GLAST LAT Project DOE Mini-review 12 October 2004

GLAST LAT Project DOE Mini-review 12 October 2004 Introduction Technical and Production Status L. Klaisner Instrument Science Operations Center Plans Gamma-ray Large Area Space Telescope S. Ritz R. Cameron Project Status, Cost and Schedule Klaisner S. Ritz L. 1

GLAST LAT Project DOE Mini-review 12 October 2004 Why study ’s? Gamma rays carry a wealth of information: – rays do not interact much at their source: they offer a direct view into Nature’s largest accelerators. – similarly, the Universe is mainly transparent to rays: can probe cosmological volumes. Any opacity is energy-dependent. – conversely, rays readily interact in detectors, with a clear signature. Large Area – rays are neutral: no complications Telescope (LAT) due to magnetic fields. Point directly back to sources, etc. Two GLAST instruments: LAT: 20 Me. V – >300 Ge. V GBM: 10 ke. V – 25 Me. V Launch: February 2007 S. Ritz GLAST Burst Monitor (GBM) 2

GLAST LAT Project DOE Mini-review 12 October 2004 GLAST Science GLAST will have a very broad menu that includes: • • Systems with supermassive black holes Gamma-ray bursts (GRBs) Pulsars Solar physics Origin of Cosmic Rays Probing the era of galaxy formation Discovery! Particle Dark Matter? Other relics from the Big Bang? Testing Lorentz invariance. New source classes. Huge increment in capabilities. GLAST draws the interest of both the High Energy Particle Physics and High Energy Astrophysics communities. GLAST is the highest-ranked initiative in its category in the National Academy of Sciences 2000 Decadal Survey Report. S. Ritz 3

GLAST LAT Project DOE Mini-review 12 October 2004 GLAST LAT High Energy Capabilities EGRET on GRO firmly established the field of high-energy gamma-ray astrophysics and demonstrated the importance and potential of this energy band. GLAST is the next great step beyond EGRET, providing a huge leap in capabilities: • Very large FOV (~20% of sky), factor 4 greater than EGRET • Broadband (4 decades in energy, including unexplored region E > 10 Ge. V) • Unprecedented PSF for gamma rays (factor > 3 better than EGRET for E>1 Ge. V) • Large effective area (factor > 5 better than EGRET) • Results in factor > 30 -100 improvement in sensitivity • Much smaller deadtime per event (25 microsec, factor >4, 000 better than EGRET) S. Ritz • No expendables long mission without degradation 4

GLAST LAT Project Sources DOE Mini-review 12 October 2004 EGRET 3 rd Catalog: 271 sources S. Ritz 5

GLAST LAT Project Sources DOE Mini-review 12 October 2004 LAT 1 st Catalog: >9000 sources possible S. Ritz 6

GLAST LAT Project DOE Mini-review 12 October 2004 Anticenter Region simulation: S. Digel S. Ritz 7

GLAST LAT Project Overview of LAT • Precision Si-strip Tracker (TKR) 18 XY tracking planes. Single-sided silicon strip detectors (228 mm pitch) Measure the photon direction; gamma ID. • Hodoscopic Cs. I Calorimeter(CAL) Array of 1536 Cs. I(Tl) crystals in 8 layers. Measure the photon energy; image the shower. • Segmented Anticoincidence Detector (ACD) 89 plastic scintillator tiles. Reject background of charged cosmic rays; segmentation removes self-veto effects at high energy. ACD e+ • Electronics System Includes flexible, robust hardware trigger and software [surrounds filters. 4 x 4 array of TKR towers] DOE Mini-review 12 October 2004 Tracker e– Calorimeter Systems work together to identify and measure the flux of cosmic gamma rays with energy 20 Me. V - >300 Ge. V. S. Ritz 8

GLAST LAT Project DOE Mini-review 12 October 2004 GLAST LAT Collaboration United States • • California State University at Sonoma University of California at Santa Cruz - Santa Cruz Institute of Particle Physics Goddard Space Flight Center – Laboratory for High Energy Astrophysics Naval Research Laboratory Ohio State University Stanford University (SLAC and HEPL/Physics) University of Washington University, St. Louis France PI: Peter Michelson (Stanford & SLAC) • ~120 Members (including ~60 Affiliated Scientists, plus 20 Postdocs, and 25 Graduate Students) IN 2 P 3, CEA/Saclay Italy • INFN, ASI • Stockholm University LAT Project is a partnership between Japanese GLAST Collaboration NASA and DOE, with international • Hiroshima University contributions from France, Italy, Japan and Sweden. • ISAS, RIKEN Managed at Stanford Linear Accelerator Swedish GLAST Collaboration • Royal Institute of Technology (KTH) Center (SLAC). S. Ritz 9

GLAST LAT Project DOE Mini-review 12 October 2004 Highlights of Recent Activities • • S. Ritz Successful Mission CDR! Collaboration meeting at SLAC 27 -30 September – Instrument test data analysis workshop – Hardware and software status – Science organization and planning – Operations planning – Cooperation with other experiments (multi-wavelength planning) – Ge. V-Te. V Symposium (joint with Mission Science Working Group) Senior Scientist Advisory Committee – year 1 data release plan proposal – new members – performance updating – science planning policies Data Challenges – very successful DC 1; planning/working now for DC 2 10

GLAST LAT Project DOE Mini-review 12 October 2004 Instrument Test Data Analysis • A suite of detailed test data-taking runs is being defined for each stage of the build. Using the data, there are two basic categories of data analysis: – (mostly) automated, basic go/no-go tests. These are done by I&T, with ~instant result turn-around to support the schedule. – this work: more detailed analyses using (mostly) the same data. A key opportunity to look for more subtle, sophisticated, and detailed effects: » To uncover and quantify any instrumental effects early that could have an impact on science data analysis & feedback realism into the Monte Carlo » Are there additions to the go/no-go test suite? » To apply reconstruction algorithms to real data » To start the work that will evolve in the Instrument Science Operations Center (ISOC) » To grow a group to participate in the beam tests analysis effort (after instrument delivery) – Relies on strong collaboration-wide support. First workshop in June, second in September. Regular meetings via vrvs. S. Ritz 11

GLAST LAT Project DOE Mini-review 12 October 2004 Operations Phase LAT Organization Chart § Dr. Rob Cameron appointed LAT Instrument Science Operations Center manager – extensive operations experience at SAO / Chandra X-ray Center § LAT Collaboration Science Groups (LSGs) responsible for collaboration’s analysis and extraction of science results from LAT data – 11 Science Groups plus Multi-l Coordination Working Group – each science group to have 2 coleads; with one resident at Stanford – day-to-day efforts coordinated by Analysis Coordinator, also resident at Stanford-SLAC S. Ritz 12

GLAST LAT Project DOE Mini-review 12 October 2004 Science Analysis Groups § process started for updating the groups § groups organized around expected collaboration publications, particularly during the 1 st year all-sky survey phase; each group should have responsibility for 2 -3 key (category 1) papers. Science Analysis Groups 1. 2. 3. 4. 5. 6. 7. 8. 9. 10. 11. Catalogs Galactic Diffuse and Molecular Clouds Extragalactic Diffuse Blazars and Other AGNs Other Galaxies (including clusters) Pulsars, SNRs, and Plerions Unidentified Sources and Population Studies Dark Matter and Exotic Physics Gamma-Ray Bursts Solar System Sources Calibration and Analysis Methods LAT Multiwavelength Observation Coordination Group S. Ritz 13

GLAST LAT Project DOE Mini-review 12 October 2004 Space at SU – SLAC for ISOC and Analysis efforts Fred Kavli Building at SLAC – KIPAC (Kavli Institute of Particle Astrophysics and Cosmology) Roger Blandford, Director Steve Kahn, Deputy Director S. Ritz 14

GLAST LAT Project DOE Mini-review 12 October 2004 Space at SU – SLAC for ISOC and Analysis efforts new building on campus - replacement space for HEPL - campus part of KIPAC S. Ritz 15

GLAST LAT Project DOE Mini-review 12 October 2004 Ge. V-Te. V Symposium 30 September at SLAC LAT Team and Mission Science Working Group have held ~annual joint science symposia on a wide variety of topics. This year: Ge. V-Te. V Astrophysics in the GLAST Era + Very useful workshop discussion about cooperation among experiments! S. Ritz 16

GLAST LAT Project Data Challenges DOE Mini-review 12 October 2004 • DC 1 early alpha-testing. “End-to-end” testing of analysis software. • Provide feedback on what works and what is missing from the data formats and tools. • Walk before running: design a progression of studies. – DC 1. Modest goals. Contains most essential features of a data challenge. • 1 simulated day all-sky survey simulation • find the sources, including GRBs • a few physics surprises • exercise: – exposure, orbit/attitude handling, data processing pipeline components, analysis tools – DC 2 in 2005. More ambitious goals. ~One simulated month. • toy one-month catalog. • add source variability (AGN flares, pulsars). add GBM. – DC 3 in 2006. Support for flight science production. S. Ritz see http: //www-glast. slac. stanford. edu/software/Workshops/Feb 04 DC 1 Close. Out/coverpage. htm 17

GLAST LAT Project The DC 1 Sky DOE Mini-review 12 October 2004 One day all-sky survey. Generated E>20 Me. V. E>100 Me. V with some other cuts for illustration Lots to analyze! A few surprises to find… S. Ritz 18

GLAST LAT Project DOE Mini-review 12 October 2004 Data Challenge 1 Sky 3 C 273 isotropic diffuse 3 C 279 Sources – 3 EG and more, with a twist S. Ritz a number of physics surprises in the DC 1 data, including: • 110 Ge. V gamma-ray line source at the galactic center • new source populations • all surprises were detected at some level! 19

GLAST LAT Project DOE Mini-review 12 October 2004 LAT Data Challenges: Updated Plan for DC 2, based on lessons from DC 1 S. Ritz – 1 simulated month of all-sky survey gammas (backgrounds: see next slide) – key sky addition: source variability • AGN variability, including bright flares, quiescent periods • expand burst variety. Include GBM. • pulsars, including Gemingas, w/ orbit position effects. – more realistic all-sky attitude profile – background rate varies with orbit position – more physics surprises – update geometry (including s/c); add nominal hardware problems (and misalignments? ); add deadtime effects and corrections – Analysis Goals: • produce toy 1 -month catalog • try out transient releases and quicklook analyses, monitor sources • point source sensitivity and localization studies • try first systematic pulsar searches (timing!) • diffuse analyses • recognize simple hardware problems (connect with ISOC) • benchmark processing times, data volume, data transfers. 20

GLAST LAT Project Summary DOE Mini-review 12 October 2004 • Strong involvement of physicists at all levels of the project – ready for earliest instrument test data analysis – strategizing/prioritizing as issues arise – getting ready early to do great science via data challenges and updating organization of science groups – increasing cooperation with other experiments, helping to lead the way. • Very strong support by SLAC of the international science collaboration and the management of the fabrication. • The hardware is coming! Great excitement in a team that continues to grow even closer and stronger. S. Ritz 21