Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)   Publisher：Institute of Physics Publishing  

DOI： 10.3847/1538-4357/aaaa6a

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/0004-637X/827/1/72

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1051/0004-6361/201526559

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1088/0004-6256/145/2/32

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1051/0004-6361/200913815

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1086/592948

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Springer Science and Business Media LLC  

Abstract

In the coldest regions of molecular clouds, carbon and oxygen are incorporated into icy dust grains. Despite its outsized role in star and planet formation, sequential formation of ice is poorly constrained. Infrared spectroscopy probes ice chemistry, but previous telescopes observed insufficient lines of sight to map a single cloud. Here we present cospatial maps of H₂O, CO₂ and CO ice over the central region of the Chamaeleon I molecular cloud, using 44 lines of sight observed with the James Webb Space Telescope. Correlations at column densities ten times larger than previous work suggest additional CO₂ ice formation in CO ice for the densest lines of sight. This large statistical sampling within a single cloud represents a step change in ice mapping, eliminating averaging over clouds with different intrinsic chemical environments. Mapping opens the door to probing gas–grain exchanges, snow lines and chemical evolution in the densest regions and drawing conclusions on the impact of ice chemistry on wider astrophysics.

DOI： 10.1038/s41550-025-02511-z

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Other Link： https://www.nature.com/articles/s41550-025-02511-z

Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

Abstract

Filamentary molecular clouds are an essential intermediate stage in the star formation process. To test whether these structures are universal throughout cosmic star formation history, it is crucial to study low-metallicity environments within the Local Group. We present an analysis of Atacama Large Millimeter/submillimeter Array (ALMA) archival data at the spatial resolution of  ~0.1 pc for 17 massive young stellar objects (YSOs) in the Small Magellanic Cloud (SMC; Z  ~ 0.2 Z _⊙). This sample represents approximately 30% of the YSOs confirmed by Spitzer spectroscopy. Early ALMA studies of the SMC have shown that the CO emission line traces an H₂ number density of  ≳10⁴ cm⁻³, an order of magnitude higher than in typical Galactic environments. Using the CO(J = 3–2) data, we investigate the spatial and velocity distribution of molecular clouds. Our analysis shows that about 60% of the clouds have steep radial profiles from the spine of the elongated structures, while the remaining clouds have a smooth distribution and are characterized by lower brightness temperatures. We categorize the former as filaments and the latter as nonfilaments. Some of the filamentary clouds are associated with YSOs with outflows and exhibit higher temperatures, likely reflecting their formation conditions, suggesting that these clouds are younger than the nonfilamentary ones. This indicates that even if filaments form during star formation, their steep structures may become less prominent and transition to a lower-temperature state. Such transitions in structure and temperature have not been reported in metal-rich regions, highlighting a key behavior for characterizing the evolution of the interstellar medium and star formation in low-metallicity environments.

DOI： 10.3847/1538-4357/ada5f8

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ada5f8/pdf

Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.48550/arXiv.2411.04451

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：EDP Sciences  

In the absence of laboratory data, state-of-the-art quantum chemical approaches can provide estimates of the binding energy (BE) of interstellar species with grains. Without BE values, contemporary astrochemical models are compelled to utilize wild guesses, often delivering misleading information. Here, we employed a fully quantum chemical approach to estimate the BE of seven diatomic radicals – CH, NH, OH, SH, CN, NS, and NO – that play a crucial role in shaping the interstellar chemical composition, using a suitable amorphous solid water model as a substrate since water is the principal constituent of interstellar ice in dense and shielded regions. While the BEs are compatible with physisorption, the binding of CH in some sites shows chemisorption, in which a chemical bond to an oxygen atom of a water molecule is formed. While no structural change has been observed for the CN radical, it is believed that the formation of a hemibonded system between the outer layer of the water cluster and the radical is the reason for the unusually large BE in one of the binding sites considered in our study. A significantly lower BE for NO, consistent with recent calculations, is obtained, which helps explain the recently observed HONO/NH₂OH and HONO/HNO ratios in the low-mass hot corino IRAS 16293–2422 B with chemical models.

DOI： 10.1051/0004-6361/202451642

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Frontiers Media SA  

SO and SO₂ are two potential candidates to trace the different evolutionary phases of the low-mass star-formation process. Here, we report observations of SO and SO₂ along with their isotopologues, ³⁴SO and ³⁴SO_2, respectively, in four distinct phases of the low-mass star-formation process (prestellar core, first hydrostatic core, Class 0, and Class I) with an unbiased survey carried out using the Institut de Radioastronomie Millimetrique (IRAM) 30 m telescope. Interestingly, the estimated abundances of SO and SO₂ show an increasing trend from the prestellar phase to the Class 0 stage and then a decrease in the Class I phase. A similar trend is obtained for OCS and H₂S. In contrast, the obtained SO/SO₂ ratio decreases gradually from the prestellar core to the Class I stage. We have used the three-phase Rokko chemical code to explain our observations. The modeled abundances of SO and SO₂ exhibit an increase within the inner region as the cold gas transforms into a hot gas. The modeled abundance ratio of SO to SO₂ exhibits a notably high value in cold gas environments. This ratio decreases to less than 1 within the temperature range of 100–300 K and then increases to approximately 1 beyond 300 K. In the outer region, the simulated ratio consistently exceeds the value of 1. Our work is an observational testbed for modeling the chemistry of SO/SO₂ during low-mass star formation. However, our findings may require more sample sources with higher resolution and a more robust model for validation.

DOI： 10.3389/fspas.2024.1427048

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Springer Science and Business Media LLC  

DOI： 10.1038/s41550-024-02307-7

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Other Link： https://www.nature.com/articles/s41550-024-02307-7

Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/2041-8213/ad50cc

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Springer Science and Business Media LLC  

DOI： 10.1038/s41550-023-02155-x

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Other Link： https://www.nature.com/articles/s41550-023-02155-x

Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

Abstract

The destiny of complex organic molecules (COMs) in star-forming regions is interlinked with various evolutionary phases. Therefore, identifying these species in diversified environments of identical star-forming regions would help to understand their physical and chemical heritage. We identified multiple COMs utilizing the Large Program Astrochemical Surveys At Institut de Radio Astronomie Millimétrique (IRAM) data, dedicated to chemical surveys in Sun-like star-forming regions with the IRAM 30 m telescope. It was an unbiased survey in the millimeter regime, covering the prestellar core, protostar, outflow region, and protoplanetary disk phase. Here, we report the transitions of seven COMs, namely, methanol (CH₃OH), acetaldehyde (CH₃CHO), methyl formate (CH₃OCHO), ethanol (C₂H₅OH), propynal (HCCCHO), dimethyl ether (CH₃OCH₃), and methyl cyanide (CH₃CN) in sources L1544, B1-b, IRAS4A, and SVS13A. We found a trend among these species from the derived abundances using the rotational diagram method and Monte Carlo Markov chain fitting. We have found that the abundances of all of the COMs, except for HCCCHO, increase from the L1544 (prestellar core) and peaks at IRAS16293-2422 (class 0 phase). It is noticed that the abundance of these molecules correlates with the luminosity of the sources. The obtained trend is also visible from the previous interferometric observations and considering the beam dilution effect.

DOI： 10.3847/1538-4357/acfc4d

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/acfc4d/pdf

Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

Abstract

Recent millimeter/submillimeter facilities have revealed the physical properties of filamentary molecular clouds in relation to high-mass star formation. A uniform survey of the nearest, face-on star-forming galaxy, the Large Magellanic Cloud (LMC), complements the Galactic knowledge. We present ALMA survey data with a spatial resolution of ∼0.1 pc in the 0.87 mm continuum and HCO⁺ (4–3) emission toward 30 protostellar objects with luminosities of 10⁴–10^5.5L_⊙ in the LMC. The spatial distributions of the HCO⁺ (4–3) line and thermal dust emission are well correlated, indicating that the line effectively traces dense, filamentary gas with an H₂ volume density of ≳10⁵ cm⁻³ and a line mass of ∼10³–10⁴M_⊙ pc⁻¹. Furthermore, we obtain an increase in the velocity line widths of filamentary clouds, which follows a power-law dependence on their H₂ column densities with an exponent of ∼0.5. This trend is consistent with observations toward filamentary clouds in nearby star-forming regions within ≲1 kpc from us and suggests enhanced internal turbulence within the filaments due to surrounding gas accretion. Among the 30 sources, we find that 14 are associated with hub-filamentary structures, and these complex structures predominantly appear in protostellar luminosities exceeding ∼5 × 10⁴L_⊙. The hub-filament systems tend to appear in the latest stages of their natal cloud evolution, often linked to prominent H ii regions and numerous stellar clusters. Our preliminary statistics suggest that the massive filaments accompanied by hub-type complex features may be a necessary intermediate product in forming extremely luminous high-mass stellar systems capable of ultimately dispersing the parent cloud.

DOI： 10.3847/1538-4357/acefb7

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/acefb7/pdf

Publishing type：Research paper (scientific journal)  

DOI： 10.1093/pasj/psad046

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：Springer Science and Business Media LLC  

DOI： 10.1038/s41550-022-01875-w

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Other Link： https://www.nature.com/articles/s41550-022-01875-w

Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

Abstract

We report near-infrared (2.5–5 μm) long-slit (∼30″) spectroscopy of a young stellar object in the direction toward the Galactic center with the Infrared Camera on board the AKARI satellite. The present target is suggested to be AFGL 2006 based on its very red color and close location. The spectra show strong absorption features of H₂O and CO₂ ices, and emission of H i Brα recombination line and the 3.3 μm band, the latter of which originates from polycyclic aromatic hydrocarbons (PAHs) or materials containing PAHs. The spectra show a broad, complex absorption feature at 4.65 μm, which is well explained by a combination of absorption features of CO ice, CO gas, and XCN, and H i Pfβ emission. The spectra also indicate excess emission at 4.4 μm. The characteristics of the spectra suggest that the object is a massive young stellar object. The XCN feature shows a good correlation with the Brα emission, suggesting that the photolysis by ultraviolet photons plays an important role in the formation of the XCN carriers, part of which are attributed to OCN⁻. The 4.4 μm emission shows a good correlation with the 3.3 μm PAH emission, providing supporting evidence that it comes from the aromatic C–D stretching vibration. The formation of OCN⁻ is of importance for the formation process of prebiotic matter in the interstellar medium (ISM), while the detection of aromatic C–D emission provides valuable information on the deuteration process of PAHs in the ISM and implications on the hiding site of the missing deuterium in the ISM.

DOI： 10.3847/1538-4357/ac9b15

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ac9b15/pdf

Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/2041-8213/ac81c1

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Other Link： https://iopscience.iop.org/article/10.3847/2041-8213/ac81c1/pdf

Language：English   Publishing type：Part of collection (book)   Publisher：IntechOpen  

We observed the formation of CO, CH3OH, and H2O ices using a cryogenic transmission electron microscope, to determine if chiral ice crystals could form under the conditions of interstellar molecular clouds and young stellar objects (protoplanetary disks) and to clarify the crystalline structure of these ices. Our results suggest that the following ice crystals are chiral: crystalline CO (α-CO) formed on amorphous H2O (a-H2O) grains in a 10-K molecular cloud, crystalline CH3OH formed by the heating of amorphous CH3OH on a-H2O grains at 40–60 K in young stellar objects, and several polymorphs of hydrogen-ordered cubic ice crystals formed by the heating of a-H2O at 80–100 K and direct condensation at 120–140 K in protoplanetary disks. We also investigated candidates for other chiral ices using published data. We found that NH3 I and NH3·H2O I are chiral at low temperature and pressure conditions. If one-handed circularly polarized light is irradiated during the nucleation of these chiral ice crystals, homochiral crystals can be formed. These results have important implications for the origin of interstellar organic molecule homochirality.

DOI： 10.5772/intechopen.106708

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/ac4260

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ac4260/pdf

Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

<title>Abstract</title>
It is speculated that there might be some linkage between interstellar aldehydes and their corresponding alcohols. Here an observational study and astrochemical modeling are coupled together to illustrate the connection between them. The ALMA cycle 4 data of a hot molecular core, G10.47+0.03, are utilized for this study. Various aldehydes (acetaldehyde, propanal, and glycolaldehyde), alcohols (methanol and ethylene glycol), and a ketone (acetone) are identified in this source. The excitation temperatures and column densities of these species were derived via the rotation diagram method assuming local thermodynamic equilibrium conditions. An extensive investigation is carried out to understand the formation of these species. Six pairs of aldehyde–alcohol are considered for this study: (i) methanal and methanol, (ii) ethanal and ethanol, (iii) propanal and 1-propanol, (iv) propenal and allyl alcohol, (v) propynal and propargyl alcohol, and (vi) glycolaldehyde and ethylene glycol. One pair of ketone–alcohol (acetone and isopropanol) and ketene–alcohol (ethenone and vinyl alcohol) are also considered. Two successive hydrogenation reactions in the ice phase are examined to form these alcohols from aldehydes, ketone, and ketene, respectively. Quantum chemical methods are extensively executed to review the ice-phase formation route and the kinetics of these species. Based on the obtained kinetic data, astrochemical modeling is employed to derive the abundances of these aldehydes, alcohols, ketone, and ketene in this source. It is seen that our model could successfully explain the observed abundances of various species in this hot molecular core.

DOI： 10.3847/1538-4357/ac1f31

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ac1f31/pdf

Publishing type：Research paper (scientific journal)   Publisher：Cambridge University Press (CUP)  

<title>Abstract</title>
In this era of spatially resolved observations of planet-forming disks with Atacama Large Millimeter Array (ALMA) and large ground-based telescopes such as the Very Large Telescope (VLT), Keck, and Subaru, we still lack statistically relevant information on the quantity and composition of the material that is building the planets, such as the total disk gas mass, the ice content of dust, and the state of water in planetesimals. <italic>SPace Infrared telescope for Cosmology and Astrophysics (SPICA)</italic> is an infrared space mission concept developed jointly by Japan Aerospace Exploration Agency (JAXA) and European Space Agency (ESA) to address these questions. The key unique capabilities of <italic>SPICA</italic> that enable this research are (1) the wide spectral coverage <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline1.png" />
<tex-math>
$10{-}220\,\mu\mathrm{m}$
</tex-math>
</alternatives>
</inline-formula>, (2) the high line detection sensitivity of <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline2.png" />
<tex-math>
$(1{-}2) \times 10^{-19}\,\mathrm{W\,m}^{-2}$
</tex-math>
</alternatives>
</inline-formula> with <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline3.png" />
<tex-math>
$R \sim 2\,000{-}5\,000$
</tex-math>
</alternatives>
</inline-formula> in the far-IR (SAFARI), and <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline4.png" />
<tex-math>
$10^{-20}\,\mathrm{W\,m}^{-2}$
</tex-math>
</alternatives>
</inline-formula> with <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline5.png" />
<tex-math>
$R \sim 29\,000$
</tex-math>
</alternatives>
</inline-formula> in the mid-IR (<italic>SPICA</italic> Mid-infrared Instrument (SMI), spectrally resolving line profiles), (3) the high far-IR continuum sensitivity of 0.45 mJy (SAFARI), and (4) the observing efficiency for point source surveys. This paper details how mid- to far-IR infrared spectra will be unique in measuring the gas masses and water/ice content of disks and how these quantities evolve during the planet-forming period. These observations will clarify the crucial transition when disks exhaust their primordial gas and further planet formation requires secondary gas produced from planetesimals. The high spectral resolution mid-IR is also unique for determining the location of the snowline dividing the rocky and icy mass reservoirs within the disk and how the divide evolves during the build-up of planetary systems. Infrared spectroscopy (mid- to far-IR) of key solid-state bands is crucial for assessing whether extensive radial mixing, which is part of our Solar System history, is a general process occurring in most planetary systems and whether extrasolar planetesimals are similar to our Solar System comets/asteroids. We demonstrate that the SPICA mission concept would allow us to achieve the above ambitious science goals through large surveys of several hundred disks within <inline-formula>
<alternatives>
<inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" mime-subtype="png" xlink:href="S132335802100031X_inline6.png" />
<tex-math>
$\sim\!2.5$
</tex-math>
</alternatives>
</inline-formula> months of observing time.

DOI： 10.1017/pasa.2021.31

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Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

DOI： 10.3847/1538-4357/ac0ae6

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ac0ae6/pdf

Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-3881/ac09f9

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Astronomical Society  

DOI： 10.3847/1538-4357/ac0531

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Other Link： https://iopscience.iop.org/article/10.3847/1538-4357/ac0531/pdf

Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1093/mnras/stab1173

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Other Link： http://academic.oup.com/mnras/article-pdf/505/1/1530/38463480/stab1173.pdf

Language：English   Publishing type：Research paper (scientific journal)  

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/2041-8213/aba695

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Other Link： https://iopscience.iop.org/article/10.3847/2041-8213/aba695

Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Chemical Society (ACS)  

DOI： 10.1021/acsearthspacechem.0c00098

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Language：English   Publishing type：Research paper (scientific journal)   Publisher：American Chemical Society (ACS)  

DOI： 10.1021/acsearthspacechem.9b00065

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/aaf72a

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/aacd0c

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.3847/1538-4357/aa89e5

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DOI： 10.3847/1538-4357/aa7ece

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Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.5303/PKAS.2017.32.1.105

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Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.5303/PKAS.2017.32.1.077

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.5303/PKAS.2017.32.1.083

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Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.5303/PKAS.2017.32.1.141

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DOI： 10.3847/0004-637X/829/2/94

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DOI： 10.3847/0004-637X/818/2/161

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DOI： 10.3847/0004-637X/817/2/145

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Language：English   Publishing type：Research paper (international conference proceedings)  

DOI： 10.1088/1742-6596/728/6/062006

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1088/0004-637X/807/1/29

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Language：English   Publishing type：Research paper (international conference proceedings)   Publisher：Cambridge University Press  

DOI： 10.1017/S1743921316003161

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Language：English   Publishing type：Research paper (international conference proceedings)  

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Language：English  

DOI： 10.1088/0004-637X/792/1/80

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Publisher：Sissa Medialab  

DOI： 10.22323/1.207.0112

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1093/mnras/stt2495

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DOI： 10.1088/0004-637X/784/1/53

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1088/2041-8205/773/2/L37

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (international conference proceedings)  

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Language：English   Publishing type：Research paper (international conference proceedings)   Publisher：Proceedings of Science (PoS)  

Scopus

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1088/0004-6256/144/6/179

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (scientific journal)   Publisher：The Korean Astronomical Society  

DOI： 10.5303/pkas.2012.27.4.171

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DOI： 10.1088/0004-637X/752/1/15

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DOI： 10.1117/12.926717

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DOI： 10.1088/2041-8205/731/1/L20

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DOI： 10.1051/eas/1146006

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DOI： 10.1117/12.856568

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Authorship：Lead author   Language：English   Publishing type：Research paper (international conference proceedings)  

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (international conference proceedings)  

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Authorship：Lead author,　Corresponding author   Language：English   Publishing type：Research paper (international conference proceedings)  

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Language：English   Publishing type：Research paper (scientific journal)  

DOI： 10.1093/pasj/60.sp2.S435

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Language：Japanese   Publishing type：Meeting report   Publisher：The Japanese Society for Planetary Sciences  

CiNii Article

CiNii Books

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Event date： 2023.7

Language：English   Presentation type：Oral presentation (invited, special)  

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Event date： 2025.3

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Event date： 2024.11

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Event date： 2024.8

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Country：Japan  

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Country：Japan  

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Country：Japan  

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Country：India  

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Event date： 2023.8

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Event date： 2023.4

Language：English   Presentation type：Poster presentation  

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Event date： 2023.3

Language：Japanese   Presentation type：Oral presentation (general)  

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Event date： 2023.3

Language：Japanese   Presentation type：Poster presentation  

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Event date： 2023.2

Language：Japanese   Presentation type：Oral presentation (general)  

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Event date： 2023.2

Language：Japanese   Presentation type：Oral presentation (general)  

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Event date： 2022.12

Language：English   Presentation type：Poster presentation  

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Event date： 2022.11 - 2022.12

Language：English   Presentation type：Poster presentation  

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Event date： 2022.11

Language：English   Presentation type：Poster presentation  

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Event date： 2022.8

Language：English   Presentation type：Poster presentation  

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Event date： 2022.5

Language：Japanese   Presentation type：Oral presentation (invited, special)  

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Event date： 2021.1

Language：English   Presentation type：Oral presentation (invited, special)  

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Event date： 2020.9 - 2020.10

Presentation type：Oral presentation (general)  

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Event date： 2020.2

Language：Japanese   Presentation type：Oral presentation (general)  

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Event date： 2020.2

Language：English   Presentation type：Oral presentation (general)  

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Event date： 2020.1

Language：Japanese   Presentation type：Oral presentation (general)  

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Event date： 2020.1

Language：English   Presentation type：Oral presentation (general)  

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Event date： 2019.9

Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (invited, special)  

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Language：Japanese   Presentation type：Oral presentation (invited, special)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Language：Japanese   Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (invited, special)  

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Language：English   Presentation type：Public lecture, seminar, tutorial, course, or other speech  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (keynote)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (invited, special)  

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Language：English   Presentation type：Poster presentation  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (invited, special)  

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Language：English   Presentation type：Oral presentation (invited, special)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (keynote)  

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Language：English   Presentation type：Oral presentation (invited, special)  

Venue：JAPAN Tokyo  

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Language：English   Presentation type：Oral presentation (invited, special)  

Venue：JAPAN 東京  

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Language：Japanese   Presentation type：Oral presentation (invited, special)  

Venue：JAPAN 東京  

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Language：English   Presentation type：Oral presentation (general)  

Venue：Chile Puerto Varas  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (invited, special)  

Venue：Netherlands Leiden  

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Language：Japanese   Presentation type：Oral presentation (general)  

Venue：JAPAN 松山  

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Language：English   Presentation type：Oral presentation (general)  

Venue：JAPAN 仙台  

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Presentation type：Poster presentation  

Venue：Viet Nam Quy Nhon  

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Language：Japanese   Presentation type：Oral presentation (general)  

Venue：JAPAN つくば  

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Language：English   Presentation type：Oral presentation (general)  

Venue：Netherlands Leiden  

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Language：English   Presentation type：Oral presentation (general)  

Venue：United States Charlottesville  

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Language：Japanese   Presentation type：Oral presentation (general)  

Venue：JAPAN 札幌  

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Language：Japanese   Presentation type：Oral presentation (general)  

Venue：United States Annapolis  

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Language：Japanese   Presentation type：Oral presentation (general)  

Venue：JAPAN 兵庫  

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Language：English   Presentation type：Oral presentation (general)  

Venue：JAPAN 東京  

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Language：English   Presentation type：Poster presentation  

Venue：United States Honolulu  

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Language：English   Presentation type：Poster presentation  

Venue：United States Honolulu  

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Language：English   Presentation type：Oral presentation (general)  

Venue：JAPAN 東京  

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Language：English   Presentation type：Oral presentation (general)  

Venue：JAPAN 神奈川  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Poster presentation  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (invited, special)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：English   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Language：Japanese   Presentation type：Oral presentation (general)  

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Author：Other 

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Author：Myself 

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Author：Myself 

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Author：Myself 

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Author：Myself 

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