GALACTIC PHYSICS WITH CTA Ryan C. G. Chaves 1 for the the CTA - - PowerPoint PPT Presentation

▶
galactic physics with cta
SMART_READER_LITE
LIVE PREVIEW

GALACTIC PHYSICS WITH CTA Ryan C. G. Chaves 1 for the the CTA - - PowerPoint PPT Presentation

Jul 29, 2023 180 likes •682 views

GALACTIC PHYSICS WITH CTA Ryan C. G. Chaves 1 for the the CTA Consortium 1 CNRS/IN2P3 / Univ. Montpellier, France THE NEXT GENERATION: CTA The Future of Research on Cosmic Gamma Rays Galactic Physics with CTA, August 2015 2 GALACTIC

slide-1
SLIDE 1

GALACTIC PHYSICS WITH CTA

Ryan C. G. Chaves1 for the the CTA Consortium

1CNRS/IN2P3 / Univ. Montpellier, France

slide-2
SLIDE 2

THE NEXT GENERATION: CTA

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 2

slide-3
SLIDE 3

GALACTIC PHYSICS: CORE THEMES

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 3

THEME 1

Understanding the origin and role of relativistic cosmic particles

What are the sites of high-energy particle acceleration in the Galaxy? What are the mechanisms for cosmic particle acceleration? What role do accelerated particles play in feedback on star formation?

THEME 2

Probing extreme environments

What physical processes are at work close to neutron stars and black holes? What are the characteristics of relativistic jets, winds, and explosions?

slide-4
SLIDE 4

GALACTIC KEY SCIENCE PROGRAMS

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 4

Galactic Plane Survey Cosmic-ray PeVatrons / Supernova remnant RX J1713.7-3946

Dubus+ (CTA) 13

slide-5
SLIDE 5

GALACTIC KEY SCIENCE PROGRAMS

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 5

Large Magellanic Cloud Star Forming Systems

Credit: R. Gendler

slide-6
SLIDE 6

LMC

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 6

A unique target to study extreme Galactic-type VHE sources & difguse emission (CRs) Face-on satellite galaxy:

  • No source confusion
  • Relatively nearby, and

no distance ambiguity Very active:

  • Only 1% mass of the

Milky Way

  • Yet 10% the SFR

Potential pointing pattern

  • verlaid on starry sky image

N.B. Advantage of large CTA FoV

slide-7
SLIDE 7

LMC SIMULATIONS

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 7

Include:

  • known VHE sources
  • N 157B: most energetic pulsar, ~1038 erg/s
  • 30 Dor C: superbubble
  • N 132D: radio-loud SNR (50% Lradio Cas A)
  • luminous point-like sources
  • CR-enriched regions
  • Youngest SNR: SN 1987A
slide-8
SLIDE 8

`

LMC SIMULATIONS

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015 8

`

H.E.S.S.-like performance 1 pointing, 16 h, 0.8-100 TeV CTA performance 6 pointings, 340 h, 0.2-100 TeV

atomic gas contours

slide-9
SLIDE 9

STAR FORMATION & COSMIC RAYS

9 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Key science questions: What is the impact of CRs on the ISM & how do they propagate? What is the relationship between star formation & particle acceleration in systems on difgerent scales? Motivated also by:

  • well-established correlation in FIR
  • correlation seen recently in GeV -rays
slide-10
SLIDE 10

GALACTIC STAR FORMING SYSTEMS

10 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Cygnus & Carina regions will be mapped at high resolution

slide-11
SLIDE 11

TESTING UNIVERSAL RELATIONS

11 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Complementary Galactic and extragalactic science

Estimated calorimetric gamma-ray flux Estimated CTA sensitivity Current detections

slide-12
SLIDE 12

GPS IN CONTEXT

12 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

CTA Survey

slide-13
SLIDE 13

GPS IN CONTEXT

13 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-14
SLIDE 14

GPS IN CONTEXT

14 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Deil, Chaves+ (H.E.S.S.) 15

~mCrab and uniform sensitivity with CTA GPS in just 2 years

slide-15
SLIDE 15

GRADED SENSITIVITY APPROACH

15 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

First 2 years: ~2–4 mCrab 10-yr program

CTA N CTA S

slide-16
SLIDE 16

GPS OBJECTIVES

16

Increase population of known Galactic VHE sources x 3–9+ Discover new VHE source classes and unexpected phenomena Search for Galatic CR PeVatrons Measure large-scale difguse emission Detect new -ray binaries & other variable or transient sources Provide fjrst-look science data to other KSPs & General Observers Produce a multi-purpose legacy dataset to MWL community

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-17
SLIDE 17

SOURCE POPULATION

17

Increase population of known Galactic VHE sources x 3–9++

log N – log S plot

Renaud+09

T A R G E T R A N G E

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-18
SLIDE 18

NEW SOURCE CLASSES

18

Discover new VHE source classes and unexpected phenomena

Deil, Chaves+ (H.E.S.S.) 15

CTA discovery space

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-19
SLIDE 19

PEVATRON SEARCH

19

Search for Galatic CR PeVatrons

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

CTA South SST s further improve multi-T eV sensitivity + Access to inner Galaxy

slide-20
SLIDE 20

GPS SIMULATIONS

20 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Source populations modeled:

  • Both SNRs & PWNe
  • Fitted to known detections (T

eVCat) Expected difguse emission: Both IC & π0 components (GALPROP) Energy range: 1-10 T eV ctools open-source software with latest IRFs for North & South arrays Actual GPS observation scheme (1620 h) Most realistic simulations to date & work on-going

slide-21
SLIDE 21

GPS SIMULATIONS

21

Full-plane coverage: longitude ± 180°, latitude b ± 10° Deeper inner galaxy exposure: ℓ ± 80°

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Fine detail revealed with ~arcmin PSF

Knoedlseder+ (CTA)

slide-22
SLIDE 22

GPS SIMULATIONS: ZOOM

22 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-23
SLIDE 23

CR/PEVATRON OBJECTIVES

23

Discover Galactic CR PeVatrons responsible for CR knee Specifically:

Where & how in the Galaxy are CRs accelerated up to PeV energies? What is the distribution of PeVatrons in the Galaxy? Are we sitting in a particular location of the Galaxy, or is there a uniform CR sea within the whole Galaxy (understanding diffusion by observing gamma-ray accelerators and their surroundings)? Do young shell-type SNRs accelerate hadronic CRs up to PeV energies? If so, up to which energies, and how effective is this acceleration (probing the theory of non-linear DSA)?

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-24
SLIDE 24

WHERE ARE THE PEVATRONS?

24 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

O n e w a y t

  • g

e t t

  • C

R k n e e ( ~ 3 P e V ) e n e r g i e s , q u i t e s p e c i fj c : Y

  • u

n g , f a s t ( 2 , k m s

  • 1

) S N R s h

  • c

k i n d e n s e w i n d ( C S M ) f r

  • m

a T y p e I I S N & R S G p r

  • g

e n i t

  • r

e . g . 3 3

  • y

r

  • l

d C a s A , b u t = 2 . 6 ± . 2 Г

s t a t

± . 2

s y s t

O t h e r h i s t

  • r

i c a l S N R s a r e c h a l l e n g i n g a s w e l l , c . f . u p d a t e d T y c h

  • (

S N I a ) s p e c t r u m f r

  • m

V E R I T A S ( = 1 . 9 5 ± . 5 1 Г

s t a t

± . 3

s y s t

→ = 2 . 9 2 ± . 4 1 Г

s t a t

) A r e P e V a t r

  • n

s s h

  • r

t l i v e d ? M H D i n s t a b i l i t y q u e n c h e d a f t e r ~ 1 y r s ( ~ a g e R X J 1 7 1 3 ) , e . g . S c h u r e & B e l l 2 1 3 E

m a x

~ P e V f

  • r
  • n

l y ~ 1 y r s

  • r

l e s s O b s e r v a t i

  • n

s t r a t e g y f

  • r

C h e r e n k

  • v

t e l e s c

  • p

e s ? H i d d e n i n t h e e x i s t i n g d a t a b u t c

  • n

f u s e d /

  • b

s c u r e d ? J u s t n e e d m

  • r

e s t a t i s t i c s / b e t t e r s e n s i t i v i t y a t m u l t i

  • T

e V E ? N

  • t

l

  • k

i n g a t t h e r i g h t

  • b

j e c t s , b i a s e d b y w e l l

  • k

n

  • w

n S N R s ? M

  • l

e c u l a r c l

  • u

d s ?

slide-25
SLIDE 25

WHERE ARE THE PEVATRONS?

25 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

HGPS horizon CTA GPS horizon

GPS ideal strategy to identify PeVatron candidates

  • few mCrab sensitivity

along entire plane

  • E-range up to

hundreds of T eV

  • arcmin PSF to reduce

source confusion

Adapted from Carrigan, Chaves+ (H.E.S.S.) 13

slide-26
SLIDE 26

PEVATRON IDENTIFICATION

26 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Specifjcally, candidates should exhibit:

  • No VHE cut-ofg or break: 3- signal above 50 T

eV

  • Hard photon spectrum:   2.0

de Oñ a Wilhelmi+ (CTA)

slide-27
SLIDE 27

PEVATRON CHARACTERIZATION

27 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Solid lines: =  2.0 Dashed lines: =  2.2

KSP follow-up of top 3 candidates: +50 h deep observations of each to confjrm & measure spectra

CTA simulations

de Oñ a Wilhelmi+ (CTA)

slide-28
SLIDE 28

SNR RX J1713

28 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

Deeper obs. (+50 h min.) of most prominent -ray SNR T

  • disentangle leptonic /

hadronic acceleration e.g. through precision imaging of shell morphology T

  • probe surrounding

molecular environment (e.g. Gabici & Aharonian 07) Leveraging next-gen PSF to better match gas studies

slide-29
SLIDE 29

MORPHOLOGICAL APPROACH

29 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

50 h CTA simulation

Nakamori+ (CTA) 15

slide-30
SLIDE 30

SPECTRAL APPROACH

30 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

If leptonic component dominant, search for hidden hadronic component

Nakamori+ (CTA) 15

slide-31
SLIDE 31

CONCLUSIONS

31 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

CTA Galactic physics program to focus on: Galactic Plane Survey for discovery, foundation for deeper

  • bservations, and legacy for MWL community

LMC to probe Galactic-type sources & diffuse CRs in face-on galaxy PeVatrons, not only detection but characterization, and SNR RX J1713 as unique SNR and potential hadronic accelerator

slide-32
SLIDE 32

BACKUP

32 The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-33
SLIDE 33

Galactic KSPs Research questions

A wide coverage of core science themes that drive CTA

slide-34
SLIDE 34

The Large Magellanic Cloud

0.05° ~ 3ʹ angular resolution sensitivit y ~1035 erg s-1

Abramowski+ (H.E.S.S.) 15

slide-35
SLIDE 35

N 132D: A radio-loud middle-aged SNR

50% Lradio

  • f Cas A

Not quite VHE detection ~5 σ X-rays:

Abramowski+ (H.E.S.S.) 14

slide-36
SLIDE 36

N 157B: The Crab Nebula's twin

Pulsar has largest known Edot ~ 4.8 × 1038 erg s-1

Abramowski+ (H.E.S.S.) 14

slide-37
SLIDE 37

30 Dor C: A TeV superbubble

Largest SFR in Local Group Largest X-ray synchrotro n shell known (47 pc) 10x as bright as SN 1006 Powered by

Abramowski+ (H.E.S.S.) 14

ldiff = sqrt(2 D t) < ~47 pc D(10 TeV) < ~3.3 × 1026 (t/106 yr)−1 cm2 s−1 2-3 orders lower than ~Galactic requires MFA / B turbulence still open question: leptonic vs. hadronic

slide-38
SLIDE 38

SN 1987A: The youngest SNR

High shock speed High ambient density Hadronic? Upper limit

  • nly for

now, but more

  • bservation

s planned & emission predicted to increase

Predicted: ∼8 × 10−14 cm−2 s−1 in 2013 ∼2.5 × 10−14 cm−2 s−1 in 2010 F (> 1 TeV) < 5 × 10−14 cm−2 s−1 99% CL during 2003-2012

Abramowski+ (H.E.S.S.) 14

slide-39
SLIDE 39

The LMC in VHE γ-rays: Recap

Abramowski+ (H.E.S.S.) 14

slide-40
SLIDE 40

The LMC in VHE γ-rays: Spectra

Abramowski+ (H.E.S.S.) 14

slide-41
SLIDE 41

SFS KSP New Simulations

slide-42
SLIDE 42

VHE source distribution

Still lack statistics to disentangle? Not sensitivity limited in latitude? Roughly fjts plausible counterpart distributions

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-43
SLIDE 43

FYI: CTA GPS by ~2022

HGPS Sensitivity

along b = –0.3° for a 5-σ detection

The Future of Research on Cosmic Gamma Rays – Galactic Physics with CTA, August 2015

slide-44
SLIDE 44

Triple the exposure Improved gamma-hadron separation Improved angular resolution

slide-45
SLIDE 45

X-rays (XMM-Newton) convolved with H.E.S.S. PSF

Are cosmic rays escaping the shell and interacting with molecular clouds? i.e. is there TeV emission beyond the shell?

slide-46
SLIDE 46

Precision VHE spectra to ~50 TeV

slide-47
SLIDE 47

Precision VHE spectra to ~50 TeV

  • Exp. cut-ofg

around ~10 TeV ( not a → PeVatron)

slide-48
SLIDE 48
slide-49
SLIDE 49