記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/adc72a

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We present high-resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations at 0.89 mm of the Class II brown dwarf 2MASS J04442713+2512164 (2M0444), achieving a spatial resolution of 0<jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:mover accent="true">
<mml:mrow>
<mml:mi>.</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>″</mml:mi>
</mml:mrow>
</mml:mover>
</mml:math>

</jats:inline-formula>046 (∼6.4 au at the distance to the source). These observations targeted continuum emission together with <jats:sup>12</jats:sup>CO (3–2) molecular line. The line emission traces a Keplerian disk, allowing us to derive a dynamical mass between 0.043 and 0.092 <jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> for the central object. We constrain the gas-to-dust disk size ratio to be ∼7, consistent with efficient radial drift. However, the observed dust emission suggests that a dust trap is present, enough to retain some dust particles. We perform visibility fitting of the continuum emission, and under the assumption of annular substructure, our best fit shows a gap and a ring at 98.1<jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:msubsup>
<mml:mrow/>
<mml:mrow>
<mml:mo>−</mml:mo>
<mml:mn>8.4</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mo>+</mml:mo>
<mml:mn>4.2</mml:mn>
</mml:mrow>
</mml:msubsup>
</mml:math>

</jats:inline-formula> mas (∼14 au) and 116.0<jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:msubsup>
<mml:mrow/>
<mml:mrow>
<mml:mo>−</mml:mo>
<mml:mn>4.8</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mo>+</mml:mo>
<mml:mn>4.2</mml:mn>
</mml:mrow>
</mml:msubsup>
</mml:math>

</jats:inline-formula> mas (∼16 au), respectively, with a gap width of 20 mas (∼3 au). To ensure robustness, the data were analyzed through a variety of methods in both the image and <jats:monospace>uv</jats:monospace> planes, employing multiple codes and approaches. This tentative disk structure could be linked to a possible planetary companion in the process of formation. These results provide the first dynamical mass of the lowest mass object to date, together with the possible direct detection of a substructure, offering new insights into disk dynamics and planet formation in the very low-mass regime. Future higher spatial resolution ALMA observations will be essential to confirm these findings and further investigate the link between substructures and planet formation in brown dwarf disks.</jats:p>

DOI： 10.3847/2041-8213/add71f

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-3881/adb1ba

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the binary Class 0 protostellar system BHR 71 IRS1 and IRS2 as part of the Early Planet Formation in Embedded Disks (eDisk) ALMA Large Program. We describe the <jats:sup>12</jats:sup>CO (<jats:italic>J</jats:italic> = 2–1), <jats:sup>13</jats:sup>CO (<jats:italic>J</jats:italic> = 2–1), C<jats:sup>18</jats:sup>O (<jats:italic>J</jats:italic> = 2–1), H<jats:sub>2</jats:sub>CO (<jats:italic>J</jats:italic> = 3<jats:sub>2,1</jats:sub>–2<jats:sub>2,0</jats:sub>), and SiO (<jats:italic>J</jats:italic> = 5–4) molecular lines along with the 1.3 mm continuum at high spatial resolution (∼0.″08 or ∼5 au). Dust continuum emission is detected toward BHR 71 IRS1 and IRS2, with a central compact component and extended continuum emission. The compact components are smooth and show no sign of substructures such as spirals, rings, or gaps. However, there is a brightness asymmetry along the minor axis of the presumed disk in IRS1, possibly indicative of an inclined geometrically and optically thick disk-like component. Using a position–velocity diagram analysis of the C<jats:sup>18</jats:sup>O line, clear Keplerian motions were not detected toward either source. If Keplerian rotationally supported disks are present, they are likely deeply embedded in their envelope. However, we can set upper limits of the central protostellar mass of 0.46 <jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> and 0.26 <jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> for BHR 71 IRS1 and BHR 71 IRS2, respectively. Outflows traced by <jats:sup>12</jats:sup>CO and SiO are detected in both sources. The outflows can be divided into two components, a wide-angle outflow and a jet. In IRS1, the jet exhibits a double helical structure, reflecting the removal of angular momentum from the system. In IRS2, the jet is very collimated and shows a chain of knots, suggesting episodic accretion events.</jats:p>

DOI： 10.3847/1538-4357/ad655e

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.1051/0004-6361/202449981

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/ad4c6b

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>Young protostellar binary systems, with expected ages less than ∼10<jats:sup>5</jats:sup> yr, are little modified since birth, providing key clues to binary formation and evolution. We present a first look at the young, Class 0 binary protostellar system R CrA IRAS 32 from the Early Planet Formation in Embedded Disks ALMA large program, which observed the system in the 1.3 mm continuum emission, <jats:sup>12</jats:sup>CO (2−1), <jats:sup>13</jats:sup>CO (2−1), C<jats:sup>18</jats:sup>O (2−1), SO (6<jats:sub>5</jats:sub>−5<jats:sub>4</jats:sub>), and nine other molecular lines that trace disks, envelopes, shocks, and outflows. With a continuum resolution of ∼0.″03 (∼5 au, at a distance of 150 pc), we characterize the newly discovered binary system with a separation of 207 au, their circumstellar disks, and a circumbinary disklike structure. The circumstellar disk radii are 26.9 ± 0.3 and 22.8 ± 0.3 au for sources A and B, respectively, and their circumstellar disk dust masses are estimated as 22.5 ± 1.1 <jats:italic>M</jats:italic>
<jats:sub>⊕</jats:sub> and 12.4 ± 0.6 <jats:italic>M</jats:italic>
<jats:sub>⊕</jats:sub>, respectively. The circumstellar disks and the circumbinary structure have well-aligned position angles and inclinations, indicating formation in a smooth, ordered process such as disk fragmentation. In addition, the circumstellar disks have a near/far-side asymmetry in the continuum emission, suggesting that the dust has yet to settle into a thin layer near the midplane. Spectral analysis of CO isotopologues reveals outflows that originate from both of the sources and possibly from the circumbinary disklike structure. Furthermore, we detect Keplerian rotation in the <jats:sup>13</jats:sup>CO isotopologues toward both circumstellar disks and likely Keplerian rotation in the circumbinary structure; the latter suggests that it is probably a circumbinary disk.</jats:p>

DOI： 10.3847/1538-4357/ad3442

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

DOI： 10.3847/1538-4357/ad34b7

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We performed radiative transfer calculations and observing simulations to reproduce the 1.3 mm dust-continuum and C<jats:sup>18</jats:sup>O (2–1) images in the Class I protostar R CrA IRS7B-a, observed with the ALMA Large Program “Early Planet Formation in Embedded Disks (eDisk).” We found that a dust disk model passively heated by the central protostar cannot reproduce the observed peak brightness temperature of the 1.3 mm continuum emission (∼195 K), regardless of the assumptions about the dust opacity. Our calculation suggests that viscous accretion heating in the disk is required to reproduce the observed high brightness temperature. The observed intensity profile of the 1.3 mm dust-continuum emission along the disk minor axis is skewed toward the far side of the disk. Our modeling reveals that this asymmetric intensity distribution requires flaring of the dust along the disk vertical direction with the scale height following <jats:italic>h</jats:italic>/<jats:italic>r</jats:italic> ∼ <jats:italic>r</jats:italic>
<jats:sup>0.3</jats:sup> as a function of radius. These results are in sharp contrast to those of Class II disks, which show geometrically flat dust distributions and lower dust temperatures. From our modeling of the C<jats:sup>18</jats:sup>O (2–1) emission, the outermost radius of the gas disk is estimated to be ∼80 au, which is larger than that of the dust disk (∼62 au), to reproduce the observed distribution of the C<jats:sup>18</jats:sup>O (2–1) emission in IRS 7B-a. Our modeling unveils a hot and thick dust disk plus a larger gas disk around one of the eDisk targets, which could be applicable to other protostellar sources in contrast to more evolved sources.</jats:p>

DOI： 10.3847/1538-4357/ad1f57

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.5303/PKAS.2024.39.2.027

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/ad003a

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the Class I source Oph IRS 63 in the context of the Early Planet Formation in Embedded Disks large program. Our ALMA observations of Oph IRS 63 show a myriad of protostellar features, such as a shell-like bipolar outflow (in <jats:sup>12</jats:sup>CO), an extended rotating envelope structure (in <jats:sup>13</jats:sup>CO), a streamer connecting the envelope to the disk (in C<jats:sup>18</jats:sup>O), and several small-scale spiral structures seen toward the edge of the dust continuum (in SO). By analyzing the velocity pattern of <jats:sup>13</jats:sup>CO and C<jats:sup>18</jats:sup>O, we measure a protostellar mass of <jats:italic>M</jats:italic>
<jats:sub>⋆</jats:sub> = 0.5 ± 0.2 <jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> and confirm the presence of a disk rotating at almost Keplerian velocity that extends up to ∼260 au. These calculations also show that the gaseous disk is about four times larger than the dust disk, which could indicate dust evolution and radial drift. Furthermore, we model the C<jats:sup>18</jats:sup>O streamer and SO spiral structures as features originating from an infalling rotating structure that continuously feeds the young protostellar disk. We compute an envelope-to-disk mass infall rate of ∼10<jats:sup>−6</jats:sup>
<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup> and compare it to the disk-to-star mass accretion rate of ∼10<jats:sup>−8</jats:sup>
<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup>, from which we infer that the protostellar disk is in a mass buildup phase. At the current mass infall rate, we speculate that soon the disk will become too massive to be gravitationally stable.</jats:p>

DOI： 10.3847/1538-4357/acf7c1

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>Precise estimates of protostellar masses are crucial to characterize the formation of stars of low masses down to brown dwarfs (BDs; <jats:italic>M</jats:italic>
<jats:sub>*</jats:sub> &lt; 0.08 <jats:italic>M</jats:italic>
<jats:sub>☉</jats:sub>). The most accurate estimation of protostellar mass uses the Keplerian rotation in the circumstellar disk around the protostar. To apply the Keplerian rotation method to a protostar at the low-mass end, we have observed the Class 0 protostar IRAS 16253-2429 using the Atacama Large Millimeter/submillimeter Array (ALMA) in the 1.3 mm continuum at an angular resolution of 0.″07 (10 au), and in the <jats:sup>12</jats:sup>CO, C<jats:sup>18</jats:sup>O, <jats:sup>13</jats:sup>CO (<jats:italic>J</jats:italic> = 2–1), and SO (<jats:italic>J</jats:italic>
<jats:sub>
<jats:italic>N</jats:italic>
</jats:sub> = 6<jats:sub>5</jats:sub>−5<jats:sub>4</jats:sub>) molecular lines, as part of the ALMA Large Program Early Planet Formation in Embedded Disks project. The continuum emission traces a nonaxisymmetric, disk-like structure perpendicular to the associated <jats:sup>12</jats:sup>CO outflow. The position–velocity (PV) diagrams in the C<jats:sup>18</jats:sup>O and <jats:sup>13</jats:sup>CO lines can be interpreted as infalling and rotating motions. In contrast, the PV diagram along the major axis of the disk-like structure in the <jats:sup>12</jats:sup>CO line allows us to identify Keplerian rotation. The central stellar mass and the disk radius are estimated to be ∼0.12–0.17 <jats:italic>M</jats:italic>
<jats:sub>☉</jats:sub> and ∼13–19 au, respectively. The SO line suggests the existence of an accretion shock at a ring (<jats:italic>r</jats:italic> ∼ 28 au) surrounding the disk and a streamer from the eastern side of the envelope. IRAS 16253-2429 is not a proto-BD but has a central stellar mass close to the BD mass regime, and our results provide a typical picture of such very-low-mass protostars.</jats:p>

DOI： 10.3847/1538-4357/ace624

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/ace35c

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

DOI： 10.3847/1538-4357/ace52d

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/acdedf

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We present observations of the Class 0 protostar IRAS 16544–1604 in CB 68 from the “Early Planet Formation in Embedded Disks (eDisk)” ALMA Large program. The ALMA observations target continuum and lines at 1.3 mm with an angular resolution of ∼5 au. The continuum image reveals a dusty protostellar disk with a radius of ∼30 au seen close to edge-on and asymmetric structures along both the major and minor axes. While the asymmetry along the minor axis can be interpreted as the effect of the dust flaring, the asymmetry along the major axis comes from a real nonaxisymmetric structure. The C<jats:sup>18</jats:sup>O image cubes clearly show the gas in the disk that follows a Keplerian rotation pattern around a ∼0.14 <jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> central protostar. Furthermore, there are ∼1500 au scale streamer-like features of gas connecting from northeast, north–northwest, and northwest to the disk, as well as the bending outflow as seen in the <jats:sup>12</jats:sup>CO (2–1) emission. At the apparent landing point of the NE streamer, there is SO (6<jats:sub>5</jats:sub>–5<jats:sub>4</jats:sub>) and SiO (5–4) emission detected. The spatial and velocity structure of the NE streamer can be interpreted as a free-falling gas with a conserved specific angular momentum, and the detection of the SO and SiO emission at the tip of the streamer implies the presence of accretion shocks. Our eDisk observations have unveiled that the Class 0 protostar in CB 68 has a Keplerian-rotating disk with a flaring and nonaxisymmetric structure associated with accretion streamers and outflows.</jats:p>

DOI： 10.3847/1538-4357/acdd7a

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/accd71

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>Studying the physical and chemical conditions of young embedded disks is crucial to constrain the initial conditions for planet formation. Here we present Atacama Large Millimeter/submillimeter Array observations of dust continuum at ∼0.″06 (8 au) resolution and molecular line emission at ∼0.″17 (24 au) resolution toward the Class 0 protostar L1527 IRS from the Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum emission is smooth without substructures but asymmetric along both the major and minor axes of the disk as previously observed. The detected lines of <jats:sup>12</jats:sup>CO, <jats:sup>13</jats:sup>CO, C<jats:sup>18</jats:sup>O, H<jats:sub>2</jats:sub>CO, c-C<jats:sub>3</jats:sub>H<jats:sub>2</jats:sub>, SO, SiO, and DCN trace different components of the protostellar system, with a disk wind potentially visible in <jats:sup>12</jats:sup>CO. The <jats:sup>13</jats:sup>CO brightness temperature and the H<jats:sub>2</jats:sub>CO line ratio confirm that the disk is too warm for CO freezeout, with the snowline located at ∼350 au in the envelope. Both molecules show potential evidence of a temperature increase around the disk–envelope interface. SO seems to originate predominantly in UV-irradiated regions such as the disk surface and the outflow cavity walls rather than at the disk–envelope interface as previously suggested. Finally, the continuum asymmetry along the minor axis is consistent with the inclination derived from the large-scale (100″ or 14,000 au) outflow, but opposite to that based on the molecular jet and envelope emission, suggesting a misalignment in the system. Overall, these results highlight the importance of observing multiple molecular species in multiple transitions to characterize the physical and chemical environment of young disks.</jats:p>

DOI： 10.3847/1538-4357/accf87

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>While dust disks around optically visible, Class II protostars are found to be vertically thin, when and how dust settles to the midplane are unclear. As part of the Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded, Class I protostar IRAS 04302+2247, also nicknamed the “Butterfly Star.” With a resolution of 0.″05 (8 au), the 1.3 mm continuum shows an asymmetry along the minor axis that is evidence of an optically thick and geometrically thick disk viewed nearly edge-on. There is no evidence of rings and gaps, which could be due to the lack of radial substructure or the highly inclined and optically thick view. With 0.″1 (16 au) resolution, we resolve the 2D snow surfaces, i.e., the boundary region between freeze-out and sublimation, for <jats:sup>12</jats:sup>CO <jats:italic>J</jats:italic> = 2–1, <jats:sup>13</jats:sup>CO <jats:italic>J</jats:italic> = 2–1, C<jats:sup>18</jats:sup>O <jats:italic>J</jats:italic> = 2–1, <jats:italic>H</jats:italic>
<jats:sub>2</jats:sub>CO <jats:italic>J</jats:italic> = 3<jats:sub>0,3</jats:sub>–2<jats:sub>0,2</jats:sub>, and SO <jats:italic>J</jats:italic> = 6<jats:sub>5</jats:sub>–5<jats:sub>4</jats:sub>, and constrain the CO midplane snow line to ∼130 au. We find Keplerian rotation around a protostar of 1.6 ± 0.4<jats:italic> M</jats:italic>
<jats:sub>⊙</jats:sub> using C<jats:sup>18</jats:sup>O. Through forward ray-tracing using RADMC-3D, we find that the dust scale height is ∼6 au at a radius of 100 au from the central star and is comparable to the gas pressure scale height. The results suggest that the dust of this Class I source has yet to vertically settle significantly.</jats:p>

DOI： 10.3847/1538-4357/acd5c9

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>We present an overview of the Large Program, “Early Planet Formation in Embedded Disks (eDisk),” conducted with the Atacama Large Millimeter/submillimeter Array (ALMA). The ubiquitous detections of substructures, particularly rings and gaps, in protoplanetary disks around T Tauri stars raise the possibility that at least some planet formation may have already started during the embedded stages of star formation. In order to address exactly how and when planet formation is initiated, the program focuses on searching for substructures in disks around 12 Class 0 and 7 Class I protostars in nearby (&lt;200 pc) star-forming regions through 1.3 mm continuum observations at a resolution of ∼7 au (0.″04). The initial results show that the continuum emission, mostly arising from dust disks around the sample protostars, has relatively few distinctive substructures, such as rings and spirals, in marked contrast to Class II disks. The dramatic difference may suggest that substructures quickly develop in disks when the systems evolve from protostars to Class II sources, or alternatively that high optical depth of the continuum emission could obscure internal structures. Kinematic information obtained through CO isotopologue lines and other lines reveals the presence of Keplerian disks around protostars, providing us with crucial physical parameters, in particular, the dynamical mass of the central protostars. We describe the background of the eDisk program, the sample selection and their ALMA observations, and the data reduction, and we also highlight representative first-look results.</jats:p>

DOI： 10.3847/1538-4357/acd384

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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/acb3bd

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/aca47f

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

DOI： 10.3847/1538-4357/ac6fcf

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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/ac341d

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

DOI： 10.3847/1538-4357/ab8065

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記述言語：英語   掲載種別：研究論文（学術雑誌）  

<jats:title>Abstract</jats:title>
<jats:p>Pairs of azimuthal intensity decrements at near-symmetric locations have been seen in a number of protoplanetary disks. They are most commonly interpreted as the two shadows cast by a highly misaligned inner disk. Direct evidence of such an inner disk, however, remains largely illusive, except in rare cases. In 2012, a pair of such shadows were discovered in scattered-light observations of the near face-on disk around 2MASS J16042165-2130284, a transitional object with a cavity ∼60 au in radius. The star itself is a “dipper,” with quasi-periodic dimming events on its light curve, commonly hypothesized as caused by extinctions by transiting dusty structures in the inner disk. Here, we report the detection of a gas disk inside the cavity using Atacama Large Millimeter/submillimeter Array (ALMA) observations with ∼0.″2 angular resolution. A twisted butterfly pattern is found in the moment 1 map of the CO (3–2) emission line toward the center, which is the key signature of a high misalignment between the inner and outer disks. In addition, the counterparts of the shadows are seen in both dust continuum emission and gas emission maps, consistent with these regions being cooler than their surroundings. Our findings strongly support the hypothesized misaligned inner disk origin of the shadows in the J1604-2130 disk. Finally, the inclination of the inner disk would be close to −45° in contrast with 45°; it is possible that its internal asymmetric structures cause the variations on the light curve of the host star.</jats:p>

DOI： 10.3847/2041-8213/aae88b

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開催年月日： 2025年9月 - 2025年10月

記述言語：日本語   会議種別：口頭発表（一般）  

国名：日本国  

開催年月日： 2025年9月 - 2025年10月

記述言語：日本語   会議種別：口頭発表（一般）  

国名：日本国  

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開催年月日： 2025年9月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Kagoshima University   国名：日本国  

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開催年月日： 2025年9月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：海峡メッセ下関   国名：日本国  

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開催年月日： 2025年8月

記述言語：日本語   会議種別：口頭発表（一般）  

国名：日本国  

開催年月日： 2025年6月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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開催年月日： 2025年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：京都産業大学，京都   国名：日本国  

開催年月日： 2025年1月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：National Taiwan University (NTU)   国名：台湾  

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開催年月日： 2024年11月

記述言語：日本語   会議種別：口頭発表（一般）  

国名：日本国  

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開催年月日： 2024年6月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Kagoshima University   国名：日本国  

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開催年月日： 2024年5月

記述言語：英語   会議種別：ポスター発表  

開催地：Ringberg Castle   国名：ドイツ連邦共和国  

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開催年月日： 2024年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：東京大学本郷キャンパス/オンライン   国名：日本国  

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開催年月日： 2024年1月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：National Central University   国名：台湾  

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開催年月日： 2023年10月 - 2023年11月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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開催年月日： 2023年4月

記述言語：英語   会議種別：ポスター発表  

開催地：Kyoto International Conference Center, Kyoto   国名：日本国  

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開催年月日： 2023年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：立教大学   国名：日本国  

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開催年月日： 2023年2月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：The Great Roots Resort, New Taipei City   国名：台湾  

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開催年月日： 2022年12月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Miyakojima, Okinawa   国名：日本国  

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開催年月日： 2022年9月 - 2022年10月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：National Chung Cheng University   国名：台湾  

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開催年月日： 2022年8月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Quy Nhon   国名：ベトナム社会主義共和国  

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開催年月日： 2022年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：オンライン   国名：日本国  

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開催年月日： 2022年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：広島大学/オンライン   国名：日本国  

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開催年月日： 2022年1月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Online  

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開催年月日： 2021年2月

記述言語：日本語   会議種別：口頭発表（一般）  

国名：日本国  

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開催年月日： 2021年2月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Online   国名：大韓民国  

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開催年月日： 2020年9月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：弘前大学/オンライン   国名：日本国  

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開催年月日： 2020年2月

記述言語：英語   会議種別：ポスター発表  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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開催年月日： 2020年

記述言語：英語   会議種別：ポスター発表  

開催地：Online  

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開催年月日： 2019年12月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Tokyo University   国名：日本国  

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開催年月日： 2019年11月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Waikoloa Beach Marriott Resort & Spa, The Big Island of Hawaii   国名：アメリカ合衆国  

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開催年月日： 2019年11月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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開催年月日： 2019年11月

記述言語：英語   会議種別：ポスター発表  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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開催年月日： 2017年11月

記述言語：英語   会議種別：口頭発表（一般）  

開催地：KASI, Daejeon   国名：大韓民国  

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開催年月日： 2017年9月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：北海道大学   国名：日本国  

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開催年月日： 2017年3月

記述言語：日本語   会議種別：口頭発表（一般）  

開催地：九州大学   国名：日本国  

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記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：University of Vienna, Vienna   国名：オーストリア共和国  

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記述言語：英語   会議種別：口頭発表（招待・特別）  

開催地：Taipei   国名：台湾  

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記述言語：英語   会議種別：公開講演，セミナー，チュートリアル，講習，講義等  

開催地：Academia Sinica Institute of Astronomy and Astrophysics   国名：台湾  

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記述言語：日本語   会議種別：公開講演，セミナー，チュートリアル，講習，講義等  

開催地：大阪公立大学   国名：日本国  

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