adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Recycling Model of Phobos Formation: Rubble-pile Satellites 
Authors: Gustavo Madeira, Sébastien Charnoz, Yun Zhang, Ryuki Hyodo, Patrick Michel, Hidenori Genda, Silvia Giuliatti Winter
Figure caption: (a) Time span (left scale; solid line) and number of cycles (right scale; dotted line) to form a Phobos analog as a function of the initial disk mass. (b) Mass of the largest satellite in the cycle relative to the initial disk mass in the same cycle, with different colors corresponding to different disk mass. (c) Average optical depth of the residual ring coexisting with Phobos. We assumed a particle size of 10 m and friction angle of 40°. The open points in panel (b) correspond to the cycles that form a Phobos analog. The annotations in panel (c) give the mass of the residual ring.
Paper: Exploring the Recycling Model of Phobos Formation: Rubble-pile Satellites 
Authors: Gustavo Madeira, Sébastien Charnoz, Yun Zhang, Ryuki Hyodo, Patrick Michel, Hidenori Genda, Silvia Giuliatti Winter
Figure caption: (a) Time span (left scale; solid line) and number of cycles (right scale; dotted line) to form a Phobos analog as a function of the friction angle. (b) Mass of the largest satellite in the cycle in relation to the initial disk mass in the same cycle. (c) Average optical depth of the residual ring coexisting with Phobos. We assumed an initial disk mass of 1.1 × 104 M P and a particle size of 10 m. The open points in panel (b) correspond to the cycles that form a Phobos analog, while the annotations in panel (c) give the residual ring mass.
Paper: Exploring the Recycling Model of Phobos Formation: Rubble-pile Satellites 
Authors: Gustavo Madeira, Sébastien Charnoz, Yun Zhang, Ryuki Hyodo, Patrick Michel, Hidenori Genda, Silvia Giuliatti Winter
Figure caption: Temporal evolution of the (a) semimajor axis of the Phobos ancestor and Deimos, (b) eccentricity of Deimos, and (c) characteristic angles associated with the 2:1 MMR (see text). The Phobos ancestor is initially at 4 R M, and Deimos is at ∼7 R M. The N-body simulation approximately reproduces part of cycle 1 shown in Figure 4.
Paper: Exploring the Recycling Model of Phobos Formation: Rubble-pile Satellites 
Authors: Gustavo Madeira, Sébastien Charnoz, Yun Zhang, Ryuki Hyodo, Patrick Michel, Hidenori Genda, Silvia Giuliatti Winter
Figure caption: (a) Average optical depth of the ring coexisting with Phobos and (b) instant of the beginning of the recycling process (after Mars formation) as a function of the particle size. The solid lines with circles, dotted–dashed lines with stars, and dotted lines with triangles give the cases with ϕ = 25°, 40°, and 80°, respectively. The different colors correspond to different initial disk masses. The gray regions correspond to the forbidden region for the optical depth of the ring and instant of the giant impact.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Speckle ACFs of triple stars recorded at SOAR (negative intensity rendering, standard orientation, arbitrary scale). In each panel, the white dot O marks the center, other labels indicate correct peaks corresponding to components’ pairs (other peaks are symmetric counterparts or complementary pairs). (a) ϵ Cha on 2022.05, separations 0.″054 and 0.″147; insert shows the power spectrum. (b) I 385 on 2022.31, separations 0.″29 and 0.″41. (c) 06478+0822 on 2022.77, separations 0.″073 and 0.″34. (c) 08447−2126 on 2022.28, separations 0.″067 and 0.″48.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbital motion of the inner triple I 385. Top: motion of B relative to A (full line and green asterisks) or relative to the AD photocenter (blue dashed line and small diamonds). The magenta line and triangles show the orbit of A,D on the same scale. Star A is placed at the coordinate origin. The plot on the bottom shows angular separations of A,D versus time. The inner pair was closer than 0.″1 throughout most of the 20th century and for this reason it has been missed by visual observers.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Location of ϵ Cha components Aa, B, and Ab (red squares) on the (V, V − K) CMD. The error bar indicates the distance modulus uncertainty of ±0.08 mag. The magenta curve is a 5 Myr PARSEC isochrone for solar metallicity (Bressan et al. 2012) with masses marked by asterisks and numbers.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of ϵ Cha. The right-hand plot shows the full circular outer orbit (crosses denote the less accurate micrometer measurements, squares show the resolved speckle data). The left-hand plot shows SOAR measurements of the inner pair (magenta ellipse and triangles) and the wavy line of the Aa,B motion with the superimposed wobble. The blue dashed line shows outer orbit without wobble.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of HIP 32475 with periods of 12.2 yr and 80.3 yr. The blue dashed line marks the outer orbit without wobble that describes motion of BC around A, the black solid line is the motion of B relative to A. The orbit of B,C is plotted around coordinate origin on the same scale by the magenta line and triangles.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Closest neighbors of ϵ Cha (axis scale in arcseconds) in Gaia DR3.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Azimuthally averaged transmission in F606W and all four NIRCam passbands, from the zone of highest signal-to-noise ratio (S/N) in the transmission map (13° of azimuth in the spiral disk, on either side of the line between spiral and elliptical nuclei). This quantifies the sharp outer edge to the dust lanes seen in Figure 2, which is so complete that it is obvious even when averaged over all structure in the disk. Labeled curves show the various filter bands; F356W and F444W are distinguished by line thickness to reduce crowding. Unmasked pixels have been averaged in 10 pixel or 0.″3 radial bins. The radial location of the background elliptical-galaxy nucleus is shown for reference. The standard deviation of the mean in each bin would be only slightly wider than the plotted lines, so the structure reflects real variation within the galaxy. With a 26° sector width, spiral features give attenuation signatures where they cross it. At this redshift z = 0.051, 1″ = 1.008 kpc. Matching ripples in the profiles (most pronounced at radii 16.″5 and 20.″5) for F150W, F356W, and F444W may indicate genuine asymmetric structure in one of the galaxies, since each image was independently masked and modeled. Their amplitude would suggest an accuracy of 1.5% from such structure. This motivates our fitting techniques for reddening behavior to incorporate such local systematic factors as nuisance parameters.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Transmission (and attenuation) maps from HST and JWST data, spanning the observed range 0.33–4.4 μm. These represent our estimates of the transmitted light at each point; regions with more dust, giving less transmitted light, appear darker. The edge of the dust disk almost exactly crosses the background nucleus (marked with a black plus sign). The combination of better galaxy symmetry and better S/N makes the dust features best detectable at 0.9 μm, despite the larger attenuation at shorter wavelengths. The background galaxy is so dim at 0.33 μm that we can derive only spatially averaged quantities from that filter; for display, these data are median-smoothed by 0.″15 here. All brightness scales are the same, from 0.3–1.3, as shown in the scale bar (in transmission or residual intensity, to put unity at a conveniently visible level). The center of the spiral lies off the frame to the upper right. Each image section spans 15.″0 × 15.″9. Bright background objects and foreground stellar associations appear, which were masked for measurements of the dust effects. The F444W images shows ringlike artifacts to the right, from modeling the spiral disk, where masking during isophotal fits left poor residuals.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Sector of the disk of VV 191b used for the measurements in Figure 3, overlaid on the F090W attenuation map. The orientation is the same as in Figure 2, with north 24° clockwise from the right. Circular segments show fiducial radii from the nucleus of the spiral VV 191b, while radial lines show the azimuthal boundaries of the measured region with highest S/N (center ±13°). Black areas indicate distant background galaxies, gravitationally lensed images, or foreground star-forming regions masked from the fit here and in determining the wavelength behavior of attenuation. The center of the elliptical galaxy VV 191a is shown with a plus sign.
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Steps in the dust analysis, shown using the NIRCam F090W data. Upper left, original image (I in Equation (1)). Upper right, smooth and symmetric model for the foreground spiral (F in Equation (1)) . Lower left, model for the background elliptical (B in Equation (1)). Lower right, derived transmission map for the foreground galaxy (T = (I − F)/B), which is meaningful only in regions where the errors due to galaxy structure are small (as shown in Section 3).
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: Cumulative distributions of area with transmission less than the value on the x-axis for the three best-measured filter bands within the best-measured disk sector as shown in Figure 4. The mapped radial range 14–21 kpc is shown as a whole (solid line) and broken into inner (dotted–dashed) and outer (dashed) halves, as marked on the F606W panel. Pixels affected by unresolved sources, background galaxies, and emission from star-forming regions have been masked.(The data used to create this figure are available.)
Paper: JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191
Authors: William C. Keel, Rogier A. Windhorst, Rolf A. Jansen, Seth H. Cohen, Jake Summers, Benne Holwerda, Sarah T. Bradford, Clayton D. Robertson, Giovanni Ferrami, Stuart Wyithe, Haojing Yan, Christopher J. Conselice, Simon P. Driver, Aaron Robotham, Norman A. Grogin, Christopher N. A. Willmer, Anton M. Koekemoer, Brenda L. Frye, Nimish P. Hathi, Russell E. Ryan, Nor Pirzkal, Madeline A. Marshall, Dan Coe, Jose M. Diego, Thomas J. Broadhurst, Michael J. Rutkowski, Lifan Wang, S. P. Willner, Andreea Petric, Cheng Cheng, Adi Zitrin
Figure caption: The overall geometry of VV 191, illustrated with a composite of the HST F606W and F336W data in the blue channel, JWST NIRCam F090W in the green, and NIRCam F356W in red. Each is shown with a logarithmic intensity mapping, starting from slightly below the sky level to closely match the SDSS-style sinh mapping. The field shown is 29.″6 × 55.″0. The image is shown rotated by 27° clockwise from cardinal orientation in this display, to align with the separation of the galaxies. This shows the backlit dust lanes in front of the elliptical VV 191a, as well as a probable gravitationally lensed arc and counterimage behind VV 191a, and additional background galaxies with a wide range of colors and likely redshifts.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Possible scenario of forming hierarchical systems with comparable-mass components: triplets, quadruplets, and double twins.
Paper: Dynamics of Four Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of HIP 42910; periods 6.8 yr and 125 yr.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: Histograms illustrating the distribution of orbital eccentricity (top left), orbital period (top right), planet radius (bottom left), and planet mass (bottom right). In the top two panels, the yellow distribution indicates terrestrial VZ planets and the blue distribution is all known terrestrial planets. In the bottom two panels, the red distribution is all known planets within the VZ, regardless of their size. In all four plots the black distribution is all known planets regardless of radius or location.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: Histograms displaying distributions of stellar properties: stellar effective temperature (top left), surface gravity (top right), J-band magnitude (bottom left), and distance to star (bottom right). In yellow is the distribution for the host stars of terrestrial VZ planets, in blue is the host stars of all terrestrial planets, and the black distribution is all known planets regardless of size or location.
Paper: The Demographics of Terrestrial Planets in the Venus Zone
Authors: Colby Ostberg, Stephen R. Kane, Zhexing Li, Edward W. Schwieterman, Michelle L. Hill, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, James W. Head, Cayman T. Unterborn
Figure caption: Terrestrial planets from the NEA that spend any part of their orbit in the VZ. The inner VZ boundary is indicated by the left line, and the right line is the outer VZ boundary. Earth and Venus are shown for reference (blue stars).
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Our best-fit planetary model for a wide-orbit solution for the MOA-2020-BLG-208 event light curve, shown in black. The plot shows magnification over time (HJD′). The lower panel shows the residual of the observations from the fit model. Unfilled observation points are observations that were excluded from the fitting due to poor seeing or a χ 2 cut. See text for instrument details. Zoomed inset figures show the peak of the primary magnification, the anomaly, and a portion of light curve with a significant fitting difference compared to the close-orbit solution (see Figure 2). The best-fit single-source single-lens model is shown in gray.(The data used to create this figure are available.)
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: Our best-fit planetary model for a close-orbit solution for the MOA-2020-BLG-208 event light curve. All other details are the same as in Figure 1.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: The marginalized posterior distributions of the close model’s MCMC states. The thresholds for the data point colors are for χ 2 at 1, 4, 8, and 16, with samples above 16 not shown. Compare to the wide-solution model in Figure 5.
Paper: MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert
Authors: Greg Olmschenk, David P. Bennett, Ian A. Bond, Weicheng Zang, Youn Kil Jung, Jennifer C. Yee, Etienne Bachelet, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Brandon Munford, Yasushi Muraki, Arisa Okamura, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Michael D. Albrow, Sang-Mok Cha, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Grant Christie, Tony Cooper, John Drummond, Jonathan Green, Steve Hennerley, Jennie McCormick, L. A. G. Monard, Tim Natusch, Ian Porritt, Thiam-Guan Tan, Shude Mao, Dan Maoz, Matthew T. Penny, Wei Zhu, V. Bozza, Arnaud Cassan, Martin Dominik, Markus Hundertmark, R. Figuera Jaimes, K. Kruszyńska, K. A. Rybicki, R. A. Street, Y. Tsapras, Joachim Wambsganss, Ł. Wyrzykowski, P. Zieliński, Gioia Rau
Figure caption: The marginalized posterior distributions of the wide model’s MCMC states. The thresholds for the data point colors are for χ 2 at 1, 4, 8, and 16, with samples above 16 not shown. Compare to the close-solution model in Figure 6.