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W. Hofmann
MPI for Nuclear Physics
CTA Observatory GmbH
Heidelberg
GCT Inauguration
Meudon, 2014
W. Hofmann
MPI for Nuclear Physics
CTA Observatory GmbH
Heidelberg
for the CTA Consortium
Current
Instruments
Current Galactic VHE sources (with distance estimates)
CTA
10 x Sensitivity, Large Collection
Area
all topics
10 x Sensitivity, Large Collection
Area
all topics
Energies down to 20 GeV
Cosmology++
Energies up to 300 TeV
Pevatrons
8o Field of View
surveys, extended objects
10 x Sensitivity, Large Collection
Area
all topics
Rapid Slewing in 20 seconds
transients
Energies down to 20 GeV
Cosmology++
Energies up to 300 TeV
Pevatrons
8o Field of View
surveys, extended objects
Few ‘ Angular Resolution
morphology
10 x Sensitivity, Large Collection
Area
all topics
Rapid Slewing in 20 seconds
transients
Energies down to 20 GeV
Cosmology++
Energies up to 300 TeV
Pevatrons
10% Energy Resolution
lines, features
NASA
NOVEL:
ALL-SKY COVERAGE
North+South
South North
>60o zenith
45o-60o
30o-45o
NOVEL:
WORLD-WIDE COOPERATION
31 Countries
192 Institutes
1270 Members
NOVEL:
OPERATION AS OBSERVATORY
Delivery to user: FITS data files,
FERMI-like analysis tools
All CTA data will be fully open after a proprietary period;
open analysis tools
Cherenkov Image
3-D Reconstruction of cascade using images from multiple telescopes
FROM CURRENT ARRAYS TO CTA
light pool radius
R ≈100-150 m
≈ typical telescope spacing
Sweet spot for
best triggering
and reconstruction:
most showers miss it!
large detection area
more images per shower
lower trigger threshold
The ideal solution
large 7 km2 array of
small telescopes, for
rate-limited highest
energies
~km2 array of
medium-sized
telescopes
few large telescopes
for lowest energies
70 SSTs
25 MSTs
4 LSTs
with some realism added
CTA ENERGY COVERAGE
1 000
10 000
100 000
1 000 000
10 000 000
0,01 0,1 1 10 100 1000
Série1
Eff. detection
area (m2)
Energy (TeV)
optimal
working
range
optimal
working
range
CTA
H.E.S.S. I
(DIFFERENTIAL) SENSITIVITY
15 CDR Template, 1 June 2015
(TeV)R
Energy E
2-10
1-10
110
210
)-1 s-2
x Flux Sensitivity (erg cm2
E
13-10
12-10
11-10
www.cta-observatory.org (2015-05-11)
CTA South 50 h
Differential sensitivity (5 bins per decade in energy)
MAGIC 50 h
VERITAS 50 h
HAWC 1 year
HAWC 5 year
CTA North 50 h
Differential sensitivity (5 bins per decade in energy)
Fermi
10 yrs
Integral
10 Ms
CTA AS A SURVEY MACHINE
Simulated
CTA Galactic Survey 8o 5o
Longitude
H.E.S.S. survey
CTA Survey
CTA AS A PEVATRON HUNTER
© J. Hahn
Gamma rays
from proton
interactions
(flat proton SED)
100 TeV 10 PeV 1000 PeV
1 PeV 100 PeV
CTA AS A TRANSIENT FACTORY
Huge advantage over
Fermi in energy range
of overlap for ~minute
to ~week timescale
phenomena Explosive transients,
AGN flares, binary
systems
Disadvantage Slewing time ~20 s and
limited (cf Fermi) Field
of View
External triggers critical
Time (s)
102
103
104
105
106
107
108
109
1010
10
)-1 s-2Differential Flux Sensitivity (erg cm
-1310
-1210
-1110 -1010
-910
-810
-710
-610
-510
-410
-310
E = 25 GeV
E = 40 GeV
E = 75 GeV
Fermi-LAT
CTA10 years
1 hour
CTA CDR - SCIENCE, 24 June 2015
19
CTA AS A TRANSIENT FACTORY
Simulated z=4.3
GRB, E > 30 GeV
A BIT OF HISTORY
NOVEMBER 2005: 5 PAGE DOCUMENT
62 signatories
JANUARY 2006
SUBMISSION TO ESFRI
ESFRI ROADMAP 2006
ASPERA ROADMAP
2006
Werner Hofmann, ESFRI Subcommittee, Jan. 08 27
C TA An advanced facility for ground-based high-energy gamma ray astronomy
The Cherenkov Telescope Array facility
aims to explore the sky in the 10 GeV to 100 TeV energy range
builds on demonstrated technologies
combines guaranteed science with significant discovery potential
is a cornerstone towards a multi-messenger exploration of the nonthermal universe
C TA An advanced facility for ground-based high-energy gamma ray astronomy
CTA as a user facility
Significant fraction of open time (~50%)
Guaranteed time for CTA consortium (~50%)
Probably local staff for basic operation, plus experts when needed
Facilities to make data available to outside users
Data public after certain time (~1 y)
Significant fraction of operating funds / user support / data center support needs to come from external (EC?) sources
Not to scale !
Option: Mix of telescope types
C TA An advanced facility for ground-based high-energy gamma ray astronomy
10-14
10-13
10-12
10-11
10 100 1000 104
105
E x
F(>
E)
[Te
V/c
m2s]
E [GeV]
Possible CTA sensitivity
Crab
10% Crab
1% Crab
GLAST
MAGIC
H.E.S.S.
Current Simulations
20 wide-angle 10 m telescopes de la Calle Perez, Biller, astro-ph 0602284
30 m stereo telescopes Konopelko Astropart.Phys. 24 (2005) 191
E.F(>E)
[TeV/cm2s]
looks a bit optimistic
looks a bit optimistic
C TA An advanced facility for ground-based high-energy gamma ray astronomy
(Very optimistic) Schedule
06 07 08 09 10 11 12 13
Site exploration
Array design
Component prototypes
Telescope prototypes
Array construction
Partial operation
Full operation
GLAST
FP 7 Design Study
“Letter of Intent” (100 pages, physics + conceptual design)
Technical proposal
CTA TELESCOPES
Not to scale !
2006
2008
CTA DESIGN
CONCEPTS 2008
LST
CTA DESIGN
CONCEPTS 2008
MST
CTA DESIGN
CONCEPTS 2008
SST
ESFRI ROADMAP
2008
ASPERA ROADMAP
2008
ASPERA ROADMAP
2008
Credit:
Multimedia Service,
Institute of Astrophysics of Canary Islands
2010
Argentina, Brazil, France, Germany, Italy, Japan,
Namibia, Poland, South Africa, Spain, Switzerland, UK
2012: DECLARATION OF INTENT
SIGNED BY MINISTRIES
ASTRI SST (2014)
SST-1M (2015)
GCT (2015)
GCT (2015)
MST (2015)
LST (2015)
LST PROTOTYPE GROUND BREAKING
LA PALMA, OCT 9, 2015
TECHNICAL DESIGN REPORT
INFRASTRUCTURE VISIONS
WE’RE LEGAL
CTAO GmbH founded in July 2014
Swiss contribution to
share capital
WE’VE GOT A CASE
CTA SCIENCE PROGRAMME
Key Science Programmes Ensure that important science questions
for CTA are addressed in a coherent
fashion and with a well-defined strategy,
Conceived to provide legacy data sets for
the entire community
Example: galactic and
extragalactic
surveys
Deep investigation of known sources
Follow-up of KSP discovered sources
Multiwavelength campaigns
Follow-up of ToOs from other wavebands
/ messengers
Search for new sources
…
Proposal-Driven User Programme
WE’RE ALMOST THERE !