adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star
Authors: Melissa J. Hobson, Andrés Jordán, E. M. Bryant, R. Brahm, D. Bayliss, J. D. Hartman, G. Á. Bakos, Th. Henning, Jose Manuel Almenara, Khalid Barkaoui, Zouhair Benkhaldoun, Xavier Bonfils, François Bouchy, David Charbonneau, Marion Cointepas, Karen A. Collins, Jason D. Eastman, Mourad Ghachoui, Michaël Gillon, Robert F. Goeke, Keith Horne, Jonathan M. Irwin, Emmanuel Jehin, Jon M. Jenkins, David W. Latham, Dan Moldovan, Felipe Murgas, Francisco J. Pozuelos, George R. Ricker, Richard P. Schwarz, S. Seager, Gregor Srdoc, Stephanie Striegel, Mathilde Timmermans, Andrew Vanderburg, Roland Vanderspek, Joshua N. Winn
Figure caption: Top: mass–radius diagram for M dwarf planets with masses and radii measured to better than 25%, as reported in TEPCAT. The markers are color-coded by host star mass. TOI-3235 b and its analog TOI-5205 b are plotted with star and hexagon symbols, respectively, and labeled. Theoretical mass–radius curves from Mordasini et al. (2012) are plotted with dashed and dotted lines. Center: period–radius diagram for the same planets. The markers are scaled by planet mass and color-coded by equilibrium temperature (black when it could not be computed). TOI-3235 b and TOI-5205 b are labeled. Bottom: planet mass vs. stellar mass diagram for the same planets. The markers are color-coded by host star metallicity. TOI-3235 b and TOI-5205 b are plotted with star and hexagon symbols, respectively, and labeled.
Paper: Observable Signatures of Stellar-mass Black Holes in Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, Imre Bartos
Figure caption: The spectral energy distribution for nonthermal (thick solid black) and thermal (thick solid brown) emission in the fiducial model (Section 2.2) at R = 1 pc. The left, middle, and right components in black lines represent synchrotron emission, synchrotron self-Compton (SSC), and second-order inverse Compton (IC) scattering, respectively. Solid and dashed blue lines represent emission from the host AGN and its variability, respectively. Dotted cyan, green, red, purple, gray, gold, pink, and orange lines indicate the sensitivities of ZTF, Vera Rubin and the Roman Space Telescope, Chandra and XMM-Newton, HiZ-GUNDAM and Einstein Probe, the Burst Alert Telescope (BAT) and XRT, NuSTAR and FORCE, WISE, and JWST, respectively. The results are also shown for models with lower accretion rate onto BH (f acc = 0.1, thin solid lines) or lower efficiencies of electron acceleration (ϵ e = 0.01, thin dashed) in panel (a) or lower magnetic field amplification (ϵ B = 10−5, thin dotted) or a higher jet efficiency (η j = 1, thin dashed–dotted) in panel (b).
Paper: Observable Signatures of Stellar-mass Black Holes in Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, Imre Bartos
Figure caption: Same as Figure 3 but for BH sources at R = 0.01 pc.
Paper: Observable Signatures of Stellar-mass Black Holes in Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, Imre Bartos
Figure caption: The luminosity and duration as a function of the distance from the SMBH (R) for emission from breakout of shocks produced around solitary BHs in the fiducial model. (a) The shock kinetic (solid black), breakout (dashed black), and nonthermal (solid orange) luminosity. (b) The duration of emission, t duration. The BH locations adopted in the fiducial model are indicated with filled circles superposed on the black solid lines.
Paper: Observable Signatures of Stellar-mass Black Holes in Active Galactic Nuclei
Authors: Hiromichi Tagawa, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, Imre Bartos
Figure caption: Schematic picture of quiescent phases (left panel) and the breakout emission from the head of a jet launched from a solitary BH (right panel) embedded in an AGN disk.
Paper: Modeling the Solar Wind during Different Phases of the Last Solar Cycle
Authors: Zhenguang Huang, Gábor Tóth, Nishtha Sachdeva, Lulu Zhao, Bart van der Holst, Igor Sokolov, Ward B. Manchester, Tamas I. Gombosi
Figure caption: Panel (a) shows the open magnetic field area (black, left axis) and the optimal Poynting flux parameter (red, right axis) as a function of the times of the Carrington rotations. Panel (b) shows the Spearman’s correlation coefficient r and the linear regression between the area of the open field regions and the optimal Poynting flux parameter with error bars indicating the standard error. Panel (c) shows the average unsigned ∣B  r ∣ in the open field regions (black, left axis) and the optimal Poynting flux parameter (red, right axis) as a function of the times of the Carrington rotations. Panel (d) shows the Spearman’s correlation coefficient r and the linear regression between the average ∣B  r ∣ and the optimal Poynting flux parameter with error bars indicating the standard error.
Paper: Modeling the Solar Wind during Different Phases of the Last Solar Cycle
Authors: Zhenguang Huang, Gábor Tóth, Nishtha Sachdeva, Lulu Zhao, Bart van der Holst, Igor Sokolov, Ward B. Manchester, Tamas I. Gombosi
Figure caption: AWsoM simulated solar wind bulk velocity, density, temperature and magnetic field (from top to bottom) compared with hourly OMNI observations (black lines) at 1 au, for the Carrington rotation 2106 (the left panels, a relatively quiet Sun) and 2137 (the right panels, a more active Sun). The blue lines correspond to the simulation results with different Poynting flux parameters. The red line highlights the results obtained with the optimal value based on the best match with the observed solar wind density and velocity. Note the greater variation in plasma quantities for CR2137.
Paper: Modeling the Solar Wind during Different Phases of the Last Solar Cycle
Authors: Zhenguang Huang, Gábor Tóth, Nishtha Sachdeva, Lulu Zhao, Bart van der Holst, Igor Sokolov, Ward B. Manchester, Tamas I. Gombosi
Figure caption: The distances between the simulated and observed solar wind for CR2106 (the left panel) and CR2137 (the right panel). The x-axis shows the value of the Poynting flux parameter while the y-axis plots the distances between the simulations and OMNI observations. The top row shows the distances between the simulated and observed densities, while the second row shows the distances between the velocities. The third row displays the average of velocity and density distances. The optimal Poynting flux parameter (colored with red) for each panel is found at the minimum of the curves.
Paper: Modeling the Solar Wind during Different Phases of the Last Solar Cycle
Authors: Zhenguang Huang, Gábor Tóth, Nishtha Sachdeva, Lulu Zhao, Bart van der Holst, Igor Sokolov, Ward B. Manchester, Tamas I. Gombosi
Figure caption: The average Poynting flux in the open field regions during the last solar cycle. The red horizontal line shows the average value (47.42 Wm−2) of the Poynting flux and the red dashed horizontal lines indicate the standard deviation ±13.12  Wm−2.
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: KDE showing the 95% confidence-interval regions for the subpopulation of interest (Figure 1 and Section 2) at Z = 0.02. The speed corresponds to the CoM velocity magnitude. The mass corresponds to the BH or total binary mass of the system, depending on whether or not the system is isolated or bound. We show the different reported lens masses of OB110462 as error bars and the transverse space velocity, according to Lam et al. (2022), Sahu et al. (2022), and the more recent analysis from Mróz et al. (2022). The transverse space velocity value from Lam et al. (2022) is an upper limit. Top: subpopulations of isolated BHs (BH﹩{}_{\sin }﹩, BH1, BH2) and compact-object binaries (BH–MS, NS–MS). Bottom: subpopulations of double compact object mergers (BH–NS, BH–BH, NS–NS).
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Number of systems of interest per unit star-forming mass. The various yields are calculated based on a population of 5 × 106 massive binaries per metallicity (Section 2). BH﹩{}_{\sin }﹩ (solid gray) represents isolated BHs from single-star origin. BH1 (solid blue) and BH2 (solid orange) represent disrupted BHs from binary origin; the subscripts 1 and 2 indicate that the progenitor is the initially more and less massive star, respectively. BH–MS (solid yellow) and NS–MS (solid purple) represent bound binaries, comprised of a compact object with a main-sequence companion, just after the first supernova. Double compact objects that will merge within the Hubble time are shown as dotted lines: BH–NS (green), BH–BH (cyan), and NS–NS (burgundy). The color scheme is the same in all figures.
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Normalized distributions of the semimajor axis of all binary subpopulations. Compact objects with a main-sequence companion (NS–MS, BH–MS) are shown in solid lines. NS–MS and BH–MS are X-ray binary candidates, particularly if they are in close or eccentric orbits where periastron passage triggers X-ray emitting processes. Double compact object mergers (BH–NS, BH–BH, and NS–NS) are shown in dotted lines. They are in very short periods as we are only considering those that will merge within the Hubble time. The gray shaded region denotes the excluded region of binaries or a companion to the lens mass of OB110462, as derived by Sahu et al. (2022).
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: BH mass distribution at Z = {0.0142, 0.01, 0.001, 0.0001}. The number of isolated BHs from single origin increase as a function of mass for all metallicities. This effect is enhanced at lower metallicities. Low-mass (≲10  M ⊙) BH lenses can be used to explore binary evolution, while high-mass (≳10  M ⊙) BH lenses can be used to understand single stellar evolution (Section 3.6).
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Results using the (alternative) natal kick model from Bray & Eldridge (2016). Besides the natal kick distribution, all other assumptions are identical to the default model (Appendix A). Additionally, the layout here is identical to that of Figure 2, which allows for a direct comparison (more details in Appendix B).
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: KDE contours showing the 95% confidence-interval regions for the isolated BH and compact binary subpopulations at Z = {0.0142, 0.01, 0.001, 0.0001}. The bulk of the single BH population at Z = 0.001 (bottom left panel) are low speed (≈0 km s−1) and with masses >10  M ⊙ and therefore barely visible in this KDE. For more details, see Section 2 and Figure 2.
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: KDE contours showing the 95% confidence-interval regions for double compact object merger subpopulations at Z = {0.0142, 0.01, 0.001, 0.0001}. The bulk of the BH–BH population at Z = 0.01 (top right panel) are low speed (≈0 km s−1) and with masses around ≳30  M ⊙ and therefore barely visible in this KDE. For more details, see Section 2 and Figure 2.
Paper: A Binary Origin for the First Isolated Stellar-mass Black Hole Detected with Astrometric Microlensing
Authors: Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Fraction of isolated BHs of single origin (﹩{N}_{\sin }/{N}_{\mathrm{tot}}﹩), for masses above the threshold mass M, as a function of the simulated metallicities. Isolated high-mass (≳10 M ⊙) BHs are predominantly of single-star origin. The darker lines are discontinuous at high metallicities because stellar winds remove enough mass that there are no BHs with mass ≳20  M ⊙ in our model (Appendix A).
Paper: Statistical Study of Ejections in Coronal Hole Regions As Possible Sources of Solar Wind Switchbacks and Small-scale Magnetic Flux Ropes
Authors: Nengyi Huang, Sophia D'Anna, Haimin Wang
Figure caption: An example of CHs detected using CHIMERA algorithm. The background is the blended images of AIA 171, 193 and 211 Å. The white contours are the boundaries of CHs calculated hourly and combined for 4 hr, and the red solid line boxes mark the cut areas where ejections are identified. The pink and cyan rectangles are indicating the location of PSP source regions provided by the modeling team, using GONG and HMI magnetogram, respectively.
Paper: Statistical Study of Ejections in Coronal Hole Regions As Possible Sources of Solar Wind Switchbacks and Small-scale Magnetic Flux Ropes
Authors: Nengyi Huang, Sophia D'Anna, Haimin Wang
Figure caption: The identified events overplotted on the 193 Å synoptic map. The dates are from 2020 June 9 to 2020 June 13, when the modeled PSP footpoint is in the Earth’s side. The green and pink dots represent for locations of identified standard and blowout jets, respectively.
Paper: Statistical Study of Ejections in Coronal Hole Regions As Possible Sources of Solar Wind Switchbacks and Small-scale Magnetic Flux Ropes
Authors: Nengyi Huang, Sophia D'Anna, Haimin Wang
Figure caption: The base size distributions of the identified blowout (left panel) and standard (right panel) jets.
Paper: Statistical Study of Ejections in Coronal Hole Regions As Possible Sources of Solar Wind Switchbacks and Small-scale Magnetic Flux Ropes
Authors: Nengyi Huang, Sophia D'Anna, Haimin Wang
Figure caption: The lifetime distributions of the identified blowout (left panel) and standard (right panel) jets.
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Measured D/H vs. 13C/H ratios in (A) the Ryugu’s particles and (B) the CI chondrite Orgueil with their confidence and prediction interval bands at 95%. All points lying outside of the prediction interval bands are considered outliers and are not included in the main trend estimate for the final estimation of the water D/H ratios (Table 1).
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Hydrogen isotopic values (δD) estimated for water from the D/H vs. C/H correlation measured by SIMS for Ryugu, Orgueil, and Mighei (this study, indicated by a star) and compared to the range estimated previously for the different carbonaceous chondrite groups (Piani et al. 2021). Error bars indicate the 95% error estimated from SIMS analyses of the samples and standards for Ryugu, Orgueil, and Mighei. Solid lines and dashed lines indicate averages and two standard errors on the measurements for each chondrite group. For reference, the D/H ratios of the protosolar H2 and the Earth oceans are also reported in the figure (Geiss & Gloecker 2003).
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Measured D−/H− vs. 13C−/H− ratios in Ryugu’s particles, the Murchison (CM), and the Orgueil (CI) carbonaceous chondrites (raw data). All data were acquired in the same analytical session in 2022 March. Linear fits (solid lines) and 95% confidence interval bands (dashed lines) are shown for all Ryugu’s points and for Orgueil chondrite with the exception of points outside the prediction interval at 95% confidence (see Section 4.2 and Figure A4 for details). Error bars represent 2σ internal errors.
Paper: Hydrogen Isotopic Composition of Hydrous Minerals in Asteroid Ryugu
Authors: Laurette Piani, Kazuhide Nagashima, Noriyuki Kawasaki, Naoya Sakamoto, Ken-ichi Bajo, Yoshinari Abe, Jérôme Aléon, Conel M. O'D. Alexander, Sachiko Amari, Yuri Amelin, Martin Bizzarro, Audrey Bouvier, Richard W. Carlson, Marc Chaussidon, Byeon-Gak Choi, Nicolas Dauphas, Andrew M. Davis, Tommaso Di Rocco, Wataru Fujiya, Ryota Fukai, Ikshu Gautam, Makiko K. Haba, Yuki Hibiya, Hiroshi Hidaka, Hisashi Homma, Peter Hoppe, Gary R. Huss, Kiyohiro Ichida, Tsuyoshi Iizuka, Trevor R. Ireland, Akira Ishikawa, Shoichi Itoh, Noriko T. Kita, Kouki Kitajima, Thorsten Kleine, Shintaro Komatani, Alexander N. Krot, Ming-Chang Liu, Yuki Masuda, Kevin D. McKeegan, Mayu Morita, Kazuko Motomura, Frédéric Moynier, Izumi Nakai, Ann Nguyen, Larry Nittler, Morihiko Onose, Andreas Pack, Changkun Park, Liping Qin, Sara S. Russell, Maria Schönbächler, Lauren Tafla, Haolan Tang, Kentaro Terada, Yasuko Terada, Tomohiro Usui, Sohei Wada, Meenakshi Wadhwa, Richard J. Walker, Katsuyuki Yamashita, Qing-Zhu Yin, Tetsuya Yokoyama, Shigekazu Yoneda, Edward D. Young, Hiroharu Yui, Ai-Cheng Zhang, Tomoki Nakamura, Hiroshi Naraoka, Ryuji Okazaki, Kanako Sakamoto, Hikaru Yabuta, Masanao Abe, Akiko Miyazaki, Aiko Nakato, Masahiro Nishimura, Tatsuaki Okada, Toru Yada, Kasumi Yogata, Satoru Nakazawa, Takanao Saiki, Satoshi Tanaka, Fuyuto Terui, Yuichi Tsuda, Sei-ichiro Watanabe, Makoto Yoshikawa, Shogo Tachibana, Hisayoshi Yurimoto
Figure caption: Scanning electron microscope (SEM) images of a piece of particle A0094 pressed in indium and location of the SIMS analyses. (A) Backscattered electron (BSE) image of the pressed particle fragment before SIMS analyses. (B) Combined X-ray elemental map of the particle fragment. The particle is dominated by Mg-rich phyllosilicates (purple), sulfides (yellow), and carbonates (light green). Large holes and cracks (black) were avoided for SIMS analyses. (C)–(D) BSE images of areas measured by SIMS. The numbers correspond to the analysis numbers as provided on ORDaR. Red crosses indicate analyses that were rejected due to small holes or cracks identified by SEM after the SIMS measurements.