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 !