adsabs/AstroCLIMB huggingface dataset:
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top: CSFH as a function of the redshift. The circles with error bars show the results and 1σ uncertainties from J. C. J. D’Silva et al. (2023) at z < 5. The stars with error bars show the results and 1σ uncertainties at z ≳ 5 from Paper I. The horizontal error bars show both the 1σ spread of the redshift distribution in each bin and the width of the bin. The hatched region shows the 16th–84th percentile spread of the model fit to the data points from Paper I. Middle: CBHARH as a function of the redshift. Points and hatches have the same meaning as the top panel. The upward (downward) facing arrows show the lower (upper) limits at z ≳ 5.5 from Paper I. The last points of the CBHARH are highlighted in white to signify that they are uncertain and were not used in the model fitting. Bottom: percentage ratio of the model fits to the CBHARH and CSFH. The solid line shows the median, and the hatched regions show the 16th–84th percentiles propagated from the fits.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Corner plot of the posterior distribution of fesc for both stars (top left) and AGN (lower right) when fitting to the G. D. Becker & J. S. Bolton (2013) ﹩{\dot{n}}_{{\rm{ion}}}﹩ at z ≈ 4.75, the CMB optical depth at z > 15 and the unity ratio of ﹩{\dot{n}}_{{\rm{ion}}}(z=3)﹩ from AGN to stars found by B. M. Smith et al. (2020). The green shaded regions show the uniform prior distributions on fesc. Vertical dashed lines for the 1D histograms are the median and 16th–84th  percentiles. The median and 16th–84th  are quoted on top of the histograms, while the best-fit values are quoted in the legend. Black contours (bottom left) show the 16th, 50th, and 84th percentile levels of the posterior samples. The green square in the bottom left panel and the green lines in all panels show the maximum likelihood/best-fit values.
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Optical depth of CMB photons as a function of the redshift, τCMB(<z). The black hatched region shows the results for the hybrid model, as in Figure 6. The red-filled region shows the same AGN limits as in Figure 3. The blue-filled region shows the same stellar limits as in Figure 2, except that the upper/lower bounds correspond to primordial/solar metallicity to encompass the entire range of stellar chemistry. The filled horizontal band shows the 1σ range obtained from the Planck analysis of the CMB (Planck Collaboration 2020a, 2020b).
Paper: Dissecting Reionization with the Cosmic Star Formation and Active Galactic Nuclei Luminosity History
Authors: Jordan C. J. D'Silva, Simon P. Driver, Claudia D. P. Lagos, Aaron S. G. Robotham, Nathan J. Adams, Christopher J. Conselice, Brenda Frye, Nimish P. Hathi, Thomas Harvey, Anton M. Koekemoer, Rafael Ortiz, Massimo Ricotti, Clayton Robertson, Ross M. Silver, Stephen M. Wilkins, Christopher N. A. Willmer, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Dan Coe, Norman A. Grogin, Madeline A. Marshall, Nor Pirzkal, Russell E. Ryan, Haojing Yan
Figure caption: Top: cosmic ionizing emissivity as a function of the redshift, ﹩{\dot{n}}_{{\rm{ion}}}(z)﹩, from AGN only. The red-filled region minimum/maximum bounds by considering fesc = 1%/100% with the lighter red showing the 1σ uncertainty of the CAGNH fit propagated through. Bottom: neutral fraction as per Equation (3). The filled regions have the same meaning as the top panels. The gold star with the horizontal error bar shows the midpoint and 1σ uncertainty of reionization inferred from Planck Collaboration (2020a).
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Lomb–Scargle periodograms (left panel) and window functions (right panel) for J0551 from different datasets: HiPERCAM (blue), ARCTIC (green), GMOS (red), and the combined dataset (black). The horizontal dashed red line indicates the 4σ noise threshold computed from the mean noise level. The orange curves show the residual (prewhitened) periodograms after removing the identified frequencies. Vertical gray lines mark the prewhitened frequencies in each dataset.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The SED fitting (top) and the ﹩{L}_{{{\rm{C}}}^{18}{\rm{O}}(2-1)}﹩ fitting (bottom) results for the well-mixed model compared with the models that are settled. The figures follow the same notations as in Figure 3. The blue line shows the results for the well-mixed model, with the well-mixed dust grains, while the green, blue, and purple lines (and scatters) are three models with dust settling, which has αv = 10−4, 10−3, 10−2, respectively. Their best-fit Mdust are shown in the top panel. In the lower panel, three different grid points with ε = 0.02, 0.01, 0.005 are shown as scatter points, with their best-fit ε indicated by blue crosses and with their values annotated with arrows. The black horizontal line represents the observed ﹩{L}_{{{\rm{C}}}^{18}{\rm{O}}(2-1)}﹩, with the gray area indicating its uncertainty.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Combined normalized light curve of J0551 obtained with ARCTIC (green), GMOS (red), and HiPERCAM (blue) between 2023 November and 2025 April. Each point represents normalized flux as a function of Barycentric Julian Date (BJD–2460000). The data from different instruments were normalized by subtracting either a mean or unity flux level to ensure consistency across observing runs. The dashed horizontal line marks the zero-flux reference. The inset shows a zoomed-in view of the ARCTIC observations from 2024 January 19, covering a 4.8 hr sequence that reveals short-term variability on timescales of minutes. See Section 3 for more details.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Detected pulsation frequencies from HiPERCAM (blue), ARCTIC (green), GMOS (red), and the combined dataset (black), plotted as a function of their signal-to-noise ratios. Each symbol marks a prewhitened frequency, with the symbol size reflecting its associated uncertainty. Gray vertical bands indicate frequencies detected in at least two independent datasets, merged within a tolerance of ±11 μHz, consistent with the alias width expected from the temporal sampling of our ground-based observations.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The radial profiles of dust continuum (top) and C18O line emission (bottom) for well-mixed (orange lines) and structured (blue lines) models and the intermediate ones (gray dashed lines) in between. The dust and gas outer radii are also shown in two vertical dotted–dashed gray lines, and the vertical dashed gray line shows where the observation is getting optically thick in the inner disk. The notation follows Figure 5.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Evolutionary tracks in the radius-effective temperature plane for our DAQ models with different stellar masses and two core compositions. Solid (dashed) lines refer to ONe (CO) core composition. The diagonal solid and dashed lines mark the onset of crystallization.
Paper: DiskMINT: Self-consistent Thermochemical Disk Models with Radially Varying Gas and Dust—Application to the Massive, CO-Rich Disk of IM Lup
Authors: Dingshan Deng, Uma Gorti, Ilaria Pascucci, Maxime Ruaud
Figure caption: The results for the structured model compared with the MAPS observations in ALMA band 3. The top panel shows the comparison with the dust continuum emission at 110 GHz (A. Sierra et al. 2021), and the middle and bottom panels show the comparison with the C18O (1–0) line (K. Zhang et al. 2021). The notation follows Figure 5.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Volume mixing ratio of H2O (left) and CH4 (right) in the upper atmosphere of TOI-270 d (P = 1 mbar) for different magma ocean model scenarios. We show models with Kzz = 107 cm2 s−1, although the differences in the H2O and CH4 volume mixing ratios are negligible for different values of Kzz. Volume mixing ratios are plotted as a function of the iron mass fraction, shown as a percentage of the total mass of the nucleus (core + mantle). Different line styles represent different combinations of mantle–atmosphere and core–mantle boundary temperatures (Tm−a and Tc−m, respectively). The green shaded regions show the constraints on the volume mixing ratios of H2O and CH4 reported by B. Benneke et al. (2024), inferred from the JWST transmission spectrum of the planet.
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Metallicity ([M/H], left) and C/O ratio (right) of the upper atmosphere of TOI-270 d (P = 1 mbar) for different magma ocean model scenarios. [M/H] and C/O are plotted as a function of the iron mass fraction, shown as a percentage of the total mass of the nucleus (core + mantle). The metallicity [M/H] is calculated as [(C + O)/H] relative to solar abundances (M. Asplund et al. 2009), since carbon- and oxygen-bearing species are the main drivers of the metallicity constraints presented in B. Benneke et al. (2024). Different line styles represent different combinations of mantle–atmosphere and core–mantle boundary temperatures (Tm−a and Tc−m, respectively). The green shaded regions show the constraints on [M/H] and C/O reported by B. Benneke et al. (2024), inferred from the JWST transmission spectrum of the planet. The black dotted line in the right-hand panel shows the solar C/O value from M. Asplund et al. (2009).
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Schematic of the modeling framework used in this study. Chemical equilibrium between the core, mantle, and atmosphere is calculated using the model from H. E. Schlichting & E. D. Young (2022). Upper atmospheric temperature profiles are calculated using HELIOS (M. Malik et al. 2017). FASTCHEM COND (J. W. Stock et al. 2022) is used to find equilibrium chemical abundances throughout the upper atmosphere, accounting for rainout condensation. After iterating between HELIOS and FASTCHEM COND until convergence is reached, we account for photochemical processes and vertical mixing using Photochem (N. F. Wogan et al. 2023, 2025).
Paper: Magma Ocean Interactions Can Explain JWST Observations of the Sub-Neptune TOI-270 d
Authors: Matthew C. Nixon, R. Sander Somers, Arjun B. Savel, Jegug Ih, Eliza M.-R. Kempton, Edward D. Young, Hilke E. Schlichting, Tim Lichtenberg, Luis Welbanks, William Misener, Anjali A. A. Piette, Nicholas F. Wogan
Figure caption: Temperature profiles for TOI-270 d from HELIOS. Each panel shows a different combination of core–mantle and mantle–atmosphere boundary temperatures. The different colors and line styles for each profile represent different iron mass fractions, shown as a percentage of the mass of the nucleus of the planet (i.e., the iron and silicate components).
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Left: light curve of the target obtained with HiPERCAM on 2024 November 22 (see Section 3). HiPERCAM filters us, gs, rs, is, zs are shown from top to bottom. Right: corresponding Fourier transform of the same light curve, illustrating the detected periodicities.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Left: light curve of the target obtained with HiPERCAM on 2025 January 8 (see Section 3). HiPERCAM filters us, gs, rs, is, zs are shown from top to bottom. Right: corresponding Fourier transform of the same light curve, illustrating the detected periodicities.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Fourier transforms of the light curves obtained with APO and Gemini.
Paper: Multiperiodic Pulsations of the Unique DAQ White Dwarf J0551+4135: Insights into a Merger Remnant
Authors: Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Alejandro H. Córsico, Gracyn Jewett, Adam Moss, Alberto Rebassa-Mansergas, Alex J. Brown, Maria Camisassa, Pierre Bergeron
Figure caption: Light curves obtained with APO and Gemini.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Heating rates shown on a meridional slice through the active region. The first column is at t = 0 minute, the second at t = 30 minutes, and the third at t = 60 minutes post-eruption. The first row shows the Alfvén wave heating rate, the second row shows the negative divergence of the electron heat flux, the third row shows the radiative cooling rate, and the fourth row shows the adiabatic heating rate. The white lines represent the magnetic field lines in the flux rope and surrounding corona.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Current sheet formation (top row) and heating (electron and proton temperatures; middle and bottom rows, respectively) on a meridional plane through the active region at t = 5, 15, 30, 45, and 60 minutes post-eruption (columns from left to right). We represent the current sheet using the J/B ratio (top row), which increases its value by orders of magnitude. The magnetic field lines are shown in white (top) and black (middle and bottom) with the arrows representing the polarity.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: For the flux rope base parcel, the top panel shows the electron (black) and proton (blue) temperature and density (green) evolution with time/distance. The bottom panel shows the evolution of the heating/cooling rates, including Alfvén wave heating (gray), heat conduction (red), adiabatic expansion (yellow), and radiative cooling (purple). Panel (A) (shaded purple) shows a snapshot at t = 15 minutes in the Z = 0 plane through the active region of the wave dissipation, the field lines (black), and the trajectory of the parcel before (red) and after (black). Panel (B) (shaded blue) shows the heat conduction on a meridional plane through the CME, intersecting with the parcel location (blue) at t = 45 minutes. Panel (C) (shaded green) shows the heat conduction on a meridional plane through the CME, intersecting with the parcel location (black) at t = 2.5 hr.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: For the prominence parcel, the top panel shows the electron (black) and proton (dotted blue) temperature and density (green) evolution with time/distance. The bottom panel shows the evolution of the heating/cooling rates, including Alfvén wave heating (gray), heat conduction (red), adiabatic expansion (yellow), and radiative cooling (purple). Panel (A) (shaded purple) shows a snapshot at t = 45 minutes of the heat conduction, where the black line is the trajectory of the parcel. Panel (B) (shaded green) shows a snapshot at t = 75 minutes of the adiabatic expansion, where the black line is the trajectory of the parcel at that time.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: For the cavity parcel, the top panel shows the electron (black) and proton (blue) temperature and density (green) evolution with time/distance. The bottom panel shows the evolution of the heating/cooling rates, including Alfvén wave heating (gray), heat conduction (red), adiabatic expansion (yellow), and radiative cooling (purple). Panel (A) (shaded green) shows a snapshot at t = 3.5 hr of the heat conduction, where the black line is the location of the parcel at that time.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Absolute value of thermal (black), kinetic (red), magnetic (blue), and gravitational potential (purple) energy density as per unit volume (top) and per unit particle (bottom) for the cavity parcel.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: The left panel shows the initial locations of the example plasma parcels in the flux rope at t = 0, projected onto a meridional plane through the active region. The right panel shows the Lagrangian trajectories of the example plasma parcels at 6 hr post-eruption in the same plane through the active region. Both panels use the electron temperature for context.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Absolute value of thermal (black), kinetic (red), magnetic (blue), and gravitational potential (purple) energy density as per unit volume (top) and per unit particle (bottom) for the prominence parcel.
Paper: 3D Non-equilibrium Ionization and Spectroscopic Modeling of Coronal Mass Ejections. II. CME Energy Budget
Authors: E. M. Wraback, W. B. Manchester, E. Landi, J. Szente
Figure caption: Absolute value of thermal (black), kinetic (red), magnetic (blue), and gravitational potential (purple) energy density as per unit volume (top) and per unit particle (bottom) for the flux rope base parcel.
Paper: Little Red Dots at an Inflection Point: Ubiquitous V-shaped Turnover Consistently Occurs at the Balmer Limit
Authors: David J. Setton, Jenny E. Greene, Anna de Graaff, Yilun Ma, 逸伦 马, Joel Leja, Jorryt Matthee, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Harley Katz, Ivo Labbe, Michael V. Maseda, Ian McConachie, Tim B. Miller, Sedona H. Price, Katherine A. Suess, Pieter van Dokkum, Bingjie Wang, 冰洁 王, Andrea Weibel, Katherine E. Whitaker, Christina C. Williams
Figure caption: A median stack of the spectra (red) of all spectra with high-confidence slope changes. On the top, we show four AGN-AGN models, which are generated by scattering 1% of the light from an intrinsic AGN continuum model (M. J. Temple et al. 2021, blue dashed line) and attenuating the remainder of the light by the indicated τV using a M. Kriek & C. Conroy (2013) dust law with a dust index of −1. The AGN models are normalized so that the contribution from the scattered component is 1 at 3645 Å, which is also where the spectra in the stack are normalized. In the next two rows, we show the same set of AGN models, but replacing the UV component with an τv ∼ 0.75 star-forming galaxy (row 2) and dust-free post-starburst galaxy (row 3) normalized to the UV. Models that meet the B − R > 0.95 cut are shown as solid lines, and models that do not are shown as dashed lines. Finally, we show a two-component galaxy model with the same unreddened poststarburst as the previous row, with the reddened AGN is replaced by the same stellar population undergoing varying reddening. In all cases, models can produce a change in slope at 3645 Å, but only with a very specific configuration of galaxy age, galaxy/AGN flux balance, and reddening. It is unlikely that any two-component model where the two components originate from different physical origins would result in this uniform inflection location.