掲載種別：研究論文（学術雑誌）   出版者・発行元：American Association for the Advancement of Science (AAAS)  

Active galaxies contain a supermassive black hole at their center that grows by accreting matter from the surrounding galaxy. The accretion process in about the central 10 parsecs has not been directly resolved in previous observations because of the small apparent angular sizes involved. We observed the active nucleus of the Circinus Galaxy using submillimeter interferometry. A dense inflow of molecular gas was evident on subparsec scales. We calculated that less than 3% of this inflow is accreted by the black hole, with the rest being ejected by multiphase outflows, providing feedback to the host galaxy. Our observations also reveal a dense gas disk surrounding the inflow that is gravitationally unstable, which drives the accretion into about the central 1 parsec.

DOI： 10.1126/science.adf0569

掲載種別：研究論文（学術雑誌）  

DOI： 10.1051/0004-6361/202347376

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

We investigated dusty and dust-free gas dynamics for a radiation-driven sub-parsec-scale outflow in an active galactic nucleus (AGN) associated with a supermassive black hole 10⁷M_⊙ and bolometric luminosity 10⁴⁴ erg s⁻¹ based on the two-dimensional radiation-hydrodynamic simulations. A radiation-driven “lotus-like” multi-shell outflow is launched from the inner part (r ≲ 0.04 pc) of the geometrically thin disk, and it repeatedly and steadily produces shocks as mass accretion continues through the disk to the center. The shape of the dust sublimation radius is not spherical and depends on the angle (θ) from the disk plane, reflecting the nonspherical radiation field and nonuniform dust-free gas. Moreover, we found that the sublimation radius of θ ∼ 20°–60° varies on a timescale of several years. The “inflow-induced outflow” contributes to the obscuration of the nucleus in the sub-parsec region. The column density of the dust-free gas is N_H ≳ 10²² cm⁻² for r ≲ 0.04 pc. Gases near the disk plane (θ ≲ 30°) can be the origin of the Compton-thick component, which was suggested by the recent X-ray observations of AGNs. The dusty outflow from the sub-parsec region can be also a source of material for the radiation-driven fountain for a larger scale.

DOI： 10.3847/1538-4357/accc2b

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/accc2b/pdf

掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

Dust-obscured galaxies (DOGs), which are observationally characterized as faint in the optical and bright in the infrared, are the final stage of galaxy mergers and are essential objects in the evolution of galaxies and active galactic nuclei (AGNs). However, the relationship between the torus-scale gas dynamics around AGNs and the DOGs’ lifetime remains unclear. We obtained the evolution of the spectral energy distributions (SEDs) of a galaxy merger system with AGN feedback from postprocessed pseudo-observations based on an N-body/smoothed particle hydrodynamics (SPH) simulation. We focused on a late-stage merger of two identical galaxies with a supermassive black hole (SMBH) of 10⁸M_⊙. We found that the infrared luminosity of the system reaches ultra- and hyperluminous infrared galaxy classes (10¹² and 10¹³L_⊙, respectively). The DOG phase corresponds to a state in which the AGNs are buried in dense gas and dust, with the infrared luminosity exceeding 3.3 × 10¹²L_⊙. We also identified subcategories of DOGs, namely bump and power-law DOGs, from the SEDs and their evolution. The bump DOGs tend to evolve to power-law DOGs over several Myrs. We found that contribution from the hot dust around the nucleus in the infrared radiation is essential for identifying the system as a power-law DOG; the gas and dust are distributed nonspherically around the nucleus, therefore, the observed properties of DOGs depend on the viewing angle. In our model, the lifetime of merger-driven DOGs is less than 4 Myr, suggesting that the observed DOG phase is a brief aspect of galaxy mergers.

DOI： 10.3847/1538-4357/ac87a2

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac87a2/pdf

掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

Abstract

A recent hydrodynamic model, the radiation-driven fountain model (Wada et al. 2016), presented a dynamical picture that active galactic nuclei (AGNs) tori sustain their geometrical thickness by gas circulation around AGNs, and previous papers have confirmed that this picture is consistent with multiwavelength observations of nearby Seyfert galaxies. Recent near-infrared observations implied that CO rovibrational absorption lines (ΔJ = ± 1, v = 0 − 1, λ ∼ 4.7 μm) could probe the physical properties of the inside tori. However, the origin of the CO absorption lines has been under debate. In this paper, we investigate the origin of the absorption lines and conditions for detecting them by performing line radiative transfer calculations based on the radiation-driven fountain model. We find that CO rovibrational absorption lines are detected at inclination angles θ_obs = 50°–80°. At the inclination angle θ_obs = 77°, we observe multi-velocity components: inflow (v_LOS = 30 km s⁻¹), systemic (v_LOS = 0 km s⁻¹), and outflows (v_LOS = −75, − 95, and −105 km s⁻¹). The inflow and outflow components (v_LOS = 30 and −95 km s⁻¹) are collisionally excited at the excitation temperatures of 186 and 380 K up to J = 12 and 4, respectively. The inflow and outflow components originate from the accreting gas on the equatorial plane at 1.5 pc from the AGN center and the outflowing gas driven by AGN radiation pressure at 1.0 pc, respectively. These results suggest that CO rovibrational absorption lines can provide us with the velocities and kinetic temperatures of the inflow and outflow in the inner few parsec region of AGN tori, and the observations can probe the gas circulation inside the tori.

DOI： 10.3847/1538-4357/ac755f

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac755f/pdf

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：EDP SCIENCES S A  

Aims. We investigate the physical properties - such as the stellar mass (M-*), star-formation rate, infrared (IR) luminosity (L-IR), X-ray luminosity (L-X), and hydrogen column density (N-H) - of mid-IR (MIR) galaxies and active galactic nuclei (AGN) at z < 4 in the 140 deg(2) field observed by eROSITA on SRG using the Performance-and-Verification-Phase program named the eROSITA Final Equatorial Depth Survey (eFEDS).Methods. By cross-matching the WISE 22 mu m (W4)-detected sample and the eFEDS X-ray point-source catalog, we find that 692 extragalactic objects are detected by eROSITA. We have compiled a multiwavelength dataset extending from X-ray to far-IR wavelengths. We have also performed (i) an X-ray spectral analysis, (ii) spectral-energy-distribution fitting using X-CIGALE, (iii) 2D image-decomposition analysis using Subaru Hyper Suprime-Cam images, and (iv) optical spectral fitting with QSFit to investigate the AGN and host-galaxy properties. For 7088 WISE 22 tim objects that are undetected by eROSITA, we have performed an X-ray stacking analysis to examine the typical physical properties of these X-ray faint and probably obscured objects.Results. We find that (i) 82% of the eFEDS-W4 sources are classified as X-ray AGN with log L-X > 42 erg s(-1); (ii) 67 and 24% of the objects have log (L-IR/L-circle dot) > 12 and 13, respectively; (iii) the relationship between L-X and the 6 mu m luminosity is consistent with that reported in previous works; and (iv) the relationship between the Eddington ratio and N-H for the eFEDS-W4 sample and a comparison with a model prediction from a galaxy-merger simulation indicates that approximately 5.0% of the eFEDS-W4 sources in our sample are likely to be in an AGN-feedback phase, in which strong radiation pressure from the AGN blows out the surrounding material from the nuclear region.Conclusions. Thanks to the wide area coverage of eFEDS, we have been able to constrain the ranges of the physical properties of the WISE 22 mu m-selected sample of AGNs at z < 4, providing a benchmark for forthcoming studies on a complete census of MIR galaxies selected from the full-depth eROSITA all-sky survey.

DOI： 10.1051/0004-6361/202141547

Web of Science

掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

<title>Abstract</title>
We investigate how magnetically driven outflows are powered by a rotating, weakly magnetized accretion flow onto a supermassive black hole using axisymmetric magnetohydrodynamic simulations. Our proposed model focuses on the accretion dynamics on an intermediate scale between the Schwarzschild radius and the galactic scale, which is ∼1–100 pc. We demonstrate that a rotating disk formed on a parsec-scale acquires poloidal magnetic fields via accretion, and this produces an asymmetric bipolar outflow at some point. The formation of the outflow was found to follow the growth of strongly magnetized regions around disk surfaces (magnetic bubbles). The bipolar outflow grew continuously inside the expanding bubbles. We theoretically derived the growth condition of the magnetic bubbles for our model that corresponds to a necessary condition for outflow growth. We found that the north–south asymmetrical structure of the bipolar outflow originates from the complex motions excited by accreting flows around the outer edge of the disk. The bipolar outflow comprises multiple mini-outflows and downflows (failed outflows). The mini-outflows emanate from the magnetic concentrations (magnetic patches). The magnetic patches exhibit inward drifting motions, thereby making the outflows unsteady. We demonstrate that the inward drift can be modeled using a simple magnetic patch model that considers magnetic angular momentum extraction. This study could be helpful for understanding how asymmetric and nonsteady outflows with complex substructures are produced around supermassive black holes without the help of strong radiation from accretion disks or entrainment by radio jets such as molecular outflows in radio-quiet active galactic nuclei, e.g., NGC 1377.

DOI： 10.3847/1538-4357/ac38a8

arXiv

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac38a8/pdf

記述言語：英語  

DOI： 10.3847/1538-4357/ac3cb9

記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1093/pasj/psab065

DOI： 10.1051/0004-6361/202141075

記述言語：英語   掲載種別：研究論文（学術雑誌）  

We compare high angular resolution mid-infrared (mid-IR) and Atacama Large Millimeter/submillimeter Array (ALMA) far-infrared (far-IR) images of twelve nearby (median 21 Mpc) Seyfert galaxies selected from the Galaxy Activity, Torus, and Outflow Survey (GATOS). The mid-IR unresolved emission contributes more than 60% of the nuclear (diameters of 1.5″ ∼ 150 pc) emission in most galaxies. By contrast, the ALMA 870  μm continuum emission is mostlyresolved with a median diameter of 42 pc and typically along the equatorial direction of the torus (Paper I). The Eddington ratios and nuclear hydrogen column densities (NH) of half the sample are favorable to launching polar and/or equatorial dusty winds, according to numerical simulations. Six of these show mid-IR extended emission approximately in the polar direction as traced by the narrow line region and perpendicular to the ALMA emission. In a few galaxies, the nuclear NH might be too high to uplift large quantities of dusty material along the polar direction. Five galaxies have low NH and/or Eddington ratios and thus polar dusty winds are not likely. We generated new radiative transfer CAT3D-WIND disk+wind models and model images at 8, 12, and 700  μm. We tailored these models to the properties of the GATOS Seyferts in this work. At low wind-to-disk cloud ratios, the far-IR model images have disk-and ring-like morphologies. The characteristic "X"-shape associated with dusty winds is seen better in the far-IR at intermediate-high inclinations for the extended-wind configurations. In most of the explored models, the mid-IR emission mainly comes from the inner part of the disk and cone. Extended biconical and one-sided polar mid-IR emission is seen in extended-wind configurations and high wind-to-disk cloud ratios. When convolved to the typical angular resolution of our observations, the CAT3D-WIND model images reproduce qualitative aspects of the observed mid-and far-IR morphologies. However, low to intermediate values of the wind-to-disk ratio are required to account for the observed large fractions of unresolved mid-IR emission in our sample. This work and Paper I provide observational support for the torus+wind scenario. The wind component is more relevant at high Eddington ratios and/or active galactic nucleus luminosities, and polar dust emission is predicted at nuclear column densities of up to ∼1024 cm-2. The torus or disk component, on the other hand, prevails at low luminosities and/or Eddington ratios.

DOI： 10.1051/0004-6361/202141219

Scopus

記述言語：英語  

DOI： https://doi.org/10.1051/0004-6361/201834963

担当区分：責任著者   記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： https://doi.org/10.3847/1538-4357/ac013d

担当区分：責任著者   掲載種別：研究論文（学術雑誌）  

We studied the absorption features of CO lines against the continuum originating from the heated dust in the obscuring tori around active galactic nuclei (AGNs). We investigated the formation of absorption lines corresponding to the CO rotational transitions using three-dimensional non-LTE line transfer simulations considering the dust thermal emission. As in Papers I-III of this series, we performed post-processed radiative transfer calculations using the "radiation-driven fountain model"(Wada et al. 2016), which yields a geometrically thick obscuring structure around the nucleus. This model is consistent with the spectral energy distribution of the nearest type-2 Seyfert galaxy, the Circinus galaxy. We found that the continuum-subtracted channel maps of J = 4-3 and higher transitions show absorption regions along the disk midplane for an edge-on viewing angle. The spectra consist of multiple absorption and emission features, reflecting the internal inhomogeneous and turbulent structure of the torus. The deepest absorption feature is caused by the gas on the near side of the torus between r = 10 and 15 pc, which is located in front of the AGN-heated dust inside r ≃ 5 pc. We also found that a spatial resolution of 0.5-1.0 pc is necessary to resolve the absorption features. Moreover, the inclination angle must be close to the edge-on angle (i.e., ⪆85 ) to observe the absorption features. The findings of the present study imply that combining our radiation-hydrodynamic model with high-resolution observations of CO (7-6) by ALMA can provide new information about the internal structure of the molecular tori in nearby AGNs.

DOI： 10.3847/1538-4357/ac013d

Scopus

掲載種別：研究論文（学術雑誌）  

The nuclear obscurer of active galactic nuclei (AGN) is poorly understood in terms of its origin, geometry, and dynamics. Aims. We investigate whether physically motivated geometries emerging from hydro-radiative simulations can be dierentiated with X-ray reflection spectroscopy. Methods. For two new geometries, the radiative fountain model and a warped disk, we release spectral models produced with the ray tracing code XARS. We contrast these models with spectra of three nearby AGN taken by NuSTAR and Swift/BAT. Results. Along heavily obscured sightlines, the models present dierent 420 keV continuum spectra. These can be dierentiated by current observations. Spectral fits of the Circinus Galaxy favour the warped disk model over the radiative fountain, and clumpy or smooth torus models. Conclusions. The necessary reflector (NH 1025 cm2) suggests a hidden population of heavily Compton-thick AGN amongst local galaxies. X-ray reflection spectroscopy is a promising pathway to understand the nuclear obscurer in AGN.

DOI： 10.1051/0004-6361/201834963

Scopus

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/abd40a

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/2007.15198v2

記述言語：英語   掲載種別：研究論文（国際会議プロシーディングス）   出版者・発行元：Proceedings of the International Astronomical Union  

DOI： 10.1017/S1743921320004251

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/abba39

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

出版者・発行元：Astronomy and Astrophysics  

DOI： 10.1051/0004-6361/202038282

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

It is widely believed that in active galactic nuclei (AGNs) a supermassive black hole with an accretion disk is surrounded by an optically and geometrically thick torus at sub-parsec scale. However, it is not clear how is the mass supply toward the central engine caused and how it is related with the internal structures of the tori. The magnetic field in the tori may contribute to the accretion process via the magneto-rotational instability (MRI). Using global three dimensional magnetohydrodynamic (MHD) simulations taking the effects of X-ray heating and radiative cooling into account studied the numerical resolution for azimuthal direction for MRI driving. We found that a strongly magnetized disk consisted of a cold ($< 10^3$ K) and warm ($10^4$ K) gas is developed in about 30 rotational periods. We also found in high resolution model that the mean azimuthal magnetic fields reverse their direction quasi-periodically. We confirmed that the typical wave length of the MRI should be resolved with a least 20 azimuthal grid cells.

DOI： 10.3390/galaxies6040139

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）  

We investigate the properties of the ionized gas irradiated by an active galactic nucleus (AGN) based on our “radiation-driven fountain” model for the nearest type-2 Seyfert galaxy, the Circinus galaxy. We conducted “quasi-three-dimensional” spectral analysis using the spectral synthesis code CLOUDY and obtained the surface brightness distributions of lines, such as Hα, Hβ, [O III], [N II], and [S II] for the central 16 pc region. The ionized regions observed based on these lines show a conical morphology around the rotation axis, even if we do not phenomenologically postulate the presence of an optically thick “torus.” This region also shows non-uniform internal structures, reflecting the inhomogeneous structure of fountain flows. Using ionization diagnostic diagrams, we investigated the spectral properties of the ionized gas. The diagrams based on the line ratios of [N II]/Hα and [S II]/Hα show that most regions of the cone have the same properties as those in the narrow line regions (NLRs) in AGNs, whereas using [O I]/Hα, the central 10 pc regions are rather LINER-like. The gas density, temperature, and ionizing parameter in regions identified as “NLR” are typically n ∼ 300–1500 cm‑3, T ∼ (1–3) × 104 K, and U ∼ 0.01, respectively. The morphology and [O III] intensity are similar to the base of the observed [O III] cone in the Circinus galaxy, implying some physical connections with the origin of the ∼100 pc scale NLR.

DOI： 10.3847/1538-4357/aae204

記述言語：英語   掲載種別：研究論文（学術雑誌）  

We used the Atacama Large Millimeter/Submillimeter Array (ALMA) to map the CO(3–2) and [C I](1–0) lines, as well as their underlying continuum emission, from the central ∼200 pc region of the Circinus galaxy that hosts the nearest type 2 Seyfert-class active galactic nucleus (AGN), with a spatial resolution of ∼6–15 pc. The lines and continuum-emitting regions consist of a circumnuclear disk (CND; 74 pc × 34 pc) and spiral arms. The distribution of the continuum emission revealed a temperature-dependent dust geometry and possibly polar dust elongation in the torus region. The molecular mass of the CND is {M}{{H}2}∼ 3× {10}6 {M}ȯ , with a beam-averaged H2 column density of ∼5 × 1023 cm‑2 toward the AGN position, which contributes significantly to the nuclear obscuration. The [C I](1–0)/CO(3–2) ratio at the AGN position is unusually high, suggesting an X-ray-dominated region-type chemistry. We decomposed the observed velocity fields into rotational and dispersion components, and revealed a multiphase dynamic nature in the r ≲ 10 pc torus region, i.e., the diffuse atomic gas is more spatially extended along the vertical direction of the disk than the dense molecular gas. Through comparisons with our model predictions based on the radiation-driven fountain scheme, we indicate that atomic outflows are the driver of the geometrical thickness of the atomic disk. This supports the validity of the radiation-driven fountain scheme in the vicinity of this AGN, which would explain the longstanding mystery of the physical origin of the AGN torus.

DOI： 10.3847/1538-4357/aae20b

記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/2041-8213/aaa8df

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

In this study, we investigate the line emissions from cold molecular gas based on our previous “radiation-driven fountain model,” which reliably explains the spectral energy distribution of the nearest type 2 Seyfert galaxy, the Circinus galaxy. Using a snapshot of the best-fit radiation-hydrodynamic model for the central r≤slant 16 pc, in which non-equilibrium X-ray-dominated region chemistry is solved, we conduct post-processed non-local thermodynamic equilibrium radiation transfer simulations for the CO lines. We obtain a spectral line energy distribution with a peak around J≃ 6, and its distribution suggests that the lines are not thermalized. However, for a given line of sight, the optical depth distribution is highly non-uniform between {τ }ν \ll 1 and {τ }ν \gg 1. The CO-to-H2 conversion factor ({X}{CO}), which can be directly obtained from the results and is not a constant, depends strongly on the integrated intensity and differs from the fiducial value for local objects. {X}{CO} exhibits a large dispersion of more than one order of magnitude, reflecting the non-uniform internal structure of a “torus.” In addition, we found that the physical conditions differ between grid cells on a scale of a few parsecs along the observed lines of sight; therefore, a specific observed line ratio does not necessarily represent a single physical state of the interstellar medium.

DOI： 10.3847/1538-4357/aa9e53

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Monthly Notices of the Royal Astronomical Society  

DOI： 10.1093/mnras/stx2381

Scopus

出版者・発行元：Astronomy and Astrophysics  

DOI： 10.1051/0004-6361/201730650

Scopus

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/aa8dfa

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

出版者・発行元：Astrophysical Journal Letters  

DOI： 10.3847/2041-8213/aa808f

Scopus

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

DOI： 10.3847/2041-8205/828/2/L19

記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Astronomical Society of Japan  

DOI： 10.1093/pasj/psv124

担当区分：筆頭著者   記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：American Astronomical Society  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：研究論文（学術雑誌）  

記述言語：英語   掲載種別：学位論文（博士）  

出版者・発行元：Astrophysical Journal  

DOI： 10.3847/1538-4357/ab4cf0

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1909.06748v3

出版者・発行元：Galaxies  

DOI： 10.3390/galaxies6040139

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1812.08419v2

出版者・発行元：Astrophysical Journal  

DOI： 10.3847/1538-4357/aae204

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1808.07195v1

出版者・発行元：Astrophysical Journal  

DOI： 10.3847/1538-4357/aae20b

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1809.09154v1

出版者・発行元：Astrophysical Journal Letters  

DOI： 10.3847/2041-8213/aaa8df

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1801.06564v1

出版者・発行元：Astrophysical Journal  

DOI： 10.3847/1538-4357/aa9e53

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1711.10117v1

出版者・発行元：Astrophysical Journal  

DOI： 10.3847/1538-4357/aa8dfa

Scopus

arXiv

その他リンク： http://arxiv.org/pdf/1708.08574v2

開催年月日： 2020年3月

記述言語：英語   会議種別：口頭発表（招待・特別）  

国名：ブラジル連邦共和国  

開催年月日： 2019年9月

記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：Onsala   国名：スウェーデン王国  

開催年月日： 2019年7月

記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：Sesto   国名：イタリア共和国  

開催年月日： 2018年12月

記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：Puerto Varas   国名：チリ共和国  

開催年月日： 2018年7月

記述言語：英語   会議種別：口頭発表（招待・特別）  

開催年月日： 2017年9月

記述言語：英語   会議種別：口頭発表（一般）  

開催年月日： 2015年3月

記述言語：日本語  

開催地：大阪大学  

国内学会

開催年月日： 2014年12月

記述言語：英語  

開催地：東京大学  

国際学会

開催年月日： 2014年12月

記述言語：英語  

開催地：台北  

国際学会

開催年月日： 2014年11月

記述言語：日本語  

開催地：筑波大学  

国内学会

開催年月日： 2014年7月

記述言語：英語  

開催地：Sesto、イタリア  

国際学会

開催年月日： 2014年2月

記述言語：英語  

開催地：北海道大学、札幌市（北海道）  

国際学会

開催年月日： 2013年10月

記述言語：英語  

開催地：ソウル大学、韓国  

国際学会

開催年月日： 2013年7月

記述言語：英語  

開催地：ハイデルベルグ、ドイツ  

国際学会

開催年月日： 2012年12月

記述言語：英語  

開催地：松山市、愛媛  

国際学会

開催年月日： 2012年11月

記述言語：英語  

開催地：Hsinchu, 台湾  

国際学会

開催年月日： 2012年10月

記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：Chongqing and online   国名：中華人民共和国  

開催年月日： 2012年9月

記述言語：英語  

開催地：Jeju, Korea  

国際学会

開催年月日： 2012年8月

記述言語：英語  

開催地：Beijing, China  

国際学会

開催年月日： 2011年6月

記述言語：英語  

開催地：リングバーグ、ドイツ  

国際学会

開催年月日： 2011年4月

記述言語：日本語  

開催地：ガルヒン、ドイツ  

その他

開催年月日： 2010年7月

記述言語：英語  

開催地：ダーラム、イギリス  

国際学会

開催年月日： 2010年6月

記述言語：英語  

開催地：スペイン、バロセロナ  

国際学会