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Dr Yukikatsu Terada (Saitama University / JAXA)8/24/26, 10:00 AMOral
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Dr Shoji Ogawa (Tokyo University of Science)8/24/26, 10:20 AMInvited
XRISM is opening a new window on the X-ray spectroscopy of active galactic nuclei (AGNs), providing unprecedented views of the physical and chemical properties of gas in the vicinity of supermassive black holes. In this talk, I will review selected recent XRISM results on AGNs. Possible topics include the geometry and kinematics of circumnuclear material, elemental abundance ratios, and...
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Dr Kotaro Fukushima (Tokyo University of Science)8/24/26, 10:55 AMInvited
While many presenters at this conference are confined within the virial radius of the Milky Way, and even more seem to reside within the Galactic disk (surprisingly!), the scientific rationale of XRISM encompasses the circulation of matter and the transfer of energy on a cosmic scale. Achieving these objectives undoubtedly requires observations of extragalactic objects, including galaxies,...
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Hiroya Yamaguchi (ISAS/JAXA)8/24/26, 11:30 AMInvited
XRISM has opened a new era of high-resolution X-ray spectroscopy, providing unprecedented measurements of the dynamics, composition, and physical state of astrophysical plasmas. As the mission enters its extended phase, the key question is how to maximize its scientific legacy beyond the achievements of the initial observing program. In this talk, I will present the scientific strategy for...
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Asca Miyamoto (JAXA/ISAS)8/24/26, 1:30 PMOral
Cosmic dust is essential for star and planet formation, the formation of molecules, and the chemical evolution of galaxies. However, its primary production sites and formation mechanisms remain poorly understood. Dust-forming Wolf-Rayet (WR) binaries provide ideal laboratories for investigating dust formation conditions (Williams+2009). Among them, WR 140 is an ideal target because its orbital...
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Shun Inoue (Kyoto University)8/24/26, 1:45 PMOral
Pre-main-sequence stars exhibit strong magnetic activity (e.g., Koyama
et al. 1996), and increasing attention has been paid to how the resulting X-rays affect the chemical evolution of surrounding
protoplanetary disks (e.g., Washinoue et al. 2024). Although theoretical
and simulation studies have advanced rapidly, observational verification
remains limited.The Fe Kα emission line at...
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Yuken Ohshiro (The University of Tokyo)8/24/26, 2:00 PMOral
Accreting white dwarfs (WDs) in close binaries are key laboratories for studying binary evolution and accretion physics, yet their masses and accretion structures remain difficult to determine. In magnetic WDs, accreting gas is channeled toward the poles, forming accretion columns in which shock heating produces hot plasma that emits thermal X-rays. The orbital- and spin-phase dependence of...
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Dr Marina Yoshimoto (Ehime University)8/24/26, 2:15 PMOral
An X-ray binary is a system where mass and angular momentum are transferred from a companion star to a compact object through accretion, resulting in the emission of X-rays. We use spectroscopic techniques to measure its accretion geometry.
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AX J1910.7+0917 is known as the slowest X-ray pulsar, with a spin period of ~10 hr. In the PV phase, we serendipitously detected an outburst from AX... -
Dr Tomohiro Hakamata (ISAS/JAXA)8/24/26, 2:30 PMOral
Cyg X-3 is a high-mass X-ray binary (HMXB) consisting of a Wolf–Rayet (WR) star and a compact object. The dense stellar wind from the WR star is photoionized by X-rays from the compact object, producing numerous emission and absorption lines that probe the wind structure. Owing to the high spectral resolution of XRISM, several tens of spectral lines have been detected, providing effective...
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Gabriel Grell (NASA Goddard Space Flight Center)8/24/26, 2:45 PMOral
The helium-like K$\alpha$ line complexes are valuable diagnostics of electron density, temperature, and ionization conditions of astrophysical plasmas. The ratios of these lines can be altered by the presence of lithium-like ions, both through inner-shell ionization as well as resonant Auger-Meitner Destruction (RAD), in which the He-like intercombination lines are diminished by line...
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Chulsoo Kang (Ehime University)8/24/26, 3:15 PMPoster
High-inclination black hole X-ray binaries (BHXRBs) provide unique opportunities to investigate highly ionized disk winds. 4U 1630−472 is one of the most active BHXRBs, exhibiting outbursts repeatedly with an interval of about 600 days. Previous observations have revealed highly ionized absorption lines attributed to disk winds in this source. Here, we report a possible signature of a highly...
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Daiki Miura (The University of Tokyo, ISAS / JAXA)8/24/26, 3:15 PMPoster
In X-ray binaries, accreted plasma is photoionized by intense X-ray radiation from the vicinity of the compact object. While the geometry and dynamics of this plasma have been traditionally probed via absorption lines from highly ionized Fe ions, the recent detection of mildly-ionized Fe XVII-XXIV ions by XRISM/Resolve significantly expands our diagnostic capabilities. Resolving absorption...
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Kentaro Okada (Kindai University)8/24/26, 3:15 PMPoster
Characteristic X-ray emission from neutral iron is observed in the Galactic Center (Koyama et al. 1996, PASJ, 48, 249). Its spatial distribution is correlated with molecular clouds, and its main origin is thought to be photoionization by past flares of the supermassive black hole Sagittarius A (Sgr A). Compton scattering of the neutral iron $K\alpha$ line within molecular clouds produces a...
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Haruki Kuramoto (The University of Osaka)8/24/26, 3:15 PMPoster
To explain the hard X-ray emission of AGN, an extremely hot "corona" (electron
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temperature ~100 keV) has been introduced, but its heating mechanism remains
unknown. Determining the disk-corona geometry is key to understanding this heating
and cooling, and spectroscopy and polarimetry are the two most powerful probes:
spectroscopy uses the Fe fluorescence line to constrain the inner disk... -
Atsuya Uchida (Kyoto university)8/24/26, 3:15 PMPoster
In core-collapse supernovae, the Ni/Fe ratio is an indicator of the neutron excess near the core—set by electron capture and neutrino interactions—and thus serves as a probe of the explosion mechanism. This excess is imprinted on the iron-group elements: neutron-rich material yields stable isotopes such as ⁵⁸Ni rather than ⁵⁶Ni, so a high ratio directly signals neutron-rich ejecta. In...
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Kaname Ando (Saitama University)8/24/26, 3:15 PMPoster
Neutron stars (NSs) are degenerate stars that support their own mass by the degeneracy pressure of neutrons. They are key research objects not only in astrophysics but also in nuclear physics, especially in investigations of neutron-rich nuclei. Constraining their mass and radius observationally is important for constraining the equation of state of nuclear materials inside NSs.
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One effective... -
Kota Satomura (The University of Tokyo, ISAS / JAXA)8/24/26, 3:15 PMPoster
The physics of mass transfer and accretion flows in High-Mass X-ray Binaries (HMXBs) is the key to understanding binary evolution, including the formation of gravitational-wave progenitors. In particular, the neutral Fe Kα fluorescence lines originating from cool gas in stellar winds and accretion flows serves as a tracer of the matter distribution within these systems. Vela X-1, consisting of...
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Shintaro Kaneko (Rikkyo Univ.)8/24/26, 3:15 PMPoster
Transition-edge sensor (TES) microcalorimeters offer higher thermometric sensitivity than semiconductor-based microcalorimeters such as XRISM/Resolve, enabling superior energy resolution and scalable multiplexed arrays for future X-ray and soft gamma-ray missions. To advance their technological readiness, we operated approximately 200 TES pixels with microwave SQUID multiplexing in the...
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Leo Hirata (The University of Tokyo, ISAS / JAXA)8/24/26, 3:15 PMPoster
Accurate measurements of the intracluster medium (ICM) temperature are essential for understanding the dynamical state of galaxy clusters. XRISM/Resolve provides temperature diagnostics based on Fe K-shell line ratios independent of conventional collisional ionization equilibrium (CIE) model fitting. However, discrepancies between observed and CIE-predicted intensities of the Fe XXV Heα x,y...
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悠世 松村 (埼玉大学理工学研究科)8/24/26, 3:15 PMPoster
Supernova remnants(SNR) can generate reflected shock waves when they collide with molecular clouds. The existence of such reflected shock waves has been suggested for various celestial objects based on indirect evidence, such as temperature structures. However, there are currently very few examples of direct observations of plasma motion associated with reflected shock waves. Therefore, we...
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Daijiro Hitotsuyanagi (Kyoto University)8/24/26, 3:15 PMPoster
Young solar-type stars produce frequent and energetic stellar flares. By solar analogy, such energetic stellar flares can drive coronal mass ejections (CMEs) and energetic particles, potentially affecting exoplanetary atmospheres. Although stellar CMEs are difficult to detect directly, extreme-ultraviolet and soft X-ray coronal mass-loss dimmings are often observed in solar CMEs and may...
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Kai Matsunaga8/24/26, 4:15 PMPoster
Accretion disks in X-ray binaries regulate mass transfer onto compact objects and drive radiative and kinetic feedback to their surroundings. Here we report X-ray spectroscopy of the eclipsing neutron star low-mass X-ray binary AX J1745.6–2901 with XRISM/Resolve.
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The phase-averaged Fe~XXVI Ly$\alpha$ absorption profile exhibits two absorption minima with relative depths that are inconsistent... -
Guangyuan Zhao (Tokyo University of Science)8/24/26, 4:15 PMPoster
The Fe Kα line probes the structure and kinematics of circumnuclear gas around supermassive black holes. XRISM observed NGC 4151 fourteen times between December 2023 and December 2024. XRISM Collaboration (2024) and Miller et al. (2026) showed that its Fe Kα profile contains multiple velocity components, with contributions from the broad-line region (BLR) and the dusty torus. We then conducted...
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Keita Hasegawa (Kyoto University)8/24/26, 4:15 PMPoster
We present an XRISM/Resolve study of the eclipsing supergiant high-mass X-ray binary 4U$~$1538$-$522. The system consists of a neutron star and the B0.2 Ia supergiant QV Nor, and its nearly edge-on geometry makes it well suited for tracing fluorescent material through the orbital modulation of iron K-shell emission. XRISM observed the source for approximately 290 ks, covering about 90% of its...
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Jun Kurashima (University of Miyazaki)8/24/26, 4:15 PMPoster
Neutron-star kicks are thought to arise from asymmetric explosive mass ejection in core-collapse supernovae. X-ray studies have shown that intermediate-mass elements, such as Si and S, are preferentially expelled opposite to the direction of neutron-star motion in young supernova remnants, supporting a hydrodynamic origin of the kicks (Katsuda et al. 2018). Fe-rich ejecta, produced in the...
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Gen Fujimoto (Tokyo University)8/24/26, 4:15 PMPoster
Cosmic-ray acceleration is one of the long-standing unresolved problems in high-energy astrophysics. Galactic cosmic rays are widely considered to be accelerated at supernova-remnant shocks through diffusive shock acceleration. However, it remains unclear what physical conditions enable the efficient transfer of shock kinetic energy into non-thermal particles.
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To investigate these conditions,... -
Yuya Sakamoto (Tohoku University)8/24/26, 4:15 PMPoster
Active galactic nuclei (AGNs) are a key population for understanding the evolution of supermassive black holes (SMBHs). Although the broad-line region (BLR) and dusty torus serve as gas reservoirs, their compact structures remain poorly constrained. With high energy resolution, XRISM/Resolve can decompose the Fe K$\alpha$ line into multiple velocity components. However, linking these velocity...
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Dr Toshihiro Takagi (Ehime University)8/24/26, 4:15 PMPoster
SS 433 is a unique Galactic microquasar undergoing persistent supercritical accretion and launching relativistic baryonic jets. Its X-ray spectrum exhibits highly ionized Doppler-shifted emission lines from precessing bipolar jets. We present the emission-line profiles and their variability revealed by XRISM observations conducted to date, providing new insights into the structure and...
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Mr Itsuki Aihara (Tokyo University of Science)8/24/26, 4:15 PMPoster
Minor mergers can induce sloshing motions, leaving characteristic thermodynamic and kinematic signatures in cluster cores. A3571 is an X-ray-bright cluster at $z\sim0.04~(R_{500}=1.25~\mathrm{Mpc})$. Outside its central region, its thermodynamic structure resembles that of the Perseus cluster, despite the absence of a prominent cool core. We observed the central $\sim300~\mathrm{kpc}$ region...
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Nonoka Ishii (Department of physics, Kyoto University)8/24/26, 4:15 PMPoster
Type I bursts are transient explosions triggered by the thermonuclear burning of the accreted matter accumulated on neutron star (NS) surfaces. The accreted fuels burn through the $\alpha$-capture process branching from the hot CNO cycle, subsequently triggering hydrogen burning such as rapid-proton capture ($rp$) process. While burst light curves or fluences serve as useful probes for these...
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Osuke Akita (Saitama University)8/24/26, 4:15 PMPoster
Type Ia supernovae are explosive thermonuclear explosions in white dwarfs, and they play a important role in astrophysics, for example, as standard candles for measuring distances to distant objects. However, multiple scenarios have been proposed for the progenitor systems and explosion mechanisms of Type Ia supernovae, and many aspects remain unresolved. On the other hand, the velocity...
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Kazuya Nakayama (Kyoto University)8/24/26, 4:15 PMPoster
Algol is a well-known eclipsing binary system consisting of a B-type primary and a magnetically active K-type secondary star. Owing to the strong coronal activity of the secondary, Algol is one of the brightest stellar X-ray sources. During stellar flares, coronal plasma is rapidly heated to temperatures exceeding $10^7$ K, making high-resolution X-ray spectroscopy a powerful tool for...
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Yuma Aoki8/25/26, 9:30 AMOral
The Fe K$\alpha$ emission from the Sgr A complex is mainly attributed to irradiation by past Sgr A$^\ast$ activity. On the other hand, low-energy cosmic rays may also produce steady Fe K$\alpha$ emission through inner-shell ionization. Indeed, previous radio observations have suggested a high ionization rate due to low-energy cosmic rays in the Galactic Center region.
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The Fe K$\alpha_{3,4}$... -
Anje Yoshimoto (Nara Women's University)8/25/26, 9:45 AMOral
The origin of the Galactic Center X-ray Emission (GCXE) remains unclear. Although 10 – 40% of the GCXE has been resolved into detected point sources with Chandra, it is unknown whether the remaining emission originates solely from unresolved point sources or from truly diffuse plasma.
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Using the XRISM/Resolve data, we resolved the fine structures of the Fe-Heα and Fe-Lyα lines and measured... -
Yuki Omiya (ISAS/JAXA)8/25/26, 10:00 AMOral
Galaxy cluster mergers release enormous gravitational energy into the intracluster medium (ICM), driving bulk motions, shocks, turbulence, magnetic-field amplification, and particle acceleration. However, the connection between thermal-gas dynamics and diffuse radio emission remains poorly understood.
In this talk, I will present recent XRISM/Resolve results, focusing on Abell 3667. XRISM...
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Daisuke Ito (Nagoya University)8/25/26, 10:15 AMPoster
Observational evidence for the long-predicted "cooling flow" in the cores of galaxy clusters has rarely been found, and AGN are considered the most promising heating source suppressing this cooling.Understanding this AGN feedback requires knowledge of the velocity structure of the intracluster medium (ICM), which is a key physical parameter. M87, the central galaxy of the Virgo Cluster, is an...
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Yutaro Nagai (Kyoto University)8/25/26, 10:15 AMPoster
GX 301$-$2 is a massive X-ray binary hosting a $\sim$700 s neutron star and a B-type supergiant companion on a highly eccentric ($e \sim 0.46$), $\sim$42-day orbit. Past Chandra observations detected a Compton shoulder on its strong Fe K$\alpha$ fluorescence line, indicating dense scattering material near the neutron star, but limited CCD spectral resolution left the line profile and physical...
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Yoshizumi Okada (Aoyamagakuin university)8/25/26, 10:15 AMPoster
Collisionless shocks in astrophysical plasmas, such as supernova remnants (SNRs), are ubiquitous phenomena. The electron-to-ion temperature ratio immediately behind the shock is expected to be as low as their mass ratio, $\beta \equiv kT_{\mathrm{e}}/kT_{i} = m_{\mathrm{e}}/m_{i}$ in the extreme collisionless limit. However, SNR observations have revealed significantly higher values of...
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Haruto Higuchi (Tokyo University of Science)8/25/26, 10:15 AMPoster
The North Polar Spur (NPS), a bright X-ray and radio structure, has often been interpreted as the northern thermal limb of the eROSITA bubbles, attributed to an outflow from the Galactic Center. Using Suzaku observations, we found that the large-scale spatial distribution of Galactic soft X-ray emission can be described by three components: a Galactic halo, a disk-associated component, and a...
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Momo Hayashi (TUS)8/25/26, 10:15 AMPoster
Magnetic cataclysmic variables (MCVs) host a strongly magnetized white dwarf accreting gas from a companion star. The gas forms an accretion column with a standing shock near the magnetic poles. This column is the source of the X-ray emission.
Recent observations of AM Her with XRISM revealed a spin-phase dependence of the equivalent widths of the Fe XXV and Fe XXVI resonance lines (Terada...
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Kazuki Fujikawa (東京大学 理学系研究科)8/25/26, 10:15 AMPoster
PDS 456 is an extraordinary quasar hosting a super-Eddington accreting Active Galactic Nucleus (AGN). Its extreme accretion activity and powerful relativistic winds make it an ideal object for investigating AGN feedback and the physical mechanisms of mass ejection from supermassive black holes.
The X-ray observation satellite XRISM, launched in 2023, has an energy resolution approximately...
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Yuta Tsuchihashi (埼玉大学)8/25/26, 10:15 AMPoster
Accurate characterization and subtraction of background components in X-ray energy spectra are crucial for reliably detecting faint signals from astrophysical sources. During XRISM observation of M81 conducted between May 8 and 12, 2024, strong solar flares of up to X5.8 class occurred. The background spectrum observed by Xtend during this period shows an enhancement of the continuum X-ray...
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Riki Sato (The University of Tokyo)8/25/26, 10:15 AMPoster
Ultra-fast outflows (UFOs) are highly ionized accretion-disk winds in active galactic nuclei. A major unresolved question is how these outflows are accelerated. Proposed mechanisms include large-scale magnetic fields, radiation pressure, and magnetic reconnection.
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We investigate PDS 456 using a 500 ks simultaneous XRISM and NuSTAR observation. Broadband X-ray spectra reveal soft X-ray... -
Yugo Motogami (Saitama university)8/25/26, 10:15 AMPoster
T CrB is a symbiotic recurrent nova comprising a white dwarf (WD) and a red giant, with outbursts recorded in 1886 and 1946. Recent optical monitoring shows a decline after years in a high-luminosity state, similar to its pre-eruption behavior, suggesting another outburst in the near future. X-ray spectroscopy probes accretion flows and reflecting material near the WD. The origin of the 6.4...
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Keigo Okabe (Aoyama Gakuin University / ISAS)8/25/26, 10:15 AMPoster
High-mass X-ray binaries (HMXBs) consist of a neutron star or black hole and a companion star with a mass $\gtrsim10M_\odot$. Vela X-1 is a prototypical HMXB with a high inclination angle ($\gtrsim73^\circ$; e.g., van Kerkwijk et al., 1995), where the line-of-sight accretion structure varies with the orbital phase. In this work, we aim to investigate the spatial structures of photoionized...
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Naoya Ogura (The university of Tokyo)8/25/26, 10:15 AMPoster
Type Ia supernovae (SNe Ia) are thermonuclear explosions of white dwarfs and major producers of silicon, sulfur, and iron, yet how they explode remains unresolved. Probing the velocity distribution of a supernova remnant (SNR) is key to constraining its explosion mechanism and surrounding environment.
3C 397 is one of the most promising candidates for the explosion of a white dwarf close to...
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Mr Masaki Maekawa (Hiroshima University)8/25/26, 11:15 AMPoster
The low-mass X-ray binary GX340+0 is an extremely bright source near the Eddington limit. We analyzed data from the Resolve detector aboard the XRISM satellite. To eliminate the effect of dust scattering, we extracted data exclusively from the central 16 pixels. Because the source is highly luminous and the statistics when using only High-res data were insufficient, we applied a novel analysis...
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宇宿 智哉 (愛媛大学)8/25/26, 11:15 AMPoster
We present the results of simultaneous X-ray and optical spectroscopic observations of the microquasar SS 433 with XRISM/Resolve and the Seimei Telescope in 2024 and 2025. The X-ray jet emission lines exhibit single-peaked profiles, whereas the optical H$\alpha$ jet lines show one to three distinct components that form and decay on timescales of one to a few days. This contrast suggests that...
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Koh Sakamoto (Kyoto university)8/25/26, 11:15 AMPoster
Viewed nearly edge-on, Hercules X-1 undergoes deep X-ray eclipses that act as a natural coronagraph: with the bright continuum blocked, only the reprocessed emission from the accretion disk and disk wind remains. We present XRISM/Resolve spectroscopy of three eclipses of Her X-1 taken in September 2024. The $\sim$5 eV resolution cleanly separates the iron K complex into neutral fluorescence...
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Masaru Kato (Kindai University)8/25/26, 11:15 AMPoster
Low-ionization Fe $K\alpha$ emission has been detected from RS CVn-type stars during large flares. Its origin has often been attributed to fluorescence following photoionization of photospheric iron by hard X-rays from flare loops, although a contribution from non-thermal particles cannot be ruled out. During quiescence, however, the low-ionization Fe $K\alpha$ emission is weak, and only a few...
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Kazunori Suda (Tokyo University of Science)8/25/26, 11:15 AMPoster
XRISM observed the central $100\times100$ kpc region of the nearby cool-core
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cluster Abell 2199 (z=0.03). It revealed that the intracluster medium (ICM) redshift is consistent with that of the brightest cluster galaxy, within the optical-redshift uncertainty. This indicates that they form a kinematically coherent core system, which offset from the mean cluster redshift by... -
Hiroumi Matsuhashi (The university of Tokyo)8/25/26, 11:15 AMPoster
Xtend’s wide 38'×38' field of view (FoV) serendipitously captures other time-variable sources present during primary target observations. During AO1 N63A observations, the high-mass X-ray binary pulsar LMC X-4 serendipitously entered the FoV. While past studies of its 30-day superorbital modulation yielded only fragmented snapshots, we achieved unprecedented, continuous 8-day monitoring during...
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Tomohiro Suzumura (The University of Tokyo, ISAS/JAXA)8/25/26, 11:15 AMPoster
Supernova explosions drive the material circulation and structural evolution of galaxies by supplying heavy elements and injecting kinetic energy. Investigating the plasma states of supernova remnants and their ambient interactions is crucial to understanding explosion mechanisms and post-explosion asymmetries. Cassiopeia A (Cas A), a young corecollapse supernova remnant, provides an ideal...
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Aiko Miyamoto (The University of Osaka)8/25/26, 11:15 AMPoster
Understanding the distribution and kinematics of matter around active galactic nuclei (AGNs) is essential for elucidating how mass accretes onto central supermassive black holes. The neutral Fe Kα line in AGN X-ray spectra often shows both a broad component with velocity widths of several thousand km/s and a narrow component with widths of several hundred km/s, as increasingly revealed by the...
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Iroha Ichiseki (The University of Tokyo)8/25/26, 11:15 AMPoster
Type Ia supernovae are one of the key sites of iron-group element production, yet their explosion mechanisms and progenitors remain unresolved. In young Type Ia supernova remnants (SNRs), localized structures such as ejecta knots preserve imprints of the explosion and its environment. Their abundances, kinematics, and ionization states have stimulated diverse discussions on explosion models,...
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Koki Negishi (Meiji University)8/25/26, 11:15 AMPoster
High-resolution X-ray spectroscopy with XRISM has opened a new window on odd-Z nucleosynthesis by enabling the detection of emission lines from odd-Z elements such as P, Cl, and K, whose cosmic origins have remained largely unconstrained. To date, however, secure detections of these elements have been limited to the young Galactic supernova remnant Cassiopeia A. Extending such measurements to...
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Chintan Shah (NASA Goddard Space Flight Center)8/25/26, 1:30 PMInvited
High-resolution spectra from XRISM Resolve open a new window on astrophysical plasmas, but their diagnostic power depends critically on the accuracy of atomic data. In this lecture, I will introduce how laboratory measurements with electron beam ion traps (EBITs) provide benchmark data for interpreting X-ray spectra, including line ratios, ionization balance, and velocity diagnostics. I will...
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Erwin Lau (Nara Women's University)8/25/26, 2:30 PMInvited
Hot gas in galaxy clusters is often modeled as sitting in simple hydrostatic equilibrium, but real clusters are dynamically alive: turbulence and bulk flows left over from mergers and accretion provide additional, "non-thermal" pressure support that has long been a major uncertainty in cluster astrophysics and cosmology, simply because it could not be directly measured. XRISM's Resolve...
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Prof. Mauro Dadina (INAF)8/25/26, 3:45 PMInvited
This talk briefly traces the historical path that led to ESA’s NewAthena flagship mission for X-ray astronomy, framing its design within the broader development of high-energy astrophysics. After a swift look at this evolution, I will outline the major technical challenges involved in designing an observatory capable of addressing the astronomical community's fundamental questions. I will then...
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