Pos(MULTIF2019)041 , XRISM That Is a Successor of FORCE Produced Many New Scientiﬁc Results, Hitomi Project Has Been On-Going

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PoS(MULTIF2019)041 , XRISM https://pos.sissa.it/ that is a successor of FORCE produced many new scientific results, Hitomi project has been on-going. Following XRISM 0.9. A result is obtained to support that the Crab nebula − , but with much better spatial resolution of 15 arcsec in Hitomi 7% of that of the thermal pressure, is obtained, and the metal abundance in ICM is < ∗ 0.9, although they need further confirmation because of low statistical significance of 3- is the 6th Japanese X-ray astronomy satellite launched on 2016 Feb 17. Although it was − ishida@astro.isas.jaxa.jp . To fulfill the calorimeter science, the σ pressure, only owing to extremely high spectral resolution of the non-dispersive SXS detector (X-ray micro- Speaker. calorimeter). From the observations of the Perseus cluster, a stringent upper limit of the turbulent found consistent to that of the solarsmall vicinity. photon Power counts of is the demonstrated high in resolutionsearch N132D spectroscopy was even and performed with in IGR Crab J16318-4848. and G21.5 Emission/absorption line unfortunately lost about 1 month from the launch, was born from an electron-capture supernova.G21.5 New absorption line structures4 are detected from Hitomi we have started preparing the next generation hard X-ray mission HPD. They are planned to be launched by the end of March 2022 and late 2020’s, respectively. the hard X-ray imager onboard ∗ Copyright owned by the author(s) under the terms of the Creative Commons c ⃝ Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Manabu Ishida The Institute of Space and AstronauticalE-mail: Science / JAXA, Japan Multifrequency Behaviour of High Energy Cosmic3-8 Sources June - 2019 XIII - MULTIF2019 Palermo, Italy The scientific results from the X-rayHitomi observatory PoS(MULTIF2019)041 . Hitomi Manabu Ishida ]) are fabricated, 8

scientiﬁc instruments. ]) and Hard X-ray Tele- 3 , ]) are mounted on the focal Extensible 2 9 Optical Bench Optical Hitomi observatory Hitomi 1 Soft X-ray Telescope - I Soft X-ray Telescope - S Soft X-ray Telescope X-ray Telescope Hard ]) and the Soft X-ray Imager (SXI: [ 7 prior to the launch, is the 6th Japanese X-ray astronomy Overview of the ]) are attached onto side panels of the spacecraft. The SGD also 10 ASTRO-H observatory Figure 1: shows a schematic view of allocation of the Soft X-ray Imager Hard X-ray Imager Hard 1 Hitomi ]) are mounted on top of the optical bench. The SXT and HXT have equivalent 6 , Soft X-ray Spectrometer 5 , Soft Gamma-ray Detector 4 we show the energy band that is covered with all the detector systems onboard ]. Figure 2 , originally named 1 covers the band from 0.2 keV to 600 keV with moderate energy overlaps among the four In Fig. Hitomi respectively. On the other hand, the two Hard X-ray Imagers (HXIs: [ Hitomi detector systems. has two modules. All thesimultaneously. detector systems are co-aligned so that they can observe the same target scope (HXT: [ two modules each. The SXTs haveSXT-I, a the focal Soft length X-ray of Spectrometer 5.6 (SXS: m, [ and on the focal plane of the SXT-S and plane of the HXTs. Since theon focal a length separate of plate the connected HXTs atafter is the the as launch. end long of as In 12 the addition m, extensible toGamma-ray the optical the Detectors HXIs bench detector (SGDs: are systems (EOB), [ assembled with which focusing is optics deployed described above, the Soft 1. Introduction to Scientiﬁc results from Hitomi satellite developed by JAXA, underand vast so international on collaboration [ including NASA,Two ESA, kinds CSA of X-ray mirror assemblies, Soft X-ray Telescope (SXT:[ PoS(MULTIF2019)041 and Mar. 25 Mar. Chandra Manabu Ishida

in an extremely 3 was lost on 2015 Crab (PWN) T Hitomi SGD Mar. 20 Mar. detectors. detectors. G21.5-0.9 (PWN)

Soft Gamma-ray Detector Soft Gamma-ray Hitomi Hitomi , and it provides us with the highest Mar. 15 Mar. Hitomi RXJ1856-3754 (NS) HXI

2 Hard X-ray Imager Hard Mar. 10 Mar. SXI (HMXB) IGRJ16318-4848 Mar. 5 Mar. The energy band covered with the The energy band covered with the Soft X-ray Imager . Soft X-ray Spectrometer 3 50 mK. Since the heat capacity of a solid is proportional to Mar. 1 Mar. N132D (SNR) Figure 3: Figure 2: ∼ , we summarize the order of starting up the detector systems across the time line, shows the effective area of the SXT-S/SXS system for a point source and the energy- 3 4 observations and scientific results 2016 Feb. 25 SXS Perseus cluster Figure The Soft X-ray Spectrometer, or the SXS, is the X-ray micro-calorimeter which detects an In this paper, we hereafter concentrate on scientific results obtained with the SXS. This is In Fig. Hitomi low-temperature environment, it becomes possible tosingle detect X-ray tiny photon. temperature increase caused by a resolving power of the SXS, compared with those of the grating systems onboard X-ray photon as a slight(HgTe). increase For of this temperature to be of possible,to an the a X-ray temperature absorber absorber of is made thermally of connected to mercury a telluride heat sink which is cooled spectral resolution data that have never been achieved in the X-ray band above 2 keV. because the SXS is one of the main instruments of March 26th due toseveral malfunction pieces of in the its orbit. attitudetargets, & as During shown orbit one in Fig. month control from system, the and commissioning was start, broken we up have data into on six 2. 2.1 Summary of the observations and the Soft X-ray Spectrometer (SXS) together with targets in the field ofsioning view of that science is instruments common began among with the17th, the detector SXS followed systems. about by The one the commis- week SXI, after the HXI, launch and 2015 SGD February in this order. Unfortunately, Scientific results from Hitomi PoS(MULTIF2019)041 . 5 CCD 01756 . 0 Chandra . This is = Suzaku z Manabu Ishida 1250 = E ∆ / E 0*-#0.17<:1#4;#16" 0*-#0.17<:1#4;#16" # -0-#0)5;975#3966129:1;598!#%#$& ]). A couple of humps at apparent energies 11 ([ 3 (4#00/*#+=1 Suzaku (4#00/# )41 (4#* lines), respectively. A CCD camera, which is a standard imaging α ]). 11 and Ly above 0.6 keV. The energy resolution, on the other hand, is better with the 6.8 keV correspond to K-shell emission lines from He-like and hydrogenic iron α ':#00*** ,8#00*/ a) Effective area, and b) energy-resolving power of the micro-calorimeter SXS. ∼ . The effective are of the SXS is larger than the grating spectrometers of An X-ray spectrum of Perseus cluster taken with the SXS, together with that of the Figure 4: a) b) The Perseus cluster is the X-ray-brightest nearby galaxy cluster with a redshift 6.6 keV and XMM-Newton ∼ 30 times as powerful as that of the CCD cameras. 2.2 The Perseus cluster cameras for comparison ([ we show an X-ray spectrumtaken of with the the core XIS of (CCD Perseus camera) onboard cluster taken with the SXS, together with that Figure 5: of lines (so-called He detector widely used by current X-ray missions,species can in only resolve different emission ionization lines states. offrom the The same different atomic SXS, angular on momentum the states5.9 other of keV hand, the is can same 4.97 resolve ionization eV atomic in state. transitions FWHM, The which spectral means resolution the at energy resolving power XMM-Newton grating spectrometers in lower energy band. The SXS is more advantageous above 2 keV. In Fig. Scientific results from Hitomi and ∼ PoS(MULTIF2019)041 60 kpc ∼ ]. 13 Manabu Ishida b)

observed this cluster ~100 km/s detected a gradient of the Hitomi 6.62 K. 7 Hitomi ~200 km/s 6.60 10 × ! 5 6.58 " 6.56 3 arcmin region of Perseus cluster [

]. In panel a), × 13 *5/70;/>2/+ 4 1 ]. The velocity dispersion in panel b) is slightly 1 arcmin = 21 kpc 1 arcmin − 6.54 Energy (keV) ) relative to the cD galaxy NGC 1275. Thanks to 1 15 1 − − ! 6.52 16 km s 6 km s a) (Obs 3+4) ± ± α

6.50 16 km s = 13 ~ -60 km/s = 148 v bulk (!&) (!' (!'$ (!'& (!'( (!') (!( (!($ Fe He σ v 24301 counts 6.48 shows distributions of the bulk velocity and the velocity dispersion of across the cluster core. This can be interpreted as the sloshing motion % $ # " # 7

1 3 0 2 1 "!' #!'

0.5 1

1.5

ratio

omlzdcut s counts normalized keV

1 − 1 − −

7,916 /2/+ 5674,31

! ! # # ~ -60 km/s ]. Figure The SXS spectrum of the central 3 shows an SXS spectrum of the Perseus cluster averaged over the central ~ +40 km/s 13 6 [ 1 ] or a recent sub-cluster infall [ − examined motions of the hot gas within central 200 kpc region of the Perseus cluster 14 a) Bulk velocity and b) velocity dispersion of the central 200 kpc region of the Perseus cluster Figure 6: km s ]. Figure 6 1 arcmin = 21 kpc 1 arcmin Hitomi 13 , ]. 12 13 bulk velocity of 100 km s Figure 7: [ by AGN [ the central 200 kpc region of the Perseus cluster [ and energy widths ofany these significant lines, bulk respectively. velocity In (13 the central region, the hot gas does not show the high spectral resolution148 of the SXS, the velocity dispersion is successfully measured to be The cluster is filled with a hot plasma with a temperature of 2.2.1 Measurements of dynamical motions [ Scientific results from Hitomi for 290 ks in total. In this section we overview scientific results obtained from the Perseus cluster. region. A bulk velocity of the hot gas and its velocity dispersion are evaluated from centroids PoS(MULTIF2019)041 1 = − v σ if 27 . 2 Manabu Ishida b), and larger = 4 τ component of the ] for more detail. w 16 2 keV (Fig. ∼ ?5A%&368> E . It is confirmed that 8 is only 0.02-0.07. This implies that we need kT / 5 can be as large as unity. See [ ) 2 v τ σ ], + H G F 13 [ 2 bulk 100 kpc) indicates that its optical depth is 1 v − line region. The red curve shows the spectrum expected for the ( ∼ , plasma temperature of an X-ray-emitting hot plasma had been ( p ′ α m µ 3 at the center and the NW bubble, though it is less than 100 km s 1 -4@86&=?78<&E;B:?CB&2&<;>8& . 1B4B!&,&'(%&"&%+*&,&$!(% − ’s SXS, enable us to measure plasma temperatures through intensity ratios line region of iron has been carried out. The SXS spectrum, together with α XMM-Newton = 150-200 km s a) than any other high resolution spectrometer, and is the only non-dispersive ]. v 4 σ Hitomi and 16 The SXS spectrum of He line is really suppressed in the central region of the Perseus cluster. A radial profile of . Even if Chandra 1 α − Prior to the advent of the high resolution spectrometers, such as the grating spectrometers It has been pointed out that the cluster hot gas can be optically thick for the resonance scat- -component suppression out to 5 effective area (Fig. detector which is indispensable characteristic for diffuseto X-ray surely sources, make the SXS a has breakthrough beencan in expected be the measured X-ray through spectroscopy. a The spectroscopy following with kinds the of SXS. the temperature 0 km s w 2.2.3 Measurements of temperatures onboard of various lines. Since the SXS has better energy resolution above Figure 8: optically thin case [ iron He measured with a high-energy cutoff ofnow including a the continuum spectrum. The high resolution spectrometers, in the other observed region.less than Gaussianity 100 in kpc. the The line ICMrelative in profile to the the indicates Perseus thermal that cluster support is the quiet turbulence and scale the is dynamical support of the cluster tering. If so, theits intensity intensity of is the enhanced resonance inanalysis line the around the cluster is He outskirts. suppressed toward Inthe the order expected cluster to spectrum center see in whereas if red this color, is is true, shown a in detailed Fig. spectral 2.2.2 Resonance scattering enhanced to 100-200 km s Scientific results from Hitomi not take into account the dynamicalof motion dark of matter. the Perseus cluster hot gas in estimating the amount PoS(MULTIF2019)041 t e n and ]. α 17 keV, which 5 Manabu Ishida of silicon, for . α 7 Z T = > e ion z β for all the elements. In

α T T 1/2 α and Ly ) σ 2 th ion ≫ α σ T keV + 10 and the degree of ionization Fe XXV He 2 v ion Fe XXVI Ly Fe XXVI = Fe XXV He σ -5.0 e T e T of a Gaussian representing each T =( +5.3 σ = v th Ion mass (amu) v+th ), for example. This ratio depends σ σ σ Z 1 T of bright lines as a function of the ion mass in the atomic mass unit (amu). For clarity, the data points for = 7.3 → 3 ion α α best•fit best•fit best•fit best•fit = kT of the central region of the Perseus cluster in n Ca XX Ly Ca XIX He ion α 6 T . e is the elapsed time since the onset of the plasma heating. Ar XVII He β α T t α can be measured with an intensity ratio of emission lines S XVI Ly S XVI Ly can be measured with an intensity ratio of emission lines from S XV He β ··· σ ··· ) 5 ) Z is a kinetic temperature of an ion and can be measured through an e 30 40 50 60 T Si XIV Ly T The total velocity dispersion ··· that accurate measurements of the velocity dispersions of sulfur and ) 9 ion Left: T

400 300 200 100 Velocity dispersion (km/s) dispersion Velocity Fig. 9. is the electron density and e A chart of ion temperature measurement in the central region of the Perseus cluster[ n (associated with the electron transition ]. In this chart, the velocity dispersion —which is the β 17 He only upon the electron temperature of the plasma. The latter can be parameterized with so-called the ionization parameter Ion temperature ( energy width of any emission line. Ionization temperature ( Excitation temperature ( different excitation states of the same element in the same ionization state, such as He from different ionization states ofexample. the This same ratio element, depends such upon as an He electron temperature where [ As an example, we show measurement of 9 Figure 9: • • • calcium, in addition to thosethat of the calcium iron, lines are are indispensable. intrinsically very This weak, and is, we however, have hampered lost by significant amount the of facts the sulfur is consistent with the electronvelocities temperature. among Note different that elements weis for should understood measuring utilize from difference the of Fig. ion the temperature. thermal For this to be done, it emission line— of sulphur, calcium andtheir iron atomic in mass various unit ionization (amu). states This aremotion is shown and a as that root-mean-square a of associated function the with of width the stemmingline turbulent from motion is ion’s described thermal the in velocity §2.2.1. dispersion Ofand of them, the the the blue green turbulent dashed motion, dashed whichsolid curve curve is is is common the the among root-mean-square line of all them. width the The associated elements, best-fit with ion temperature the is ion’s thermal motion. The red Fig. In the case if the plasmathe is case in of complete shock-heated thermal ionizing equilibrium, plasma such as observed in SNR, Scientific results from Hitomi PoS(MULTIF2019)041 of β 5 keV) on 8.0 lines from Cr Manabu Ishida α emission lines from ) α β lines are only a few eV. (He triplet of Ni from He XXV α α Fe (w) XXVII Energy (keV) Energy Ni XXVII ], and the elemental abundance of + Ni 19 XXIV and Mn-K Fe α was still in the commissioning phase. The CCD spectrum (XMM-Newton) 7.4 7.6 7.8 0.5 0.2 0.1 TheHitomiSXS spectra theof Perseusa cluster. Conroy+2014 7 Hitomi I Fe (AGN) Figure1 Mernier+2016 XXIV ] Mn 18 a), as well as to discriminate He Perseus core (290 ks) Perseus core (150 ks) 44 objects (4 Ms) early-type galaxies 10 Si S Ar Ca Cr Mn Ni source is very important in that such possibility is denied at least for the XMM-Newton Sloan Digital Sky Survey (optical) Hitomi SXS Calibration

Energy (keV) Energy

ion T 2.5 2 1.5 1 0.5 0

, the SXS is able to unambiguously detect weak K XXIII (X/Fe) ratio abundance 10 Cr 5.5 6.0 c) a) b)

0.4 0.2

) keV s (counts Flux

–1 b). Note that the equivalent widths of Cr-K –1 c b The SXS spectra of a) Cr-Fe energy range, and b) Ni energy range. The weak K 10 Better energy resolution also contribute to enhance sensitivity to weak lines. As a matter of Since the cluster hot gas is formed through shock-heating of the cosmic primordial gas at abundances from Ca to Ni are updated. [ These observations resolved the Ni-overabundance problem[ Figure 10: and Mn are clearly detected. The panel c) shows metal abundances of the Perseus clusters evaluated. The the rare metals, Cr andFe Mn (Fig. (Fig. 2.2.4 Metal abundance in ICM fact, as shown in Fig. central region of the Perseus cluster. photons, for lower energy X-raysgate were valve, attenuated which by had the still beryllium been plate closed attached because on the Dewar’s around the virial radius, acceleratedshocked by ions the should cluster’s originally gravitational potential have much byratio. greater the thermal If dark energy matter, such than the energy theform imbalance electrons of ions’ remains, by dynamical their the motion. mass cluster ThisThe could should affect SXS have the measurement estimation a of of lot the of dark matter “hidden” in energy the universe. in the Scientiﬁc results from Hitomi large errors of the velocity dispersionsthe ion of temperature. sulfur and calcium result in the large error ( PoS(MULTIF2019)041 6.45 , and σ emission α Manabu Ishida (6.404 keV) 1 ]. The iron-peak 20 Fe-Kα ]. This claim raised a big ] a little more detail. 25 Energy (keV) Energy 27 ].

1 28 ]. There are three major plasma MOS [ . See [ (6.391 keV) 2 21 11 An SXS spectrum of a K Fe-Kα AGN + ICM continuum 6.1 6.15 6.2 6.25 6.3 6.35 6.4 0 ]. Among these plasma codes, however, there T

0.1 0.2

(FWHM) for the ﬁrst time. Note that a CCD keV Counts s Counts

-1 24 -1 1 XMM-Newton line from neutral iron fromgalaxy NGC the 1275 Perseus [ cluster’s cD Figure 12: 8 − % ], as shown in Fig. 7.1 keV. The SXS, however, does not show any sign of T line (6.40 keV) from an AGN has long been a matter of 26

∼ α shows the SXS spectrum of NGC 1275, the cD galaxy of the T T 12 T

], and CHIANTI[ % T 23 band 6.1-6.45 keV. The line is weak with an equivalent width of only α D x ]. The thick arrow indi- % 26 % ], ATOMDB[ 22 line from the cD galaxy NGC 1275 % α The SXS spectrum of the Perseus cluster D % T % ] for more detail about the plasma codes cross-calibration. The origin of the narrow iron K Now that we have a high resolution spectral data of the thin-thermal hot plasma in the Perseus It has been pointed out that there exists a possible 3.5 keV emission line in an integrated spec- 21 20 eV. Nevertheless, the SXS successfully detected the line at a confidence level of 5.4 this issue also in this field. Figure debate for a long time. The SXS high resolution spectroscopy showed its potential power to resolve ∼ 2.2.7 Fe K Perseus cluster, in the Fe K even measured its width to be 500-1,600 km s Figure 11: cates the location of the 3.5 keV line. still remain some 20% difference7.8 even keV). in The SXS the data well-studied on theto iron Perseus [ and cluster nickel are of emission great regions use (6.4- in resolving these differences. Refer emission line in the region 3.3-3.7 keV[ in the band 2.85-4.1 keV[ sensation, because it can beand interpreted as if a so, decay its of the mass dark is matter estimated candidate to “sterile neutrino”, be cluster, we can cross-calibrate so-called the plasma codes [ 2.2.6 Possible 3.5 keV line trum of 73 clusters of galaxies observed with the 2.2.5 Testing atomic codes the Perseus cluster is now revealed to be the same as the solar composition[ Scientific results from Hitomi elements (Cr through Ni) aregalaxies the with products various of redshift type and total Iathe mass SNe. universe with in Systematic the the iron observations future peak will of elements make clusters as it of a clear key. chemical evolution of codes: SPEX[ T % PoS(MULTIF2019)041 α 300 70 + − α 6.4 keV α Manabu Ishida S XV He 16 counts 1 − ] concluded that the line ) is different from that of 1 28 km s − ]. 620 30 +770 − km s line bands. Note that the bulk velocities 275 = 520 α . The grating spectrometers can do so for bulk 1 = + V =3 − is smaller than that of the broad line region v data, the authors[ 1 − 9 band of iron and sulphur, whose spectra are shown α α ]. The line width corresponds to a velocity of 160 Chandra 10,000 km s 31 [ ≥ 14 17 counts Fe XXV He . Similarity of its X-ray spectrum, including a 6.4 keV iron K 2 − 1 − cm 24 but only for bright sources. km s ]. The result therefore has rejected the possibility that the neutral iron 1 10 . − 1 810 29 × [ − +640 − 1 2 relative to the LMC’s rest frame ( − 4848 4848 is a high-mass X-ray binary (HMXB) that suffers extremely strong ab- ≃ 1 − − − H = 1140 N ]. We remark that, the bulk velocity of iron, measured from the line central energy, 1,000 km s 30 km s bulk The SXS spectra of N132D in the iron and sulphur K [ ≥ =3 V 640 810 13 + − IGR J16313 N132D is a young and O-rich core-collapsed supernova remnant (SNR) that is brightest among The measured velocity width 500-1,600 km s 140 , in Fig. emission line, which is shown in Fig. sorption with 2.4 IGR J16313 emission line, suggests this source todetected. be an Although accreting the X-ray SXS pulsar, yet exposuretitude no time control X-ray is pulsation like unfortunately has the very been case small, of again N132D, due we to still imperfect obtained at- 19 counts in total for an iron K Figure 13: 1 (BLR) 2,750 km s of iron and sulphur determined from the line central energy are different[ sulphur, which can be regarded asemission being originates at from rest the in supernova the ejecta LMCLMC, while frame. sulphur and emission This that comes result the from implies ejecta ISM thatnumber material is the of in counts iron highly can asymmetric. directly measure These velocitiesthanks of results to emission demonstrate lines the from that high extended even sensitivity objects of a like SNR, the very SXS small to the emission lines. emission line at 6.4 keVIn emanates combination from with the the BLR, or image the analysis accretion of disk in the case of NGC 1275. all SNRs in the Largethe Magellanic pointing Cloud (LMC). onto Although N132D onlyobtained due 3.7 in to ksec total exposure insufficient 17 is and calibration retained 16 of for counts the in attitude the He control system, we have 2.3 N132D observation can only measure the width Scientific results from Hitomi the width probably originates from a molecularseveral torus, hundred or km s a circum-nuclear disk, whose velocity is less than PoS(MULTIF2019)041 ). ], ⊙ and 32 [ M 3 made − ⊙ M cm parameter 10 ξ 1.8 Hitomi Manabu Ishida ]. Nomoto et 10 ]. 34 × ]. Together with [ 31 3 -ray flux and time, 1 36 γ − ≥ e band[ -ray precludes us from ]. The spectra in these n γ α 37 was not able to detect any emission line originates from α level [ Hitomi σ measured with the SXI and the HXI Fe I K ) ℓ 19 counts e n 4848 in the iron K − (= H 1 N − data, however, 10 ). From this ionization state, so-called Energy (keV) km s I–IV , typical of the core-collapsed SN, extensive search in 1 70 − (Fe +300 − 3 + km s parameter and ], and a maximum velocity of 2,500 km s 4 = 160 XMM-Newton ξ 33 σ E: 6405.4 ± 2.5 eV E: 6405.4 =3 V and

6.37 6.38 6.39 6.4 6.41 6.42 6.43

6 4 2 0 erg [ Counts 50 An SXS spectrum of IGR J16313 0.9 10 − Chandra × 1 < ) is confined. This Figure 14: 2 0.9 is one of the composite-type supernova remnants (SNRs) whose emission is dom- cm. These numbers indicate that the fluorescent iron K ℓ e − 13 , and X-ray have been made, but without success. The remaining space is the vicinity of n / α 10 , which is the most accurate and smallest width measurement that has ever been achieved. ] proposed that the Crab nebula was the remnant of an electron-capture supernova, which X . This result adds a new piece of support for the electron-capture SN picture. 1 L × ⊙ − Utilizing an extreme high sensitivity for emission/absorption lines of the SXS, The Crab nebula has been one of the observation standards for X-ray and G21.5 35 7 M = 1 ≤ ξ the central pulsar, but very intense radiation from the pulsar from radio to ℓ doing search for the ejecta. constrain the electron density and the scale of the fluorescing material to be a spectroscopic search for a hint of ejecta in the vicinity of the Crab pulsar [ ( al. [ To reinforce or deny thisthe idea, free it expansion is velocity important ofradio, to 10 H search the nebula for missing ejecta. Assuming is caused by electron capture in the O-Ne-Mg core of an intermediate mass progenitor (8-10 2.5 Crab and G21.5 This, together with the iron K-edgetion energy state measurement of made iron with is the not SXI, more results than in Fe the ioniza- a cold stellar wind from theof observing massive companion similar HMXB star. systems This with observation the provides XRISM strong mission motivation (§3.1). and its origin hasanomalous been aspects such believed as to having an be uncomfortably a small observed core-collapsed ejecta mass supernova 4.6 (SN). It has, however, some reevaluation of the emission/absorption line from the< Crab nebula. The obtained upper limit ofinated the by a ejecta pulsar mass wind is of nebula. absorption A lines blind at search 4.235 for keV the and emission/absorption 9.296 line detected keV a at couple more than 3 km s Scientific results from Hitomi kinetic energy PoS(MULTIF2019)041 in with XRISM XRISM Manabu Ishida , which is the abbre- ) is the next generation XRISM 0.9, and the screened Crab data. − shows an outlook of 16 . We do not adopt the high-energy instru- . Figure Hitomi 11 . Black, red, and blue respectively show the background- σ 0.9, the unfiltered G21.5 − . As can be seen from the spectra, both absorption lines are 0.9 in the spectral regions including the absorption lines 4.235 keV − 15 . The science instruments are three identical pairs of an X-ray mirror 17 . These sensors are stacked along the X-ray path from the mirror and . We have a micro-calorimeter system and a CCD camera. Both will be 0.9, whereas no such lines are seen in the Crab spectra. The origin of these made an extremely high resolution spectroscopy with a non-dispersive de- − Hitomi Hitomi Focusing On Relativistic universe and Cosmic Evolution Hitomi (= is shown in Fig. The SXS spectra of G21.5 X-Ray Imaging and Spectroscopy Mission FORCE Although FORCE hard X-ray mission now being plannedof in Japan in collaboration withand NASA’s GSFC. a An detector outlook that coverwith an a focal energy length range of of 12and m). 1-79 hence It keV we is with plan highly a difficult to to make focalcovering cover a the length the hybrid band low of detector 1-79 energy 10 comprising keV side, of with mas a an and (or single that SOI a two detector, (Silicon adopted CdTe, pairs On in covering Insulator) the CMOS, high energy side. The latter is the same 3.2 Focusing On Relativistic universe and Cosmic Evolution: FORCE lines are still unclear, although they may be due to absorption by neutron3. star’s atmosphere. Future missions 3.1 X-Ray Imaging and Spectroscopy Mission: XRISM detected from G21.5 tector inorbit for the firstIt time, is, its life, however, clearly just demonstrated onethe that month X-ray there for calorimeter. is the Motivated science surely by observations, a thisto was big fact, retrieve too discovery JAXA, the short. in space science collaboration to with with be theviation NASA, explored have calorimeter of with attempted with the recovery mission comparison with made under completely the same design as that of JAXA’s H-2A rocket by the end of Japanese fiscal year 2021 (March 2022). Figure 15: unsubtracted spectrum for the screened G21.5 ments HXT/HXI and SGD for reduction of the development cost. We plan to launch energy regions are shown in Fig. Scientific results from Hitomi and 9.296 keV. The significance levels are bot 3.65 PoS(MULTIF2019)041 is (58 arc- FORCE Manabu Ishida NuSTAR . . No HXI/SGD No ]) and 6 Hitomi below 10 keV. FORCE (1.7 arcmin [ XMM-Newton Hitomi in comparison with that of 12 XRIMS An outlook of the future hard X-ray mission An outlook of Figure 17: Figure 16: ]). A preliminary experiment has verified that the requirement of the HDP is met for a single The HPD of 15 arcsec is comparable with that of The X-ray mirror is a light-weight silicon mirror provided by NASA’s GSFC. A reflector sub- 38 Hitomi XRISM shell of the reflector. strate is lumbered from apolish, silicon Pt/C ingot, multilayer and is then applied onto polishedsitive the up at concave to high surface 79 mechanical of keV. accuracy. The the(HPD), requirement substrate After which of to is the the form better a angular than reflector that resolution of sen- is the 15 HXT arcsec onboard in half-power diameter embedded in a welldetector of system an is named active WHXI shield, (Wide-band Hybrid aiming X-ray at Imager). reducing non-X-ray background. The entire sec [ expected to carry out a highWith spatial such resolution high imaging spectroscopy spatial over resolution, 10main we keV objective for will of the be the first able mission time. to isscale. to carry complete out They a a include census lot identifying ofWay, of black revealing stellar-mass new holes the black science. across nature holes cosmic The that intermediate-mass timeblack original and holes are black in mass currently holes, the universe missing and over in the surveying redshift the accreting range from Milky supermassive 0 to 3. See the document by K. Mori in this Scientific results from Hitomi PoS(MULTIF2019)041 was lost Hitomi Manabu Ishida On-ground Hitomi ASTRO-H Hard X-ray that aims at recover- Ground-based x-ray FORCE at 6 keV) of the non-dispersive 250 , Journal of Astronomical Telescopes, , 1 = Society of Photo-Optical Instrumentation Journal of Astronomical Telescopes, E , ∆ / E . . 13 , but with much better spatial resolution of 15 arcsec Journal of Astronomical Telescopes, Instruments, and ) is not so high. , , vol. 9144 of σ , p. 914428. 2014. 10.1117/12.2056804. ]. Power of the high resolution spectroscopy even with 0.9. A result is obtained to support that the Crab nebula − 18 Hitomi , produced many new scientific results even within this short Society of Photo-Optical Instrumentation Engineers (SPIE) 12 [ (2018) 011210 (2018) 011213 4 4 . is now planned to be launched in late 2020’s. Hitomi 7% of the thermal pressure (§2.2.1) and the metal abundance in ICM Hitomi < , p. 914426. 2014. 10.1117/12.2054633. , vol. 9144 of line from the cD galaxy NGC 1275. Of them, the stringent upper limit of α FORCE (2018) 021402 papers of 4 project has been on-going to recover the remaining calorimeter science. Following is the 6th Japanese X-ray astronomy satellite developed in collaboration with US, Eu- Nature Instruments, and Systems (ASTRO-H) X-ray Astronomy Satellite Systems calibration of the Astro-H/Hitomi soft x-ray telescopes H. Awaki, H. Kunieda, A. Furuzawa, Y.Telescope Haba, (HXT) T. Hayashi, R. Iizuka et al., H. Mori, T. Miyazawa, H. Awaki, H.calibration Matsumoto, of Y. the Babazaki, Hitomi A. Hard Bandai X-ray et Telescopes al., R. Iizuka, T. Hayashi, Y. Maeda, M. Ishida, K. Tomikawa, T. Sato et al., Conference Series T. Takahashi, M. Kokubun, K. Mitsuda, R. L. Kelley, T. Ohashi, F. Aharonian et al., Y. Soong, T. Okajima, P. J. Serlemitsos,ASTRO-H S. Soft L. X-ray Odell, Telescope (SXT) B. D.Engineers Ramsey, (SPIE) M. Conference V. Gubarev Series et al., Instruments, and Systems XRISM 0.9, although their significance (3-4 , we started preparing the next generation hard X-ray mission [5] [4] [1] [2] [3] − References The Hitomi the turbulent pressure, only consistent to that of theas solar the two vicinity (§2.2.4) are particularly important, and they are published was born from an electron-captureG21.5 supernova. New absorption line structures are detected from small photon counts is demonstratedsearch in was performed N132D in and Crab IGR and J16318-4848. G21.5 Emission/absorption line XRISM ing the lost science of the HXI onboard in HPD. They are planned to be launched by the end of MarchReferences 2022 and late 2020’s, respectively. volume for full detail. 4. Summary Scientific results from Hitomi rope, and Canada, andon was 2016 launched March on 25th, 2016 aboutcontrol Feb 1 system. 17. month Nevertheless, from Unfortunately, however, thelife, launch, owing due to to extremely malfunction high of spectral resolution the ( attitude & orbit detector SXS (X-ray micro-calorimeter). The observations ofentific the results: Perseus cluster velocity, produce resonance many scattering, sci- 3.5 temperature, keV metal line, abundance, and test Fe of K atomic codes, PoS(MULTIF2019)041 . , 780 443 (2017) 478 Design and Journal of , Publ. Atron. X-ray , Manabu Ishida Inorbit (2016) 117 In-orbit (2003) 225 551 (2018) 021407 Hard x-ray 4 535 590 Phys. Rep. Astrophys. J. Publ. Atron. Soc. , ]. Origin of central , , Publ. Atron. Soc. Japan Nature Publ. Atron. Soc. Japan , , ]. , Nature . , (2018) 011212 4 Astrophys. J. , 1606.01165 [ 0909.5003 [ XMM-Newton Observations of the Perseus (2018) 021411 4 Early-type Galaxy Archeology: Ages, (2016) A157 (2009) L62 14 ]. 592 705 Journal of Astronomical Telescopes, Instruments, and ]. , ]. Shocks and cold fronts in galaxy clusters ]. ]. 1710.04648 . [ ]. ]. Astrophys. J. Lett. Astron. Astrophys. 1709.08829 , , [ ]. ]. ]. (2018) 10 Journal of Astronomical Telescopes, Instruments, and Systems 1712.06612 [ , 1711.00240 [ 70 1303.6629 [ (2018) 021410 astro-ph/0701821 (2018) 21 [ 4 70 (2018) 11 (2018) 9 1711.10035 1607.04487 astro-ph/0301482 1803.00242 70 (2014) 33 Soc. Japan [ F. Mernier, J. de Plaa, C.abundances Pinto, in J. the S. hot Kaastra, intra-cluster P. medium. Kosec,XMM-Newton Y. I. EPIC Y. Zhang Individual et and al., average abundance ratios from C. Conroy, G. J. Graves andAbundance P. Ratios, G. and van Effective Dokkum, Temperatures from Full-spectrum Fitting Hitomi Collaboration, F. Aharonian, H. Akamatsu,Solar F. abundance Akimoto, ratios S. of W. Allen, the L. iron-peak elements Angelini in et the al., Perseus cluster [ M. Markevitch and A. Vikhlinin, Hitomi Collaboration, F. Aharonian, H. Akamatsu,Measurements F. of Akimoto, resonant S. scattering W. in Allen, the L. Perseus Angelini Cluster et core al., with Hitomi SXS Hitomi Collaboration, F. Aharonian, H. Akamatsu,Temperature F. structure Akimoto, in S. the W. Perseus Allen, cluster L. core Angelini observed et with al., Hitomi E. Churazov, W. Forman, C. Jones and H. Böhringer, performance of Soft Gamma-ray Detector onboardAstronomical the Telescopes, Instruments, Hitomi and (ASTRO-H) satellite Systems T. Tamura, Y. Maeda, K. Mitsuda, A.Spectroscopy C. of Fabian, the J. Core S. of Sanders, theIntracluster A. Perseus Medium Cluster Furuzawa with et Suzaku: al., Elemental Abundances inHitomi the Collaboration, F. Aharonian, H. Akamatsu,The F. quiescent Akimoto, intracluster S. medium W. Allen, in N. the[ Anabuki core et of al., the Perseus cluster Hitomi Collaboration, F. Aharonian, H. Akamatsu,Atmospheric F. gas Akimoto, dynamics S. in W. Allen, the L. Perseus70 cluster Angelini observed et with al., Hitomi Cluster. I. The Temperature and Surface Brightness Structure H. Tajima, S. Watanabe, Y. Fukazawa, R. Bland ford, T. Enoto, A. Goldwurm et al., H. Nakajima, Y. Maeda, H. Uchida, T. Tanaka, H. Tsunemi, K. Hayashida et al., K. Nakazawa, G. Sato, M. Kokubun, T. Enoto, Y. Fukazawa, K. Hagino et al., [ M. A. Leutenegger, M. Audard, K.In-flight R. verification Boyce, of G. the V. calibration Brown, and M.Spectrometer performance P. Chiao, of M. the E. ASTRO-H Eckart (Hitomi) et Soft al., X-ray H. Matsumoto, H. Awaki, M. Ishida,performance A. of Furuzawa, the S. Hard Yamauchi, Y. X-ray Maeda TelescopeJournal et (HXT) of al., on Astronomical board Telescopes, the Instruments, Hitomi and (ASTRO-H) Systems satellite performance of the soft X-ray imagingJapan system aboard Hitomi (ASTRO-H) imager onboard Hitomi (ASTRO-H) Systems (2007) 1 [9] [8] [6] [7] [20] [19] [16] [17] [18] [15] [12] [13] [14] [11] [10] Scientific results from Hitomi PoS(MULTIF2019)041 , , , ]. 837 , (1997) 112 (2018) 13 ]. Annual Rev. Manabu Ishida , 70 The Crab 1508.07631 [ Publ. Atron. Soc. Japan Astrophys. J. Lett. , , ]. 1712.05407 CHIANTI - An atomic [ Astrophys. J. Suppl. , (2015) A56 ]. 582 (2018) 12 Publ. Atron. Soc. Japan 1207.0576 , [ ]. Updated Atomic Data and Calculations ]. 70 . A Search for “Dwarf” Seyfert Nuclei. III. SPEX: a new code for spectral analysis of X 1712.02365 [ . An Optical Study of the Circumstellar Environment (2012) 128 ]. 15 (1997) 354 Astron. Astrophys. 1707.00054 756 , [ Highlights from the X-ray Astronomy Satellite Hitomi 113 (2018) 16 (1982) 803 . 70 Recent developments concerning the Crab Nebula. astro-ph/0002374 [ ]. ]. 1402.2301 Publ. Atron. Soc. Japan 299 [ ]. , (2018) 14 Astron. J. Astrophys. J. , 70 , UV and X-ray Spectroscopy of Astrophysical and Laboratory Plasmas (1985) 119 Nature , , in 23 (2000) 861 (2014) 13 ]. , p. 46, Jun, 2017. XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop 1711.07727 [ 537 789 1607.07420 [ , in line emission from an active galactic nucleus α Publ. Atron. Soc. Japan , astro-ph/9704107 [ (2018) 17 1711.06289 315 Astron. Astrophys. 70 Astrophys. J. K. Nomoto, W. M. Sparks, R.Nebula’s A. progenitor Fesen, T. R. Gull, S. MiyajiHitomi and Collaboration, D. F. Sugimoto, Aharonian, H. Akamatsu,Search F. for Akimoto, thermal S. X-ray W. Allen, features from L.Publ. the Angelini Atron. Crab et Soc. nebula al., Japan with the Hitomi soft X-ray spectrometer K. Davidson and R. A. Fesen, J. Sollerman, P. Lundqvist, D. Lindler,Observations R. of A. the Chevalier, Crab C. Nebula Fransson, and T. R. Its Gull Pulsar et in al., the Far-Ultraviolet and in the Optical Hitomi Collaboration, F. Aharonian, H. Akamatsu,Hitomi F. observations Akimoto, of S. the W. Allen, LMC L. SNRejecta Angelini N et 132 al., D: Highly redshifted X-ray emissionHitomi from Collaboration, iron F. Aharonian, H. Akamatsu,Glimpse F. of Akimoto, the S. highly W. Allen, obscured L. HMXB Angelini IGR et J16318-4848 al., with Hitomi R. A. Fesen, J. M. ShullAround and the A. Crab P. Nebula Hurford, for X-Ray Spectroscopy database for emission lines. Version 8 (2017) L15 M. Ishida and Hitomi Collaboration, (ASTRO-H) (MULTIF2017) Hitomi Collaboration, F. Aharonian, H. Akamatsu,Hitomi F. observation Akimoto, of S. radio W. Allen, galaxy L. NGCof Angelini 1275: Fe-K et The al., first X-ray microcalorimeter[ spectroscopy L. C. Ho, A. V. Filippenko and W. L. W. Sargent, F. A. Aharonian, H. Akamatsu, F.Hitomi Akimoto, Constraints S. on W. Allen, the L. 3.5 Angelini, keV K. Line A. in Arnaud the et Perseus Galaxy al., Cluster A. R. Foster, L. Ji, R. K. Smith and N. S. Brickhouse, G. Del Zanna, K. P. Dere, P. R. Young, E. Landi and H. E.E. Mason, Bulbul, M. Markevitch, A. Foster,Detection R. of a. an K. Unidentified Smith, Emission M. LineAstrophys. Loewenstein in J. and the S. Stacked W. X-Ray Randall, Spectrum of Galaxy Clusters Spectroscopic Parameters and Properties of the Host Galaxies J. S. Kaastra, R. Mewe and H. Nieuwenhuijzen, Hitomi Collaboration, F. Aharonian, H. Akamatsu,Atomic F. data Akimoto, and S. spectral W. Allen, modeling L. constraintsPerseus Angelini from cluster high-resolution et with X-ray al., Hitomi observations of the & UV spectra. pp. 411–414, Jan, 1996. [35] [36] [31] [32] [33] [34] [30] [28] [29] [27] [24] [25] [26] [23] [21] [22] Scientific results from Hitomi PoS(MULTIF2019)041 70 Astrophys. , Manabu Ishida Publ. Atron. Soc. Japan , by JAXA as a project is July 2022. mission approved ? FORCE 16 FORCE ]. ]. When will the 1301.7307 [ We expect that the approval of 1802.05068 [ (2013) 103 770 J. F. A. Harrison, W. W. Craig, F.The E. Nuclear Christensen, Spectroscopic C. Telescope J. Array Hailey, (NuSTAR) High-energy W. W. X-Ray Zhang, Mission S. E. Boggs et al., Hitomi Collaboration, F. Aharonian, H. Akamatsu,Hitomi F. X-ray Akimoto, observation S. of W. Allen, the L. pulsar(2018) Angelini wind 38 et nebula al., G21.5-0.9 [37] [38] DISCUSSION JAMES HOWARTH BEAL: Scientific results from Hitomi MANABU ISHIDA: