CALET on the Interna/onal Space Sta/on
ASI Workshop May 31, 2016
Pier Simone Marrocchesi Univ. of Siena and INFN Pisa
CALET Collabora,on O. Adriani25, Y. Akaike2, K. Asano7, Y. Asaoka8,31, M.G. Bagliesi29, G. Bigongiari29, W.R. Binns32, S. Bonechi29, M. Bongi25, P. Brogi29, J.H. Buckley32, G. Castellini25, M.L. Cherry12, G. Collazuol26, V. Di Felice28, K. Ebisawa9, H. Fuke9, T.G. Guzik12, T. Hams3, M. Hareyama23, N. Hasebe31, K. Hibino10, M. Ichimura4, K. Ioka11, M.H. Israel32, A. Javaid12, K. Kasahara31, J. Kataoka31, R. Kataoka16, Y. Katayose33, C. Kato22, N. Kawanaka30, H. Kitamura15, H.S. Krawczynski32, J.F. Krizmanic2, S. Kuramata4, T. Lomtadze27, P. Maestro29, P.S. Marrocchesi29, A.M. Messineo27, J.W. Mitchell14, S. Miyake5, K. Mizutani20, A.A. Moiseev3, K. Mori9,31, M. Mori19, N. Mori25, H.M. Motz31, K. Munakata22, H. Murakami31, Y.E. Nakagawa9, S. Nakahira8, S. Nakahira8, J. Nishimura9, S. Okuno10, J.F. Ormes24, S. Ozawa31, F. Palma28, P. Papini25, A.V. Penacchioni29, B.F. Rauch32, S. Ricciarini25, K. Sakai3, T. Sakamoto1, M. Sasaki3, Y. Shimizu10, A. Shiomi17, R. Sparvoli2, P. Spillan,ni25, I. Takahashi1, M. Takayanagi9, M. Takita7, T. Tamura10, N. Tateyama10, T. Terasawa7, H. Tomida9, S. Torii8,31, Y. Tunesada18, Y. Uchihori15, S. Ueno9, E. Vannuccini25, J.P. Wefel12, K. Yamaoka13, S. Yanagita6, A. Yoshida1, K. Yoshida21, and T. Yuda7
1) Aoyama Gakuin University, Japan 2) CRESST/NASA/GSFC and Universi,es Space Research Associa,on, USA 3) CRESST/NASA/GSFC and University of Maryland, USA 4) Hirosaki University, Japan 5) Ibaraki Na,onal College of Technology, Japan 6) Ibaraki University, Japan 7) ICRR, University of Tokyo, Japan 8) JAXA, Japan 9) JAXA/ISAS, Japan 10) Kanagawa University, Japan 11) KEK, Japan 12) Louisiana State University, USA 13) Nagoya University, Japan 14) NASA/GSFC, USA 15) Na,onal Inst. of Radiological Sciences, Japan 16) Na,onal Ins,tute of Polar Research, Japan
17) Nihon University, Japan 18) Osaka City University, Japan 19) Ritsumeikan University, Japan 20) Saitama University, Japan 21) Shibaura Ins,tute of Technology, Japan 22) Shinshu University, Japan 23) St. Marianna University School of Medicine, Japan 24) University of Denver, USA 25) University of Florence, IFAC (CNR) and INFN, Italy 26) University of Padova and INFN, Italy 27) University of Pisa and INFN, Italy 28) University of Rome Tor Vergata and INFN, Italy 29) University of Siena and INFN, Italy 30) The University of Tokyo, Japan 31) Waseda University, Japan 32) Washington University-‐St. Louis, USA 33) Yokohama Na,onal University, Japan
ASI Workshop May 31, 2016 P. S. Marrocchesi 2
② August 24th: The HTV-‐5 Transfer Vehicle (HTV-‐5) is grabbed by the ISS robo/c arm.
CALET is taking data on the ISS !!
P. S. Marrocchesi 3
① August 19th: AMer a successful launch of the Japanese H2-‐B rocket by the Japan Aerospace Explora/on Agency (JAXA) at 20:50:49 (local /me), CALET started its journey from Tanegashima Space Center to the ISS.
③ August 24th: The HTV-‐5 docks to the ISS at 6:28 (EDT).
④ August 25th: CALET is emplaced on port #9 of the JEM-‐EF and data communica/on with the payload is established. ASI Workshop May 31, 2016
CALorimetric Electron Telescope (CALET): INSTRUMENT OVERVIEW
- CHarge Detector (CHD) (Charge Measurement Z=1-‐40) - Imaging Calorimeter (IMC) (Par/cle ID, Direc/on) Total Thickness of Tungsten (W): 3 X0 , 0.1 λλΙΙ Layer Number of Scifi Belts: 8 Layers × 2(X,Y)
- Total Absorp,on Calorimeter (TASC) (Energy Measurement, Par/cle ID) PWO 20mm x 20mm x 320mm
Total Depth of PWO: 27 X0 (24 cm) , 1.2 λλΙΙ
CHD (Charge Detector)
IMC (Imaging Calorimeter)
TASC (Total Absorption Calorimeter)
Function Charge Measurement (Z = 1 - 40) Arrival Direction, Particle ID Energy Measurement, PID
Sensor (+ Absorber)
Plastic Scintillators: 2 layers Unit Size: 32mm x 10mm x 450mm
Scintillating Fibers: 16 layers single readout: 1mm2 x 448 mm Total thickness of Tungsten: 3 X0
PWO logs: 12 layers Unit size: 19mm x 20mm x 326mm
Total Thickness of PWO: 27 X0
Readout PMT+CSA 64-anode MAPMT+ ASIC APD/PD+CSA
PMT+CSA ( for Trigger)
P. S. Marrocchesi 5
1 TeV electron
ASI Workshop May 31, 2016
CHD
IMC
TASC
CHD-‐FEC
IMC-‐FEC
TASC-‐FEC
Plastic Scintillator"
Scintillating Fiber"
PWO crystal log
CHD
TASC(Completed) CFRP Structure
IMC
14 × 1 layer (x,y) = 28! 32mm x 10mm x 450mm
448 x 8 (x,y) layers = 7168 !1mm2 x 448 mm!
16 x 6 (x,y) layers = 192"19mm x 20mm x 326mm!
Main Flight Components
CALET: a unique set of key instruments. q TASC: a thick, homogeneous calorimeter allows to
extend electron measurements into the TeV energy region with ~2% energy resolu/on.
q IMC: a high granularity (1mm) imaging pre-‐shower
with tracking capabili,es iden/fies the star/ng point of electromagne/c showers.
q TASC+IMC provide a strong rejec,on power 〜〜105 to separate electrons from the abundant protons. q CHD: a charge detector combined with mul/ple dE/dx
samples from IMC iden/fies individual elements.
P. S. Marrocchesi 6 ASI Workshop May 31, 2016
CGBM (Calet Gamma-‐ray Burst Monitor)
HXM x2
LaBr3(Ce)
SGM x1
BGO
7keV-‐1MeV
0.1-‐20MeV
P. S. Marrocchesi 7
ASC (Advanced Stellar Compass)
CGBM/SGM
MDC (Mission Data Controller)
FRGF( Flight Releasable Grapple Fixture)
CGBM/HXM
CHD
IMC
TASC
§ Standard Payload Size § Mass: 612.8 kg § Power: 507 W (Max)
§ Telemetry: o Medium rate: 600 kbps o Low rate: 50 kbps
CALET System Overview )
HVPS (HV Power System)
CALORIMETER MODULE
Geometric Factor: 1200 cm2sr for electrons, light nuclei
1000 cm2sr for gamma-‐rays
4000 cm2sr for ultra-‐heavy nuclei
• ΔE/E :
~2% (>10 GeV) for e, gamma
~30-‐35 % for protons, nuclei
• e/p separa,on : ~10-‐5
• Charge resolu,on : 0.15 -‐ 0.3 e
• Angular resolu,on :
0.2° for gamma-‐rays > ~50 GeV
GPSR (GPS Receiver)
ASI Workshop May 31, 2016
Photomultiplier (PMT) HV
- 80 channels (redundant DC/DC with linear regulator stage)
- range: 0 to -870 V with 10-bit resolution (minimum step 850 mV)
- 30 outputs @500 µA, 50 outputs @300 µA
delivered by ASI to JAXA
under the coordina/on of
IFAC-‐CNR – Florence
G. Castellini
S.B. Ricciarini
Avalance Photodiode (APD) HV
- 22 channels (redundant DC/DC stage) - range: 0 to -450 V with 10-bit
resolution (minimum step 440 mV) - ripple voltage ≈ 150 mVpp at maximum
current for all channels
8 8 ASI Workshop May 31, 2016
Observations with High Energy Trigger!
6.7x105 events /day (~7.8Hz)
~1.1 x 108 events triggered in total
Accumulated triggered event number
Live Time: 8.1x106 sec (86%)!
Accumulated observa/on /me (live, dead)
Live /me ra/o ~86%
Concept of on-orbit
operations!
day
night
• Single He trigger (for calibra/on)
P. S. Marrocchesi 9 Vulcano Workshop May 22-‐28, 2016
High energy trigger is always ac/ve
P. S. Marrocchesi 9
High Energy Observation for 171 days: October 13, 2015 – March 31, 2016!
ASI Workshop May 31, 2016
using CHD only
He
p
Using mul/ple dE/dx measurements from the IMC scin/lla/ng fibers (upstream the interac/on point), a complementary charge measurement from IMC is ploqed vs the CHD charge assignment (abscissa). A clear separa/on between p and He can be seen from preliminary data analysis.
p
He
data selec/on is NOT representa/ve of elemental abundances
Atomic Number Z
P. S. Marrocchesi 10
CHARGE IDENTIFICATION
ASI Workshop May 31, 2016
data selec/on is NOT representa/ve of elemental abundances
N
O
C
B
Carbon candidate Z = 6 CAL Energy deposit ~6.6 TeV
Atomic Number Z
P. S. Marrocchesi 11
only CHD info
ASI Workshop May 31, 2016
P. S. Marrocchesi 12
Fe candidate Z = 26 CAL Energy deposit ~15.6 TeV
only CHD info
Si
Fe
Ne Mg
S Ca Ar Ti Cr
data selec/on is NOT representa/ve of elemental abundances
Atomic Number Z
ASI Workshop May 31, 2016
Ni candidate Z = 28 CAL Energy deposit ~768 GeV P. S. Marrocchesi 13
Fe O Si
Ca ADC Upper limit
Trans-‐Iron candidates
ASI Workshop May 31, 2016
CALET Main Target: Identification of Electron Sources
Expected flux !for 5 year mission !
Expected Anisotropy! from Vela SNR
~10% @1TeV
> 10 GeV ~ 2.7 x 107
>100 GeV ~ 2.0 x 105
>1000 GeV ~ 1.0 x 103
Some nearby sources, e.g. Vela SNR, might have unique signatures! in the electron energy spectrum in the TeV region (Kobayashi et al. ApJ 2004)
Identification of the unique signature from nearby SNRs, !such as Vela in the electron spectrum by CALET
P. S. Marrocchesi 14
Calculated results normalized to the observed at 100 GeV Original flux x 0.65 Pulsar or Dark Matter ?
ASI Workshop May 31, 2016
Energy[GeV]±e100 1000
]-1
sr
-1 s
-2 c
m2
Flux
[GeV
×3 E
0.005
0.01
0.02
0.03
-e++e-e
(BG)-e++e)-ePAMELA (
FermiATICH.E.S.S.syst. error in H.E.S.S.CALET expectation (5yrs)
1cE2L3L ., JHEP 1303 (2013) 063.et alIbe
Dark Matter or Pulsar with Electrons
Decay of Dark Matter (LSP)
Expected e++e- spectrum by Lightest Super Symmetry Particle (LSP) (black line) with CALET measurement after 5-year (red dots), consistent with present data of positron excess and e++e-
spectrum
Best fit results for the single pulsar extra source !(Ecut = 1TeV) to AMS-02 positron fraction data and AMS-02 total flux data compared with the results of the DRAGON simulation.!In the lower panel the fractional residuals are plotted, showing an agreement better than 10%. in the most relevant energy range.
Single Pulsar (Geminga or Monogem)
Motz et al., JCAP 12(2015) 047
P. S. Marrocchesi 15 ASI Workshop May 31, 2016
q The break also appears in the spectra of NUCLEI measured by CREAM up to several TeV/n
The slope of Z>2 NUCLEI at high energy looks similar to He and different from protons
q PAMELA detected a spectral break in PROTON and HE spectra at R ~ 240 GV
A single power-‐law seems inadequate to fit the spectra of nuclei
Measurements of cosmic nuclei spectra
P. S. Marrocchesi 17 ASI Workshop May 31, 2016
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• Measurements by AMS-‐02 with p and He below MDR ~ 2 TV seem to confirm the presence of a spectral break in the same region as reported by PAMELA and CREAM.
² CALET is carrying on an accurate scan of the energy region around the spectral break with an energy resolu/on ~30 – 40 % and larger GF ~ 0.12 m2 sr
ASI Workshop May 31, 2016
P. S. Marrocchesi 19
² AMer one year on the ISS, CALET is expected to close the gap between AMS02 and CREAM above 1 TV. It will also extend the inves/ga/on on the spectral shapes of proton and He to the mul/-‐TeV region.
[P.S. Marrocchesi, arXiv:1512.08059] ASI Workshop May 31, 2016
q INDIRECT MEASUREMENTS BY AIRSHOWERS: hints of a proton cutoff below 1 PeV?
Explora/on of the sub-‐PeV region
In 5 yrs CALET can perform DIRECT measurements of p and He fluxes in the mul/-‐TeV region.
P. S. Marrocchesi 20
Superposi,on with CREAM direct measurements
ARGO YBJ: (P + HE) SPECTRUM
ICRC 2015 E_cutoff (p+He) ~ 700 TeV ?
ASI Workshop May 31, 2016
CALET explores the Multi-TeV region
Requirements for proton calorimetry: • proton interaction requires > 0.5 λINT
• at 100 TeV energy scale, longitudinal containment of the e.m. core of the shower requires > 20 X0
λλINT X0 (normal incidence)
CREAM 0.5 + 0.7 20
CALET 1.3 30
AMS-02
0.5 17
CALET expected in 5 yrs (red points)
P. S. Marrocchesi 21
CALET Energy reach in 5 years:
² Proton spectrum to ≈ 900 TeV
² He spectrum to ≈ 400 TeV/n
² Spectra of C,O,Ne,Mg,Si to ≈ 20 TeV/n
² B/C ratio to ≈ 4 - 6 TeV/n
² Fe spectrum to ≈ 10 TeV/n
Elemental spectra Proton and He
ASI Workshop May 31, 2016
P. S. Marrocchesi 22
q • Energy dependence of the diffusion
constant: D ~ Eδ
• δ~0.6 below 100 GeV/n. At higher energy the ra/o is expected to flaqen out (otherwise CR anisotropy should be larger than observed)
• Observa/on up to several TeV/n free from the atmospheric produc/on of boron by heavier cosmic nuclei
Dedicated UH trigger: larger trigger acceptance à 0.4 m2sr Sta/stcs:: ≅ 10 x TIGER (with UH trigger) ≅ 4 x TIGER (with full geometry and energy reconstruc/on)
Cleaner measurements (smaller correc/ons for hadronic interac/ons above atmosphere)
Secondary to Primary ra/o (B/C and Fe/Sub-‐Fe)
UH Composition to Z=40
ASI Workshop May 31, 2016
² CALET was successfully launched on HTV-‐5 from Tanegashima Space Center on August 19, 2015 berthing to the ISS on August 25. AMer func/onal check-‐out, CALET completed a calibra/on and ini/al opera/on phase on November 17, 2015, and standand opera/on mode began.
² It is an instrument primarily dedicated to the observa/on of electrons in the TeV region to provide crucial informa/on on nearby sources and
From Oct.13, 2015 -‐ March 31, 2016 nearly 1.2 x 106 electron candidate events above 10 GeV have been observed among 1.1 x 108 triggered events. Electron event candidates were observed above 1 TeV.
² Cosmic rays from proton to Fe and Ultra Heavy ions (26 < Z < 40), as well as astrophysical gamma-‐rays have been observed. Energy spectra, rela/ve elemental abundances and secondary-‐to-‐primary ra/os are being measured.
² CALET’s CGBM has measured the light-‐curves of 20 GRB’s as of May 15, 2016.
² 5 year observa/ons are planned.
Summary
P. S. Marrocchesi 23 ASI Workshop May 31, 2016
La partecipazione italiana alla missione CALET di JAXA e’ stata finanziata da ASI per un totale corrente di 2.3 MEuro e cofinanziata dalle is/tuzioni che partecipano alla missione: • Univ. di Siena (prime contractor) • IFAC (CNR) -‐ Firenze • Univ. di Firenze • Univ. di Padova • Univ. di Pisa • Univ. di Roma -‐ Tor Vergata Il contributo hardware italiano, oltre al sistema flight di alte tensioni fornito da ASI e coordinato da IFAC, include la proposta coordinata dall’Univ. di Siena di estendere il programma scien/fico di CALET alla rivelazione di nuclei cosmici fino a Z=40 con il disegno, l’implementazione proto/pale e rela/vi tests su fascio del sistema di iden/ficazione in carica (CHD). Il contributo all’analisi viene affequato da personale universitario a tempo indeterminato, da personale a tempo determinato reclutato secondo l’accordo aqua/vo del progeqo con ASi e da doqorandi coper/ da borsa triennale di doqorato.
Partecipazione italiana alla missione CALET
P. S. Marrocchesi 24 ASI Workshop May 31, 2016
P. S. Marrocchesi 25
Indirect Dark Maqer Search with Gamma rays Energy Range 4 GeV-‐10 TeV (or > 1GeV)
Effec/ve Area 600 cm2 (10GeV)
Field-‐of-‐View 2 sr
Geometrical Factor 1100 cm2sr
Energy Resolu/on 3% (10 GeV)
Angular Resolu/on 0.35 ° (10GeV)
Poin/ng Accuracy 6ʹ′
Point Source Sensi/vity 8 x 10-‐9 cm-‐2s-‐1
Observa/on Period (planned) 2015-‐2020 (5 years)
Gamma-ray Detection Performance
Detection of High Energy Gamma-rays!
2 year observation
Gamma-ray Line shape
Energy Spectrum
Position
Vela: ~ 300 photons above 5 GeV** !
Simulation of Galactic Diffuse Radiation ~5,700 photon* are expected per one year
~1,700 photon* from extragalac/c gamma-‐ ray background (EGB) each year
Simulation of point source observations in one year!
*) Trigger efficiency included below 10 GeV **) 100 % efficiency over 5 GeV
ASI Workshop May 31, 2016