adsabs/AstroCLIMB huggingface dataset:
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Resolved stellar populations based on SED fitting of the JWST imaging. The top row shows maps of the stellar mass (left), SFR (middle), and specific SFR (right) from spatially resolved SED modeling of the JWST images. The bottom row shows the radial surface density profiles of the stellar mass, SFR, and specific SFR, respectively. A clear central depression can be seen in the specific SFR, a feature that is typically seen in bulge–disk systems growing inside out.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Surface brightness profiles of F444W (left), Hα (center), and the radial Hα equivalent-width profile (right) made as described in Section 4. The top row shows radially averaged profiles, while the bottom shows the full vertical profile. The Hα distribution is much less centrally concentrated than the 4.4 μm continuum emission resulting in an Hα equivalent-width profile that rises from the center to 2 kpc, consistent with this z = 5.388 galaxy growing inside out in a bulge–disk system.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Velocity-coded map of the Magellanic System in an orthographic projection with LMC at the center, displaying the locations of 28 HST/COS background quasar sight lines (circles) from K22 with respect to the H I emission (color scale). The sight lines are color coded based on the column-density-weighted central LSR velocity of the Magellanic Si II absorption. Magellanic absorbers are those with v LSR > 150 km s−1 (see text in Section 2). Sight lines with Si II nondetections at Magellanic velocities are marked with red symbols with a cross. The map includes high-velocity 21 cm H I emission data from T. Westmeier (2018), color coded by LSR velocity.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Total column density of Magellanic gas as a function of LMC impact parameter. The profiles of six low ions and one intermediate ion (Si III) are shown in red. For comparison, the profiles for the high ions Si IV and C IV are included in green; these data are taken from K22 along with additional C IV and Si IV components identified toward RBS 567 and IRAS Z06229–6434. Open circles with downward arrows indicate 3σ upper limits, while circles with upward arrows represent lower limits from saturated lines. The best-fit log–linear relations for MCMC runs with 1σ scatter (shaded regions) are shown as solid lines with the relation labeled in the bottom left corner of each panel. The best-fit relations using the normalized impact parameter instead of ρ LMC are the same with the slopes scaled by R 200 = 115 ± 15 kpc (see K22). In this plot, Magellanic components are defined as those with v LSR > 150 km s−1.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Velocity-position analysis of gas in the LMC CGM. LSR velocity is plotted against LMC impact parameter both for individual components (steel-blue stars) and for the column-density-weighted central velocity of all Magellanic components along each sight line (large blue stars). The solid vertical lines in steel blue connect the different velocity components of each sight line and illustrate the dispersion of LMC gas in each direction. The horizontal dashed–dotted black line represents the LMC systemic velocity of 280 km s−1. The shaded gray area indicates the region within ±50 km s−1 of the LMC velocity. The shaded area in magenta marks the region where the gas velocities change substantially; this truncation point separates the inner CGM from the Stream.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Column-density profiles of the CGM in four low ions, comparing the LMC to isolated dwarf galaxies in the literature. The red points show the total column density of LMC components at v LSR > 230 km s−1 (a range chosen to exclude the Stream) as a function of impact parameter normalized by the virial radius. Open symbols indicate the 3σ upper limits for nondetections. The 50th percentile solution of the power-law model for MCMC runs for the LMC is shown in the red solid line with 1σ scatter of the fit shown in shaded red. For comparison, the profiles from the CGM of isolated dwarf galaxies taken from Y. Zheng et al. (2024a) are shown in black in each panel with 1σ uncertainty in gray.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: HST/COS metal-line profiles showing the absorption at Magellanic velocities toward 1H0419–577, as an example of our data quality and fitting methodology. Normalized flux is plotted against the LSR velocity in blue. The solid red lines represent the full Voigt-profile fits to the low ions from this study, while the solid green lines show the fits to the high ions from K22. The individual components are shaded in different colors, with centroids marked by tick marks. The color scheme differs between low and high ions.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Same as Figure 2. We indicate the locations of blended regions with “B” in red and exclude these regions from the fitting.
Paper: The Truncated Circumgalactic Medium of the Large Magellanic Cloud 
Authors: Sapna Mishra, Andrew J. Fox, Dhanesh Krishnarao, Scott Lucchini, Elena D'Onghia, Frances H. Cashman, Kathleen A. Barger, Nicolas Lehner, Jason Tumlinson
Figure caption: Same as Figure 2.
Paper: Small-scale Current Sheets and Associated Switchback Activity in the Inner Heliosphere
Authors: Sydney Furman, Alexandros Chasapis, David Malaspina, Peter Tatum, Benjamin Short, Harriet George, Mihailo Martinović
Figure caption: An example of the magnetic field (B), PVI index, and normalized deflection parameter (z) over a 6 hr period during PSP’s fourth solar encounter. B is shown in panel (a) in RTN coordinates, the PVI index is shown in panel (b), and the normalized deflection parameter is shown in panel (c). Three regions are shown, marked as Region 1, 2, and 3, shaded in red, green, and blue, respectively. Region 1 shows switchback activity along with many current sheets. Region 2 is less turbulent, without any switchbacks, and few current sheets are detected. Region 3 shows minimal switchbacks, but many current sheets are present.
Paper: Small-scale Current Sheets and Associated Switchback Activity in the Inner Heliosphere
Authors: Sydney Furman, Alexandros Chasapis, David Malaspina, Peter Tatum, Benjamin Short, Harriet George, Mihailo Martinović
Figure caption: SDK for each component of the magnetic field measured by PSP during the three intervals highlighted in Figure 1. Each panel corresponds to a 1 hr region, with Region 1 in panel (a), Region 2 in panel (b), and Region 3 in panel (c). Each line corresponds to one of the magnetic field vector components measured in RTN coordinates. The x-axis shows the time lag value in seconds, corresponding to the scale at which the magnetic field increments were calculated.
Paper: Small-scale Current Sheets and Associated Switchback Activity in the Inner Heliosphere
Authors: Sydney Furman, Alexandros Chasapis, David Malaspina, Peter Tatum, Benjamin Short, Harriet George, Mihailo Martinović
Figure caption: Orbital plots showing how the number of switchback regions and current sheets changes as PSP orbits the Sun. Each line is one of the three encounters examined here. The horizontal and vertical axes show the spacecraft position in X and Y heliocentric coordinates, respectively, roughly corresponding to the plane of the ecliptic. The left panel shows the number of current sheets within a 1 hr window for each point of the orbit. The right panel shows the percentage of time with normalized deflection value z > 0.5, indicating stronger switchback activity. A small region circled in red indicates a CME encountered by PSP.
Paper: Small-scale Current Sheets and Associated Switchback Activity in the Inner Heliosphere
Authors: Sydney Furman, Alexandros Chasapis, David Malaspina, Peter Tatum, Benjamin Short, Harriet George, Mihailo Martinović
Figure caption: A two-dimensional histogram relating PVI maxima to local normalized deflection values. Pink boxes indicate more events occurring with the associated z and PVI values than the values associated with the blue boxes. Each column has been normalized to one, making the values in each box the quotient of the total events in each box and the total events in the corresponding column. White boxes indicate no events were detected with those associated PVI and z values. The color bar shows the raw number of events detected.
Paper: Small-scale Current Sheets and Associated Switchback Activity in the Inner Heliosphere
Authors: Sydney Furman, Alexandros Chasapis, David Malaspina, Peter Tatum, Benjamin Short, Harriet George, Mihailo Martinović
Figure caption: A two-dimensional histogram relating PVI maxima and the percent of the hour during which they occurred that PSP spent in a switchback region. Deeper blues correspond to a higher frequency of events. Similar to the above two-dimensional histogram, each column has been normalized to one. White boxes indicate no events were detected with those associated PVI and z values. The color bar shows the raw number of events detected.
Paper: Bolometric Corrections for FU Ori Object Accretion Disk Luminosities
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand
Figure caption: The normalized filter profiles for the LSST, Roman, and WISE filters (colored lines), plotted against our fiducial ﹩\dot{M}={10}^{-4.5}\ {M}_{\odot }﹩ yr−1 FU Ori object SED model (black). The filled boxes at the top show the approximate total wavelength coverage of each survey or mission. The optical ZTF and Gaia filters overlap the LSST bands, and the 2MASS filters overlap the Roman bands.
Paper: Bolometric Corrections for FU Ori Object Accretion Disk Luminosities
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand
Figure caption: The bolometric corrections (filled circles) and our polynomial fits (solid lines). The visible range surveys in the top row are ZTF (left), Gaia (center), and LSST (right). The infrared surveys along the bottom are Roman (left), 2MASS (center), and WISE (right).
Paper: Bolometric Corrections for FU Ori Object Accretion Disk Luminosities
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand
Figure caption: The M  Ks  vs. extinction-corrected J − Ks color–magnitude space, with the locations of V960 Mon (blue point) and HBC 722 (green “x”) marked. The grid of accretion disk model values is plotted in gray, with constant R outer tracing approximately vertical lines and constant L acc approximately horizontal. The values at the top of the grid mark R outer in units of R ⊙ for each set of models, and values along the lower boundary of the grid mark a few L acc values in units of L ⊙ for reference. Models with R outer > 200 R ⊙ converge in this color space. Notice that both V960 Mon and HBC 722 lie along tracks that agree with their measured R outer values (blue and red text, respectively) in this space.
Paper: An Extremely Low-density Exoplanet Spins Slow
Authors: Quanyi Liu, 权毅 刘, Wei Zhu, 伟 祝, Kento Masuda, 田賢人 増, Jessica E. Libby-Roberts, Aaron Bello-Arufe, Caleb I. Cañas
Figure caption: Light curves from different reductions (upper panel) and different wavelength channels (lower channel). The out-of-transit variations of jwst and Eureka! reduction are ∼650 and ∼580 ppm, respectively, and <1.3 and >1.3 μm channels are ∼950 and ∼880 ppm. A spot-crossing event occurred near the midtransit. Its amplitude decreases with increasing wavelength, as expected.
Paper: An Extremely Low-density Exoplanet Spins Slow
Authors: Quanyi Liu, 权毅 刘, Wei Zhu, 伟 祝, Kento Masuda, 田賢人 増, Jessica E. Libby-Roberts, Aaron Bello-Arufe, Caleb I. Cañas
Figure caption: The white light curve and the best-fit oblate model of Kepler-51d. The top panel shows the original data points (blue and gray), the 5 minutes-binned data points (black), and the best-fit oblate model (red). Data points affected by the spot-crossing event are shown in gray and excluded in the modeling. The middle panel shows the residuals after subtracting the best-fit spherical model, thus highlighting the systematic trend in the original light curve. The bottom panel shows the residuals after subtracting the full model (including both spherical model and the systematic trend) to highlight the detectability of the oblateness signal. The vertical dashed lines in all panels indicate the four contact points according to the best-fit oblate model. The oblate model used here has f ⊥ = 0.05 and θ ⊥ = 55°.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: Schematic of the “home” positions of the four slits in the VELC spectroscopy channel. The inner filled black circle corresponds to the occulter (radius = 1.05 R ⊙). The white circular patch indicates the FOV, i.e., 1.05–1.5  R ⊙. Solar north and east directions are straight up and to the left, respectively.
Paper: New Results on the Onset of a Coronal Mass Ejection from 5303 Å Emission Line Observations with VELC/ADITYA-L1
Authors: R. Ramesh, V. Muthu Priyal, Jagdev Singh, K. Sasikumar Raja, P. Savarimuthu, Priya Gavshinde
Figure caption: Optical layout of VELC.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Lifetime of carbonaceous dust grains in the putative ring as a function of grain size. Curves with circle and triangle symbols mark the starting distances that correspond to the 3:1 spin–orbit resonances with P = 11.4 hr and 22.8 hr, while red and blue curves correspond to ring opening angles of 0° and 15°, respectively. We used Makemake’s heliocentric distance at the time of the occultation on 2011 April 23.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: SED of different potential ring materials, normalized to the observed flux density at 18 μm (JWST/MIRI F1800W filter). The colors are the same as in Figure 8. Solid and dashed curves correspond to the same material but using 100 nm and 200 nm grain sizes, respectively. The orange dashed–dotted curve is for graphite grains with 500 nm grain size. The black symbols with error bars are the mean MIRI F1800W and F2550W and MIPS 24 μm flux densities.
Paper: Prominent Mid-infrared Excess of the Dwarf Planet (136472) Makemake Discovered by JWST/MIRI Indicates Ongoing Activity
Authors: Csaba Kiss, Thomas G. Müller, Anikó Farkas-Takács, Attila Moór, Silvia Protopapa, Alex H. Parker, Pablo Santos-Sanz, Jose Luis Ortiz, Bryan J. Holler, Ian Wong, John Stansberry, Estela Fernández-Valenzuela, Christopher R. Glein, Emmanuel Lellouch, Esa Vilenius, Csilla E. Kalup, Zsolt Regály, Róbert Szakáts, Gábor Marton, András Pál, Gyula M. Szabó
Figure caption: Time evolution (from left to right) of small grains around Makemake under the influence of solar radiation pressure.
Paper: Limits on Planetary-mass Primordial Black Holes from the OGLE High-cadence Survey of the Magellanic Clouds
Authors: Przemek Mróz, Andrzej Udalski, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Radosław Poleski, Jan Skowron, Krzysztof Ulaczyk, Mariusz Gromadzki, Krzysztof Rybicki, Patryk Iwanek, Marcin Wrona, Mateusz J. Mróz
Figure caption: Expected number of microlensing events in the OGLE High-cadence Magellanic Cloud Survey assuming that the entire dark matter is composed of PBHs or other compact objects of a given mass. The dashed and dotted lines mark the contributions from the sources in the LMC and SMC, respectively.
Paper: GRB 240529A: A Tale of Two Shocks
Authors: Tian-Rui Sun, Jin-Jun Geng, Jing-Zhi Yan, You-Dong Hu, Xue-Feng Wu, Alberto J. Castro-Tirado, Chao Yang, Yi-Ding Ping, Chen-Ran Hu, Fan Xu, Hao-Xuan Gao, Ji-An Jiang, Yan-Tian Zhu, Yongquan Xue, Ignacio Pérez-García, Si-Yu Wu, Emilio Fernández-García, María D. Caballero-García, Rubén Sánchez-Ramírez, Sergiy Guziy, I. Olivares, Carlos Jesus Pérez del Pulgar, A. Castellón, S. Castillo, Ding-Rong Xiong, Shashi B. Pandey, David Hiriart, Guillermo García-Segura, William H. Lee, I. M. Carrasco-García, Il H. Park, S. Jeong, Petrus J. Meintjes, Hendrik J. van Heerden, Antonio Martín-Carrillo, Lorraine Hanlon, Bin-Bin Zhang, L. Hernández-García, Maria Gritsevich, Andrea Rossi, Elisabetta Maiorano, Felice Cusano, Paolo D'Avanzo, Matteo Ferro, Andrea Melandri, Massimiliano De Pasquale, Riccardo Brivio, Min Fang, Lu-Lu Fan, Wei-Da Hu, Zhen Wan, Lei Hu, Ying-Xi Zuo, Jin-Long Tang, Xiao-Ling Zhang, Xian-Zhong Zheng, Bin Li, Wen-Tao Luo, Wei Liu, Jian Wang, Hong-Fei Zhang, Hao Liu, Jie Gao, Ming Liang, Hai-Ren Wang, Da-Zhi Yao, Jing-Quan Cheng, Wen Zhao, Zi-Gao Dai
Figure caption: Modeling the multiwavelength afterglow of GRB 240529A with the two external shocks. The dotted and dashed lines represent emissions from the former and the later shocks, respectively, and the the solid lines are the sum of them. The X-ray data are taken from the Swift/XRT website (http://www.swift.ac.uk/xrt_curves/01231488/). The optical data are taken from Section 2 and GCN circulars (C. Adami et al. 2024; J. An et al. 2024; A. de Ugarte Postigo et al. 2024; D. Dutton et al. 2024; S. Y. Fu et al. 2024; G. Lim et al. 2024; G. Mo et al. 2024; T. Mohan et al. 2024; M. Niwano et al. 2024; M. Odeh et al. 2024; N. Pankov et al. 2024; A. K. Ror et al. 2024; A. Rossi et al. 2024; J. Vinko et al. 2024). The radio data are taken from L. Rhodes et al. (2024). Note that the prompt emission and the steep decay of the later burst are not used in the fitting. The optical data have been corrected for Galactic extinction of E(B − V) = 0.29 mag (E. F. Schlafly & D. P. Finkbeiner 2011). The excess of the modeling flux at the short wavelengths hints at the potential extinction of the host galaxy.
Paper: GRB 240529A: A Tale of Two Shocks
Authors: Tian-Rui Sun, Jin-Jun Geng, Jing-Zhi Yan, You-Dong Hu, Xue-Feng Wu, Alberto J. Castro-Tirado, Chao Yang, Yi-Ding Ping, Chen-Ran Hu, Fan Xu, Hao-Xuan Gao, Ji-An Jiang, Yan-Tian Zhu, Yongquan Xue, Ignacio Pérez-García, Si-Yu Wu, Emilio Fernández-García, María D. Caballero-García, Rubén Sánchez-Ramírez, Sergiy Guziy, I. Olivares, Carlos Jesus Pérez del Pulgar, A. Castellón, S. Castillo, Ding-Rong Xiong, Shashi B. Pandey, David Hiriart, Guillermo García-Segura, William H. Lee, I. M. Carrasco-García, Il H. Park, S. Jeong, Petrus J. Meintjes, Hendrik J. van Heerden, Antonio Martín-Carrillo, Lorraine Hanlon, Bin-Bin Zhang, L. Hernández-García, Maria Gritsevich, Andrea Rossi, Elisabetta Maiorano, Felice Cusano, Paolo D'Avanzo, Matteo Ferro, Andrea Melandri, Massimiliano De Pasquale, Riccardo Brivio, Min Fang, Lu-Lu Fan, Wei-Da Hu, Zhen Wan, Lei Hu, Ying-Xi Zuo, Jin-Long Tang, Xiao-Ling Zhang, Xian-Zhong Zheng, Bin Li, Wen-Tao Luo, Wei Liu, Jian Wang, Hong-Fei Zhang, Hao Liu, Jie Gao, Ming Liang, Hai-Ren Wang, Da-Zhi Yao, Jing-Quan Cheng, Wen Zhao, Zi-Gao Dai
Figure caption: The corner plot of the fitting result in Figure 2. It shows all the one- and two-dimensional projections of the posterior probability distributions of seven model parameters listed in Table 2. The one-dimensional histograms are marginal posterior distributions of these parameters, in which the vertical dashed lines indicate the 16th, 50th, and 84th percentiles of the samples, respectively.