4) INAF – Osservatorio Astronomico di Roma Italy – (5) Università di Padova, Dip. Fisica e Astronomia, Italy (6) INAF – Osservatorio Astrofisico di Catania, Italy – (7) INAF – Osservatorio Astrofisico di Torino, Italy – (8) Centre for Space Research, NorthWest University, Potchefstroom, 2520 , South Africa – (9) INAF Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Bologna, 40129 Bologna, Italy – (10) INAF Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Milano, Italy – (11) INAF Osservatorio Astrofisico di Capodimonte, Napoli, Italy – (12) Ins<tuto Astronomico e Geofisico (IAGUSP), Universidade de Sao Paulo, Brazil (14) INAF – Osservatorio Astronomico di Bologna, Italy For the ASTRI collabora?on and CTA consor?um h1ps://www.ctaobservatory.org/ h1p://www.brera.inaf.it/astri/ Abstract ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Educa<on, University and Research. Within this framework, INAF is currently developing a widefieldofview (9.6 degrees in diameter) endtoend prototype of the smallsize telescope (SST) of the Cherenkov Telescope Array, CTA, sensi<ve in the energy band from a few TeV up to hundreds TeV. The ASTRI telescope is based on a dualmirror SchwarzschildCouder (ASTRI SST2M) op<cal design, with a compact (F# = 0.5) op<cal configura<on named ASTRI SST2M telescope. This allows us to adopt an innova<ve modular focal plane camera based on silicon photomul<pliers, with a logical pixel size of 6.2mm x 6.2mm. Moreover, planned, and already being developed, an SST miniarray based on 7 iden<cal telescopes represents an evolu<on of the ASTRI SST2M telescope. The University of Sao Paulo (Brazil) and NorthWest University (South Africa) have jointed INAF to collaborate to the miniarray implementa<on. The ASTRI/CTA miniarray will be part of the main CTA Observatory, represen<ng a precursor around which the final array of CTA will grow up at the southern site. ASTRI/CTA miniarray, in addi<on to a technical assessment study (in the perspec<ve of the full CTA implementa<on) it will be possible to perform an early scien<fic program. In par<cular we wish to start inves<ga<ng the poorly known energy range beyond a few and 100 TeV, thus exploring e.g. the cutoff regime of cosmic accelerators. Energy threshold: • ~ 1 TeV Telescope properties: • Optical design = Schwarzschild-Couder • Primary mirror, M1 = 4.3m Ø • M1 type = Segmented (18 elements in 3 concentric rings) • Secondary mirror, M2 = 1.8m Ø (2.2m Radius of Curvature) • M2 type = Monolithic • M1-M2 distance = 3m • Effective area = 6.5m 2 • F/D 1 = 0.5, F = 2.15m Camera properties: • Sensors type = SiPMs • Number of logical pixels = 1984 • Pixel size = 0.17° (plate scale = 37.5mm/°) • Field of View = 9.6° The deployment and opera<on of the ASTRI SST–2M miniarray to be installed at the CTA southern site will verify the following array proper<es: the array performance (reliability and cost) at the chosen site; the trigger algorithms; the wide field of view performance to detect very high energy showers with the core located at a distance up to 250 m; the HW/SW configura<ons for the array; the datahandling chain. … and in par<cular… through deep observa<ons of a few selected targets, it will allow us to compare the actual performance with the Monte Carlo expecta<ons, and to perform the first CTA science, by means of a few solid detec@ons during the first year … assuming the following performance [4]… a limi@ng flux a factor 2 be1er than H.E.S.S. above a few TeV for an array composed of 7 telescopes an angular resolu@on of 0.08 o at 10 TeV an energy resolu@on of the order of 15% at 10 teV The ASTRI miniarray opera?ons in the context of CTA The ASTRI Project [1,2] is being developed following two major steps: the first step consists of the design, deployment and opera<on in Italy of an endtoend prototype of a CTA [3] smallsize telescope (in a dualmirror op<cal configura<on (SST2M) and equipped with a modular SiPMbased camera) inaugura?on 24 September 2014; the second step consists of the deployment and the opera<on of a miniarray composed of a few SST–2M telescopes at the final CTA southern site in 2016, which could cons<tute the first seed of the future CTA Project. The ASTRI/CTA miniarray concept INAF Observing Sta<on at Serra La Nave (Mt. Etna, Sicily, 1735 m a.s.l.) Fullyfunc<onal facility Site of the ASTRI SST2MPrototype CTA Southern Site Site of the ASTRI SST2MMiniarray ASTRI/CTA miniarray preliminary scien?fic cases The CTA Southern site will provide an excellent view of most of the Galac<c plane and of the Galac<c Bulge. Several Galac<c sources have been detected so far [5,6] above a few tens of TeV, including shelltype supernova remnants (SNR), pulsar wind nebulae (PWN, such as the Crab Nebula), binary systems, the Galac<c Center, as well as a number of uniden<fied sources apparently emiRng only above 100 GeV with no lowerenergy counterparts. Supernovae Remnants . RX J1713.73946 is a young shelllike SNR which could be considered as an excellent laboratory to inves<gate the cosmic ray accelera<on. The recent detec<on of this SNR by Fermi [7] and the combined study with H.E.S.S., show that the highenergy and very highenergy (VHE) emission could be interpreted in the framework of a leptonic scenario. The ASTRI SST–2M miniarray improved sensi<vity in the 10100 TeV energy range will allow us to inves<gate the possible cutoff at VHE predicted by the leptonic scenario and/or the spectral tail typical of hadronic models. Moreover, by combining the improved sensi<vity with the op<mal angular resolu<on, the ASTRI SST–2M miniarray might allow us to inves<gate the VHE emission in the different regions of this source, studying their spectra. New surprises . The large op<cal field of view of the ASTRI miniarray will allow us to monitor, during a single poin<ng, a few TeV sources simultaneously. Although the actual sensi<vity will substan<ally drop for offaxis sources within the op<cal FoV, a few targets can be monitored simultaneously. Detec<on of hard and intense Galac<c sources could be feasible, e.g. in the case of Vela–X and Vela–Jr. Moreover, it would be the chance to detect intense (a few Crab units) flares from hardspectra serendipitous sources. The quest for Pevatrons . Tycho's SNR is the best candidate as Pevatron [8], but it will not be accessible from the CTA southern site. Interes<ngly, Kepler's SNR, which will be accessible to CTA, is very similar to Tycho’s in many respects. The H.E.S.S. telescope observed Kepler's SNR for 13 hrs and provided upper limits on the energy flux in the range 230 GeV – 12.8 TeV of 8.6x10 13 erg cm 2 s 1 [9]. Indeed, theore<cal models [10,11] predict that the high energy emission from Kepler's SNR should be only a factor 25 below the H.E.S.S. upper limits. Hence, the ASTRI SST–2M miniarray could be able to detect this young SNR by means of a deep observa<on. Blazars . 1ES 0229+200 is an extreme BL Lac object [12,13]. The emission spectrum measured as a result of the injec<on of VHE/UHE photons at the source is strongly suppressed above ~10 TeV for a wide range of EBL models, whereas a cosmicrayinduced cascade displays a significantly harder spectrum above this energy. As discussed in [13] a clear detec<on of VHE emission above a few tens of TeV from such a blazar could provide a striking evidence for nonstandard phenomena, either an anomalous transparency of the Universe at these energies [14,15] or gammaray emission resul<ng from an electromagne<c cascade ini<ated by ultrarela<vis<c protons accelerated in the blazar jet and beamed toward the observer. A list of promising EHBLs is currently under study [16] and will provide a fundamental target list for the future ASTRI SST–2M mini array. The la1er would also demonstrate the possibility that rela<vis<c jets are the accelerators of the s<ll enigma<c UHECR. End-to-end prototype The telescope endtoend concept References : [1]Pareschi et al., ICRC Proc. 2013 [2]Vercellone et al., 2012, AIPC, 1505, 749. [3]Ac<s et al., 2011, Exp. Astr., 32, 193. [4]Di Pierro et al.,ICRC Proceeding 2013. [5]Aharonian, et al., 2005, Science, 307, 1938. [6]Hinton & Hofmann, 2009, ARA&A, 47, 523 [7]Abdo et al., 2011, ApJ, 734, 28. [8]Morlino & Caprioli, 2012, A&A, 538, A81. [9]Aharonian et al., 2008, A&A, 488, 219. [10] Berezhko et al., 2006, A&A, 452, 217. [11]Morlino & Caprioli, 2012, AIPC, 1505, 241. [12]Tavecchio et al., 2011, MNRAS, 414, 3566. [13]Murase et al., 2012, ApJ, 749, 63. [14]Horns & Meyer, 2012, JCAP, 02, 33. [15]De Angelis et al., 2013, MNRAS ,432, Issue 4, p.3245. [16]Tavecchio et al., 2013, Physical Review D, vol. 86, Issue 8, id. 085036. Acknlowedgements CTA: We gratefully acknowledge suppport from the agencies and organiza<ons listed under Funding Agencies at this website: ASTRI is a Flagship Project financed by the Italian Ministry of Educa<on, University, and Research (MIUR). ASTRI/CTA miniarray flux sensi<vity Mirrors Secondary (monolith) Primary (18 segments) h1p://www.ctaobservatory.org
Transcript of The$ASTRI/CTAmini.array$of$Small$Size$Telescopes ...Proceeding2013.![5] New$surprises Limiting flux...
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Limiting flux
§ a factor 2 better than H.E.S.S. above a few TeV for an array composed by 7 telescopes
Angular resolution
§ a few (4-5) arcmin Energy resolution
§ of the order of 10-15 %
The ASTRI/CTA mini-‐array of Small Size Telescopes as a precursor of the Cherenkov Telescope Array
G. Pareschi1, G. Agne1a 2, E. Antolini3, L.A. Antonelli4, D. Bas<eri5, G. Bellassai6, C. Bigongiari7, S. Billo1a6, B. Biondo2, M. Boe1cher8, G. Bonanno6, G. Bonnoli1, P. Bruno6, A. Bulgarelli9, R. Canestrari1, M. Capalbi2, G. Capobianco7, P. Caraveo10, A. Carosi4, E. Cascone11, O. Catalano2, P. Conconi1, V. Confor<9, G. Cusumano2, V. De Caprio11, A. De Luca10, E. M. de Gouveia Dal Pino12, A. Di Paola4, F. Di Pierro7, D. Fan<nel13, M. Fiorini10, D. Fugazza1, D. Gardiol7, C. Gargano2, S. Garozzo6, F. GianoR9, S. Giarrusso2, E. Giro13, A. Grillo6, D. Impiombato2, S. Incorvaia10, A. La Barbera2, N. La Palombara10, V. La Parola2, G. La Rosa2, L. Lessio13, G. Leto6, S. Lombardi4, F. Lucarelli4, M.C. Maccarone2, G. Malaspina1, D. Marano6, E. Mar<neR6, C. Melioli12, R. Millul1, T. Mineo 2, G. Morlino 4, R. Nemmen15, L. Perri1, G. Rodeghiero5, P. Romano2, G. Romeo6, F. Russo2, B. Sacco2, J. Schwarz1, A. Segreto2, D. Selvestrel13, G. Sironi1, G. SoRle2, A. Stamerra7 , E. Strazzeri2, L. StringheR10, G. Tagliaferri1, C. Tanci3, V. Testa4, M.C. Timpanaro6, G. Toso10, G. Tos<3, M. Trifoglio9, P. Vallania7, S. Vercellone2, A. Volpicelli7, V. Zitelli14 for the CTA Consor<um and the ASTRI collabora<on (1) INAF – Osservatorio Astronomico di Brera, Milano/Merate, Italy – (2) INAF -‐ Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Italy – (3) Università di Perugia, Italy -‐ (4) INAF – Osservatorio Astronomico di Roma Italy – (5) Università di Padova, Dip. Fisica e Astronomia, Italy -‐ (6) INAF – Osservatorio Astrofisico di Catania, Italy – (7) INAF – Osservatorio Astrofisico di Torino, Italy – (8) Centre for Space Research, North-‐West University, Potchefstroom, 2520 , South Africa – (9) INAF -‐ Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Bologna, 40129 Bologna, Italy – (10) INAF -‐ Is<tuto di Astrofisica Spaziale e Fisica Cosmica di Milano, Italy – (11) INAF Osservatorio Astrofisico di Capodimonte, Napoli, Italy – (12) Ins<tuto Astronomico e Geofisico (IAG-‐USP), Universidade de Sao Paulo, Brazil -‐ (14) INAF – Osservatorio Astronomico di Bologna, Italy -‐ For the ASTRI collabora?on and CTA consor?um h1ps://www.cta-‐observatory.org/ h1p://www.brera.inaf.it/astri/
Abstract ASTRI ("Astrofisica con Specchi a Tecnologia Replicante Italiana") is a flagship project of the Italian Ministry of Educa<on, University and Research. Within this framework, INAF is currently developing a wide-‐field-‐of-‐view (9.6 degrees in diameter) end-‐to-‐end prototype of the small-‐size telescope (SST) of the Cherenkov Telescope Array, CTA, sensi<ve in the energy band from a few TeV up to hundreds TeV. The ASTRI telescope is based on a dual-‐mirror Schwarzschild-‐Couder (ASTRI SST-‐2M) op<cal design, with a compact (F# = 0.5) op<cal configura<on named ASTRI SST-‐2M telescope. This allows us to adopt an innova<ve modular focal plane camera based on silicon photo-‐mul<pliers, with a logical pixel size of 6.2mm x 6.2mm. Moreover, planned, and already being developed, an SST mini-‐array based on 7 iden<cal telescopes represents an evolu<on of the ASTRI SST-‐2M telescope. The University of Sao Paulo (Brazil) and North-‐West University (South Africa) have jointed INAF to collaborate to the mini-‐array implementa<on. The ASTRI/CTA mini-‐array will be part of the main CTA Observatory, represen<ng a precursor around which the final array of CTA will grow up at the southern site. ASTRI/CTA mini-‐array, in addi<on to a technical assessment study (in the perspec<ve of the full CTA implementa<on) it will be possible to perform an early scien<fic program. In par<cular we wish to start inves<ga<ng the poorly known energy range beyond a few and 100 TeV, thus exploring e.g. the cut-‐off regime of cosmic accelerators.
Energy threshold: • ~ 1 TeV
Telescope properties: • Optical design = Schwarzschild-Couder • Primary mirror, M1 = 4.3m Ø • M1 type = Segmented (18 elements in 3 concentric rings) • Secondary mirror, M2 = 1.8m Ø (2.2m Radius of Curvature) • M2 type = Monolithic • M1-M2 distance = 3m • Effective area = 6.5m2 • F/D1 = 0.5, F = 2.15m
Camera properties: • Sensors type = SiPMs • Number of logical pixels = 1984 • Pixel size = 0.17° (plate scale = 37.5mm/°) • Field of View = 9.6°
The deployment and opera<on of the ASTRI SST–2M mini-‐array to be installed at the CTA southern site will verify the following array proper<es: ü the array performance (reliability and cost) at the chosen site; ü the trigger algorithms; ü the wide field of view performance to detect very high energy showers with the
core located at a distance up to 250 m; ü the HW/SW configura<ons for the array; ü the data-‐handling chain.
… and in par<cular…
through deep observa<ons of a few selected targets, it will allow us to compare the actual performance with the Monte Carlo expecta<ons, and to perform the first CTA science, by means of a few solid detec@ons during the first year
… assuming the following performance [4]…
ü a limi@ng flux a factor 2 be1er than H.E.S.S. above a few TeV for an array composed of 7 telescopes
ü an angular resolu@on of 0.08o at 10 TeV
ü an energy resolu@on of the order of 15% at 10 teV
The ASTRI mini-‐array opera?ons in the context of CTA
The ASTRI Project [1,2] is being developed following two major steps: ü the first step consists of the design, deployment and opera<on in Italy of an end-‐to-‐end prototype
of a CTA [3] small-‐size telescope (in a dual-‐mirror op<cal configura<on (SST-‐2M) and equipped with a modular SiPM-‐based camera) è inaugura?on 24 September 2014;
ü the second step consists of the deployment and the opera<on of a mini-‐array composed of a few
SST–2M telescopes at the final CTA southern site in 2016, which could cons<tute the first seed of the future CTA Project.
The ASTRI/CTA mini-‐array concept INAF Observing Sta<on at Serra La Nave (Mt. Etna, Sicily, 1735 m a.s.l.) Fully-‐func<onal facility Site of the ASTRI SST-‐2M Prototype
CTA Southern Site Site of the ASTRI SST-‐2M Mini-‐array
ASTRI/CTA mini-‐array preliminary scien?fic cases The CTA Southern site will provide an excellent view of most of the Galac<c plane and of the Galac<c Bulge. Several Galac<c sources have been detected so far [5,6] above a few tens of TeV, including shell-‐type supernova remnants (SNR), pulsar wind nebulae (PWN, such as the Crab Nebula), binary systems, the Galac<c Center, as well as a number of uniden<fied sources apparently emiRng only above 100 GeV with no lower-‐energy counterparts.
Supernovae Remnants. RX J1713.7-‐3946 is a young shell-‐like SNR which could be considered as an excellent laboratory to inves<gate the cosmic ray accelera<on. The recent detec<on of this SNR by Fermi [7] and the combined study with H.E.S.S., show that the high-‐energy and very high-‐energy (VHE) emission could be interpreted in the framework of a leptonic scenario. The ASTRI SST–2M mini-‐array improved sensi<vity in the 10-‐100 TeV energy range will allow us to inves<gate the possible cut-‐off at VHE predicted by the leptonic scenario and/or the spectral tail typical of hadronic models. Moreover, by combining the improved sensi<vity with the op<mal angular resolu<on, the ASTRI SST–2M mini-‐array might allow us to inves<gate the VHE emission in the different regions of this source, studying their spectra.
New surprises. The large op<cal field of view of the ASTRI mini-‐array will allow us to monitor, during a single poin<ng, a few TeV sources simultaneously. Although the actual sensi<vity will substan<ally drop for off-‐axis sources within the op<cal FoV, a few targets can be monitored simultaneously. Detec<on of hard and intense Galac<c sources could be feasible, e.g. in the case of Vela–X and Vela–Jr. Moreover, it would be the chance to detect intense (a few Crab units) flares from hard-‐spectra serendipitous sources.
The quest for Pevatrons. Tycho's SNR is the best candidate as Pevatron [8], but it will not be accessible from the CTA southern site. Interes<ngly, Kepler's SNR, which will be accessible to CTA, is very similar to Tycho’s in many respects. The H.E.S.S. telescope observed Kepler's SNR for 13 hrs and provided upper limits on the energy flux in the range 230 GeV – 12.8 TeV of 8.6x10-‐13 erg cm-‐2 s-‐1 [9]. Indeed, theore<cal models [10,11] predict that the high energy emission from Kepler's SNR should be only a factor 2-‐5 below the H.E.S.S. upper limits. Hence, the ASTRI SST–2M mini-‐array could be able to detect this young SNR by means of a deep observa<on.
Blazars. 1ES 0229+200 is an extreme BL Lac object [12,13]. The emission spectrum measured as a result of the injec<on of VHE/UHE photons at the source is strongly suppressed above ~10 TeV for a wide range of EBL models, whereas a cosmic-‐ray-‐induced cascade displays a significantly harder spectrum above this energy. As discussed in [13] a clear detec<on of VHE emission above a few tens of TeV from such a blazar could provide a striking evidence for non-‐standard phenomena, either an anomalous transparency of the Universe at these energies [14,15] or gamma-‐ray emission resul<ng from an electromagne<c cascade ini<ated by ultra-‐rela<vis<c protons accelerated in the blazar jet and beamed toward the observer.
A list of promising E-‐HBLs is currently under study [16] and will provide a fundamental target list for the future ASTRI SST–2M mini-‐array. The la1er would also demonstrate the possibility that rela<vis<c jets are the accelerators of the s<ll enigma<c UHECR.
End-to-end
prototype
The telescope end-‐to-‐end concept
References: [1]-‐Pareschi et al., ICRC Proc. 2013 [2]-‐Vercellone et al., 2012, AIPC, 1505, 749. [3]-‐Ac<s et al., 2011, Exp. Astr., 32, 193. [4]-‐Di Pierro et al.,ICRC Proceeding 2013. [5]-‐Aharonian, et al., 2005, Science, 307, 1938. [6]-‐Hinton & Hofmann, 2009, ARA&A, 47, 523 [7]-‐Abdo et al., 2011, ApJ, 734, 28. [8]-‐Morlino & Caprioli, 2012, A&A, 538, A81. [9]-‐Aharonian et al., 2008, A&A, 488, 219. [10]-‐Berezhko et al., 2006, A&A, 452, 217. [11]-‐Morlino & Caprioli, 2012, AIPC, 1505, 241. [12]-‐Tavecchio et al., 2011, MNRAS, 414, 3566. [13]-‐Murase et al., 2012, ApJ, 749, 63. [14]-‐Horns & Meyer, 2012, JCAP, 02, 33. [15]-‐De Angelis et al., 2013, MNRAS ,432, Issue 4, p.3245. [16]-‐Tavecchio et al., 2013, Physical Review D, vol. 86, Issue 8, id. 085036.
Acknlowedgements CTA: We gratefully acknowledge suppport from the agencies and organiza<ons listed under Funding Agencies at this website: ASTRI is a Flagship Project financed by the Italian Ministry of Educa<on, University, and Research (MIUR).
ASTRI/CTA mini-‐array flux sensi<vity
Mirrors
Secondary (monolith) Primary (18 segments)
h1p://www.cta-‐observatory.org
