International collaborations in space astronomy missions - past and future
Kazuhisa MITSUDA ATC, NAOJ, & ISAS, JAXA
第39回 天文学に関する技術シンポジウム January 17, 2020, at NAOJ, Mitaka Major X-ray astronomy missions in 5 decades (not all)
UFURU EXOSAT XMM-Newton
Ariel-5 ROSAT AstroSAT Beppo-SAX SAS-3 Granat HXMT Athena HEAO-1 Chandra X-IFU Einstein RXTE Swift Nustar
Japan-led missions Hitomi XRISM Suzaku ASCA
1980 1990 2000 2010 2020 2030
2 K. MITSUDA January 17, 2020, at NAOJ Mitaka Major/minor partners • All international space missions have a major parter and (a) minor partner(s). There is no mission with equal major partners. • A Japan-led mission = A mission in which Japan is the major partner • A major partner must take final responsibility to solve any problems, using its own resources. It usually bears more than half of the total cost including launch and science operations. • Japan built four X-ray astronomy missions with international collaborations. However, there is no participation as a minor partner so far. ESA’s Athena will be the first.
K. MITSUDA 3 January 17, 2020, at NAOJ Mitaka Japan’s space astronomy missions Hitomi XRISM Japan-led missions Athena Suzaku ASCA X-IFU X-ray Ginga Tenma Hakucho
IRTS Akari WFIRST Infra-red SPICA
Solar physics Minor-partner participation Hinotori Yohkoh Hinode EUVST
HALCA Radio
1980 1990 2000 2010 2020 2030 Similar situation in IR astronomy missions. 4 K. MITSUDA January 17, 2020, at NAOJ Mitaka International collaborations: why do we need?
• To perform the best investigations by most cutting-edge instruments. • Some of such instruments can be provided by partners. • It is becoming difficult to develop an instrument by one country because of increasing complexity and cost of not only the whole mission but also even of an instrument, e.g. Athena X-IFU
K. MITSUDA 5 January 17, 2020, at NAOJ Mitaka International collaborations: major and minor partners • As a major partner, • you can invite minor partners, who have technologies you do not have. • you have to optimize whole the system and decide interfaces. • you can use your own mission/product-assurance and quality- assurance requirements in your parts. • As a minor partner, • you can access high-quality data with relatively low cost, • you have to compete with other countries/agencies for your participation, (also, politics always applies) • interface may be given from the major partner, • you need to show your mission/product/quality-assurance requirements very clearly to the major-parter, or you will asked to follow their requirements. • you may be asked to show your technical details to the major parter. K. MITSUDA 6 January 17, 2020, at NAOJ Mitaka Japan’s space astronomy missions Hitomi XRISM Japan-led missions Athena Suzaku ASCA X-IFU X-ray Ginga Tenma Learning phase Hakucho
IRTS Akari WFIRST Infra-red SPICA
Solar physics Minor-partner participation Hinotori Yohkoh Hinode EUVST
HALCA Radio
1980 1990 2000 2010 2020 2030 Participating as a minor seems more difficult than as a major partner.
7 K. MITSUDA January 17, 2020, at NAOJ Mitaka Athena X-IFU A focal-plane instrument onboard ESA’s Athena mission
• Key technologies: The microcalorimeter onboard Hitomi/ • A ~3000-pixel TES XRISM has only 36 pixels. microcalorimeter array operated at 50 mK. • ~40-pixel signal multiplexing at a cryogenic temperature of 2 K.
A microcalorimeter detects a single X-ray photon as a heat pulse. Superconducting E quantum transition edge as a thermometer. C
G Simulated velocity map of bulk motions of hot plasma in cluster TB Peille et al. — Cucchetti et al.
K. MITSUDA 8 January 17, 2020, at NAOJ Mitaka X-IFU major contributors
Major Major responsibilities # of Co-I institution Systems engineering, Project CNES, IRAP management, Sub-K cooler, Room temp. 11 electronics SRON Detector assembly, signal multiplexing 7 All 4 institutions INAF Anti-co TES detector 7 developing TES X-ray micro NASA/GSFC TES microcalorimeter array 4 calorimeters for 1K/4K coolers space JAXA 4 SQUID array amplifiers for multiplexing Other 8 countries 12
total 45
SQUID= Superconducting Quantum Interference Device
K. MITSUDA 9 January 17, 2020, at NAOJ Mitaka Can Japan build a microcalorimeter Ospace Kα instrumentα alone? α
106 TES β α α Si K Mg K α β
TES detector for material analysis−1 developedSDD at Mitsuda/Yamasaki group JAXA Mg K Fe L Fe K Si K 105 Cu L keV Mounted on the ?STEM at NIMS in Tsukuba −1
O K α 8x8 TES array 104 α Si abs edge α Olivin sample
6 β K Kα 10 TES Mg abs edge α α Si K Mg K counts s α β
−1 SDD Mg K
1000 Fe L Fe K Si K 105 Cu L
keV ? 10 −1
4 100 Si abs edge SQUID array amp. K Kα Mg abs edge counts s 1000−10
(data−model)/error 0.2 0.5 1 5 5mm 10 Energy (keV) Hayashi+2018 Detector head@100mK0
−10
8x8 array, 4.8 eV(data−model)/error FWHM0.2 energy0.5 resolution1 5 (c.f. Hitomi/XRISM= 6x6 array, 5 eVEnergy FWHM) (keV)
K. MITSUDA 10 January 17, 2020, at NAOJ Mitaka Can Japan build a microcalorimeter8.4. SUMMARY space instrument alone? 85 80-ch microwave rf-SQUID multiplexer for X-ray TES (AIST and JAXA mitsuda/yamasaki group) 40ch microwave resonators 80 frequency combs MW in Flux Bias Chip Ramp in
TES TES bias 5.0 6.0 Frequency (GHz) Flux Ramp out close to the Athena X-IFU requirements MW out (40 pix MUX, 2.5 eV FWHM) 40ch microwave resonators Figure 8.14: The histogram of the energy resolution among all 38 pixels. 100mK stage 38-pixel summed spectrum Evaluation using a 32x32 TES array from SRON 3.4 eV FWHM X-ray pulse record Nakashima 2020 Mn Kα line
10 eV ch # ch
K. MITSUDA time 11 January 17, 2020, at NAOJ Mitaka
Figure 8.15: The combined energy spectrum from 38 pixels measured simultaneously with MWMUX readout. Can Japan build a microcalorimeter space instrument alone? • Engineering jump from laboratory technology proof-of-concept (TRL=3) to instrument working in the project environment, i.e. flight environment (TRL=5) is very large. A lot of high-quality engineering effort is Design of the X-IFU required, which astronomers cannot provide. detector head by SRON • JAXA does not have/provide engineer resources for cryogenic instruments. We thus need to collaborate with industry. • However, as far as I know, no industry in Japan can provide better cryogenic engineering than ourselves, in particular for TES. • Only solution is international collaboration for now. It is necessary to change this situation in order to make more essential contribution. One of my hope is ATC and engineers there. TRL=Technology Readiness Level K. MITSUDA 12 January 17, 2020, at NAOJ Mitaka Summary • Japan’s space astronomy missions adopted international collaboration from late 1980’s, with Japan as a major partner. • The situation is changing: it is likely that contribution to large space missions as a minor parter will become more common after 2020’s. • Participation as a minor parter is more difficult than as a major parter in some aspects. • Athena X-IFU will provide a good lessons. • Although at laboratory experiment level, the capabilities of instrument we developed in Japan are compatible with the requirements of the large mission, we can not construct a space instrument or its key component as a system by ourselves, because of lack of engineering power for space instrumentation. I hope to change such situation.
K. MITSUDA 13 January 17, 2020, at NAOJ Mitaka