Cosmic Ray Energetics And Mass for the International Space...
1
Operations • Nominal data collection of 3 years on the Japanese Experimental Module Exposed Facility (JEM‐EF) • 24/7 monitoring from the Science Operation Center (SOC) at University of Maryland • Data produced at 355 kbps, or 3.7 GB/day • 32 GB of onboard data storage (4‐fold redundant) • Continuous downlink of housekeeping and science data in near real‐time for monitoring • Commanding to adjust instrument operation parameters as needed Science Mission Statement Extend the energy reach of direct measurements of cosmic rays to the highest energy possible to investigate cosmic ray origins, acceleration and propagation. Detector Systems 1 • Silicon Charge Detector (SCD) – 4 layers of 2x2 cm 2 silicon pixels used to determine incident particle charge • Carbon Targets (C‐targets) – Layers of carbon plates to induce hadronic interactions for measurement in the calorimeter • Top/Bottom Counting Detector (TCD/BCD) – Plastic scintillators for electron/proton distinction • Calorimeter (CAL) – 20 layers of alternating tungsten plates and scintillating fibers used to measure incident particle energy and trajectory within the instrument • Boronated Scintillator Detector (BSD) – Boron‐doped scintillator to capture thermal neutrons from hadronic interactions in the calorimeter providing additional e/p distinction • Science Flight Computer (SFC) – The onboard computer used to control detectors, assemble events and store science data • General Payload Attributes – Mass: 1258 kg. size: 1.85 m x 0.95 m x 1 m, power consumption: 550 W Acknowledgements The authors thank NASA GSFC WFF for project management and engineering support, and NASA JSC ISS Program Office for the launch support and the ISS accommodation. This work was supported in the U.S. by NASA grants NNX11AC52G, NNX08AC15G, NNX08AC16G and their predecessor grants, as well as by directed RTOP funds to NASA GSFC WFF. It is supported in Korea by the Creative Research Initiatives of MEST/NRF and by National Research Foundation Grants NRF‐2014R1A2A2A01002734, NRF‐ 2014R1A1A2006456. It is supported in France by IN2P3/CNRS and CNES and in Mexico by DGAPA‐UNAM and CONACYT. Balloon Heritage • 6 flights totaling 161 days over Antarctica • Flight altitude around 40 km, with residual atmospheric overburden ~3.9 g/cm 2 • Successful recovery and refurbishing of hardware • Discovery of discrepant hardening of elemental spectra • Measurements of energy spectra at high energies Abstract The Cosmic Ray Energetics And Mass (CREAM) instrument is designed to directly measure cosmic rays with energy between 10 12 ‐ 10 15 eV and composition from proton to iron thereby investigating cosmic ray origins, acceleration and propagation. CREAM has four subsystems: a silicon charge detector (SCD), top/bottom counting detectors (TCD/BCD), a calorimeter (CAL), and a boronated scintillator detector (BSD). Reconfiguring the payload for implementation on the International Space Station will provide an order of magnitude increase in exposure time and remove the atmospheric overburden as compared to previous balloon flights. In preparation for launch, the newly configured hardware must be tested, and remote monitoring and control capabilities must be established. The project overview, current status of testing, and preparations for launch are discussed here. What are Cosmic Rays? • Energetic particles which are primarily protons but include nuclei and a small amount of electrons • Originate and accelerate in both galactic and extragalactic sources • Secondary cosmic rays are produced through spallation with interstellar medium • They can be measured from the ground (indirect) or from the upper atmosphere/space (direct) • Cosmic rays are one piece of the puzzle of modern cosmology and must be investigated in order to fully understand the complexities of our Universe The CREAM team in Antarctica just before launch. Attached to the payload are solar panels (black squares) and the communication satellite (round dome on upper right of the payload). Comparison of high‐energy spectra from a nominal ISS‐CREAM mission (red circles) with existing data (black symbols). 2 Data from previous experiments include BESS (open squares), ATIC‐2 (open diamonds), JACEE (X), and RUNJOB (open inverted triangles). The CREAM heavy nuclei data: carbon (open circles), oxygen (filled squares), neon (open crosses), magnesium (open triangles), silicon (filled diamonds), and iron (asterisks). Science Questions • Do supernovae supply the bulk of cosmic rays? • What is the history of cosmic rays in the galaxy? • What is the origin of the “knee” around 3x10 15 eV in the cosmic ray energy spectrum? • Can the energy spectra of cosmic rays result from a single mechanism? References 1. H. S. Ahn et al., The Cosmic Ray Energetics And Mass (CREAM) Instrument, Nuclear Instrumental Methods A 579, 1034‐1053, 2007; H. J Hyun, et al., Development of Top/Bottom Counting Detectors for the CREAM Experiment on the ISS, Proc. 33rd Int. Cosmic Ray Conf., Rio de Janeiro, ID 1017, 2013; T. Anderson et al., The ISS‐CREAM Boronated Scintillator Detector, Proc. 33rd Int. Cosmic Ray Conf., Rio de Janeiro, ID 0350, 2013 2. E. S. Seo et al., Cosmic Ray Energetics And Mass for the International Space Station (ISS‐CREAM). Advances in Space Research, in press, 2014. 3. H. S. Ahn et al., Discrepant Hardening Observed in Cosmic‐Ray Elemental Spectra. Astrophys. J Lett. 714 L89‐L92, 2010. 4. E. S. Seo, Direct Measurements of Cosmic Rays Using Balloon Borne Experiments, Astroparticle Physics, 39/40, 76‐87, 2012. Measured energy spectra of cosmic ray protons and helium nuclei. 3 The CREAM‐I spectra are compared with selected previous measurements using open symbols for protons and filled symbols for helium: CREAM (circles), AMS (stars), BESS (squares), CAPRICE (inverted triangles). Measuring boron to carbon ratio at high energies helps distinguish between propagation models. 4 ISS‐CREAM seeks to improve measurements in the region highlighted by the circle. Cosmic ray energy spectra span many orders of magnitude. ISS‐CREAM will extend direct measurements to the highest energy currently possible, approaching the “knee.” Cosmic Ray Energetics And Mass for the International Space Station E.S. Seo 1,* , Y. Amare 1 , T. Anderson 2 , D. Angelaszek 1 , M. Buénerd 3 , M. Copley 1 , S. Coutu 2 , L. Derome 3 , C. Ebongue 1 , L. Eraud 3 , I. Faddis 1 , B. Fields 1 , M. Gupta 1 , J.H. Han 1 , I.J. Howley 1 , H.G. Huh 1 , Y.S. Hwang 4 , H.J. Hyun 4 , S. Im 2 , H.B. Jeon 4 , J.A. Jeon 5 , D.Y. Kim 1 , H.J. Kim 4 , K.C. Kim 1 , M.H. Kim 1 , K. Kwashnak 1 , H.Y. Lee 5 , J. Lee 5 , M.H. Lee 1 , J. Liang 1 , J.T. Link 6 , L. Lutz 1 , A. Malinin 1 , J. Meade 1 , A. Menchaca‐Rocha 7 , J.W. Mitchell 6 , S. Nutter 8 , O. Ofoha 1 , H. Park 4 , H.A. Park 5 , I.H. Park 5 , J.M. Park 4 , P. Patterson 1 , N. Picot‐Clemente 1 , J.R. Smith 1 , P. Walpole 1 , R.P. Weinmann 1 , J. Wu 1 , Y.S. Yoon 1 1 Inst. for Phys. Sci. and Tech., University of Maryland College Park, USA; 2 Dept. of Physics, Penn State University, USA; 3 Laboratoire de Physique Subatomique et de Cosmologie, UJF – CNRS/IN2P3 – INP, France; 4 Dept. of Physics, Kyungpook National University, Republic of Korea; 5 Sungkyunkwan University, Physics Department, Republic of Korea; 6 Astrophysics Space Division, NASA Goddard Space Flight Center, USA; 7 Instituto de Fisica, Universidad Nacional Autonoma de Mexico,Mexico; 8 Dept. of Physics & Geology, Northern Kentucky University, USA *Principal Investigator Planned Measurements • Measure elemental energy spectra of proton through iron from 10 12 to 10 15 eV • Extend the boron to carbon ratio measurement to energies previously unavailable • Identify high energy electrons to search for nearby sources Current Status • Final verification including mechanical, electromagnetic, and thermal vacuum qualification testing was completed at Goddard Space Flight Center in August 2015 • Payload was delivered to Kennedy Space Center for integration with SpaceX Dragon capsule trunk • Launch is manifested for SpaceX‐11 in 2016 • Payload will be installed on to the JEM‐EF via ISS and JEM‐EF robotic arms Path taken by CREAM‐I on its then record breaking flight of 42 days. The first circumnavigation is shown in red, the second in green, and the third in yellow. http://cosmicray.umd.edu/iss‐cream/ SpaceX Launch Research Data Center, UMD Payload Operations Center, MSFC Science Operations Center, UMD RMS Handoff Flight in Dragon Trunk Visit our homepage using this QR code! Installation on JEM‐EF 초고에너지 우주선 연구
Transcript of Cosmic Ray Energetics And Mass for the International Space...
Ope
ratio
ns•Nom
inaldata
collectionof
3yearson
theJapane
seExpe
rimen
talM
oduleExpo
sed
Facility(JE
M‐EF)
•24
/7mon
itorin
gfrom
the
Science
Ope
ratio
nCe
nter
(SOC)
atUniversity
ofMaryland
•Da
taprod
uced
at3
55kbps,or
3.7GB/day
•32
GBof
onbo
arddata
storage(4‐fo
ldredu
ndant)
•Co
ntinuo
usdo
wnlinkof
housekeeping
andsciencedata
inne
arreal‐tim
efor
mon
itorin
g•Co
mmanding
toadjustinstrumento
peratio
nparametersas
need
ed
Science Mission
Statemen
tExtend
the en
ergy re
ach of dire
ct measurements of cosmic ra
ys to
the highest e
nergy po
ssible to
investigate cosm
ic ra
y origins,
acceleratio
n and prop
agation.
Detector S
ystems1
•Silicon
Charge
Detector(SCD
)–
4layers
of2x2
cm2
silicon
pixels
used
tode
term
ine
incide
ntparticlecharge
•Ca
rbon
Targets(C‐targets)–Layers
ofcarbon
plates
toindu
cehadron
icinteractions
for
measurementinthecalorim
eter
•Top/Bo
ttom
Coun
tingDetector(TCD
/BCD
)–
Plastic
scintillators
for
electron
/proton
distinction
•Ca
lorim
eter
(CAL
)–20
layers
ofalternating
tungsten
plates
andscintillatin
gfib
ersused
tomeasure
incide
ntparticle
energy
and
trajectory
with
intheinstrument
•Bo
rona
ted
Scintillator
Detector
(BSD
)–
Boron‐do
ped
scintillatorto
capture
thermal
neutrons
from
hadron
icinteractions
inthe
calorim
eter
providing
additio
nal
e/p
distinction
•ScienceFlight
Compu
ter(SFC)–Th
eon
board
compu
terused
tocontrold
etectors,a
ssem
ble
eventsandstoresciencedata
•Gen
eral
Payloa
dAttributes
–Mass:
1258
kg.
size:
1.85
mx
0.95
mx
1m,
power
consum
ption:5
50W
Ackn
owledgem
ents
Theauthorsthank
NASAGSFCWFF
forp
rojectmanagem
ent
anden
gine
eringsupp
ort,andNAS
AJSCISSProgram
Office
forthelaun
chsupp
ortandtheISSaccommod
ation.
This
work
was
supp
orted
inthe
U.S.
byNAS
Agrants
NNX1
1AC5
2G,
NNX0
8AC1
5G,
NNX0
8AC1
6Gand
their
predecessorgrants,as
wellas
bydirected
RTOPfund
sto
NAS
AGSFCWFF.Itissupp
ortedin
Koreaby
theCreative
Research
Initiatives
ofMEST/NRF
andby
NationalR
esearch
Foun
datio
nGrants
NRF
‐201
4R1A
2A2A
0100
2734
,NRF
‐2014R1
A1A2
006456.
Itis
supp
orted
inFrance
byIN2P
3/CN
RSandCN
ESandin
Mexicoby
DGAP
A‐UNAM
and
CONAC
YT.
Ballo
on Herita
ge•6 flights to
taling 161 days
over Antarctica
•Flight altitude
aroun
d 40
km,
with
resid
ual atm
osph
eric
overbu
rden
~3.9 g/cm
2
•Successful re
covery and
refurbish
ing of hardw
are
•Discovery of disc
repant
harden
ing of elemental
spectra
•Measurements of e
nergy
spectra at high en
ergies
Abstract
TheCo
smic
RayEn
ergeticsAn
dMass(CRE
AM)instrumentis
desig
ned
todirectly
measure
cosm
icrays
with
energy
betw
een10
12‐1
015eV
andcompo
sitionfrom
proton
toiro
nthereb
yinvestigatingcosm
icrayorigins,acceleratio
nandprop
agation.
CREA
Mhasfour
subsystems:
asilicon
charge
detector
(SCD
),top/bo
ttom
coun
tingde
tectors
(TCD
/BCD
),a
calorim
eter
(CAL),
and
abo
ronated
scintillator
detector
(BSD
).Re
configuringthepayloadforim
plem
entatio
non
theInternationalS
pace
Stationwill
providean
orde
rof
magnitude
increase
inexpo
sure
timeandremovetheatmosph
eric
overbu
rden
ascomparedto
previous
balloon
flights.In
prep
arationforlaun
ch,the
newly
configured
hardware
mustbe
tested
,and
remote
mon
itorin
gand
control
capabilitiesmustbe
establishe
d.Th
eprojectoverview
,current
status
oftesting,
and
prep
arations
forlauncharediscussedhe
re.
Wha
tare
Cosm
icRa
ys?
•En
ergetic
particles
which
are
prim
arily
proton
sbu
tinclud
enu
clei
andasm
allamou
ntof
electron
s•
Orig
inate
and
accelerate
inbo
thgalacticandextragalactic
sources
•Second
arycosm
icrays
areprod
uced
throughspallatio
nwith
interstellar
med
ium
•Th
eycan
bemeasured
from
the
grou
nd(in
direct)o
rfrom
theup
per
atmosph
ere/space(dire
ct)
•Co
smic
rays
areon
epieceof
the
puzzle
ofmod
ern
cosm
ology
and
mustbe
investigated
inorde
rto
fully
unde
rstand
thecomplexities
ofou
rUniverse
TheCR
EAM
team
inAn
tarcticajust
before
laun
ch.
Attached
tothepayloadaresolarpanels
(black
squares)
andthecommun
icationsatellite
(rou
nddo
meon
uppe
rright
ofthepayload).
Comparison
ofhigh
‐ene
rgyspectrafrom
ano
minal
ISS‐CR
EAM
mission
(red
circles)
with
existingdata
(black
symbo
ls).2
Data
from
previous
expe
rimen
tsinclud
eBE
SS(ope
nsqua
res),
ATIC‐2
(ope
ndiam
onds),
JACE
E(X),
andRU
NJOB
(ope
ninverted
triangles).Th
eCR
EAM
heavy
nuclei
data:carbon
(ope
ncircles),oxygen
(filled
squares),ne
on(ope
ncrosses),magne
sium
(ope
ntriangles),silicon
(filled
diam
onds),andiro
n(asterisk
s).
Science Que
stions
•Do
supe
rnovae sup
ply the bu
lk of
cosm
ic ra
ys?
•What is the
history of cosmic ra
ys in
the galaxy?
•What is the
orig
in of the
“knee”
arou
nd 3x101
5 eV
in th
e cosm
ic ra
y en
ergy spe
ctrum?
•Can the en
ergy spe
ctra of cosmic
rays re
sult from
a single m
echanism
?
References
1.H. S. A
hn et a
l., The
Cosmic Ray Energetics A
nd M
ass (CR
EAM)
Instrument, Nuclear Instrumental M
etho
ds A 579, 1034‐1053,
2007; H
. J Hyun, et a
l., Develop
ment o
f Top
/Bottom Cou
nting
Detectors for th
e CR
EAM Experiment o
n the ISS, Proc. 33rd Int.
Cosm
ic Ray Con
f., Rio de Janeiro
, ID 1017, 2013; T. And
erson
et al., The
ISS‐CR
EAM Boron
ated
Scintillator D
etector, Proc.
33rd Int. Co
smic Ray Con
f., Rio de Janeiro
, ID 0350, 2013
2.E. S. Seo
eta
l., Cosmic Ray Energetics A
nd M
ass for th
e Internationa
l Spa
ce Statio
n (ISS‐CR
EAM).Ad
vances in Space
Research, in press, 2014.
3.H. S. A
hnet al., Disc
repa
nt Hardening
Observed in Cosmic‐Ray
Elem
ental Spectra. Astrop
hys. J Lett. 714
L89‐L92, 2010.
4.E. S. Seo, D
irect M
easurements of C
osmic Rays U
sing Ba
lloon
Bo
rne Experim
ents, Astroparticle Physic
s, 39/40
, 76‐87, 2012.
Measureden
ergy
spectraof
cosm
icrayproton
sand
helium
nuclei.3
TheCR
EAM‐Ispectraarecompa
red
with
selected
previous
measuremen
tsusing
open
symbo
lsforproton
sandfilledsymbo
lsforhe
lium:
CREA
M(circles),A
MS(stars),BE
SS(squ
ares),CA
PRICE
(inverted
triangles).
Measurin
g bo
ron to carbo
n ratio
at h
igh energies helps
distinguish
between prop
agation mod
els.4ISS‐CR
EAM
seeks to im
prove measurements in
the region
highlighted
by th
e circle.
Cosm
icrayen
ergy
spectraspan
manyorde
rsof
magnitude
.ISS‐CR
EAM
will
extend
direct
measuremen
tsto
the
highesten
ergy
curren
tlypo
ssible,app
roaching
the“kne
e.”
Cos
mic
Ray
Ene
rget
ics
And
Mas
s fo
r th
e In
tern
atio
nal S
pace
Sta
tion
E.S. Seo
1,* , Y. Am
are1, T. A
nderson2, D
. Angelaszek1, M
. Bué
nerd
3 , M. Cop
ley1, S. Cou
tu2 , L. Derom
e3, C. Ebo
ngue
1 , L. Eraud
3 , I. Fadd
is1, B
. Fields1, M
. Gup
ta1 , J.H
. Han
1 , I.J. H
owley1
, H.G. H
uh1 , Y.S
. Hwang4, H
.J. Hyun4, S. Im
2 , H.B. Je
on4 , J.A
. Jeo
n5, D
.Y. Kim
1, H
.J. Kim
4 , K.C. Kim
1 , M.H. Kim
1 , K.
Kwashn
ak1 , H.Y. Lee5, J. Lee
5 , M.H. Lee
1 , J. Liang1, J.T. Link6, L. Lutz1, A
. Malinin
1 , J. Meade
1 , A. M
enchaca‐Ro
cha7, J.W. M
itche
ll6, S. N
utter8, O
. Ofoha
1 , H. Park4, H
.A. Park5, I.H. Park5, J.M
. Park4, P. Patterson
1 , N. Picot‐Clemente
1 , J.R
. Smith
1 , P. W
alpo
le1 , R.P. W
einm
ann1, J. W
u1, Y.S. Yoo
n11 Inst. for Phys. Sci. and
Tech., University
of M
aryland Co
llege Park, USA
; 2 Dep
t. of Physic
s, Pen
n State University, U
SA; 3
Labo
ratoire
de Physiq
ue Sub
atom
ique
et de Co
smologie, U
JF –CN
RS/IN2P
3 –INP, France; 4 De
pt. of P
hysic
s, Kyungpo
okNational U
niversity, R
epub
lic of K
orea; 5
Sungkyun
kwan
University, P
hysic
s De
partment, Repu
blic of K
orea; 6
Astrop
hysic
s Space Divisio
n, NAS
A God
dard Space Flight Center, USA
; 7Institu
tode
Fisica, U
niversidad
Nacional A
uton
omade
Mexico,Mexico;
8De
pt. of P
hysic
s & Geo
logy, N
orthern Kentucky University, U
SA *Principa
l Investig
ator
Plan
ned Measuremen
ts•Measure
elem
ental
energy
spectra
ofproton
throughiro
nfrom
1012to
1015eV
•Extend
the
boron
tocarbon
ratio
measuremen
tto
energies
previously
unavailable
•Iden
tifyhigh
energy
electron
sto
search
for
nearby
sources
Curren
t Status
•Final verificatio
n includ
ing mechanical, electrom
agne
tic, and
thermal vacuu
m
qualificatio
n testing was com
pleted
at G
oddard Space Flight Center in Au
gust 2015
•Payload
was
delivered
toKenn
edySpace
Center
forintegration
with
SpaceX
Dragon
capsuletrun
k•Laun
chismanifested
forS
paceX‐11
in2016
•Payloadwillbe
installedon
totheJEM‐EFviaISSandJEM‐EFrobo
ticarms
Path
takenby
CREA
M‐Ion
itsthen
record
breaking
flightof
42days.Th
efirst
circum
navigatio
nis
show
nin
red,
thesecond
ingreen,
andthethird
inyellow.
http://cosmicray.um
d.ed
u/iss
‐cream
/
SpaceX
Laun
ch
Research Data Ce
nter,
UMD
Payload Operatio
ns
Center, M
SFC
Science Operatio
ns
Center, U
MD
RMS
Hando
ff
Flight in
Dragon
Trunk
Visit our hom
epage
using this QR code
!
Installatio
n on
JEM‐EF
초고에너지우주선연구
