adsabs/AstroCLIMB huggingface dataset:
Paper: 3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes
Authors: Benny T.-H. Tsang, Daniel Kasen, Lars Bildsten
Figure caption: Amounts of mass loss expected from the RSG envelope models as a function of injected energy, defined relative to the envelope’s total energy. Regardless of the deposited energy, 3D calculations including a convective envelope systematically result in more mass to be ejected than their 1D counterparts.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Synthetic pollution mass curve for an asteroid belt (top) and a single moon event (bottom) as a function of time post WD formation. The black dashed line shows the total mass of pollution in the convection zone, and the colored lines show the pollution mass per element. The horizontal line shows the minimum detectable mass of heavy elements. The left column shows accretion onto a DA WD, while the right shows pollution of a DB. Top row: continuous accretion of an asteroid-mass debris belt, based on the mean accretion rate of Mustill et al. (2018) and assuming the distribution of masses follows that of the solar system asteroid belt. Bottom row: accretion of a single moon of mass ∼1020 g onto a typical DA (left) and a moon of mass ∼1021 g onto a typical DB (right). These masses represent the median mass of the subset of solar system moons that satisfy the criteria for being liberated from their host planets and providing observable levels of metal pollution.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: An example plot of the parent body mass calculated from Equation (3) as a function of assumed elapsed accretion time for the DA G149-28 (top) and DB WD 2207+121 (bottom). We assume an accretion disk lifetime of 105 yr (dotted line). Settling timescales for the DB are approximately 106 yr, those for the DA are ∼400 yr, and both are marked in dashed lines for each element. The parent body solution derived from Equation (2) is plotted for each element, and the dashed orange line shows the sum of all parent body elements at each assumed elapsed accretion time.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Fraction of bodies in each population with a given mass. Densities of 3 and 2 g cm−3 are assumed to calculate masses for asteroids and moons, respectively. The asteroid curve is derived from Dohnanyi (1969), and the moon data are from the JPL Solar System Dynamics group. The parent body masses are split into DA and DB populations and assume a disk lifetime of 105 yr. The DBs tend to have larger parent body mass solutions, though the masses for both the DAs and DBs are situated toward the tail end of asteroid masses and mid-to-high moon masses. For comparison, the mass of Ceres is indicated as the dotted line. Note that the parent body masses shown are lower limit solutions.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Fraction of parent body mass for a typical rock-forming element in the convection zone of a WD as a function of time, for three different accretion disk lifetimes. The DA pollution curves decrease by nearly a factor of 10 with increasing disk times, while the DB curves decrease less significantly. The peaks of both curves shift to later times as the disk accretion time increases, reflecting changes in the time where steady state between accretion and settling is achieved.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Top: distribution of moon semimajor axes relative to the planet Hill radius, for each of the giant planets. Bottom: distribution of moon masses, including and excluding the irregular satellites. Regular satellites tend to have smaller semimajor axes and larger masses than the irregulars. The shaded portions of each graph show the approximate range of initial semimajor axes that can result in liberated moons (top) and the range of moon masses that can produce observable levels of pollution (bottom), according to our model.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Calculated minimum detectable parent body masses associated with the detection limit for Ca, assuming chondritic parent body compositions. To obtain these masses, we solve the J09 model for the minimum mass of calcium in the parent body, assuming an M CV,Ca according to Equation (5). We then calculate the minimum parent body mass solution by assuming chondritic composition, settling timescales from MWDD corresponding to the effective temperature of each WD, and a disk timescale of 105 yr.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Parent body masses calculated assuming the WD is in steady state, with four different assumed accretion disk timescales. DA parent body solutions tend to vary more dramatically with disk timescale than the DBs. Most DB parent body mass solutions are close to ∼1023, and while the DA solutions are somewhat lower, the two begin to converge as disk timescales increase.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Top: snapshots of orbits from simulation, for planets (thin black lines) and moons (colors). The times indicate the time since the WD formed, and the WD is shown as a black star at 0 au. Bottom: periapse vs. time for the moons, in the same simulation as show in the top plot. Each curve corresponds with the orbits of the same color in the top plot. Two moons are scattered onto hyperbolic orbits following a close approach to the WD.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Total masses of heavy metals observed for the WDs in Table 1, sorted by type. The DAs tend to have lower observed masses of polluting elements compared to the DBs.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: Molecular abundances (expressed as log of the VMRs) of H2O, CH4, NH3, and K, plotted against T eff for the T dwarfs from this study (tomato) and the brown dwarfs from Zalesky et al. (2019; cyan). For K, the objects from Zalesky et al. (2019) are not included, because that work considered Na+K as one alkali species, whereas herein we are treating them as individual species. The four subplots show how the molecular and alkali abundances of each species vary with T eff. All the modeled molecular abundance trends are defined by log(g) = 5.0 and solar composition (M/H = 0.0, C/O = 0.5), and we assume equilibrium chemistry unless otherwise specified. We observe that the overall trends of water, methane, and ammonia are consistent with solar chemistry curve models.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: TP profiles of nine representative T dwarfs from our collection of 50 objects. The thermal profiles indicated here are of the retrieved objects (in red) and of grid models (in blue; see the text) that they closely compare to, based on their similarities in a mix of T eff, log(g), C/O, and metallicity parameters. For each of the thermal profiles, both 1σ and 2σ confidence intervals are shown. Equilibrium condensation curves of Mg2SiO4, Fe, MaSiO3, Na2S, and K are shown by the cyan, blue, black, yellow, and magenta dashed lines, respectively.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: log g vs. T eff for our collection of early-Y dwarfs and late-T dwarfs. Here, we notice that we almost have a handful of T dwarfs with low–surface gravity values, while the Y dwarfs tend to have higher-gravity values. Based on the evolutionary models from Marley et al. (2021); shown by the dashed blue curves, the T dwarfs having the lowest log g values would be relatively young (∼100 Myr), while the Y dwarfs having the highest log g would be relatively old (∼12 Gyr). Most of the objects above the 10 Gyr curve are considered atypical, although their high gravities can be justified by the logic that underestimations of gravities occur in grid models (Schneider et al. 2015; Zalesky et al. 2019).
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: Minimum parent body mass solution relative to the observed mass of pollution in the atmosphere, as a function of the ratio of the disk timescale to the settling time. DAs would be found toward the right, so that the steady-state parent body mass is several times the observed mass in the atmosphere. DBs would be toward the left, where the parent body solution approaches the mass of the polluting metals.
Paper: Exomoons as Sources of White Dwarf Pollution
Authors: Isabella L. Trierweiler, Alexandra E. Doyle, Carl Melis, Kevin J. Walsh, Edward D. Young
Figure caption: The periapse evolution of three-planet systems for three different ranges of planet spacings in terms of mutual Hill radii: 5–10 (top), 10–20 (middle), and 20–30 (bottom). In each system, the innermost planet is at 10 au and the spacings between each consecutive planet are randomly chosen from the stated ranges. Planet masses for all three simulations are 1.3, 30.6, and 7.8 M ⊕. While the most closely packed system experiences the most orbital crossings between planets, crossings still occur in the more widely spaced systems.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: C/O vs. bulk metallicity for our ensemble of Y and T dwarfs. The brown dwarfs are color-coded according to their effective temperatures. For comparison with field stars, we overplot the brown dwarfs (C/O vs. [M/H]) with Hypatia FGK stars (C/O vs. [Fe/H]) that are within comparable parallax distances (≤30 pc) to the brown dwarfs. The two populations have highly similar distributions, owing to their similar formation environments.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: A color–magnitude diagram of a population of field brown dwarfs (Best et al. 2018, 2020), and our sample of brown dwarfs from this study (T5–T9). This collective ensemble shows L and T dwarfs, in descending order, from the top of the diagram to the bottom.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: A subset of the data (the black round points with errors) and the resulting fits (binned best fits in blue, residuals about the dashed line below in red). In blue are higher-resolution (R ∼ 25,000) representations of the best-fit spectra. The effective temperature and gravity constraints are given in the upper right hand corner of each panel.
Paper: Observational Constraints on Cosmic-Ray Escape from Ultrahigh-energy Accelerators
Authors: Quentin Luce, Sullivan Marafico, Jonathan Biteau, Antonio Condorelli, Olivier Deligny
Figure caption: Distributions of the shower-depth maximum, ﹩{X}_{\max }﹩, for the best-fit models. The contributions of the five detected mass groups are displayed with solid colored lines, as labeled in the figure. The sum of the five contributions is shown in brown. The deviance (D) and number of points (N) are shown in the top-right corner of each plot for each energy bin. Note that one event at 1,070 g cm−2 is out of the displayed ﹩{X}_{\max }﹩ range for ﹩18.9\lt {\mathrm{log}}_{10}(E/\mathrm{eV})\leqslant 19.0﹩.
Paper: Observational Constraints on Cosmic-Ray Escape from Ultrahigh-energy Accelerators
Authors: Quentin Luce, Sullivan Marafico, Jonathan Biteau, Antonio Condorelli, Olivier Deligny
Figure caption: Energy flux at Earth as a function of energy, as modeled by the best-fit parameters for the benchmark scenario. The all-particle spectrum and proton component are shown as black circles and red squares, respectively. Lighter points are not included in the fit. The best-fit components obtained for the five detected mass groups are displayed with solid colored lines, as labeled in the figure. The energy flux of the heaviest mass group, with detected mass numbers of 39–56, is below the range of interest.
Paper: Observational Constraints on Cosmic-Ray Escape from Ultrahigh-energy Accelerators
Authors: Quentin Luce, Sullivan Marafico, Jonathan Biteau, Antonio Condorelli, Olivier Deligny
Figure caption: Mass-dependent energy production rate at the sources as a function of energy, as constrained by the best-fit parameters for the benchmark scenario. The dashed lines illustrate a variation of the hadronic interaction model, with EPOS-LHC and Sibyll2.3 c shown as solid and dashed lines, respectively.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Modeling the covering fraction C  f (r) as a function of radial distance for the [O II] (left), Fe II* (middle), and Mg II emission (right) of the counter arc in the source plane. The dotted lines represent the intrinsic power law models used for the fitting. The dashed lines represent the observed model (intrinsic models after convolving them with the seeing) at the location of the counter arc in the source plane.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Same as Figure A1 but for the Mg II 2803 emission secondary component.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Isophotal ellipse fits to the flux distribution of the stellar component. Left panel: flux distribution of the stellar component, obtained from collapsing a 200 Å slab of the data cube near 9000 Å, is shown in color, with some example best-fit ellipses overlaid in white contours. Middle panel: model reconstructed from the best fit to each ellipse. Right panel: residual map (observed minus best-fit model), showing remaining structure in the central region. The color bar represents the flux in 5.5 × 10−5 erg s−1 cm−2 Å−1.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Composite RGB color image using red, green, and blue pseudocolors, collapsing three bands in the data cube (see Section 3 for details). In this image north is up and east to the left. This image shows the intricate filamentary distribution of the ionized gas.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: An example of a pPXF fit to one of the central bins. The observed spectra, the best-fit stellar continuum model, and the residuals are represented by the black, red, and green lines, respectively. The colored gray areas represent the masked spectral regions around the emission lines observed.
Paper: Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg
Authors: Charles D. Kilpatrick, David A. Coulter, Ryan J. Foley, Anthony L. Piro, Armin Rest, César Rojas-Bravo, Matthew R. Siebert
Figure caption: The combined uBVgri Swope (squares) and F435W, F438W, F606W, and F814W HST (stars) light curve of SN 2016gkg comprising photometry from +32 to +1795 days from explosion (32–1786 rest-frame days). We compare F435W and F438W to B band, F606W to V band, and F814W to i band. For comparison, we show a simulated light curve powered by 56Co → 56Fe decay (dashed line) to compare to the photometry at >250 rest-frame days. However, in the 1795-day epoch, there appears to be excess emission (solid line) beyond the predicted emission from this model, which we model here using a circumstellar interaction model assuming a wind with ﹩\dot{M}\,=\,﹩ (3–4) × 10−7 M ⊙ yr and v  w  = 150–250 km s−1.
Paper: Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg
Authors: Charles D. Kilpatrick, David A. Coulter, Ryan J. Foley, Anthony L. Piro, Armin Rest, César Rojas-Bravo, Matthew R. Siebert
Figure caption: SED of the SN 2016gkg pre-explosion counterpart from F450W, F606W, and F814W (red points), with vertical error bars including the measurement uncertainty and horizontal error bars indicating the effective filter width. We overplot two models used to describe the overall SED: a blackbody with T eff = 10,800 K and a stellar SED for an A3I star derived from Pickles & Depagne (2010) models as described in Section 3.1.
Paper: Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg
Authors: Charles D. Kilpatrick, David A. Coulter, Ryan J. Foley, Anthony L. Piro, Armin Rest, César Rojas-Bravo, Matthew R. Siebert
Figure caption: Our nebular spectra of SN 2016gkg from Keck/LRIS as described in Section 2.3. We highlight lines of [Mg I] λ4571, [O I] λ λ6300, 6364, Hα, and [Ca II] λ λ7292, 7324. For comparison, we show the latest Gemini-S/GMOS spectrum from Kuncarayakti et al. (2020), which shows that Hα emission is enhanced as the SN evolves.
Paper: Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg
Authors: Charles D. Kilpatrick, David A. Coulter, Ryan J. Foley, Anthony L. Piro, Armin Rest, César Rojas-Bravo, Matthew R. Siebert
Figure caption: The HST photometry from SN 2016gkg at +1786 rest-frame days (red) as shown in Figure 2 compared with a scaled Keck/LRIS spectrum of SN 2016gkg from +483 days (black) and the best-fitting blackbody spectrum with T eff = 3990 K (green). The scaled Keck spectrum corresponds to a much bluer color than the late-time HST photometry, implying that there is significant spectral evolution out to this late phase, such as Hα emission as in Figure 3, or there is some other source of emission dominating SN 2016gkg.
Paper: Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg
Authors: Charles D. Kilpatrick, David A. Coulter, Ryan J. Foley, Anthony L. Piro, Armin Rest, César Rojas-Bravo, Matthew R. Siebert
Figure caption: HST WFPC2, ACS, and WFC3 imaging of the site of SN 2016gkg. We highlight the location of SN 2016gkg as determined from the ACS/WFC F606W image (bottom middle) from 2018, at which time the SN exhibited m F606W = 22.79 ± 0.01 mag (AB). The counterpart appears fainter in WFC3 F438W and F606W imaging from 2021 (right top and bottom) than coincident pre-explosion emission from 2001 as observed in WFPC2 F450W and F606W (left top and bottom).
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: Distribution of quasars from 0.7 < z < 1.9 with 3.35 < log(λ RF) < 3.45 in the τ perturb, σ  ϵ  parameter space. Both τ perturb, σ  ϵ  are corrected to a rest-frame wavelength of 2500 Å. Top row: from left to right, quasars are color-coded by their L bol, M BH, and L/L edd, respectively. The median error bar is displayed in the lower left corner of the left panel. A trend of decreasing L bol with larger τ perturb and σ  ϵ  is shown in the left panel. Similar trends for M BH or L/L edd are not seen in the middle and right panels. Bottom row: same as the top row, but with the y-axis presented in the unit of gravitational radius (R  g ) with r perturb = (τ perturb∗ c)/R  g   ∝ τ perturb/M BH. The median error bar is displayed in the upper right corner of the right panel. The dashed lines are best-fit regression in the form of log(r perturb) = A∗log(σ  ϵ ) + B∗log(M BH) +  C for M BH of 108, 109, and 1010 M ⊙. Weighting τ perturb by M BH reduces the scatter seen in the top row and reveals a new trend of increasing r perturb with increasing L/L edd (see the bottom right panel).
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: Diagrams providing schematic views of the accretion disk geometry proposed in Kubota & Done (2018) for a variety of L/L edd and M BH. Note that the diagrams are drawn in the units of gravitational radius and Equation (18) is used as a reference when discussing the changing disk geometry. The blue annulus represents the hot X-ray corona, the green slab shows the warm Comptonization region of the disk, and the purple slab corresponds to the standard disk region. The effective emitting wavelength of the disk increases going from r hot to r out. The r perturb arrow connects the X-ray corona to the disk annulus emitting at an effective wavelength of 2500 Å. Left column: M BH is held fixed, and L/L edd increases from top to bottom. The size of the X-ray corona decreases, and the 2500 Å mark shifts outward with increasing L/L edd. The effective temperature/wavelength of the disk at the boundary between the warm Comptonization region (green slab) and the standard disk region (purple slab) also increases/decreases with L/L edd. Right column: L/L edd is held fixed, and M BH increases from top to bottom. When L/L edd is fixed, the disk temperature (wavelength) at the boundary between the green and purple slab should stay relatively fixed; thus, increasing M BH shifts both r warm and the 2500 Å disk annulus inward.