adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST
Authors: Dale D. Kocevski, Guillermo Barro, Elizabeth J. McGrath, Steven L. Finkelstein, Micaela B. Bagley, Henry C. Ferguson, Shardha Jogee, Guang Yang, Mark Dickinson, Nimish P. Hathi, Bren E. Backhaus, Eric F. Bell, Laura Bisigello, Véronique Buat, Denis Burgarella, Caitlin M. Casey, Nikko J. Cleri, M. C. Cooper, Luca Costantin, Darren Croton, Emanuele Daddi, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Pablo Arrabal Haro, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Kartheik G. Iyer, Brenda Jones, Stéphanie Juneau, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, Peter Kurczynski, Aurélien Le Bail, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Stephen M. Wilkins, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Results of our two-dimensional surface brightness profile fitting. The F356W images are shown in the left column, our best-fit GALFIT models are shown in the middle column, and the residuals (data minus model) are shown in the right column. The best-fit Sérsic index and effective radius for each source are listed. Here PS stands for “point source.” Images are 3″ × 3″ in size.
Paper: CEERS Key Paper. II. A First Look at the Resolved Host Properties of AGN at 3 < z < 5 with JWST
Authors: Dale D. Kocevski, Guillermo Barro, Elizabeth J. McGrath, Steven L. Finkelstein, Micaela B. Bagley, Henry C. Ferguson, Shardha Jogee, Guang Yang, Mark Dickinson, Nimish P. Hathi, Bren E. Backhaus, Eric F. Bell, Laura Bisigello, Véronique Buat, Denis Burgarella, Caitlin M. Casey, Nikko J. Cleri, M. C. Cooper, Luca Costantin, Darren Croton, Emanuele Daddi, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Eric Gawiser, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Pablo Arrabal Haro, Michaela Hirschmann, Benne W. Holwerda, Marc Huertas-Company, Taylor A. Hutchison, Kartheik G. Iyer, Brenda Jones, Stéphanie Juneau, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, Peter Kurczynski, Aurélien Le Bail, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Rachel S. Somerville, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Stephen M. Wilkins, Stijn Wuyts, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Residual images of AEGIS 482 after subtracting the best-fit point-source model in five NIRCam bands. Images are 3″ × 3″ in size.
Paper: The JWST Early-release Science Program for Direct Observations of Exoplanetary Systems II: A 1 to 20 μm Spectrum of the Planetary-mass Companion VHS 1256–1257 b
Authors: Brittany E. Miles, Beth A. Biller, Polychronis Patapis, Kadin Worthen, Emily Rickman, Kielan K. W. Hoch, Andrew Skemer, Marshall D. Perrin, Niall Whiteford, Christine H. Chen, B. Sargent, Sagnick Mukherjee, Caroline V. Morley, Sarah E. Moran, Mickael Bonnefoy, Simon Petrus, Aarynn L. Carter, Elodie Choquet, Sasha Hinkley, Kimberly Ward-Duong, Jarron M. Leisenring, Maxwell A. Millar-Blanchaer, Laurent Pueyo, Shrishmoy Ray, Steph Sallum, Karl R. Stapelfeldt, Jordan M. Stone, Jason J. Wang, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Gael Chauvin, Valentin Christiaens, Thayne Currie, Camilla Danielski, Jonathan J. Fortney, Julien H. Girard, Carol A. Grady, Alexandra Z. Greenbaum, Thomas Henning, Dean C. Hines, Markus Janson, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Pierre-Olivier Lagage, Ben W. P. Lew, Michael C. Liu, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Paul Molliere, Eric Pantin, Andreas Quirrenbach, Isabel Rebollido, Bin B. Ren, Glenn Schneider, Malavika Vasist, Mark C. Wyatt, Yifan Zhou, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gabriele Cugno, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Kyle Franson, Eileen C. Gonzales, Callie E. Hood, Alex R. Howe, Adam L. Kraus, Masayuki Kuzuhara, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Raquel A. Martinez, Johan Mazoyer, Sascha P. Quanz, Jea Adams Redai, Matthias Samland, Joshua E. Schlieder, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Johanna M. Vos, Kevin Wagner, Schuyler G. Wolff, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang
Figure caption: VHS 1256 b (red hexagon) is an analog to directly imaged exoplanets like the HR 8799 planets due to similar near-infrared colors. VHS 1256 b and other directly imaged exoplanets maintain these colors compared to similar-temperature brown dwarfs because of lower surface gravities, which allow clouds to linger in the upper atmosphere. Photometry from http://bit.ly/UltracoolSheet.
Paper: The JWST Early-release Science Program for Direct Observations of Exoplanetary Systems II: A 1 to 20 μm Spectrum of the Planetary-mass Companion VHS 1256–1257 b
Authors: Brittany E. Miles, Beth A. Biller, Polychronis Patapis, Kadin Worthen, Emily Rickman, Kielan K. W. Hoch, Andrew Skemer, Marshall D. Perrin, Niall Whiteford, Christine H. Chen, B. Sargent, Sagnick Mukherjee, Caroline V. Morley, Sarah E. Moran, Mickael Bonnefoy, Simon Petrus, Aarynn L. Carter, Elodie Choquet, Sasha Hinkley, Kimberly Ward-Duong, Jarron M. Leisenring, Maxwell A. Millar-Blanchaer, Laurent Pueyo, Shrishmoy Ray, Steph Sallum, Karl R. Stapelfeldt, Jordan M. Stone, Jason J. Wang, Olivier Absil, William O. Balmer, Anthony Boccaletti, Mariangela Bonavita, Mark Booth, Brendan P. Bowler, Gael Chauvin, Valentin Christiaens, Thayne Currie, Camilla Danielski, Jonathan J. Fortney, Julien H. Girard, Carol A. Grady, Alexandra Z. Greenbaum, Thomas Henning, Dean C. Hines, Markus Janson, Paul Kalas, Jens Kammerer, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Pierre-Olivier Lagage, Ben W. P. Lew, Michael C. Liu, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Elisabeth C. Matthews, Brenda C. Matthews, Dimitri Mawet, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Paul Molliere, Eric Pantin, Andreas Quirrenbach, Isabel Rebollido, Bin B. Ren, Glenn Schneider, Malavika Vasist, Mark C. Wyatt, Yifan Zhou, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gabriele Cugno, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Kyle Franson, Eileen C. Gonzales, Callie E. Hood, Alex R. Howe, Adam L. Kraus, Masayuki Kuzuhara, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Raquel A. Martinez, Johan Mazoyer, Sascha P. Quanz, Jea Adams Redai, Matthias Samland, Joshua E. Schlieder, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Johanna M. Vos, Kevin Wagner, Schuyler G. Wolff, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang
Figure caption: The full spectrum of VHS 1256 b using JWST's NIRSpec IFU and MIRI MRS observation modes. Bandpasses are highlighted in different colors, and error bars are displayed in gray. A single photometric point for MIRI MRS Channel 4A is shown because there is little to no signal in the MIRI MRS 4B and 4C channels. Error bars are plotted in light gray.Reduced spectra are behind the figure but also hosted online.
Paper: Probing the Nature of the First Galaxies with JWST and ALMA
Authors: María Emilia De Rossi, Volker Bromm
Figure caption: Average FIR flux associated with ALMA band 7, as a function of M * for model galaxies at z = 13. Left-hand panel: comparison between dust models that adopt different grain size distributions (standard and shock, shown in black and red, respectively) and chemical compositions (UM-D-20 and M-ND-170, shown with dashed and dotted lines, respectively; for a given size distribution, all other chemical models lead to an intermediate behavior). Right-hand panel: effects of varying the dust-to-metal ratio (D/M), gas-phase metallicity (Z g), and star formation efficiency (η) of dark matter halos; results correspond to our default dust chemistry (UM-ND-20), assuming a standard (thin lines) and shock (thick lines) grain size distribution. Different symbols depict upper limits (arrows) and a tentative value (green symbol) discussed in the literature (see the text for details). Within our model uncertainties, current upper limits are not consistent with our maximum D/M.
Paper: Probing the Nature of the First Galaxies with JWST and ALMA
Authors: María Emilia De Rossi, Volker Bromm
Figure caption: Average FIR flux within available ALMA bands (3–10) vs. central band frequency, for a model source of M * = 109 M ⊙ at z = 13. Results correspond to the same models shown in Figure 1. Left-hand panel: comparison between dust models that adopt different grain size distributions (standard vs. shock) and chemical compositions (UM-D-20 vs. M-ND-170), for a given size distribution; all other chemical models generate an intermediate behavior. Right-hand panel: effects of varying the dust-to-metal ratio (D/M), gas-phase metallicity (Z g), and star formation efficiency (η). Here, results correspond to our default dust chemistry (UM-ND-20), again assuming a standard (thin lines) and shock (thick lines) grain size distribution.
Paper: The Chocolate Chip Cookie Model: Dust-to-metal Ratio of H II Regions
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Qi Zeng, 琪 曾
Figure caption: The dependence of τ cl on stellar mass M * and metallicity 12+﹩\mathrm{log}({\rm{O}}/{\rm{H}})﹩. Top left panel: M *–Z relation; τ cl is color-coded. The circles represent the 30 subsamples of galaxies in M * and Z bins, while the small black dots in background are all sample galaxies. The solid curve is the fitted M *–Z relation of Equation (6). Top right panel: M *–τ cl relation; metallicity is color-coded. The dots connected by dotted lines represent the subsample of galaxies in 30 stellar mass and metallicity bins, while the squares show the median τ cl values in ten stellar mass bins irrespective of metallicity. The solid curve is the fitted M *–τ cl relation of Equation (7). Bottom left panel: the residual ﹩{\rm{\Delta }}\mathrm{log}{\tau }_{\mathrm{cl}}{\rm{-}}{\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩ relation color-coded with the M * of different stellar mass bins. The galaxy bins with the same stellar mass are connected by black dashed lines. The best fit and the confidence level of 1σ are shown by the blue solid curve and shadowed regions. The dashed orange diagonal line (﹩{\rm{\Delta }}\mathrm{log}{\tau }_{\mathrm{cl}}={\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})﹩) is plotted for comparison. Bottom right panel: M *–ζ relation color-coded with the metallicity. The data points are the same as that of the top left panel. The solid curve follows Equation (9).
Paper: Origin of Isotopic Diversity among Carbonaceous Chondrites
Authors: Jan L. Hellmann, Jonas M. Schneider, Elias Wölfer, Joanna Drążkowska, Christian A. Jansen, Timo Hopp, Christoph Burkhardt, Thorsten Kleine
Figure caption: Accretion ages of carbonaceous chondrite parent bodies vs. matrix mass fraction. Accretion ages are estimated based on chondrule formation ages and thermal evolution models (see Table A3 for details). Matrix mass fraction are from Hellmann et al. (2020).
Paper: The Chocolate Chip Cookie Model: Dust-to-metal Ratio of H II Regions
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Qi Zeng, 琪 曾
Figure caption: The stellar reddening E s (top panel) and nebular reddening E g (bottom panel) as a function of stellar mass for face-on SFGs. In each panel, the black line represents the median E s (or E g), where the two black dashed lines are the 16th and 84th percentiles of E s (or E g) respectively. For each stellar mass bin, the colored dots further show the median E s (or E g) of three different metallicity bins, which are color-coded according to the color bar plotted on the top of the figure.
Paper: The Chocolate Chip Cookie Model: Dust-to-metal Ratio of H II Regions
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Qi Zeng, 琪 曾
Figure caption: Sketch diagram of simplified CCC model for a face-on disk galaxy inside a fiber aperture (radius R ap), where a single layer of individual H II regions (blue clouds; intrinsic optical depth τ cl, and dust-shell thickness l) is sparsely embedded in the middle of a thick ISM disk (gray background; total optical depth τ s along the line of sight).
Paper: The Chocolate Chip Cookie Model: Dust-to-metal Ratio of H II Regions
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Qi Zeng, 琪 曾
Figure caption: The dependence of ﹩\mathrm{log}\zeta ﹩ on 12+﹩\mathrm{log}({\rm{O}}/{\rm{H}})﹩ with stellar mass color-coded, where the ﹩\mathrm{log}\zeta ﹩ is interpreted by ﹩\mathrm{log}{\tau }_{\mathrm{cl}}-\mathrm{log}({\rm{O}}/{\rm{H}})﹩. The dotted–dashed line has a slope of 1.45, and the dashed line represents the DTM as a constant.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: Comparison of metallicity-scaled molecular abundances of hot cores between SMC (red; this work), LMC (yellow), and Galactic sources (cyan). Abundances of SMC and LMC hot cores are multiplied by the corresponding metallicity factors (see Section 4.3). The area with thin vertical lines indicates the error bar for SMC/LMC sources, while those of Galactic sources indicate the lower and upper quartiles of the abundance distribution. The bar with a color gradient indicates an upper limit. See Section 4.3 for details.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: Integrated intensity distributions of molecular emission lines. Gray contours represent the 850 μm continuum distribution, and the contour levels are 3σ, 6σ, 15σ, and 40σ of the rms noise (0.03–0.04 mJy beam−1). Low signal-to-noise ratio regions (S/N<1.5) are masked. The spectra discussed in the text are extracted from the region indicated by the black open circle. The blue cross represents the infrared peak position. The synthesized beam size is shown by the gray filled circle in each panel. North is up, and east is to the left.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: ALMA spectra of molecular emission lines detected in S07. The blue lines represent fitted Gaussian profiles. For SO2 and CH3OH, the spectra are sorted in ascending order of the upper-state energy (the emission line with the lowest upper-state energy is shown in the upper left panel and that with the highest energy is in the lower right panel). The adjacent stronger line seen in SO2(164,12–163,13) was subtracted before fitting the main line.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: Results of rotation diagram analyses. Upper limit points are indicated by the down arrows. The solid lines represent the fitted straight line, while the dashed lines indicate the acceptable fits within 2σ level. Derived column densities and rotation temperatures are shown in each panel. See Section 3.3 for details.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: SO2 column densities plotted against those of SO (a) and SiO (b) for SMC (red), LMC (orange), and Galactic (gray) hot cores. The dotted lines in panel (a) represent a ratio of 2:1, 1:1, and 1:2. The correlation coefficient (R coef) is indicated.
Paper: The Detection of Hot Molecular Cores in the Small Magellanic Cloud
Authors: Takashi Shimonishi, Kei E. I. Tanaka, Yichen Zhang, Kenji Furuya
Figure caption: Location of the present hot cores, S07 and S09, within the SMC (the green solid circle). The background is a Herschel/PACS 160 μm image obtained by the HERITAGE program (Meixner et al. 2013). North is up, and east is to the left.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Top left: F606W + F814W HST/ACS image of the linear feature and its surroundings. Top right: zoomed view of the F606W image. The feature shows a compact bright spot at the narrow tip and seems to broaden toward the galaxy. Bottom left: color image, generated from the F606W and F814W images. Bottom right panels: sections of LRIS spectra near bright emission lines. The feature and the galaxy are at the same redshift. The kinematics and line strengths show complex variations along the feature.
Paper: A Candidate Runaway Supermassive Black Hole Identified by Shocks and Star Formation in its Wake
Authors: Pieter van Dokkum, Imad Pasha, Maria Luisa Buzzo, Stephanie LaMassa, Zili Shen, Michael A. Keim, Roberto Abraham, Charlie Conroy, Shany Danieli, Kaustav Mitra, Daisuke Nagai, Priyamvada Natarajan, Aaron J. Romanowsky, Grant Tremblay, C. Megan Urry, Frank C. van den Bosch
Figure caption: Morphology of the galaxy in F606W and F814W. The arrow indicates the direction of the linear feature. The galaxy is compact, with a half-light radius of r e = 1.2 kpc, and shows irregular features possibly indicating a recent merger and/or a connection to the linear feature.
Paper: Origin of Isotopic Diversity among Carbonaceous Chondrites
Authors: Jan L. Hellmann, Jonas M. Schneider, Elias Wölfer, Joanna Drążkowska, Christian A. Jansen, Timo Hopp, Christoph Burkhardt, Thorsten Kleine
Figure caption:  μ 50Ti and μ 54Cr isotope anomalies of carbonaceous chondrites. (a) Average isotopic compositions of major carbonaceous chondrite groups (black; see Table A1), individual ungrouped and anomalous carbonaceous chondrites from this study (solid blue) and previous studies (light blue; Bischoff et al. 2021 [B21]; Torrano et al. 2021 [T21]), as well as of Orgueil (CI1) and GRO 95577 (CR1). (b) Isotopic compositions of individual carbonaceous chondrites from this study and previous studies as in Figure 2(a). The red open square represents the average μ 50Ti and μ 54Cr isotope anomalies of pooled chondrules from the CV chondrite Allende (Gerber et al. 2017; Schneider et al. 2020). The mixing line between chondrules and CI chondrites (dashed line) was calculated using elemental abundances (CI chondrites, Ti = 440 ppm, Cr = 2620 ppm; chondrules, Ti = 1200, Cr = 3200) and isotopic compositions (CI chondrites, μ 50Ti = 194, μ 54Cr = 173; chondrules, μ 50Ti = 242, μ 54Cr = 58) from this and previous studies (e.g., Gerber et al. 2017; Alexander 2019; Zhu et al. 2019; Schneider et al. 2020). The solid lines represent mixing lines for chondrules and refractory inclusions (CAIs and AOAs) at a given matrix mass fraction. For the refractory inclusions we used previously published isotopic data (μ 50Ti = 900; μ 54Cr 600; Papanastassiou 1986; Birck & Lugmair 1988; Trinquier et al. 2009; Larsen et al. 2011; Davis et al. 2018; Render et al. 2019; Torrano et al. 2019) and elemental abundances (CAIs, Ti = 5400 ppm, Cr = 200 ppm; AOAs, Ti = 2200, Cr = 2000; Komatsu et al. 2001; Trinquier et al. 2009) and a 1:1 CAI–AOA ratio (e.g., Ebel et al. 2016). The CAI-to-AOA ratio in carbonaceous chondrites is not well constrained and may vary among different groups. High CAI-to-AOA ratios will result in steeper mixing lines than low CAI-to-AOA ratios.
Paper: Origin of Isotopic Diversity among Carbonaceous Chondrites
Authors: Jan L. Hellmann, Jonas M. Schneider, Elias Wölfer, Joanna Drążkowska, Christian A. Jansen, Timo Hopp, Christoph Burkhardt, Thorsten Kleine
Figure caption: Cartoon illustrating our preferred scenario for transport and mixing of dust components before and during the accretion of the carbonaceous chondrite parent bodies. Based on the model of Nanne et al. (2019) for the formation of the NC–CC dichotomy by time-varied infall from heterogeneous molecular cloud core. (a) Early infall had a CAI/AOA-like isotopic composition (blue), which reflects the isotopic composition of the early disk formed by viscous spreading. CAIs and AOAs are transported outward by the same process. (b) Isotopic composition of the infall changes to NC-like (red), which dominates the inner disk. Chondrule precursors form in the inner disk and, like CAIs and AOAs, are transported outwards through the disk. After infall stopped, the disk exhibits an isotopic gradient from NC-like in the inner disk to CAI/AOA-like material in the outer disk. Mixing between these distinct materials in the inner disk then produced the characteristic isotopic composition of the CC reservoir. (c) Radial drift of CAIs, AOAs, and chondrule precursors leads to their coupled enrichment in a pressure maximum, which is likely associated with the water ice line and the ultimate formation location of Jupiter. Chondrule formation and mixing of CAIs/AOAs, chondrules, and CI-like matrix occur in this pressure trap, where the relative proportions of these components vary depending on the timing of parent body accretion.
Paper: Origin of Isotopic Diversity among Carbonaceous Chondrites
Authors: Jan L. Hellmann, Jonas M. Schneider, Elias Wölfer, Joanna Drążkowska, Christian A. Jansen, Timo Hopp, Christoph Burkhardt, Thorsten Kleine
Figure caption: Mass-dependent Te isotope fractionation and nucleosynthetic Cr isotope anomalies of carbonaceous chondrites. (a) Tellurium isotopic compositions and concentrations of ungrouped and anomalous carbonaceous chondrites (blue). All of the samples plot on the mixing line defined by individual samples of the major carbonaceous chondrite groups (black; Hellmann et al. 2020). (b) Tellurium isotopic compositions and μ 54Cr isotope anomalies of ungrouped and anomalous carbonaceous chondrites (blue). Black open squares represent the average compositions of the major carbonaceous chondrite groups, and red open squares represent the average compositions of CO, CV, and CM as well as CR chondrules. Dashed lines are calculated chondrule-matrix mixing lines between chondrules and CI chondrites (CI, Te = 2.28 ppm, Cr = 2620 ppm; CO-CV-CM chondrules, Te = 0.35 ppm, Cr = 3200; CR chondrules, Te = 0.35 ppm, Cr = 4320 ppm; Gerber et al. 2017; Alexander 2019; Zhu et al. 2019; Hellmann et al. 2020; Schneider et al. 2020). The δ 128/126Te data are from Hellmann et al. (2020), and μ 54Cr data of carbonaceous chondrites and chondrules are compiled in Tables A1 and A2, respectively.