XRISM Media Kit

Introduction
With just 60 years of history, X-ray astronomy is a relatively new field compared with the several
thousands of years we have been studying astronomy. However, even in its short history, X-ray astronomy
has already provided the world with new views of the universe, including observations of previously
unknown objects, such as black holes and neutron stars, and the discovery of intergalactic high-energy
plasmas. X-ray astronomy has introduced observational techniques that reveal new aspects of theuniverse. The X-ray microcalorimeter instrument the X-Ray Imaging and Spectroscopy Mission (XRISM)
carries, called Resolve, is another instrument that will greatly add to this growing history.
The objective of XRISM is to reveal the universe in X-rays, exploring new cosmic frontiers in the field of
X-ray astronomy. XRISM will expand on advanced technologies from previous JAXA missions, including
a state-of-the-art spectrometer with 30 times higher energy resolution than conventional spectrometers.
Utilizing new capabilities and implementing lessons learned from past missions, JAXA is working with
NASA, ESA, domestic and international universities, and research institutes to achieve state-of-the-art
science with high reliability.
XRISM will be an X-ray observatory available to the international scientific community. XRISM will
investigate the structural formation of the universe and the evolution of galaxy clusters, the history ofmaterial circulation in the universe, and energy transport and circulation in the universe. In addition, themission will aim to pioneer new science using ultra high-resolution X-ray spectroscopy.

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Contents
Introduction

02

Products

04

XRISM Overviews
Science05

at a glance

06

Orbit

07

Mission Instruments

08

Operation Framework

09

Schedule

10

Open Use Observatory

11

XRISM in the World

13

Science Objectives
Why we observe the Universe in X-ray?

15

The Assembly of Clusters of Galaxies

16

The Chemical Makeup of the Universe

17

The Extremes of Spacetime

18

Satellite
Architecture

19

Bus Components

20

Mission Instruments
XMA

21

Resolve

23

Xtend

25

Science Operation
Toward Creating Scientific Results

27

Satellite Operations and Ground Systems

29

XRISM Team

30

Cover Images
Crab Nebula ©X-ray: NASA/CXC/SAO/F.Seward; Optical: NASA/ESA/ASU/J.Hester & A.Loll; Infrared: NASA/JPL-Caltech/Univ. Minn./R.Gehrz
MACS J0416 ©X-ray: NASA/CXC/SAO/G.Ogrean et al.; Optical: NASA/STScI; Radio: NRAO/AUI/NSF
M87 ©X-ray: NASA/CXC/Villanova University/J. Neilsen
black-hole driven outflows and jets at the centre of a galaxy ©ESA/AOES Medialab
Tycho's Supernova ©X-ray: NASA/CXC/RIKEN & GSFC/T. Sato et al; Optical: DSSXRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

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Products
News Releases and Features
JAXA Press Releases
		https://global.jaxa.jp/press/2023/
Official Twitter		
https://twitter.com/JAXA_en		
https://twitter.com/XRISM_jp
Multimedia Resources
JAXA Digital Archives
		https://jda.jaxa.jp/en/
NASA Science Visualization Studio		https://svs.gsfc.nasa.gov/
Web Resources
Official JAXA Site		
https://global.jaxa.jp/
Official Project Site		
https://xrism.isas.jaxa.jp/en/
Official Partner Site
National Aeronautics and Space Administration (NASA)		https://www.nasa.gov/xrism
European Space Agency (ESA)		
https://www.cosmos.esa.int/web/xrism

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XRISM Overviews
ScienceXRISM (X-Ray Imaging and Spectroscopy Mission) is Japan's seventh X-ray observatory. It will belaunched by an HII-A rocket from the Tanegashima Space Center in Kagoshima Prefecture in 2023.
XRISM will observe very high-temperature gases in space, ranging from hundreds to tens of millions ofdegrees Celsius. The XRISM payload consists of two instruments, Resolve and Xtend.
Resolve is a soft X-ray spectrometer that pairs a lightweight X-ray Mirror Assembly (XMA) with an X-ray
calorimeter spectrometer that can measure the "color" of X-rays in detail. Xtend is a soft X-ray imager
that can observe an area of the sky equivalent to one full moon at a time.
XRISM's most outstanding feature is its ability to distinguish color. It is particularly well suited for
astrophysical analysis of extended objects such as galaxy clusters and supernova remnants.
Based on the features of the onboard instruments, XRISM has four themes of exploration.

1. Structure formation of the universe andevolution of galaxy clusters

X-ray: NASA/CXC/ITA/INAF/J.Merten et al, Lensing: NASA/
STScI; NAOJ/Subaru; ESO/VLT, Optical: NASA/STScI/R.Dupke

2. History of the material cycle of the universe

X-ray: NASA/CXC/
Penn State Univ./L.
Townsley et al.; IR:
NASA/ESA/CSA/STScI/JWST ERO
Production TeamIn a galaxy cluster, 90% of the "normal" matter is hot gas at tensof millions of Kelvin. Observations of high-temperature gas are
essential to understanding how the structure of the universe
evolves.

From interstellar gas that forms new stars to the enriched gas freed
from massive stars in supernova explosions, matter circulates in
the universe. By studying the motion of high-temperature gas, we
can investigate how matter spreads through interstellar space.

3. The energy transport in the universe

4. Pioneering new science with unprecedented

X-ray: Chandra: NASA/CXC/SAO, IXPE: NASA/
MSFC/J. Vink et al.; Optical: NASA/STScI

high-resolution X-ray spectroscopy

NASA

Matter and energy are transported into interstellar and intergalactic
space by energetic phenomena, such as supernova explosions
and active galactic nuclei. X-ray spectroscopy of these hot
and intense phenomena can help us understand the transport
processes.

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

X-ray: NASA/CXC/SAO/F.Seward; Optical: NASA/ESA/
ASU/J.Hester & A.Loll; Infrared: NASA/JPL-Caltech/Univ.
Minn./R.Gehrz

Researchers cannot create strong gravitational and magnetic fields
in the laboratory that often occur throughout the universe. XRISM'scapabilities will also allow us to understand better how matter
behaves under "extreme conditions."

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XRISM Overviews
at a glanceName

XRISM (X-Ray Imaging and Spectroscopy Mission)

Goals and Objectives

Building on previous missions and technologies, XRISM will continue to elucidate theprocesses of matter circulation and energy transport in the high-temperature regions of theuniverse, as well as the evolution of astronomical objects. In particular, XRISM will study how:i. Cosmic structures form, and galaxy clusters evolve in the universe
ii. Matter has circulated in the universe over timeiii. Energy transports and circulates throughout the universe
iv. To pioneer new scientific discoveries using ultra-high resolution X-ray spectroscopy

LaunchTargeted Date

August 26, 2023

Launch Site

Tanegashima Space Center

Launch Vehicle

H-IIA rocket
Total length 8m
Width with solar arrays deployed 9m
Diameter 3m
wi

dth

9m

Dimensions
Structure

len

Mass

2.3 t

Altitude550 +/- 50 km

Inclination

31 degrees

Type

Circular

Period96 minutes

gth

8m

Orbit

Instruments

Xtend (Soft X-ray imager)
Resolve (Soft X-ray spectrometer)

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XRISM Overviews
Orbit

XRISM has a circular orbit around Earth with an inclinationof 31 degrees at a height of about 550 km. Each orbit takes

Altitude 550km
Inclination 31 degrees
Orbital Period 96 minutes

about 96 minutes. XRISM's attitude is controlled with anaccuracy of approximately 17 arcseconds. The STT (StarTracker Telescope) camera captures images of point-sourcestars, and the satellite's pointing direction is estimated basedon these images. The Reaction Wheels (RW) maintain orchange the direction of XRISM.
XRISM observes a single object for a certain period of time.
When the observation of a target object is completed, XRISM
slews to the next target object according to an operations
plan prepared in advance.

XRISM’s Orbit

Communication with XRISM in orbit is mainly performed using the 34m/20m antennas at the
Uchinoura Space Center (USC) in Kagoshima Prefecture and the 20m antenna at the Katsuura Space
Communication Station in Chiba Prefecture. Overseas stations will also be used to monitor the satellite
status. The S-band (2 GHz band) and the X-band (8 GHz band) are used for communication with thesatellite. The S-band is more stable and is used to transmit satellite control commands and receive
housekeeping information (power, temperature, attitude, etc.). The X-band is about four times faster thanthe S-band and is used for receiving sizeable scientific observation data.

KTU4
MSP1

JAXA
NASA

USC20/34
SSC south point

SSA dongara
SANSA Hartebeesthoek

SSC santiago
MGN1
SNT

Ground Stations for the XRISM’s operations

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XRISM Overviews
Mission Instruments

XRISM is equipped with Resolve for ultra-precise energy measurement and Xtend for imaging over awide wavelength range. XMA (X-ray Mirror Assembly) is an X-ray telescope that efficiently collects X-rays
at the sensor.

XMA

Xtend
Resolve

XMA (X-ray Mirror Assembly)
XMA is an X-ray telescope. X-rays entering the telescope will encounter the mirror’s smooth metal shells
at a very shallow angle, called grazing incidence. They'll experience total reflection, which will slightly
change their direction of travel, focusing them on a detector. The mirrors of XMA are nested one within
another, like an onion, to guide X-rays as much as possible to the focal point.
Resolve
Resolve will measure the amount of incoming X-ray energy in great detail, enabling us to measure thetemperature and composition of X-ray-emitting objects with great precision. In addition, researchers canuse the Doppler effect, a phenomenon where wavelengths of light emitted by a moving object appear to be
shifted, to determine the object's motion. Resolve was developed jointly by Japan and the United States.
Xtend
Xtend will make images from the X-rays coming from celestial objects. The CCD camera used in Xtend is
not so different from that of ordinary digital cameras. However, the Xtend camera’s CCD is designed todetect X-rays and measure their energies.

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XRISM Overviews

Operation FrameworkXRISM is a joint international project that JAXA is pursuing under a memorandum of understanding with
the National Aeronautics and Space Administration (NASA) and the European Space Agency (ESA). In
addition to the three space agencies, JAXA has been working closely with universities and research
institutes in Japan, the U.S., and Europe to develop satellites, instruments, and data-processing software.
More than 300 astrophysicists andengineers from the three space agencies,
universities, and research institutes
in Japan, the U.S., and Europe areparticipating in the project to develop
satellites, instruments, data processing
software, and scientific observation plans.

NASA

Joint
Project

ESA
Collaboration*
Spacecraft
Development

24 Domestic
Universities/
Institutes

Collaboration*

XRISM
project

16 Universities/
Institutes Abroad
U.S.A, Canada,
the Netherlands,
Switzerland, U.K.,
Germany, and so on

Domestic
Contractors

Collaboration**Instruments’ development andScience Operation Support

Data
SharingNASA etc.

Space Science
Database

Calibrated Observation Data

Scientists in the WorldXRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

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XRISM Overviews
Schedule

Post-launch Sequence
XRISM is launching on the H-IIA Launch

circulating Earth at a height of 550 km with aperiod of 96 minutes.

50
Main engine
cut off

40
30
North latitude (degrees)

Vehicle as a joint ride with the Smart Lander for
Investigating Moon (SLIM). The right figure shows
the planned trajectory of the XRISM spacecraft
after launch. XRISM will be inserted into an orbit

60

XRISM separation

20

Satellite fairing
separation

10
Second engine
cut off

0
-10
-20
-30
120

130

140

150

160

170

180

190

200

210

East longitude (degrees)

phase, there will be a Performance Verification
phase (PV phase) of about seven months toevaluate the performance of the detectors. Oncethe initial and PV phases are complete, scientificobservations will begin based on researchers'
proposals worldwide. When XRISM has completed
nearly two years of guest observations, it will be
evaluated for possible extended operations andobservations (Late phase).

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10Initial phase Critical & Commissioning Phase
Calibration & Performance
RegularVerification Phases
Operation
Phase

20
Month from launch

Schedule after the Orbit Injection
After the orbital insertion, the initial phase isdivided into two phases: a critical operation phase
to confirm whether the satellite can maintainits attitude and a commissioning phase to test
the operation of the subsystems. After the initial

Guest Observations Phase

3
7

26

30
40

Late
Phase
Operation

50
40

60
70
80

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XRISM Overviews

Open Use Observatory

Open Use for Worldwide Scientists
An observatory with publicly accessible
data, XRISM will hold an international open
call for observations to start about 10
months after launch. Experts will review thesubmitted proposals, and observation time
will be allocated to the selected observation
proposals.
After a certain period, all acquired data will bemade publicly available. In this way, we aim to
maximize the scientific results from XRISM.
First XRISM Core-to-Core Science Workshop ©Saitama University

XRISM Observation Data
As an open-use observatory, we have adopted NASA's global standard format to make XRISM
observation data widely available so that anyone who has learned how to use the software can obtain
scientific results. Analysis software is available free of charge.
As the world's open observatory
XRISM is an open-use observatory that observes cosmic X-rays with state-of-the-art technology. A user
support team was organized to maximize the scientific results by fully utilizing XRISM’s capabilities. The
role of this team is to support XRISM users. The user support team has the following three roles:
1. To properly inform prospective observers of the features of XRISM and the high performance andlimitations of the onboard instruments.
2. To inform users how to analyze XRISM data.
3. To present XRISM results published in papers to scientists and people interested in astrophysics
worldwide.
We are putting in place a system where many scientists can use XRISM data to produce a wide varietyof scientific results.

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XRISM in the WorldInternational Collaboration
X-ray astronomy has advanced significantly since
the end of the 20th century and into the 21st century
with the launch of many X-ray astronomy satellites
with complementary abilities. The Chandra X-ray
Observatory satellite from the United States and the
XMM-Newton satellite from Europe both launched

Spectral capability@6keV

XRISM
Hard X-ray
focusing area
＠1keV

Field
of view

XMM

in 1999 and were each equipped with X-ray mirrorsthat produced the largest light-collecting area inthe history of X-ray astronomy. In addition to having
X-ray CCD cameras, each satellite has a dispersive
spectrometer with excellent spectral performance inthe low-energy band. However, neither has a highresolution spectrometer that is capable of imaging.
In 2012, the U.S. launched the NuSTAR telescope,enabling hard X-ray imaging. More recently, the U.S.
IXPE satellite launched in 2021 is expanding ourunderstanding of X-ray polarization. Each of these
X-ray astronomy satellites adds new capabilities to
how we understand the X-ray sky.

NuSTAR
ChandraSpatialresolution

Soft X-ray
focusing area
＠30keV

ChandraNuSTAR

XMM-Newton

XRISM

Comparison of the specialties of X-ray astronomical satellites in orbit

Scientists around the globe are anticipating the emergence of the high-precision X-ray spectral
observations expected with XRISM.
Featuring a cutting-edge X-ray microcalorimeter and CCD camera, XRISM will enable astronomers
to observe the X-ray universe in revolutionary new detail. Compared with previous technologies, theimproved spectral resolution with XRISM is equivalent to describing the world in fewer than 100 colors
or more than 2,000 colors. XRISM’s highly accurate measurements will reveal the temperature, ionization
state, and velocity of the rarefied, high-temperature gas (plasma) that makes up the bulk of matter in theuniverse, providing critical new clues to the many mysteries of space physics.
The XRISM mission is a joint JAXA-NASA partnership with support from astronomers worldwide. The
spacecraft and the instruments have been developed by the three space agencies of Japan, the UnitedStates, and Europe. More than 150 astronomers from Japan, the U.S., and Europe participated in the
project to plan the mission’s initial observations. They have been working on a detailed observation plansince the project's inception. After six months of initial observations, XRISM will be used as a generalpurpose X-ray observatory and will be open for public observations.

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History of X-ray Astronomy Spacecrafts in Japan
With 40 years of launching X-ray astronomy spacecraft, Japan has been consistently contributing to theworld of X-ray astronomy. Observatory instruments with the latest technology have been launched in thepast 6 spacecraft, providing new and never before seen views of the universe.

1979 HakuchoTenma 1983
(Pegasus in Japanese)
Launched:1983 / Ended:1988
The newly developed gas scintillation proportional counter
doubled the possible energy resolution, enabling moredetailed spectroscopy of X-ray sources. One of the main
outcomes of this was the discovery of X-ray emisson fromhot plasma along the Galactic ridge. This emission has
been observed by succeeding spacecraft to elucidate theorigin and nature of this emission. It remains one of the mostimportant research themes in X-ray astronomy to this day.

ASCA

1993

(Flying bird)
Launched:1993 / Ended:2001
The first satellite to carry an X-ray telescopeand X-ray CCD camera, dramatically
improving sensitivity. Major contributions
included the detection of general relativistic
effects near black holes through observationsof active galactic nuclei, providing direct
evidence to support the existence of supermassive black
holes at the centers of galaxies. International publicobservations were begun for the first time, and ASCA data
has been opened to and used by scientists worldwide, with anumber of thesis projects supported.

ASTRO-H 2016
Launched:February 2016
/ Ended:March 2016
Four distinct instruments were included
to explore the mysteries of dark matterand the co-evolution of galaxies andblack holes, which controls the growth of structurein the universe. The mission was terminated only a monthafter launch due to a mishap; however, ASTRO-H achieved
revolutionary measurements of the speed of plasma in galaxy
clusters and the abundance of heavy elements.

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit(swan in Japanese)
Launched:1979 / Ended:1985
Japan's first X-ray astronomy
spacecraft, named after the blackhole "Cygnus X-1". A modulation
collimator, invented by Dr. Minoru
Oda (the author of the black holethesis in 1971 and later, Director of ISAS), was loaded
onto the satellite, allowing the location of X-ray sources tobe determined with high accuracy. A number of new X-ray
bursts were found by this spacecraft, and this mission moved
Japanese X-ray astronomy to the forefront internationally.

1987 Ginga(Galaxy in Japanese)
Launched:1987 / Ended:1991
New instrumentation included
high sensitivity detectors.
Major outcomes included
the X-ray detection of supernova 1987A shortly after thecommencement of observations, and the discovery of many
candidate black holes. A full-scale international collaboration
begun with this spacecraft to develop the instruments withresearchers from all over the world. Dr. Masatoshi Koshibadetected neutrinos from supernova 1987A using Kamiokande
in Gifu prefecture, and was later awarded the Nobel Prize inPhysics for this discovery.

2005 Suzaku(Legendary bird, the guardian of
the universe)
Launched:2005 / Scientificobservations ended 2015.
An X-ray telescope withhigher sentivitity than ASCA
and instruments to cover a wider bandpass. The major
contributions of Suzaku were to detect non-equilibrium
ionized plasma in supernova remnants, research into cosmicray acceleration mechanisms by shock waves, the detectionof X-ray reflection nebulae, detection of active galactic nuclei,
elucidating the evolution of galaxy clusters by observing theheavy element distribution in their outer regions, and the X-ray
emission from magnetars (highly magnetized neutron stars)

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Science Objectives

Why do we observe the Universe in X-rays?
The XRISM mission’s objective is to observe high-temperature plasma in the universe.
Cosmic objects composed of this plasma exist at temperatures above 1 million kelvin (K).
By observing high-temperature plasmas, we can study black holes, neutron stars, whitedwarfs, supernova remnants, clusters of galaxies, and large groups of galaxies.
1

The processes that generate shorter wavelengths of electromagnetic radiation, or light,
require higher energy (temperatures). X-rays, which have shorter wavelengths than

2visible and ultraviolet light, are mainly emitted from materials hotter than a star’s surface,around 1 to 100 million K. Such high-temperature materials are in a plasma state as
ionized gas. A high-temperature plasma that emits X-rays can spread very quickly,
requiring a strong gravitational force to keep it from dissipating. Individual objects suchas white dwarfs, neutron stars, and black holes, which are very small and heavy, attract
hot plasma. Galaxies and galaxy clusters are also strong gravitational sources withhigh-temperature plasmas. Observing X-ray spectra allows astronomers to study this hot
plasma. Measuring characteristic X-ray energies specific to the elements in the plasma
allows researchers to analyze its elemental composition and ionization state.

3

4

XRISM is an X-ray astronomy observatory that simultaneously records X-ray images andspectra. XRISM has two X-ray instruments, Resolve – an X-ray microcalorimeter, and
Xtend – an X-ray CCD camera.
Resolve is more than 20 times more accurate in measuring the energies of individual
X-ray photons than previous instruments. This resolution represents a breakthrough in
X-ray instrument performance. Observing at such a high resolution enables astronomers
to detect rare elements in high-temperature plasmas and to measure Doppler shifts due
to plasma motion and gravitational fields with unprecedented precision.
Xtend has a wider field of view (38 arcmin square vs. 3 arcmin square for Resolve) andcan therefore capture larger celestial objects and their surroundings. Xtend’s technology
has been used in observatories for nearly 30 years, and its performance in orbit is wellknown.

5

6
1.NASA/CXC/M.Weiss 2.NASA/CXC/M. Weiss 3.X-ray: NASA/CXC/RIT/SAO/J.Kastner; Optical: NASA/ESA/AURA/STScI/Univ. Washington, B.Balick
4.X-ray: NASA/CXC/RIKEN/T. Sato et al.; Optical: NASA/STScI 5.X-ray: NASA/CXC/SAO; UV: NASA/JPL-Caltech; Optical: NASA/STScI; IR: NASA/JPL-Caltech
6.X-ray: NASA/CXC/Univ. of Chicago, I. Zhuravleva et al, Optical: SDSSXRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

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Science Objectives

The Assembly of Clusters of Galaxies

How have celestial objects in the universe been formed?
Dark matter, a mysterious and unseen material, fills
the universe. Astronomers think the gravitational
force of dark matter led to the formation of the Milky
Way galaxy and other celestial bodies. Researchers
also think the gravity of dark matter causes repeatedcollisions and mergers, creating more massive objects.
The largest of these objects are clusters of galaxies
that are still growing. The mass of a galaxy cluster
is 1,000 trillion times the mass of the Sun, and morethan 80% of it is composed of dark matter. In a galaxy
cluster, most of the ordinary matter we can detect,such as hydrogen, fills the cluster as a superheatedgas at tens of millions Kelvin. The mass that’s foundin stars is just a few percent of the total mass of thegalaxy clusters.

Galaxy cluster MAXS J0416 in multi wavelength
X-ray: NASA/CXC/SAO/G.Ogrean et al.; Optical: NASA/STScI; Radio:
NRAO/AUI/NSF

XRISM will feature the first instrument designed to precisely measure the velocity of the hot gas ofgalaxy clusters using X-rays. The large mass of the dark matter also causes the motion of the gas andgalaxies to have much higher velocities than what would be caused by the normal matter. Using the
X-ray emission lines created by the hot gas will allow astronomers to study its velocity, including thatcaused by turbulent motion. XRISM will allow us to directly observe the growth process of the largest
astronomical objects in the universe, galaxy clusters.
However, dark matter is not the only heating source ofgas in the centers of galaxy clusters. Galaxies typicallyharbor supermassive black holes billions of times themass of the Sun. When gas falls into the black hole,part of the released gravitational energy can heat thegas surrounding the galaxies in clusters. XRISM aims
to measure the velocity of the wind blowing out fromthe supermassive black hole at the center of galaxy
clusters.
Complex structure in the hot, X-ray emitting gas from close
to the black hole at the center of M87
X-ray: NASA/CXC/Villanova University/J. Neilsen

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Science Objectives

The Chemical Makeup of the Universe

Shortly after the Big Bang, there was only hydrogen, helium, and a small amount of lithium. Today's
universe has many more elements, such as oxygen, carbon, iron, and silicon. What was the "cosmic
recipe" that led to the chemical evolution of our present-day universe? This is one of the mysteries
XRISM will investigate.
During their lifetimes, stars slowly turn lighter elements into heavy ones through nuclear fusion. Heavy
elements are also synthesized at the moment of a supernova, which is a large explosion at the end ofa star's life. These explosions disperse the synthesized elements into space, enabling the universe to
evolve new structures, including solar systems like our own.
The ejecta scattered by a supernova explosion forms a shock wave in space at supersonic speeds ofseveral thousand kilometers per second. It expands as a ball of superheated plasma, called a supernova
remnant, which shines brightly in X-rays like cosmic fireworks. Spectra obtained through observations
with XRISM will allow astronomers to measure with unprecedented precision the fraction and diffusion
process of elements that have been unobservable until now, helping us determine the different elemental
abundances stars create.
Heavy elements scattered in supernova
remnants spread slowly through interstellar
space and are recycled as materials for newstars and planets. Earth and its inhabitants are"star children" formed of materials from paststars. Heavy elements seep into intergalactic
space and diffuse into the hot plasma thatfills the space between galaxies in galaxy
clusters. Since different stars and supernovae
produce different elements, we can examine
the patterns of their elemental compositions
in detail, gaining new insights into billions ofyears of elemental synthesis and the history of
the stars and supernovae that created them.

Supernova remnant SN 1572
X-ray: NASA/CXC/RIKEN & GSFC/T. Sato et al; Optical: DSSXRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

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Science Objectives

The Extremes of Spacetime

So-called compact objects create conditions in space that we can’t replicate on Earth. When a star burns
out its fuel gas and dies, it leaves behind an extremely dense and massive object. This object could bea black hole, neutron star, or white dwarf depending on the size of the star. We also find supermassive
black holes, which are millions to billions of times more massive than the Sun, at the centers of mostgalaxies. These "compact objects" can attract nearby gas due to their strong gravity, releasing enormous
gravitational energy and emitting X-rays. By observing these X-rays, we can study the phenomena that
occur in an environment of ultra-strong gravity, a process that cannot be made in a laboratory. We canuse these same observations to study the state and motion of matter and obtain clues to the propertiesof compact objects themselves.
Measuring the Rotation of a Black Hole and Revealing theStructure of Spacetime
The energy of X-rays emitted from a black hole's immediate vicinitychanges due to a spacetime distortion caused by the black hole's
strong gravity. The amount the X-ray energy changes depends
on how fast the black hole rotates. XRISM will measure the X-ray
energy from the gas just before it falls into the black hole to study
the structure of spacetime. The data from XRISM will allow us toestimate the black hole's rotation velocity and verify the general
theory of relativity.
Illustration of a black hole

Unraveling the Mechanism of Gas Ejection from Compact Objects
Gas-swallowing black holes and neutron stars often produce narrow jets that shoot out in opposite
directions at speeds close to the speed of light (about 300,000 km/s) and winds that blow out at
hundreds to tens of thousands of kilometers per second. How can gas be ejected at such high speeds
from a compact object whose gravity is so strong that it is supposed to pull in everything around it? The
mechanism behind this process is still unknown. Elements
in jets and winds absorb or emit X-rays of specific energy.
By precisely measuring the intensity and energy of theseabsorption and emission lines, we can determine howmuch of each element is present and how fast the jet
is moving. Astronomers hope to better understand themechanism behind these gas eruptions by analyzing thisinformation.

Illustration of the supermassive black hole at a galactic center©ESA/AOES Medialab

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Satellite

Architecture

XRISM is packed with state-of-the-art X-ray equipment and satellite technology that makes the science
possible.
Structural design
To point a long spacecraft to a target object with an accuracy of less than one arcminute, the structure isdesigned as follows:• Fixed Optical Bench (FOB ) on which the X-ray telescope is mounted• Eight side panels for various instruments• The lower structure, consists of a base panel connecting the optical bench and side panels with two typesof detectors, as well as a thrust tube with a lower-end ring connecting the satellite to the launch vehicle.
The optical bench is made of low thermal distortion structural material and designed to achieve highshape stability against environmental changes in orbit.
Thermal Design
The instruments' heat does not flow to the optical bench or base panel, where heat distortion isundesirable. Instead, the heat is exhausted from the radiant heat exchanger mounted on the side panel.
In addition, many heat pipes are mounted to transport the heat.
Position of Observational Instruments
The two X-ray telescopes are mounted
on an optical bench, facing the

XMA for Resolve

same direction and observing thesame object simultaneously. The
two detector systems, which detect
individual X-ray photons from the sky
one at a time, are mounted on thebase panel.

XMA for Xtend

Resolve(Soft X-ray Spectrometer)

Xtend(Soft X-ray Imager)

XRISM Architecture

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Satellite

Bus Components

Main Satellite System Configuration
1. Data processing system (DHS)The DHS handles communications between devices, telemetry recording and playback, automatic, autonomous operation of
the satellite, and various other processes to keep the satellite safe. It also receives GPS signals, determines time, position,and velocity, and provides time to the satellite.
2. Communication system (RF)The satellite communication system uses S-band and X-band communication equipment to provide telemetry, command, andranging signals necessary for satellite system operation.
3. Power supply system (EPS)The electrical power system (EPS) provides the power necessary for satellite operation in sunshine and shade.
4. Attitude and Orbit Control System (AOCS)
The AOCS determines the spacecraft attitude and performs three-axis attitude control to point at a specified object bycommand. The system performs attitude change maneuvers to change the pointing direction with the attitude accuracy
required by the observation equipment. It also conducts orbit control to avoid debris collisions.

System Block Diagram
SpaceWire is a spacecraft communication network used for data communication between components
on the spacecraft.
XANT1
XANT2

SANT1-A
SANT2-A

SANT1-B
SANT2-B

GPSA1
GPSA2

Soft X-Ray Telescope
Xtend-XMA

XHYB

SHYB-ASHYB-BXFIL

SLPF-A

SLPF-B

XPA

SDIP-A

SDIP-BToXMODSTRP-A

STRP-B

S/S

TCIM-X

TCIM-S-A

TCIM-S-B

SMU-A

SMU-B

SAP1
unregulated
50 voltage

SAP1
SAP1

PCU

SHNT1

SAP2

SHNT2

SAP2

NEAC

TOP PLATESXSFWM
GPSP
SXI-S

MSE

MSE

Xtend
SWR
DH ports (A/B)

BAT1/2
Li-IonBAT
100Ah×2systems

To
RCS PRS monitor

RCS
FDV1
GN2
N2H4

N2H4TNK

FDV2

LV1

LV2

SWR3-A,B

SXI-DE

JTD

CDA

CDB

XBOX

ADRC

FWE

PSP-A

PSP-B

PSU

SXSDISTSXSSWR-A

SXSSWR-B

M-HCE

SWR

SWR

SWR

SWR

AOCP-BSI Components

SWR2-A/B

SI Components

SWR
SI ports (A)ACIMACIMRW-A/B
RW-A/B

ACIMACIMIRU-A/B
IRU-A/B

ACIMMTQ-A/B

ACIMSTT1/2/3

STT
1/2/3

MTQZ
THR4-B

THR3-B

THR2-B

THR1-B

THR4-A

THR3-A

THR2-A

THR1-A

RW1/RW2/RW3/RW4
MTQX

PE

AC-NW

ACIMRCS-A/B

ACIMMPSU-A/B

CD

Resolve

SWR
AOCP-A

PRS
FLT

SWR

DH-NW

HCE-A/BFOB

SXSDWR

BASE PANELBCCU1/2

SAP2

Resolve-XMA

GPSL1/2

IRU-A/B

ACIMACIMSG-A/B
SG-A/B

DSSE
-A/B

GAS
-A/B
SpaceWire I/F Port
DR-A

DSSH
-A/B

DR-B

SpaceWire connection (DH-NW)SpaceWire connection (AC-NW)

From
ACIM-RCS-A

MTQY

3N-THRSWR
SI ports (B)RCS PRS monitor

SpaceWire connection (SI-NW)
I/F connection
Piping

System Block Diagram

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Mission Instruments
XMA

X-ray telescope that efficiently collects X-rays
Basics
X-ray Mirror Assembly (XMA) is a telescope that focuses
X-rays from a celestial object to obtain an image. XRISM isequipped with two identical XMAs, one for Resolve and one
for Xtend.
The XMAs were developed at NASA's Goddard Space Flight
Center (GSFC). Each consists of 203 thin reflector shells
nested coaxially (see photo).
Technology
The reflector aluminum substrates were made of three different
thicknesses (152, 229, and 305 µm), starting with thinnersubstrates in the inner parts of the mirror and progressively
thicker substrate toward the outer diameter of the mirror to
reduce distortion. X-rays from sources outside the field ofview are reduced by stray light baffles (pre-collimators) madeof cylindrical aluminum shells aligned above each reflector
shell. A thermal shield was attached to the front of the precollimator to stabilize the thermal environment of the XMA.
The thermal shield was made of 0.22 micron-thick aluminizedNASA

Focal length Diameter
5.6 m
45 cm

Number of Shells
203

polyimide film on a stainless-steel mesh to provide thenecessary strength and high X-ray throughput.

Angle of incidence isabout 1 degree

Twice reflected
inwardInstalling the XMA to the spacecraft
Optical axis

Aperture
diameter

Focal length

Focal plane
Detector

Rotating hyperboloid
Rotating paraboloid

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

X-ray focusing mechanism

21Mission Instruments
XMA

NASA

The reflectors for the XMA were made by dividing
the circumference into four sections. Each of the two
XMA units required 1,624 mirror segments. It took
five technicians about a year and a half to fabricate asufficient number of segments to construct the two XMA
units. The reflectors were fabricated using the epoxy
replica method. In this method, gold was deposited on
the surface of a glass tube, which was inexpensive andsmooth enough to reflect X-rays, and then peeled off withan aluminum substrate coated with an epoxy adhesive to
make the reflectors. By eliminating the polishing process,the production cost was significantly reduced. The photoshows a row of glass tubes with gold deposited on theirsurfaces.

The reflectors were held in the XMA housing by beams
with a tooth-like structure. One by one, the reflectors weremanually inserted into the grooves of the comb teeth (leftphoto). After all the reflectors were inserted, the positionof the beams was adjusted radially to align the reflectors
with the designed locations. Finally, the eight adjusted
housings were assembled to form the complete XMA.
Although this assembly was done entirely by hand, wewere able to adjust the housings to within 100 μm of thecorrect position.

NASA

The pre-collimator, heat shield, and heater were mounted
on top of the completed XMA (only the heat shield was
mounted just before delivery to the satellite). The XMA
was ready for shipment after undergoing environmental
tests such as thermal cycling, vibration tests, and several
months of X-ray irradiation tests. The photo shows XMA
being installed in the vacuum chamber of the 100-m X-ray
beamline at NASA's Goddard Space Flight Center for
X-ray irradiation testing. The data from the calibration test
will be used to interpret data obtained from astronomical
observations.

NASA

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Mission Instruments
Resolve

Soft X-ray spectrometer for ultra-precise energy measurement

6×6-pixel X-ray microcalorimeter array at the focusof an X-ray mirror assembly (XMA). It provides
unprecedented energy resolution (ΔE ≤ 7 eV at 6keV) over a wide observation bandwidth of 0.3-

X-ray

X-ray absorber(HgTe)
Adhesive(epoxy)Temperature
measurement unit
(Silicon Semiconductor
Thermometer)
Silicon structureand supernova remnants).
Technology
Detector: A microcalorimeter detector array of 36
pixels detects minute temperature rises caused
by incident X-ray photons. It consists of an X-ray
absorber made of mercury telluride (HgTe) anda silicon semiconductor thermometer, which iscooled to -273.1°C (0.05 Kelvin) to achieve highresolution spectroscopy. Non-X-ray events createdby cosmic rays passing through the detector are
identified and eliminated by a semiconductor
detector placed behind the array.
Cooling system: The cooling system consists ofan adiabatic demagnetizing refrigerator (ADR),
superfluid helium, a mechanical refrigerator,
and a vacuum-insulated container (dewar) thathouses and mounts the refrigerators to achieve
the detector's operating temperature (0.05 Kelvin).
The superfluid helium is gradually consumed
in orbit, but even after depletion, scientificobservations can continue due to the cryogenfree capability designed into the instrument.

Heat istransferred

Heat isreleased

12 keV. It is a non-dispersive spectrograph thatcan precisely observe point sources (e.g., neutronstars) and extended sources (e.g., galaxy clusters

Thermometer

Low-temperature heat sink

Mechanism of energy measurement. Figure corresponds to one
pixel of the detector.

Photograph of the detector. The 6×6 pixel in the center measures
5mm × 5mm
Contamination baffle
Reflector
Gate valve
ApA
CSI

Aperture baffle
DMS
OVCS
MVCS
IVCS
JTS

SC-A

1711 mm

The Basics
Resolve is a precision spectrometer with a

He tankzyx

JT cryocooler

MS vent pipe
(only partially shown)He vent pipe
(only partially shown)

Cooling System. Dewar's multi-layer shielding, multi-stagerefrigerator, and superfluid helium cool the detector (inside theCSI) to 0.05K.

Filter wheel: Three types of X-ray attenuation
filters will be installed to enable observationof the brightest celestial objects. It also has aradiation isotope (Fe-55) and modulated X-ray
sources (MXS) for in-orbit energy calibration.

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

Filter wheel. Four MXS in four locations on the left ring side.

23

Mission Instruments
Resolve

Staged Manufacturing and Testing under International Cooperation to Ensure Steady Development
Resolve, developed under international cooperation, was combined with overseas equipment in stages. Some foreigncomponents, such as the filter wheel developed by Europe (ESA/SRON), were attached to the satellite structure. In
contrast, the detector system and ADR were first integrated into a component called the calorimeter spectrometer
insert (CSI) (NASA). The CSI was directly integrated into the dewar in Japan. An aperture system consisting of a seriesof thermal blocking filters (NASA) were also installed in the dewar. Since these parts are not touched again after the
dewar was closed, they were carefully checked and mounted. Resolve was thoroughly tested prior to integration with thespacecraft. Testing spanned more than 5000 hours and was conducted in five major test period during which the
instrument was cooled to it’s operating temperature. The tests included vibration, thermal testing, instrument calibration,and interference mitigations.

The NASA-developed CSI was installed in a dewar
at SHI's Niihama Works in November 2019. The
photo on the left shows NASA and SHI engineers
working to install the CSI in the dewar. The photoon the right shows it after installation.

The superfluid helium in the dewar has the property of moving in a film-like patternalong the walls toward higher temperatures. Superfluid helium must be maintained in
the tank even in the weightlessness of orbit. A device called a film flow killer system
was installed to achieve this. The photo on the left shows that the dewar was tilted
to about 80° to simulate a zero-gravity environment. It was confirmed that the film
flow killer system functioned as expected to hold the superfluid helium and that theheat penetration into the helium tank functioned as designed. The knife-edge device
that is part of the film flow killer system was developed by Japanese scientists andfabricated in a clean room at JAXA by microfabricating a silicon substrate.

The left photo shows a Resolve subsystem test. An X-ray source for groundtesting was placed on top of the dewar with the detector section installed, andenergy calibration was performed. This test was essential to achieve the spectral
performance of Resolve, as it models the response of the detector's signal toincident X-rays, including gain scale and energy resolution. The response is slightly
variable in orbit and is compensated for using the onboard X-ray source. The MXS
method of operation and data calibration were also demonstrated.

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Mission Instruments
Xtend

Soft X-ray imaging system that takes images over a wide wavelength range
The Basics
Xtend's detector is a Japan-manufactured Soft X-ray Imager (SXI). Xtend has a field of view of 38×38
arcmin, the largest ever for an X-ray telescope, and can observe a field of view larger than the full moonat once. It has an advantage in the observations of extended objects. In addition, Xtend can support
Resolve's observations by capturing objects outside its field of view.
Technology
CCDs: Using a thick depletion layer, the Xtend's CCD can detect higher energy X-rays than conventional
X-ray CCDs. The fully depleted back-illuminated element has high quantum efficiency for low-energy
X-rays. The transfer electrode surface is not exposed to the outside world. It is highly resistant tomicrometeorite impact and radiation damage, which can cause functional failure.
Cooler: Xtend's CCDs are cooled to -110°C
using a single-stage Stirling refrigerator. Thisnot only suppresses dark currents but also
reduces performance degradation effects due
to radiation damage.
ASIC: Xtend is equipped with a dedicated ASIC
(Application-Specific Integrated Circuit) that
universities developed over ten years. This
allows the CCD output signal to be read out
CCD chips of Xtend. The silver part is the light-receiving surface.
efficiently and with low power consumption.
Improvements: Xtend's CCD design is almost thesame as that of ASTRO-H, a JAXA predecessor
mission that ended prematurely in 2016, but
two improvements have been made. The CCD'sinternal potential structure has been modified
to achieve higher charge transfer efficiency
and improved radiation tolerance. Furthermore,
visible light shielding performance is improved.
The shield suppresses the generation of false
signals originating from stray light in orbit.

Xtend being inspected prior to satellite mounting

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Mission Instruments
Xtend

A screening test was conducted to select the best CCD chips
to be installed in the satellite from many candidate elements.
In this test, we picked the four best CCDs for the flight byscoring various evaluation axes, such as energy resolution
and noise characteristics. Researchers and students from allover Japan worked together to carry out multiple tests andsimultaneously analyze data for performance evaluation.

The selected elements were assembled into the flighthousing and electronics, and then tested for integration andperformance evaluation of the imaging system. The X-ray CCD
camera requires the devices to be cooled below -100°C toreduce thermal noise, and the camera housing is evacuatedto prevent condensation.

Before installation on the spacecraft, Xtend had to passmechanical environmental tests to ensure that it would
maintain its imaging performance under the harsh spaceenvironment and vibrations experienced during launch. The
completed flight camera was subjected to a thermal vacuum
test to simulate the orbital temperature environment and asound and vibration test to simulate launch conditions toconfirm that there was no change in performance before andafter the tests. The series of tests were conducted at JAXA's
experimental facility, where young researchers and many
students played an active role. Xtend was then handed overto the satellite system in perfect condition.

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Science Operation

Toward Creating Scientific Results

The Basics
After the initial operations and performance verification phase of scientific observations, XRISM will
be open to the world as an observatory for international public observations. We believe that it is vitalfor XRISM to maximize its scientific output to make XRISM data available to scientists from various
backgrounds, not just members of the satellite development team. Experts review observation proposals
from guest observers, and XRISM observes the selected objects. The raw observation data will be
converted to calibrated data and distributed to the proposer. XRISM Science Operations Team supports
guest observation proposals and scientific observation plans, standardizes the format of observation
data, performs calibration, and provides helpdesk services. The quality of XRISM's scientific output
depends on the quality of XRISM's Science Operations.
System and Technology
XRISM science operations are carried out in cooperation with the data centers at JAXA, NASA, and ESA,
where observation proposals are publicly solicited and accepted by the three space agencies. Then, theselected proposals are compiled into a detailed daily operation plan at JAXA, the site of satellite operations.
The XRISM data will then be converted to an astronomical standard data format in Japan and sent to theUnited States for calibration and processing. The data are then distributed and archived in Japan andthe United States for easy handling by observers. The key is to ensure that the data and analysis tools
incorporate all of the expertise and knowledge of the satellite developers and that they are easy to handle.
Accurately determining the on-orbit characteristics of onboard instruments is called calibration. Calibration is
critical to improve the accuracy of spectral imaging capability. It
cooperates with Science Operation Team (SOT) together with the
Resolve and Xtend development teams. It is then made available
to the public in a form that guest observers can use. SOT will also
document the information needed for the analysis. SOT will thenInternational open observations

Guestobservers

Science observation plan

Operation (Observations)manage the website for researchers. After the data are presented
to the guest observers, helpdesks in Japan, the U.S., and Europe
will support the analysis process.

Data acquisition (Raw data)
Data
processing

Standard format data
Data
processing

Calibrated data

Furthermore, with the support of the Japan Society for the
Promotion of Science (JSPS), XRISM is developing a projectto strengthen the creation of scientific results and foster the
next generation of young researchers through international
collaboration. International symposia are held in Japan, the U.S.,
and Europe to promote exchanges with other wavelengths andtheoretical researchers.

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

Data archive

Guest
observers

Helpdesk

XRISM Science Operation Team・Science Operations Center・Science Data Center
・European Space Astronomy Centre

27

Science Operation

Toward Creating Scientific Results

Development Overview
For XRISM science operations, we are utilizing positive aspects of the ASCA, SUZAKU, and ASTRO-H science
operations while improving areas that had been overlooked. We worked with several subteams to refine the plan. We
have prepared for the post-launch science operations by developing new operation tools to improve maintainability while
taking advantage of the ASTRO-H's assets, optimizing the knowledge gained from the development of the onboard
instruments, and improving the analysis for more accurate analysis.

Scientific Operations TeamThe XRISM Science Operations Team was organized during the XRISM Team Meeting held in Nara, Japan in May 2018. The teamstarted with Japanese and U.S. members. Since then, the team has been preparing together, sharing information through weekly
conference calls between Japan and the United States. It is a challenging international cooperation because of the 13-14 -hourtime difference. As of 2023, we have a large group of nearly 30 members on the Japanese side alone.

Scientific Operations Readiness Boot Camp
The development of scientific operation tools has been conducted through online
discussions, debugging, and validation by developers meeting. To facilitatesmooth communication, the developers have gathered at JAXA once or twicea year for discussions and to work each development and validation milestone,
called “Boot Camps.” The photo was taken at the camp in September 2022.

Comprehensive Operability Test
In the final stage of preparation for scientific operations, a rehearsal simulating
actual processes was necessary after the tools and procedures were completed.
The photo shows the comprehensive operability test conducted in November
2022. Satellite and scientific operations personnel are working together. Throughrepeated rehearsals and training, preparations have been made to ensure thatscience operations will be reliable after XRISM is in orbit.

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Science Operation

Satellite Operations and Ground Systems

Operation
XRISM will operate using the antenna (USC station) at the Uchinoura Space
Center (USC) as its main station. Although each communication time is only
about 10 minutes, the USC station communicates with XRISM 4-5 times daily tocheck satellite status, replay recorded data, and send satellite control commands.
In addition, the XRISM team strengthened
the satellite monitoring system based on thelessons learned from the anomalies during
the ASTRO-H operation. The satellite will bemonitored by JAXA ground stations and NASAground stations as much as possible, for 10
minutes every 3 to 4 hours.

Testing of the ground systems

Development
Learning from the anomalies that occurred during the operation of ASTRO-H,
XRISM has introduced several features to the ground operation system to ensure
safe and reliable operation.
The first is the satellite simulator. This simulator simulates the onboard computers
for data processing, attitude, and orbit control
and runs the same software. The simulator isused for initial rehearsals of critical operations,as well as for confirming operational feasibility
and for training.
The other is the satellite automatic monitoring
system, which can immediately detect satellite
anomalies. The software is common to all
JAXA space science satellites and is alreadyin use on current satellites, but monitoring
rules will be developed for XRISM and refined
through ground tests.

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

Satellite simulator. The left terminal sends commands to the satellite
simulator, while the right is the satellite simulator itself.

29

XRISM Team
Participating Organizations
Japan Aerospace Exploration Agency (JAXA), National Aeronautics and Space Administration (NASA),
European Space Agency (ESA), Tokyo Metropolitan University, Kanto Gakuin University,
Miyazaki University, Saitama University,
SRON (Netherlands Institute for Space Research), University of Geneva, Canadian Space Agency,
Chuo University, Ehime University, Fukuoka University, Fujita Medical University, Hiroshima University,
Kagoshima University, Kanazawa University, Kansai Gakuin University, Kinki University, Konan University,
Kyoto University, Nagoya University, Nara University of Education, Nara Women's University, Japan Welfare University,
Osaka University, RIKEN, Rikkyo University, Rikkyo University, Shibaura Institute of Technology, Shizuoka University,
Tohoku Gakuin University, University of Tokyo, Tokyo University of Science, Waseda University,
University of Teacher Education, Kumamoto Gakuen University, Meiji University,
Gravitation AstroParticle Physics Amsterdam, Canadian Light Source Inc., University of Chicago,
University of Durham, European Sauther Observatory, Harvard-Smithsonian Center for Astrophysics,
Lawrence Livermore National Laboratory, Leiden University, University of Maryland,
Massachusetts Institute of Technology, University of Michigan, Saint Mary's University, University of Waterloo,
University of Wisconsin, Yale University

Project Manager

Hironori Maejima

Principal Investigator

Makoto Tashiro

Project Engineer

Ken-ichi Toda

Project Scientist

Kyoko Matsushita

deputy Project Scientist
Project Manager
co-PI
Mission Systems Engineer
Mission Scientist

Hiroya Yamaguchi
Lillian Reichenthal
Richard Kelley
Leslie Hartz
Robert Petre

JAXA/ISAS
JAXA/ISAS,
Saitama University
JAXA/ISAS
Tokyo University of
Science
JAXA/ISAS
NASA/GSFC
NASA/GSFC
NASA/GSFC
NASA/GSFC

Project Scientist

Brian Williams

NASA/GSFC

Project Scientist
deputy Project Scientist

Matteo Guainazzi
Elisa Costantini

ESA
SRON

Resolve
Instrument Manager(JAXA)

Yoh Takei

JAXA/ISAS

Instrument PI (JAXA)

Yoshitaka Ishisaki

Instrument sub-PI (JAXA)
Instrument sub-PI (JAXA)
Instrument Manager(NASA)
Instrument PI (NASA)
Lead Instrument Systems
Engineer (NASA)

Ryuichi Fujimoto
Masahiro Tsujimoto

Tokyo Metropolitan
University, JAXA/ISAS
JAXA/ISAS
JAXA/ISAS

Lillian Reichenthal

NASA/GSFC

Richard Kelley

NASA/GSFC

Gary Sneiderman

NASA/GSFC

Xtend
Instrument Manager

Hiroshi Tomida

Instrument PI

Koji Mori

Instrumet sub-PI

Hiroshi Nakajima

Former Instrument PI

Kiyoshi Hayashida

JAXA/ISAS
Miyazaki University,
JAXA/ISAS
Kanto Gakuin University,
JAXA/ISAS(Osaka University)

XRISM X-Ray Imaging and Spectroscopy Mission | Media Kit

Science/Mission Operations
Science Operation Center
Yukikatsu Terada
Lead (JAXA)
Science Data Center Lead
Matt Holland(NASA)
Mission Operations Lead Shin Watanabe

Saitama University,
JAXA/ISAS
NASA/GSFC
JAXA/ISASIn Flight Calibration Planning
Lead
Eric Miller
co-Lead
Makoto Sawada

MIT
Rikkyo University

Laboratory Astrophysics
Chair
Timothy Kallman
Vice Chair
Jelle Kaastra

NASA/GSFC
SRON

Science target category
Galactic Compact chair
Galactic Compact
co-chair
Galactic Diffuse chair
Galactic Diffuse co-chair
Extra-Galactic Compact
chair
Extra-Galactic Compact
co-chair
Extra-Galactic Diffuse
chair
Extra-Galactic Diffuse cochair

Chris Done

Durham University

Teruaki Enoto

Kyoto University

Aya Bamba
Paul Plucinsky

University of Tokyo
Harvard-Smithonian CfA

Yoshihiro Ueda

Kyoto University

Erin KaraMIT

Irina Zhuravleva

University of Chicago

Yutaka Fujita

Tokyo Metropolitan
University(As of June 2023)

30