Future directions in Ground-Based Gamma-Ray Astronomy Simon Swordy - TeV Particle Astro II, UW Madison, 2006.

Slides:

Advertisements

Similar presentations

Astronomy Notes to Accompany the Text

Advertisements

The MAGIC telescope and the GLAST satellite La Palma, Roque de los Muchacos (28.8° latitude ° longitude, 2225 m asl) INAUGURATION: 10/10/2003 LAT.

Oct. 18, Review: Telescopes – their primary purpose… Across the full EM spectrum (radio through very high energy gamma- rays) telescopes fundamentally.

Web: Contact: HAWC is a collaborative effort between institutions in the United States of America.

High-energy particle acceleration in the shell of a supernova remnant F.A. Aharonian et al (the HESS Collaboration) Nature 432, 75 (2004) Nuclear Physics.

S.Mereghetti - Simbol-X: The hard X-ray Universe in focus - Bologna -15/5/20071 Studying the Galactic Ridge Emission with SIMBOL-X Sandro Mereghetti IASF.

WP-Technology Working Group Future of Ground Based Gamma-ray Astronomy Feb 8, Technology & Cost WP Working Group GOALS With the Current Generation.

Jamie Holder School of Physics and Astronomy, University of Leeds, U.K Increasing the Collection Area for IACTs at High Energies Future of Gamma Ray Astronomy.

Gus Sinnis HAWC Review December 2007 Milagro a TeV Gamma-Ray Observatory Gus Sinnis Los Alamos National Laboratory.

The National Science FoundationThe Kavli Foundation AAS 211th meeting - Austin, TX Implications of Recent UHECR Data for Multi-Messenger Studies of Cosmic.

H.E.S.S. High Energy Stereoscopic System Jon Cerny Bancroft-Rosalie School August 2002.

The Spectrum of Markarian 421 Above 100 GeV with STACEE Jennifer Carson UCLA / Stanford Linear Accelerator Center February MeV 1 GeV 10 GeV 100.

C TA An advanced facility for ground-based high-energy gamma ray astronomy Why ? CTA.

The future of ground-based gamma ray astronomy Where do we go?

On A Large Array Of Midsized Telescopes Stephen Fegan Vladimir Vassiliev UCLA.

Telescopes. Magnification (make things look bigger) easy to make a telescope with good magnification Collection of large amounts of light (see fainter.

Julie McEnery GLAST Science Lunch Milagro: A Wide Field of View Gamma-Ray Telescope Julie McEnery.

1 Arecibo Synergy with GLAST (and other gamma-ray telescopes) Frontiers of Astronomy with the World’s Largest Radio Telescope 12 September 2007 Dave Thompson.

Alexander Kappes UW-Madison 4 th TeVPA Workshop, Beijing (China) Sep. 24 – 28, 2008 The Hunt for the Sources of the Galactic Cosmic Rays — A multi-messenger.

22 February 2006 Quo Vadis ? Wide Field Imaging A Wide Angle Very Low Threshold Air Cherenkov Imaging Telescope Razmick Mirzoyan MPI Munich, Germany.

High-Energy Astrophysics

High Energy Astrophysics with the High Altitude Water Cherenkov Experiment John Pretz – Los Alamos National Lab International Astronomical Union Meeting.

© 2010 Pearson Education, Inc. Chapter 6 Telescopes: Portals of Discovery.

Studying for the Exam Relevant chapters: E, 1, 2 & 3 To prepare for the exam it is helpful to … –review readings –review lecture notes online (esp. concept.

Gus Sinnis RICAP, Rome June 2007 High Altitude Water Cherenkov Telescope  Gus Sinnis Los Alamos National Laboratory for the HAWC Collaboration.

Milagro Gus Sinnis Milagro NSF Review July 18-19, 2005 Milagro: A Synoptic VHE Gamma-Ray Telescope Gus Sinnis Los Alamos National Laboratory.

High Energy Particle Astrophysics PRC-US Collaboration Summary Report Gus Sinnis David Kieda Gus Sinnis Hu Hongbo Jordan Goodman Min Zha.

Moriond 2001Jordan GoodmanMilagro Collaboration The Milagro Gamma Ray Observatory The Physics of Milagro Milagrito –Mrk 501 –GRB a Milagro –Description.

De Angelis, Feb 07 1 Gamma astrophysics in the 50 GeV – 50 TeV domain Great results from Cherenkov telescopes (IACTs): number of VHE sources increased.

Gamma-Ray Telescopes. Brief History of Gamma Ray Astronomy 1961 EXPLORER-II: First detection of high-energy  -rays from space 1967 VELA satelllites:

Chapter 6 Telescopes: Portals of Discovery. 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning How does your eye form an image? How do.

Atmospheric shower simulation studies with CORSIKA Physics Department Atreidis George ARISTOTLE UNIVERSITY OF THESSALONIKI.

Development of Ideas in Ground-based Gamma-ray Astronomy, Status of Field and Scientific Expectations from HESS, VERITAS, MAGIC and CANGAROO Trevor C.

CTA The next generation ultimate gamma ray observatory M. Teshima Max-Planck-Institute for Physics.

Gus Sinnis Asilomar Meeting 11/16/2003 The Next Generation All-Sky VHE Gamma-Ray Telescope.

Telescopes. Light Hitting a Telescope Mirror huge mirror near a star * * * small mirror far from 2 stars In the second case (reality), light rays from.

Multi-TeV  -ray Astronomy with GRAPES-3 Pravata K Mohanty On behalf of the GRAPE-3 collaboration Tata Institute of Fundamental Research, Mumbai Workshop.

What does mean neighbours ? At the same epoch –simultaneous (transient phenomenae) –before (can affect the SIMBOL-X observing plan) –after (can complement.

Matteo Palermo “Estimation of the probability of observing a gamma-ray flare based on the analysis of the Fermi data” Student: Matteo Palermo.

MA4: HIGH-ENERGY ASTROPHYSICS Critical situation of manpower : 1 person! Only «free research» based in OAT. Big collaborations based elsewhere (Fermi,

Extending the Sensitivity Of Air-Cerenkov Telescopes Steve Biller, Oxford University (de la Calle & Biller – astro-ph/ )

C TA An advanced facility for ground-based high-energy gamma ray astronomy  Exploring the non-thermal universe  the C herenkov T elescope A rray as a.

HAWC Science  Survey of 2  sr (half the sky) up to 100 TeV energies Probe knee in cosmic ray spectrum Identify sources of Galactic cosmic rays  Extended.

Hybrid measurement of CR light component spectrum by using ARGO-YBJ and WFCTA Shoushan Zhang on behalf of LHAASO collaboration and ARGO-YBJ collaboration.

VERITAS Observations Of M 31 and some results about my recent work

Introduction Data analyzed Analysis method Preliminary results

A Future All-Sky High Duty Cycle VHE Gamma Ray Detector Gus Sinnis/Los Alamos with A. Smith/UMd J. McEnery/GSFC.

Dave Kieda & Stephan LeBohec University of Utah Department of Physics and Astronomy John Davis University of Sydney, NSW Science Potential of High Altitude.

Pheno Symposium, University of Wisconsin-Madison, April 2008John Beacom, The Ohio State University Astroparticle Physics in the LHC Era John Beacom The.

Space Telescopes.

Combining Gamma and Neutrino Observations Christian Spiering, DESY.

05/02/031 Next Generation Ground- based  -ray Telescopes Frank Krennrich April,

Gamma-Ray Burst Working Group Co-conveners: Abe Falcone, Penn State, David A. Williams, UCSC,

Next Generation Particle Astrophysics with GeV/TeV  -Rays D. Kieda University of Utah.

Sources emitting gamma-rays observed in the MAGIC field of view Jelena-Kristina Željeznjak , Zagreb.

C TA An advanced facility for ground-based high-energy gamma ray astronomy  Exploring the non-thermal universe  the C herenkov T elescope A rray as a.

Detecting Air Showers on the Ground

MPI Semiconductor Laboratory, The XEUS Instrument Working Group, PNSensor The X-ray Evolving-Universe Spectroscopy (XEUS) mission is under study by the.

MAGIC Telescopes - Status and Results 2009/ Isabel Braun Institute for Particle Physics, ETH Zürich for the MAGIC collaboration CHIPP Plenary Meeting.

The Electromagnetic Spectrum and Telescopes Rose Emanuel Journey into Space Journey Museum, July 18-20, 2012.

Prospects of Identifying the Sources of the Galactic Cosmic Rays with IceCube Alexander Kappes Francis Halzen Aongus O’Murchadha University Wisconsin-Madison.

The Large High Altitude Air Shower Observatory LHAASO.

The end of the electromagnetic spectrum

Tobias Jogler Max – Planck Institut für Physik The MAGIC view of our Galaxy Tobias Jogler for the MAGIC Collaboration.

TeV Gamma Ray Astrophysics Wei Cui Department of Physics Purdue University.

Large Area Telescopes Cosmic Rays – Gamma Rays – Neutrinos P.Kooijman.

Observation of Pulsars and Plerions with MAGIC

Lecture 4 The TeV Sky Cherenkov light Sources of Cherenkov radiation.

HAWC Science Survey of 2p sr up to 100 TeV energies Extended Sources

Presentation transcript:

Future directions in Ground-Based Gamma-Ray Astronomy Simon Swordy - TeV Particle Astro II, UW Madison, 2006

Future of ground-based gamma-rays, postulate: "Where there's a will there's a way.." Discuss..

Some History

The Crab in early x-rays from a rocket flight....

Also....

Balloon "sky survey"......

Catalog of objects, mostly not there...

What happened next? Balloon/ x-rays >20keV Then Now still awaiting NuSTAR NASA/Explorer Rocket/ x-rays<10keV etc....

WHY did <10keV do so much better? The technology of x-ray mirrors as focusing optics could be used <10keV, (now also possible >20keV, hence NuSTAR) Low energy x-ray detectors could be built from silicon -> CCDs Low energy single photon resolution became sub arcsec The energy window ~20-100keV is only being more fully explored recently because modern detector technology in SWIFT has angular resolution ~17arcmin. (Coded mask and CdZnTe).

Ground-based gamma-ray astronomy will not be able get much better than ~5arcmin (for single gamma), so several objects will always seem close to point-like (e.g. Cass A, Tycho, Crab..) It cannot compete with optical, radio, soft x-ray in the detailed morphology of sources..... but it can provide a clear outline of the extreme non-thermal pieces of our Galaxy and beyond. So.....

So what "ways" are there and where might they go? Air CerenkovFutureParticle ArraysFuture Energy Thr (GeV) ~100<50~2000<200 FOV (sq deg.) ~12~100?~5000 Livetime~8%10%?95%>95%  -ray ang. res. (deg.) ?1<0.4 Collection Area (m 2 )  -ray energy res. ~20%15%~75%40% hadron rejection >99.9%>99.95%~90%

"Easy" ways to go.. Make 'em bigger (increase to an array size of sqkm) Make 'em higher (go up a bigger mountain) "Tricky" ways to go... Lower energy threshold (going up a mountain helps, high QE devices help) Increase FOV for air cherenkov (some optical limits to this) Seemingly impossible stuff... Get better single photon angular resolution Increase live-time for air cherenkov

Distance From Center Of Array [m] Array telescopes 2.8 hexagonal rings m separation Telescope and Detector 1.ø10m equivalent 2.QE = 0.25 (Bialkali) 3.15º field of view Facts and Figures 1.Outer radius: 640m 2.Single cell area: 5543m 2 3.Total area: 1.06km 2 Some examples: S. Fegan, V. Vassiliev, UCLA "HE-ASTRO" concept

Field of view [π sr] Field of view [deg] Current IACTAs Narrow field of view <0.01 km 40 GeV km 100 GeV km 10 TeV Square KM Array Continuum of modes Trade area for solid angle Parallel mode Narrow field of view 1 km 40 GeV 2 km 100 GeV 4-5 km 10 TeV “Fly’s Eye” mode Wide field of view km 40 GeV km 100 GeV 3-4 km 10 TeV Observation Modes Collecting Area [km 2 ]

HAWC or miniHAWC? (300m versus 150m baseline) New Info…

Milagro group + collaborators

few 1000 m High-energy section ~0.05% area coverage E th ~ 1-2 TeV 250 m Medium-energy section ~1% area coverage E th ~ GeV 70 m Low-energy section ~10% area coverage E th ~ GeV Hofmann: Array layout: 2-3 Zones FoV increasing to 8-10 degr. in outer sections CTA - European Initiative (HESS+MAGIC)

Not to scale ! Option: Mix of telescope types

 Sensitivity on Crab: Whipple 5  /√hr Milagro ~8  /√yr (wide angle) VERITAS-4, etc 23  /√hr HAWC 7  /√hr (wide angle) HE-ASTRO23  /√hr (wide angle) HE-ASTRO166  /√hr (sees Crab in 3s!)

Whipple, HEGRA, CANGAROOII, Milagrito HESS, MAGIC VERITAS, CANGAROOIII, Milagro HESS2, MAGIC2 VERITAS2, CANGAROOIII+?, MiniHAWC CTA, HE-ASTRO, HAWC, +…. Ground Gamma-Ray Timeline

Some Ways Forward: In principle, collection area can be increased ad infinitum. The collection area of present ACTs is defined by the light pool size. The detector becomes larger than the light pool above ~10 5 m 2. Future ACT arrays head toward >1km 2 Higher altitude sites help ACTs and ground arrays, probably >3000m (presently ~2000m). Coverage of full sky is highly desirable -> north and south facilities. Given expected world-wide resources ( two observatories All-sky monitoring capability at <0.1 Crab level seems essential. Possibly with a co-located HAWC-type detector, or with a single HE-ASTRO-type detector, or maybe something new. The interested science community will probably grow significantly - we need to get our world-wide act together