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Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
HESS: Status and future plans
Dieter Horns (Univ. Tübingen)
on behalf of German Hermann (MPI-K, Heidelberg)
for the HESS collaboration
http://www.mpi-hd.mpg.de/hess
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Status of German Hermann?
● View from his hotel room in Walvis Bay, Namibia● He passes his greetings
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Update on the collaboration● Durham University
● Dublin Institute for Advanced Studies
● Nicolaus Copernicus Astronomical Center, Warsaw
● Jagiellonian University, Cracow
● Polish Academy of Sciences, Warsaw
● Charles University, Prague
● Yerevan Physics Institute
● University of Namibia, Windhoek
● North West University, Potchefstroom
● MPI-K, Heidelberg
● Humboldt Universität Berlin
● Ruhr-Universität Bochum
● Universität Hamburg
● Landessternwarte Heidelberg
● Universität Tübingen
● Ecole Polytechnique, Palaiseau
● Universités Paris VI-VII
● APC Paris
● CEA Saclay
● Obsérvatoire Paris Meudon
● LAPP Annécy
● Université Grenoble
● Université Montpellier
● CERS Toulouse
>100 Scientists from 24 institutes from 9 countries5 institutes have joined recently for HESS Phase II
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Controlbuilding
Security fence
ROTSE 3c robotical optical
telescope
Weather/atmospheric monitoring
120 m
Camera shelter
HESS I telescope
A tour of the site would also include: Guest houses, generator building, and
lots of wild animals!
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Recent changes: ROTSE 3c has been moved,
ATOM telescope installed● ATOM (Automatic Telescope
for Optical Monitoring) – LSW Heidelberg, PI S. Wagner
– 75 cm Alt-Az
– Multi-filter Photometry
– Automated operation implementation in progress
– “Slave” operation with HESS
● ROTSE (Robotic Optical Transient Search Experiment), PI Carl Akerlof
– 45 cm, unfiltered fast telescope
– Robotic operation
– Monitoring of ~100 Blazars
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
HESS Phase I telescopes
● Single telescope: July 2002● Full four telescopes: December 2003
20 t steel frame, f=15 mAlt-Azimuth mount,100°/min<10” pointing uncertainty380 front aluminised glass mirror tiles=107 m2 mirror surfaceCamera shelter
●960 PMT with Winston cones arranged in 60 drawers●Sector based topological trigger (3>5.3 p.e. within 1.3 ns gate)●5° degree fov (1.4 m)●Signals read out via multiplexed dual channel analogue ring storage 1 Ghz (integrated in camera)●Total weight 900 kg●Multiple (>1) telescope, ~300Hz coincidence required for system event read-out References:
Telescope & opticalsystemBernlöhr et al.
(2003), Cornils et al. (2003)Camera:
Vincent et al. (2003), System trigger:
Funk et al. (2004)
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Operational statistics
● Data taking started in July 2002, no shut-down● Shifts with a crew of three: Total of ≈300 flights
from Europe to Namibia >2 Mio km of travelling● Total data taken (until July 2006)=3623 hrs (≈900
hrs/yr)● Total amount of data stored: 18.7 Tbyte● Distribution centers: MPI-K Heidelberg, Data center
in Lyon
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Processing of data
● Calibration: Pedestals, broken pixels, relative and absolute gain calibration (see Aharonian et al. 2004)
● Two independent calibration and analyses chains (with different flavors), for a comparison see astro-ph/0607247: – “Hillas”-type analyses– Model based analyses
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Performance (“Hillas” type analyses)● Point-spread function: r68=0.08° per
event● Energy resolution: ΔE/E≈15%● Point source sensitivity: 5σ detection
1% Crab: 25 hours5% Crab: 5 hours10% Crab: 20 min50% Crab: 1.5 min100% Crab: 0.5 min
astro-ph/0607333, A&A in press
Remember: HEGRA ->100 hrs for 5% Crab
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Energy threshold
● Energy threshold as expected from simulations
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Highlight results
● Blind survey of the Galactic plane: New and so far unidentified sources, Science 307, 1938 (2004)
● Discovery of gamma-rays from an XRB system Science 309, 746, 2005
● Low level of O/NIR EBL Nature 440, 1018 (2006)● Gamma-rays from the Galactic Ridge Nature 439
695 (2006)● Gamma-ray image from RXJ1713 Nature 432, 75
(2004)See also the following talks by Berrie Giebels (Extragalactic observations) and DH (Galactic sources)
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
HESS Phase II● Aims:
– Extending the energy threshold to ~10-20 GeV– Achieve overlap in energy (and time) with GLAST– Improving the sensitivity at 100 GeV
● Approach:
– Increase mirror size to 600 m2 (equiv. 28 m⊘, 560 t steel frame)
– Increase focal length to 36 m– Decrease pixel size to 0.07° (fov=3.17°, >2t
camera)– Use well-established HESS Phase I type electronics– Combine a single telescope with the 4 Phase I
telescopes
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Artist's impression
^
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Structure in more details: Mirror dish
● Structure designed by MAN
● Parabolic dish (time dispersion)
● Adjustable Hexagonal mirror tiles
● Achieve similar optical performance as HESS Phase I CTs
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Camera design & electronics
● Diameter of 2.5 m● 2048 pixels in 128 drawers● 99 overlapping sectors (64
pixels each)● 2.5-3 t weight● Focussing (10 cm shift)● Read-out with “SAM”: Swift
Analogue memory at 1 GHz (improved version of the ARS)
● Level 1 trigger at 3 kHz
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Expected performance of HESS Phase II
Punch et al. (2006)
Based upon simulations verified with HESS Phase I
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Physics with HESS Phase II
● Study gamma-ray emission from pulsar magnetosphere
● Gamma-ray emission from XRBs● Explore the high redshift universe:
AGNs, Radio-Galaxies, GRBs● Indirect Dark matter search
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Status of HESS Phase II
● Steel construction has started, finished by spring 2007
● Installation of camera end of 2007/2008
● Phase II operational well within the beginning of the GLAST (second half of 2008)
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
News from German: Steel construction, Aug 2006
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin
Backup
Dieter Horns – University of Tübingen28-31 August 2006, Madison Wisconsin