研究者業績
基本情報
研究分野
1経歴
4-
2026年10月 - 現在
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2013年11月 - 2026年9月
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2011年4月 - 2013年10月
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2010年4月 - 2011年3月
論文
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The Astrophysical Journal 1001(1) 46-46 2026年4月3日Abstract The elemental abundances of the Fe-peak elements (such as Cr, Mn, Fe, and Ni) and Ti are important for understanding the environment of explosive nuclear burning for the core-collapse supernovae (CCSNe). In particular, the supernova remnant Cassiopeia A (Cas A), which is well known for its asymmetric structure, contains three “Fe-rich blobs,” and the composition of the Fe-peak elements within these structures could be related to the asymmetry of the supernova explosion. We report a highly asymmetric distribution of the Fe-peak elements in Cas A as revealed by XRISM observations. We found that the southeastern Fe-rich region has a significant Mn emission above the 4 σ confidence level, while the northwestern Fe-rich region has no clear signature. In addition to the significant difference in Mn abundance across these regions, our observations show that the Ti/Fe, Mn/Cr, and Ni/Fe ratios vary from region to region. The observed asymmetric distribution of Fe-peak elements could be produced by (1) the mixing of materials from different burning layers of the supernova, (2) the asymmetric distribution of the electron fraction in the progenitor star, and/or (3) the local dependence of the neutrino irradiation in the supernova innermost region. Future spatially resolved spectroscopy of Cas A using X-ray microcalorimeters will enable more detailed measurements of the distribution and composition of these elements, providing a unique tool for testing asymmetric supernova physics.
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UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XXIV 61-61 2025年9月29日
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Monthly Notices of the Royal Astronomical Society 541(2) 1403-1418 2025年6月28日ABSTRACT The Fe K$\alpha$ fluorescence line ($\sim 6.4$ keV) has been observed during solar and stellar flares. Two emission mechanisms of the Fe K$\alpha$ line, photoionization, and collisional ionization, have been discussed, and the aim of this work is to collect evidences for each mechanism employing a statistical correlation approach between the Fe K$\alpha$ line flux and rough flare properties. Here, we systematically searched the Neutron Star Interior Composition ExploreR (0.2–12 keV) archive data for the Fe K$\alpha$ line of RS Canum Venaticorum-type stars. Among our analysed 255 observation IDs with a total exposure of $\sim 700$ ks, we found 25 data sets (total $\sim 40$ ks) exhibiting the Fe K$\alpha$ emission line at 6.37–6.54 keV with its equivalent width of 44.3–578.4 eV: 18 observations during flares, six observations during unconfirmed possible flare candidates, and one at a quiescent phase. These observations indicate a positive correlation between the Fe K$\alpha$ line intensity ($L_{\rm{K \alpha } }$) and the 7.11–20 keV thermal plasma luminosity ($L_{\mathrm{HXR } }$) with its power-law index of $0.86 \pm 0.46$ (i.e. $L_{\mathrm{K \alpha } } \propto L_{\mathrm{HXR } }^{0.86\pm 0.46}$). This correlation in the range of the thermal plasma luminosity $10^{29-33}$ erg s$^{-1}$ is consistent with the photoionization origin of the line. On the other hand, the equivalent width of the Fe K$\alpha$ line ($\mathrm{EW}_{\mathrm{K \alpha } }$) has a negative correlation with the 7.11–20 keV thermal plasma luminosity with its power-law index of $-0.27 \pm 0.10$ (i.e. $\mathrm{EW}_{\mathrm{K \alpha } } \propto L_{\mathrm{HXR } }^{-0.27\pm 0.10}$). This anticorrelation is consistent with the decline of the fluorescence efficiency with increasing the stellar flare loop height. Furthermore, we found a signature of an absorption line at $6.38^{+0.03}_{-0.04}$ keV during a superflare of $\sigma$ Gem. The equivalent width of the line was $-34.7^{+2.03}_{-1.58}$ eV. We discuss the density of the Fe ions from the equivalent width using the curve of growth analysis.
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Publications of the Astronomical Society of Japan 77(Supplement_1) S154-S170 2025年6月6日Abstract Young supernova remnants (SNRs) provide crucial insights into explosive nucleosynthesis products and their velocity distribution soon after the explosion. However, these velocities are influenced by the dynamics of the circumstellar medium (CSM), which in young core-collapse SNRs originates from the progenitor’s late-phase mass loss. Cassiopeia A (Cas A), the youngest known Galactic core-collapse SNR, was studied to analyze the spatial distribution of silicon and sulfur radial velocities using two high-spectral-resolution observations from the XRISM/Resolve imaging spectrometer. Resolve’s capabilities enabled the detailed characterization of Si xiii, Si xiv, S xv, and S xvi lines, whose line shapes can be resolved and modeled using Gaussian radial velocity components. The radial velocities measured generally align with previous CCD-based results, confirming that they were not artifacts caused by blended lines or ionization variations. Modeling line profiles with two-component Gaussians improved fits in some regions, revealing distinct redshifted (back side) and blueshifted (front side) components only in a few specific areas. In most regions, however, both components were either both redshifted (north-west) or both blueshifted (south-east), consistent with the patchy ejecta shell morphology seen in optically emitting fast-moving knots. The individual line components revealed line broadening ranging from $\sigma _v \approx 200$ to $\sigma _v \approx 2000$ ${\rm km\, s^{-1 } }$. Components with $1000 \lesssim \sigma _v \lesssim 2000$ ${\rm km\, s^{-1 } }$ are consistent with previously determined reverse-shock velocities, suggesting non-equilibrated or partially equilibrated ion temperatures. Narrow components with small radial velocities found near Cas A’s projected center likely originate from shocked CSM plasma. But the low radial velocity and small $\sigma _v$ poses a challenge to identify these components with either the front side or back side of the SNR, or a blend of both sides.
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Publications of the Astronomical Society of Japan 77(Supplement_1) S144-S153 2025年5月28日Abstract The expansion structure of supernova remnants is important for understanding not only how heavy elements are distributed into space, but also how supernovae explode. The ejecta expansion structure of the young core-collapse supernova remnant Cas A is investigated, with Doppler parameter mapping of the Fe–K complex by the Resolve microcalorimeter onboard the X-ray Imaging and Spectroscopy Mission (XRISM). It is found that the Fe ejecta are blueshifted in the south-east and redshifted in the north-west, indicating an incomplete shell structure, similar to intermediate-mass elements (IMEs) such as Si and S. The Fe has a velocity shift of $\sim$1400 and $\sim$2160 km s$^{-1}$ in the north-west and south-east regions, respectively, with the error range of a few hundred km s$^{-1}$. These values are consistent with those for the IMEs in the north-west region, but larger than those for the IMEs in the south-east region, although the large error region prevented us from concluding which component has significantly higher velocity. The line broadening is larger in the center with values of $\sim$2000–3000 km s$^{-1}$, and smaller near the edges of the remnant. The radial profiles of the Doppler shift and broadening of the IMEs and Fe indicate that the Fe ejecta may expand asymmetrically as IME ejecta, although the large error regions do not allow us to confirm this. Moreover, we see little bulk Doppler broadening of the Fe lines in the north-eastern jet region whereas the IME lines exhibit significant broadening. No such narrow lines are detected in the north-west region. These findings suggest an asymmetric expansion of the ejecta potentially driven by large-scale asymmetries originating from the supernova explosion. This interpretation aligns with the large-scale asymmetries predicted by models of neutrino-driven supernova explosions.
MISC
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Conference Record of IEEE NSS-MIC2018 2018年12月1日
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2018年11月11日X-ray observations of supernova remnants (SNRs) in the last decade have shown<br /> that the presence of recombining plasmas is somewhat common in a certain type<br /> of objects. The SNR W49B is the youngest, hottest, and most highly ionized<br /> among such objects and hence provides crucial information about how the<br /> recombination phase is reached during the early evolutionary phase of SNRs. In<br /> particular, spectral properties of radiative recombination continuum (RRC) from<br /> Fe are the key for constraining the detailed plasma conditions. Here we present<br /> imaging and spectral studies of W49B with NuSTAR, utilizing the highest-ever<br /> sensitivity to the Fe RRC at > 8.8keV. We confirm that the Fe RRC is the most<br /> prominent at the western part of the SNR because of the lowest electron<br /> temperature (~ 1.2 keV) achieved there. Our spatially-resolved spectral<br /> analysis reveals a positive correlation between the electron temperature and<br /> the recombination timescale with a uniform initial temperature of ~ 4 keV,<br /> which is consistent with the rapid adiabatic cooling scenario as an origin of<br /> the overionization. This work demonstrates NuSTAR's suitability for studies of<br /> thermal emission, in addition to hard nonthermal X-rays, from young and<br /> middle-aged SNRs.
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2018, ApJL, 866, L26 2018年10月16日We report on NuSTAR observations of the mixed morphology supernova remnant<br /> (SNR) W49B, focusing on its nonthermal emission. Whereas radio observations as<br /> well as recent gamma-ray observations evidenced particle acceleration in this<br /> SNR, nonthermal X-ray emission has not been reported so far. With the<br /> unprecedented sensitivity of NuSTAR in the hard X-ray band, we detect a<br /> significant power-law-like component extending up to $\sim 20~{\rm keV}$, most<br /> probably of nonthermal origin. The newly discovered component has a photon<br /> index of $\Gamma =1.4^{+1.0}_{-1.1}$ with an energy flux between 10 and 20 keV<br /> of $(3.3 \pm 0.7) \times 10^{-13}~{\rm erg}~{\rm cm}^{-2}~{\rm s}^{-1}$. The<br /> emission mechanism is discussed based on the NuSTAR data combined with those in<br /> other wavelengths in the literature. The NuSTAR data, in terms both of the<br /> spectral slope and of the flux, are best interpreted as nonthermal electron<br /> bremsstrahlung. If this scenario is the case, then the NuSTAR emission provides<br /> a new probe to sub-relativistic particles accelerated in the SNR.
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2018年10月1日We present the results from the Hitomi Soft Gamma-ray Detector (SGD)<br /> observation of the Crab nebula. The main part of SGD is a Compton camera, which<br /> in addition to being a spectrometer, is capable of measuring polarization of<br /> gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray<br /> sources on the sky, and, the only source from which polarized X-ray photons<br /> have been detected. SGD observed the Crab nebula during the initial test<br /> observation phase of Hitomi. We performed the data analysis of the SGD<br /> observation, the SGD background estimation and the SGD Monte Carlo simulations,<br /> and, successfully detected polarized gamma-ray emission from the Crab nebula<br /> with only about 5 ks exposure time. The obtained polarization fraction of the<br /> phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1<br /> $\pm$ 10.6)% and, the polarization angle is 110.7$^o$ + 13.2 / $-$13.0$^o$ in<br /> the energy range of 60--160 keV (The errors correspond to the 1 sigma<br /> deviation). The confidence level of the polarization detection was 99.3%. The<br /> polarization angle measured by SGD is about one sigma deviation with the<br /> projected spin axis of the pulsar, 124.0$^o$ $\pm$0.1$^o$.
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日本天文学会年会講演予稿集 2018 228 2018年8月20日
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2018年5月29日We study X-ray spectra of four Narrow Line Seyfert 1 galaxies (NLS1s), Mrk<br /> 110, SWIFT J2127.4+5654, IGR J16185-5928, and WKK 4438, using Suzaku and NuSTAR<br /> data. The spectra of the four sources are reproduced with a model consisting of<br /> a cutoff power law component, a reflection component, and a soft excess<br /> component. The photon indices of all the sources are found to be ~ 2. The<br /> cutoff energies are constrained to be ~ 40 keV for Mrk 110, SWIFT J2127.4+5654,<br /> and WKK 4438, whereas a lower limit of 155 keV is obtained for IGR J16185-5928.<br /> We find that the NLS1s in our sample have systematically softer spectra and<br /> lower cutoff energies than Broad Line Seyfert 1 galaxies reported in the<br /> literature. We also perform spectral fittings with a model in which the cutoff<br /> power law is replaced with the thermal Comptonization model in order to<br /> directly obtain the electron temperature of the corona (kTe). The fits give kTe<br /> ~ 10-20 keV for Mrk 110 and SWIFT J2127.4+5654, and lower limits of kTe > 18<br /> keV for IGR J16185-5928 and kTe > 5 keV for WKK 4438. We divide the NuSTAR data<br /> of SWIFT J2127.4+5654 into three periods according to the flux. The spectral<br /> fits in the three periods hint that kTe is the lower in the higher flux period.<br /> The results of the four sources suggest a possible anti-correlation between kTe<br /> and the ratio of the luminosity of Compton up-scattered photons to the<br /> Eddington luminosity. The anti-correlation can be explained by a simple model<br /> in which electrons in the corona are cooled and heated through inverse Compton<br /> scattering and Coulomb collisions with protons, respectively.
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Publications of the Astronomical Society of Japan 70(2) 2018年3月1日
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Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 924 468-472 2018年1月1日
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Proceedings of SPIE - The International Society for Optical Engineering 10699 2018年1月1日
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Proceedings of SPIE - The International Society for Optical Engineering 10699 2018年1月1日
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Proceedings of SPIE - The International Society for Optical Engineering 10709 2018年1月1日
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Publications of the Astronomical Society of Japan 70(Special Issue 1) 2018年1月1日
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70(2) 2017年12月19日The present paper investigates the temperature structure of the X-ray<br /> emitting plasma in the core of the Perseus cluster using the 1.8--20.0 keV data<br /> obtained with the Soft X-ray Spectrometer (SXS) onboard the Hitomi Observatory.<br /> A series of four observations were carried out, with a total effective exposure<br /> time of 338 ks and covering a central region $\sim7'$ in diameter. The SXS was<br /> operated with an energy resolution of $\sim$5 eV (full width at half maximum)<br /> at 5.9 keV. Not only fine structures of K-shell lines in He-like ions but also<br /> transitions from higher principal quantum numbers are clearly resolved from Si<br /> through Fe. This enables us to perform temperature diagnostics using the line<br /> ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of<br /> the excitation temperature and ionization temperature in the Perseus cluster.<br /> The observed spectrum is roughly reproduced by a single temperature thermal<br /> plasma model in collisional ionization equilibrium, but detailed line ratio<br /> diagnostics reveal slight deviations from this approximation. In particular,<br /> the data exhibit an apparent trend of increasing ionization temperature with<br /> increasing atomic mass, as well as small differences between the ionization and<br /> excitation temperatures for Fe, the only element for which both temperatures<br /> can be measured. The best-fit two-temperature models suggest a combination of 3<br /> and 5 keV gas, which is consistent with the idea that the observed small<br /> deviations from a single temperature approximation are due to the effects of<br /> projection of the known radial temperature gradient in the cluster core along<br /> the line of sight. Comparison with the Chandra/ACIS and the XMM-Newton/RGS<br /> results on the other hand suggests that additional lower-temperature components<br /> are present in the ICM but not detectable by Hitomi SXS given its 1.8--20 keV<br /> energy band.
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70(2) 2017年12月15日The Hitomi SXS spectrum of the Perseus cluster, with $\sim$5 eV resolution in<br /> the 2-9 keV band, offers an unprecedented benchmark of the atomic modeling and<br /> database for hot collisional plasmas. It reveals both successes and challenges<br /> of the current atomic codes. The latest versions of AtomDB/APEC (3.0.8), SPEX<br /> (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band<br /> spectrum, and are in close agreement on best-fit temperature, emission measure,<br /> and abundances of a few elements such as Ni. For the Fe abundance, the APEC and<br /> SPEX measurements differ by 16%, which is 17 times higher than the statistical<br /> uncertainty. This is mostly attributed to the differences in adopted<br /> collisional excitation and dielectronic recombination rates of the strongest<br /> emission lines. We further investigate and compare the sensitivity of the<br /> derived physical parameters to the astrophysical source modeling and<br /> instrumental effects. The Hitomi results show that an accurate atomic code is<br /> as important as the astrophysical modeling and instrumental calibration<br /> aspects. Substantial updates of atomic databases and targeted laboratory<br /> measurements are needed to get the current codes ready for the data from the<br /> next Hitomi-level mission.
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70(2) 2017年12月7日We present Hitomi observations of N132D, a young, X-ray bright, O-rich<br /> core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a<br /> very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily<br /> detects the line complexes of highly ionized S K and Fe K with 16-17 counts in<br /> each. The Fe feature is measured for the first time at high spectral<br /> resolution. Based on the plausible assumption that the Fe K emission is<br /> dominated by He-like ions, we find that the material responsible for this Fe<br /> emission is highly redshifted at ~800 km/s compared to the local LMC<br /> interstellar medium (ISM), with a 90% credible interval of 50-1500 km/s if a<br /> weakly informative prior is placed on possible line broadening. This indicates<br /> (1) that the Fe emission arises from the supernova ejecta, and (2) that these<br /> ejecta are highly asymmetric, since no blue-shifted component is found. The S K<br /> velocity is consistent with the local LMC ISM, and is likely from swept-up ISM<br /> material. These results are consistent with spatial mapping that shows the<br /> He-like Fe concentrated in the interior of the remnant and the S tracing the<br /> outer shell. The results also show that even with a very small number of<br /> counts, direct velocity measurements from Doppler-shifted lines detected in<br /> extended objects like supernova remnants are now possible. Thanks to the very<br /> low SXS background of ~1 event per spectral resolution element per 100 ks, such<br /> results are obtainable during short pointed or slew observations with similar<br /> instruments. This highlights the power of high-spectral-resolution imaging<br /> observations, and demonstrates the new window that has been opened with Hitomi<br /> and will be greatly widened with future missions such as the X-ray Astronomy<br /> Recovery Mission (XARM) and Athena.
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70(2) 2017年11月21日We report a Hitomi observation of IGR J16318-4848, a high-mass X-ray binary<br /> system with an extremely strong absorption of N_H~10^{24} cm^{-2}. Previous<br /> X-ray studies revealed that its spectrum is dominated by strong fluorescence<br /> lines of Fe as well as continuum emission. For physical and geometrical insight<br /> into the nature of the reprocessing material, we utilize the high spectroscopic<br /> resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer;<br /> SXS) and the wide-band sensitivity by the soft and hard X-ray imager (SXI and<br /> HXI) aboard Hitomi. Even though photon counts are limited due to unintended<br /> off-axis pointing, the SXS spectrum resolves Fe K{\alpha_1} and K{\alpha_2}<br /> lines and puts strong constraints on the line centroid and width. The line<br /> width corresponds to the velocity of 160^{+300}_{-70} km s^{-1}. This<br /> represents the most accurate, and smallest, width measurement of this line made<br /> so far from any X-ray binary, much less than the Doppler broadening and shift<br /> expected from speeds which are characteristic of similar systems. Combined with<br /> the K-shell edge energy measured by the SXI and HXI spectra, the ionization<br /> state of Fe is estimated to be in the range of Fe I--IV. Considering the<br /> estimated ionization parameter and the distance between the X-ray source and<br /> the absorber, the density and thickness of the materials are estimated. The<br /> extraordinarily strong absorption and the absence of a Compton shoulder<br /> component is confirmed. These characteristics suggest reprocessing materials<br /> which are distributed in a narrow solid angle or scattering primarily with warm<br /> free electrons or neutral hydrogen.
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70(2) 2017年11月17日The origin of the narrow Fe-K{\alpha} fluorescence line at 6.4 keV from<br /> active galactic nuclei has long been under debate; some of the possible sites<br /> are the outer accretion disk, the broad line region, a molecular torus, or<br /> interstellar/intracluster media. In February-March 2016, we performed the first<br /> X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS)<br /> onboard the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275<br /> at the center of the Perseus cluster of galaxies. With the high energy<br /> resolution of ~5 eV at 6 keV achieved by Hitomi/SXS, we detected the<br /> Fe-K{\alpha} line with ~5.4 {\sigma} significance. The velocity width is<br /> constrained to be 500-1600 km s$^{-1}$ (FWHM for Gaussian models) at 90%<br /> confidence. The SXS also constrains the continuum level from the NGC 1275<br /> nucleus up to ~20 keV, giving an equivalent width ~20 eV of the 6.4 keV line.<br /> Because the velocity width is narrower than that of broad H{\alpha} line of<br /> ~2750 km s$^{-1}$, we can exclude a large contribution to the line flux from<br /> the accretion disk and the broad line region. Furthermore, we performed pixel<br /> map analyses on the Hitomi/SXS data and image analyses on the Chandra archival<br /> data, and revealed that the Fe-K{\alpha} line comes from a region within ~1.6<br /> kpc from the NGC 1275 core, where an active galactic nucleus emission<br /> dominates, rather than that from intracluster media. Therefore, we suggest that<br /> the source of the Fe-K{\alpha} line from NGC 1275 is likely a low-covering<br /> fraction molecular torus or a rotating molecular disk which probably extends<br /> from a pc to hundreds pc scale in the active galactic nucleus system.
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70(2) 2017年11月1日Extending the earlier measurements reported in Hitomi collaboration (2016,<br /> Nature, 535, 117), we examine the atmospheric gas motions within the central<br /> 100~kpc of the Perseus cluster using observations obtained with the Hitomi<br /> satellite. After correcting for the point spread function of the telescope and<br /> using optically thin emission lines, we find that the line-of-sight velocity<br /> dispersion of the hot gas is remarkably low and mostly uniform. The velocity<br /> dispersion reaches maxima of approximately 200~km~s$^{-1}$ toward the central<br /> active galactic nucleus (AGN) and toward the AGN inflated north-western `ghost'<br /> bubble. Elsewhere within the observed region, the velocity dispersion appears<br /> constant around 100~km~s$^{-1}$. We also detect a velocity gradient with a<br /> 100~km~s$^{-1}$ amplitude across the cluster core, consistent with large-scale<br /> sloshing of the core gas. If the observed gas motions are isotropic, the<br /> kinetic pressure support is less than 10\% of the thermal pressure support in<br /> the cluster core. The well-resolved optically thin emission lines have Gaussian<br /> shapes, indicating that the turbulent driving scale is likely below 100~kpc,<br /> which is consistent with the size of the AGN jet inflated bubbles. We also<br /> report the first measurement of the ion temperature in the intracluster medium,<br /> which we find to be consistent with the electron temperature. In addition, we<br /> present a new measurement of the redshift to the brightest cluster galaxy<br /> NGC~1275.
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70(2) 2017年10月12日Thanks to its high spectral resolution (~5 eV at 6 keV), the Soft X-ray<br /> Spectrometer (SXS) on board Hitomi enables us to measure the detailed structure<br /> of spatially resolved emission lines from highly ionized ions in galaxy<br /> clusters for the first time. In this series of papers, using the SXS we have<br /> measured the velocities of gas motions, metallicities and the multi-temperature<br /> structure of the gas in the core of the Perseus cluster. Here, we show that<br /> when inferring physical properties from line emissivities in systems like<br /> Perseus, the resonant scattering (RS) effect should be taken into account. In<br /> the Hitomi waveband, RS mostly affects the FeXXV He$\alpha$ line ($w$) - the<br /> strongest line in the spectrum. The flux measured by Hitomi in this line is<br /> suppressed by a factor ~1.3 in the inner ~30 kpc, compared to predictions for<br /> an optically thin plasma; the suppression decreases with the distance from the<br /> center. The $w$ line also appears slightly broader than other lines from the<br /> same ion. The observed distortions of the $w$ line flux, shape and distance<br /> dependence are all consistent with the expected effect of the resonant<br /> scattering in the Perseus core. By measuring the ratio of fluxes in optically<br /> thick ($w$) and thin (FeXXV forbidden, He$\beta$, Ly$\alpha$) lines, and<br /> comparing these ratios with predictions from Monte Carlo radiative transfer<br /> simulations, the velocities of gas motions have been obtained. The results are<br /> consistent with the direct measurements of gas velocities from line broadening<br /> described elsewhere in this series, although the systematic and statistical<br /> uncertainties remain significant. Further improvements in the predictions of<br /> line emissivities in plasma models, and deeper observations with future X-ray<br /> missions will enable RS measurements to provide powerful constraints on the<br /> amplitude and anisotropy of clusters gas motions.
担当経験のある科目(授業)
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物理科学課題研究 (京都大学)
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情報基礎演習 (京都大学)
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X線観測衛星による高エネルギー天文学実習 (京都大学)
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現代物理学実験 (京都大学)
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宇宙放射学ゼミナールIIＢ （X線） (京都大学)
共同研究・競争的資金等の研究課題
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日本学術振興会 科学研究費助成事業 2026年4月 - 2028年3月
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日本学術振興会 科学研究費助成事業 2025年4月 - 2027年3月
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日本学術振興会 科学研究費助成事業 2024年6月 - 2027年3月
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日本学術振興会 科学研究費助成事業 2022年4月 - 2026年3月
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日本学術振興会 科学研究費助成事業 2022年4月 - 2026年3月
社会貢献活動
3メディア報道
1その他
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2013年7月 - 2013年7月プレスリリース（朝日新聞、京都新聞、産経新聞、日本経済新聞、KBS京都）
