AGIS Advanced Gamma-ray Imaging System Jim Buckley (for the AGIS - PowerPoint PPT Presentation

AGIS Advanced Gamma-ray Imaging System Jim Buckley (for the AGIS R&D group) Washington University Toward the Future of Very High Energy Gamma-Ray Astronomy SLAC, November 8, 2007

“Towards the Future” Meetings “Ground-based Gamma-ray Astronomy: Towards the Future”, Oct. 20-21, 2005, Future Gamma-Ray Observatories APS White Paper Meeting Malibu, CA (UCLA) Thurs. 8 Feb 2007 in McGaw Hall 1:30-5:00 Bring a 1-viewgraph idea to share or just come and listen. Everyone is welcome and “Ground-based Gamma-ray Astronomy: encouraged to participate now or in the future. Towards the Future”, May 11-12, 2006, Organizing Committee: Brenda Dingus, Henric Krawczynski, Martin Pohl, Vladimir Vassiliev Additional Members of Editorial Board: Santa Fe, NM (LANL) Francis Halzen, Werner Hofmann, Steve Ritz, Trevor Weekes 8 Feb 2007 AGENDA: 1:30-1:45 Motivation & Organization 1:45-2:10 Extragalactic Working Group Satellite meeting at GLAST Symposium, 2:10-2:35 Gamma Ray Burst Working Group 2:35-3:00 Dark Matter Working Group 3:00-3:15 Break Feb 8, 2007, Palo Alto, CA 3:15-3:40 Galactic Compact Sources Working Group 3:40-4:05 Galactic Diffuse Working Group 4:05-4:30 Technology Working Group 4:30-5:00 General Discussion “Future of Very High Energy Gamma-Ray Astronomy”, May 13-14, 2007, Chicago, IL (U. Chicago) - Formation of AGIS R&D group

U.S. Gamma-ray Community VERITAS GLAST MILAGRO

Status of VHE Astronomy +90.0 1ES1218+304 Mkn421 M87 H1426+428 GRB970417a Mkn180 PG1553+113 Mkn501 1ES1101-232 t i b 1ES1959+650 8 7 5 5 b 1 4 3 a 5 1 7 5 1 3 9 0 R 0 2 3 0 3 0 1 - 5 3 1 1 / 8 a 3 1 - - - ~ + - 6 6 9 1 7 r - 6 1 3 0 7 1 2 r - X 4 2 u 3 5 9 6 1 8 9 8 1 6 8 b 5 - g - + 9 1 3 1 J 1 X 1 5 a 2 y 1 S J J J 1 I J 0 k 1 n S C R R R R R S H o 5 R e X L S S S E S o S S S S C - P P P H P K a P SgrA* M L P l e V b I +180.0 a -180.0 C r C 4 W G K R 4 V e R M C 0 X 3 1ES2344+514 BL-Lac 2 e s . o a 8 9 J C l 7 a n s + 1 W 5 ~ - 7 o A 0 J 1 8 c . 1 r 3 6 e / R . r 7 o X - s 3 J 9 0 4 8 6 5 PKS2005-489 2 . 0 - 4 6 2 2 1ES0229+20 PKS2155-304 1ES0347-121 ~58 credible sources H2356-309 ~11 PWN -90.0 ~16 AGN (15 blazars+M87) ~9 Shell-type SNR 4 X-ray binaries (HMXB, microquasars, Be-binaries) 18 unidentified sources

Science Drivers - White Paper The charge from APS Editorial board Organizational meetings Meeting at the GLAST Symposium The future of ground-based gamma-ray astronomy APS White Paper Science case for the future ground-based The Status and Future of Ground Based Gamma- Ray Astronomy gamma-ray experiment is being In the last two years ground-based gamma-ray developed by the APS whitepaper observatories have made a number of stunning working group (earlier talk by astrophysical discoveries which have attracted the PAGE NAVIGATION attention of the wider scientific community. The The charge from APS Krawczynski) high discovery rate is expected to increase during Editorial board the forthcoming years, as the VERITAS observatory Organizational meetings Meeting at the GLAST and the upgraded MAGIC and HESS observatories Symposium commence scientific observations and the space- WORKING GROUPS based gamma-ray telescope, GLAST, is launched. Extragalactic Astrophysics The continuation of these achievements into the Galactic compact objects next decade will require a new generation of SNR and cosmic rays Dark matter ground-based observatories. In view of the long Gamma-ray bursts lead time for developing and installing new Technology instruments, the Division of Astrophysics of the American Physical Society has requested the preparation of a White Paper on the status and future of ground-based gamma-ray astronomy. Scientists from the entire spectrum of astrophysics are invited to contribute to the concepts and ideas presented in the White Paper. We wish to stress that international participation is encouraged.

Scientific Drivers Wide Field Effective Energy Energy Angular Instantaneous Integrated Slew Speed of View Area Resolution Threshold Resolution Sensitivity Sensitivity PWN ✔ ✔ ✔ ✔ ✔✔ ✔✔ SNR ✔✔ ✔ ✔ ✔✔ ✔✔ Pulsars ✔ ✔ ✔✔ ✔✔ XRBs ✔ ✔ ✔ ✔ ✔✔ ✔✔ UIDs ✔✔ ✔ ✔ ✔ ✔✔ ✔ ✔✔ AGN ✔✔ ✔ ✔ ✔ ✔✔ GRBs ✔✔ ✔✔ ✔ ✔✔ ✔✔ ✔✔ Dark Matter ✔✔ ✔ ✔✔ ✔✔ ✔ ✔✔ Galactic Diffuse ✔✔ ✔ ✔ ✔✔ Galaxy Clusters ✔ ✔ ✔ ✔ ✔✔ Galaxies ✔ ✔ ✔✔ ✔✔ ☺☺ ☺ ☺ ☺☺ ☺ ☺☺ ☺ IACTs n/a ☺☺ ☺ ☺☺ EAS Detectors n/a ☺☺ ☺☺ ☺☺ ☺ ☺☺ Space Telescopes (JB version of the “Krennrich Science Matrix”)

Time-resolved Spectra Box shock acceleration with losses from escape, IC and synchrotron cooling, E. Schlafly (Stanford) and JB (left: electron spectrum, right: radiation spectrum) Instantaneous point source sensitivity and energy resolution is of critical importance for studying AGN and GRB emission. Imaging atmospheric Cherenkov instruments are unmatched for such studies.

AGIS Design Goal 9 1 0 C r a b G L A S T ( 5 y r ) V E R I T A S ( 5 0 h r ) W h i p p l e ( 5 0 h r ) 10 2 ° 1 0 F u t u r e 1 k m , 0 . 1 ] 1 s 2 m c 11 g 1 0 r e [ E d / F d 2 E 12 1 0 y t i v i t i s n e S 13 1 0 14 1 0 4 5 1 0 1 2 3 1 0 1 0 1 0 1 0 1 0 1 0 1 0 E n e r g y [ G e V ] Differential flux sensitivity of an ideal km 2 telescope array sensitivity curve (courtesy S. Fegan)

Note on Differential Sensitivity log file; S=inf; e +- particle output; S=10 4 m; e +- Energy, E (GeV) 10 4 10 3 10 2 10 -1 10 2 10 3 10 4 1 10 Number of particles (from Bernloehr, S. Funk Thesis) Toy model calculation of number of particles reaching ground level as an energy estimator for showers at zenith, impact in center of EAS detector (courtesy Slava Bugaev). Difficult to compare EAS detectors for differential flux sensitivity since first spectral measurement is typically well above the quoted threshold

Future of Ground-based Gamma-Ray Astronomy GLAST is coming! Even though GLAST will enjoy operation in vacuum, the ground-based community can not make judgements about the future of ground-based gamma-ray astronomy in a vacuum! Sensitivity estimate for future ACT and future space-based instrument using the largest launch vehicle fairing - cross-over moves down from 100 GeV to 30 GeV

Angular Resolution (VERITAS angular resolution from Krawczynski et al. (2005), future ground-array from Bugaev et al. (2007), Ideal ground-array from W. Hofmann (2005?), Kinetic limit from S. Hunter.

AGIS Specifications Instrument budget Instrument budget $100M $100M Small/dense/high-res Target energy threshold Target energy threshold <40 GeV <40 GeV Effective area Effective area 0.7-3 km 2 0.7-3 km 2 Large/sparse/low-res Number of telescopes Number of telescopes 25-100 25-100 40m 2 (7m) 40m 2 (7m) Effective mirror area (diameter) Effective mirror area (diameter) Both approaches -250m 2 (18m) -250m 2 (18m) 80-160m 80-160m Telescope spacing unform (graded) array Telescope spacing unform (graded) array Technological challenges (20m-200m) (20m-200m) come with pushing the Sensitivity at 200 GeV Sensitivity at 200 GeV 10 -13 erg cm 2 s -1 10 -13 erg cm 2 s -1 angular resolution and field of view, requiring a new optical Telescope FOV diameter Telescope FOV diameter 6, 8° 6, 8° design and very low cost Number of pixels per camera Number of pixels per camera 5,000-10,000 5,000-10,000 photodetectors and electronics Pixel diameter Pixel diameter 0.15°-0.05° 0.15°-0.05° The AGIS R&D proposal will Camera+electronics cost per channel Camera+electronics cost per channel $50-$400 $50-$400 address the most challenging Mechanical+optics cost per telescope Mechanical+optics cost per telescope $0.5M-$2.0M $0.5M-$2.0M corners of this specification phase space.

AGIS R&D Proposal NSF Proposal: (Swordy, PI) $1M/yr, 3 years; DOE Proposal: (Byrum, PI) $1M/yr, 3 yrs Adler Planetarium Lucy Fortson, Daniel Steele Argonne National Lab K.Byrum, G. Drake, V. Guarino, D. Horan, R. Wagner Barnard/Columbia Reshmi Mukherjee U.C. Santa Cruz David Williams, Michael Schneider University of Chicago Simon Swordy, Scott Wakely University of Delaware Jamie Holder Harvard-Smithsonian CfA Trevor Weekes University of Iowa Phil Kaaret Iowa State University Frank Krennrich McGill University David Hanna Penn State Abe Falcone Stanford U./SLAC Stefan Funk, Roger Romani, Hiro Tajima UCLA Stephen Fegan, Rene Ong, Vladimir Vassiliev U. Utah Stephan LeBohec, David Kieda Washington University J. Buckley, Y. Bugaev, P. Dowkontt, H. Krawczynski International advisors/participants: German Herman, Razmik Mirzoyan