adsabs/AstroCLIMB huggingface dataset:
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: Comparison between the real part of the EB correlation in SANE simulations from the full numeric as well as the m-order cut. From top to bottom, we present the full numeric, the case with m cut = 2, m cut = 3, and m cut = 4, respectively.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The comparison between the imaginary part of the EB correlation in the MAD simulations from the full numeric as well as the m-order cut. From top to bottom, we present the full numeric, the case with m cut = 2, m cut = 3, and m cut = 4, respectively.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The geometrical ring model vs. the time-averaged GRMHD SANE simulations. From top to bottom, we present the polarized images, the real part, and the phases of the EB correlation for the ring model and the phase from the time-averaged GRMHD simulation, respectively. It is inferred that the ring model does not seem to recover the full phase features in SANEs.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The phase map for the EB correlation for the time-averaged GRMHD simulations using the EHT coverage for M87* and taking into account the EHT finite resolution of 20 μas. Comparing this with Figure 6 demonstrates no noticeable differences.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The geometrical ring model vs. the time-averaged GRMHD MAD simulations. From top to bottom, we present the polarized images, the real part, and the phases of the EB correlation for the ring model and the phase from the time-averaged GRMHD simulation, respectively. It is inferred that the ring model recovers the full phase features in MADs.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The impact of time variability as a variance in the phase map of the time-averaged EB-correlation map for the MAD and SANE simulations with different BH spins.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Postage stamps of galaxies that were excluded from the morphology analysis due to their small size and low mass, but that were included in the physical property analysis. For the exclusion criteria for unresolved galaxies, see Section 3.3.2.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Composite HST image of the host galaxy of AT 2018cow from the F225W (blue), F555W (green), and F814W (red) images taken at t ≃ 1453 days (around 4 yr post-discovery). A crosshair is shown at the position of AT 2018cow, marking the existence of a spatially coincident underlying source. The underlying source is much bluer even visually than most other sources in the galaxy. Note that a faint tidal tail can be seen south of the galaxy.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Light curves illustrating the evolution of the underlying source from AT 2018cow. The HST photometry is shown as stars, and earlier measurements at similar wavelengths taken from paper I (Chen et al. 2023) are also shown. Offsets are added for visual clarity. Dashed–dotted lines corresponding to power-law declines of flux density are also added for reference (note these are not best-fit lines). Fading is observed in the F225W and F336W bands for the underlying source, but at a much slower rate than the initial decline of AT 2018cow.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Cutout HST images taken at t ≃ 703, 1119, and 1453 days in the wide bands. Epochs are shown on the left and filter names are shown at the top. Each panel shows a 1″ × 1″ box, with a circular aperture (r = 0.″12) centered at the position of AT 2018cow. A UV-bright point source is present at the position of AT 2018cow in the F225W, F336W, and F555W filters.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Cutout HST images taken at t ≃ 703 days in the narrow bands (F657N and F665N). A circular aperture (r = 0.″12) is centered at the position of AT 2018cow. Some excess emission can be seen in the F665N image.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Comparison of the density structures obtained by TARDIS to some theoretical models. The left panel shows the W7 model (brown; Nomoto et al. 1984) and the WS15DD1 model (black; Iwamoto et al. 1999); the right panel shows the double-detonation model of Shen et al. (2021), for three choices of the viewing directions (black for μ = 0 and brown for μ = ±0.93). The gray-shaded region shows the trajectory of the WS15DD1 model (left) or the double-detonation model for an average viewing direction (μ = 0, right), when the kinetic energy is changed by ±50%. The vertical red line shows the boundary between different layers (see labels). Different colors are used to show the ejecta structures for individual SNe, depending on the subclass they belong to; blue lines for the HV SNe and yellow lines for the 1999aa-like SNe. The NV SNe with large and small amounts of the unburnt carbon are denoted by pink and green lines, respectively.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Comparison between the observed spectrum and the TARDIS model spectrum for each object. In each panel, the blue line is the observed spectrum, and the orange one is the TARDIS model spectrum.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: The left panels show the distributions of the number of all the trials (blue) and the number of acceptable models (those in the top 3% in agreement with the observed one; orange), for each parameter. The right panels show the distribution of the “pass rate,” with a 1σ confidence interval (red dashed line).
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Fraction of the CO layer (left) and characteristic density (right) in increasing order from top to bottom. The different subclasses are marked by different colors for the error bars; 99aa-like SNe (orange) and HV SNe (blue), and “C-rich” NV SNe (red) and “C-poor” NV SNe (green).
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Fraction of the unburnt C + O layer to the total composition. The circles represent the NV type, the inverse triangles are for the HV type, and the crosses correspond to the 1999aa-like type. The error bars are obtained by the additional visual-inspection process to constrain the fraction of the CO layer, where only this parameter is varied while the other parameters are fixed to the best-fit values (see Section 3.1).
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Density at the photosphere for the sample of SNe Ia at different epochs. The black line is the curve described by t −2. Different symbols are used for different subclasses (see the caption of Figure 5).
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Characteristic density as compared to the fraction of the CO layer for the 14 SNe. The density is scaled at 16,000 km s−1 (for NV SNe) or 21,000 km s−1 (for HV SNe and 99aa-like SNe, respectively).
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: The left panel shows the spectra with the “best-fit” value for each parameter except for the fraction of the CO layer, showing how the amount of the CO layer affects the spectrum. The right panel is an expanded view around C II.
Paper: Systematic Investigation of Very-early-phase Spectra of Type Ia Supernovae
Authors: Mao Ogawa, Keiichi Maeda, Miho Kawabata
Figure caption: Density structure of each object based on the best-fit TARDIS model. The error bars in the density attached at the innermost and outermost velocities for each object represent the 1σ confidence interval (see the main text).
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: The ratio of the electron temperature to the total gas temperature T  e /(T  e  + T  i ) in the inner region of the accretion flow (at r = 10 GM/c 2) as a function of plasma β, computed using different ratios of the compressive to Alfvénic power (P comp/P A). The cyan curve corresponds to the earlier analytic calculation for Alfvénic turbulence by Howes (2010). The shaded region for each curve indicates the range of temperature ratios predicted for different mass accretion rates in the range ﹩{10}^{-7}\leqslant \dot{M}/{\dot{M}}_{{\rm{E}}}\leqslant {10}^{-5}﹩. In all calculations, we have set the radial velocity profile to n  R  = 1.5. The dotted lines represent the empirical relation by Mościbrodzka et al. (2016) that has been used in the literature, for different values of the parameter R high.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: Top: the ion temperature in units of ion rest mass energy as a function of radial distance, computed for a nonspinning black hole (dashed lines), and a black hole with a spin a = 0.9 (solid lines). The lines shown in green correspond to flows with vanishing viscous stresses at the ISCO (λ = 1), while the opposite extreme corresponds to λ = 0. In all calculations, we have set the plasma parameter to β = 5, the radial velocity profile to n  R  = 1.5, and the mass accretion rate set to ﹩\dot{M}\ll {10}^{-7}{\dot{M}}_{{\rm{E}}}﹩. Bottom: the ion-to-electron temperature ratio, T  i /T  e .
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: Top: ion (dashed) and electron (solid) temperatures, in units of ion rest mass energy, calculated including the effects of radiative cooling for mass accretion rates of ﹩\dot{M}={10}^{-7}{\dot{M}}_{{\rm{E}}}﹩ (red), ﹩\dot{M}\ll {10}^{-7}{\dot{M}}_{{\rm{E}}}﹩ (black dotted), and ﹩\dot{M}={10}^{-4}{\dot{M}}_{{\rm{E}}}﹩ (green). The plasma β is set to β = 5, and the radial velocity profile is set to n  R  = 1.5. Bottom: the ion-to-electron temperature ratio, T  i /T  e , for the above cases.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: The ratio of the electron temperature to the total gas temperature for ﹩\dot{M}\leqslant {10}^{-7}{\dot{M}}_{{\rm{E}}}﹩ in the inner region of a radiatively inefficient accretion flow (r = 10GM/c 2), as a function of plasma β, calculated using our covariant, semianalytic model, for different ratios of the compressive to Alfvénic power (P comp/P A). The dashed lines correspond to the empirical relation (37).
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Gaia DR3 data. Top: measured interaction time (t 0) from bootstrap resampling for each of the overlapping bins in J  ϕ −θ  ϕ . The bins are labeled in J  ϕ  (bottom) and guiding radius (top). Each bin span 60 kpc km s−1 in J  ϕ  and 0.01 radians in θ  ϕ . The values of t 0 range from 288 to 966 Myr with a median value of 524 Myr. Middle: the fit value of θ  z  at Ω z  = 45, showing the variation in intercepts of the different fits for the same bins in J  ϕ −θ  ϕ . Bottom: the offset between the time of maximum acceleration (﹩{t}_{{a}_{z},\max }﹩) and the estimated time since interaction (t 0) for the same bins in J  ϕ −θ  ϕ . The offsets range from −73 to 562 Myr with a median value of 333 Myr.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Analysis of Gaia DR3 data—center panel: background-subtracted phase spirals as a function of (J  ϕ , −θ  ϕ ). Frame: ridgeline fits to the spirals projected into θ  z  = Ω z  for different θ  ϕ  (right panels) and J  ϕ  (bottom panels) bins. The lighter lines represent the fit to the data after bootstrap resampling. The center panel shows the variation in phase spiral morphology as a function of (J  ϕ , −θ  ϕ ). In the bottom (left) panels the subtle shifts in phase spiral slope and phase angle as a function of θ  ϕ  (J  ϕ ) can be seen.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Illustration of splitting a local sample in actions and angles, what it gains, and the biases introduced. (a) Three stars that are currently in the observed sample (black box) at physical positions (R, ϕ) in the disk (star), with their radial epicycles and guiding centers (R G, θ  ϕ ) shown (dots). (b) A set of stars projected into surrounding bins at larger (blue) or smaller (red) R G and ahead (dotted bins) or behind (dashed bins) the local sample (black solid) in the direction of Galactic rotation. (c) Example number counts in radial action (or eccentricity) and radial phase angle. The colors and line styles show the distribution of ﹩\sqrt{{J}_{R}/\kappa }﹩ and θ  R , respectively, for stars in the nine different boxes in panel (b), which are all physically located within the black box, and projected across all nine boxes. (d) Illustration of where particles in a local sample (black box) might have been in the disk roughly half a solar rotation ago, coded by their (R  G , θ  ϕ ) bins from panels (b) and (c).
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Plot of the disk at the time of satellite crossing colored by the estimated time since interaction at z = 0 (t 0) using only well-resolved phase spirals (σ  t  < 100 Myr). The color bar represents the estimated time since interaction at z = 0 with white corresponding to t 0 = t true = 844 Myr, red corresponding to longer-than-expected interaction times, and blue corresponding to shorter-than-expected interaction times. The red X marks the disk crossing of the satellite (the position at this snapshot), while the black line shows the orbital track in the x–y plane. The disk is rotating counterclockwise in this projection.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Gaia data showing phase spirals unwrapped in vertical action–angle coordinates (J  z , θ  z ) as computed in a 2D grid of mass models for the Milky Way. Each panel represents the phase spiral as computed in a potential model with the parameters indicated in each panel title, where h  z  is the disk scale height in units of kpc and m is the disk mass in units of 1010 M ⊙. The rows represent increasing scale height and the columns represent increasing disk mass.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption:  z-acceleration (a  z ) from the satellite perturber vs. time for 100 particles from the M1 simulation presented in Hunt et al. (2021) in three bins of J  ϕ −θ  ϕ  (black lines). The red dashed line marks the measured t 0 of each bin, while the blue dashed lines mark the disk crossings of the satellite at −362, −583, and −1110 Myr.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Gaia DR3 data in each of the J  ϕ −θ  ϕ  bins in Figure 7 backward orbit integrated 911 Myr. The data points are colored by the median t 0 (measured at t = 0 Myr). The black line shows the orbit of Sagittarius and the black point shows its position at t = −911 Myr.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Example m = 2 phase spiral (left) and corresponding fit to the extracted ridgeline (right). For this spiral we get an interaction time of t 0 = 133 Myr.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Clump luminosity comparison of UVCANDELS (blue line) to HDUV (orange line) with their corresponding 1σ Poisson error. The black dashed lines represent two sample cuts at clump UV luminosity (expressed in absolute magnitude) M UV = −16 and −16.7 AB. The former represents a sample distinct from typical H II regions that was used as our fiducial results. The latter represents a complete sample in which detections for UVCANDELS are not affected by lower sensitivity limits.
Paper: UV-bright Star-forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 ≤ z ≤ 1
Authors: Alec Martin, Yicheng Guo, Xin Wang, Anton M. Koekemoer, Marc Rafelski, Harry I. Teplitz, Rogier A. Windhorst, Anahita Alavi, Norman A. Grogin, Laura Prichard, Ben Sunnquist, Daniel Ceverino, Nima Chartab, Christopher J. Conselice, Y. Sophia Dai, Avishai Dekel, Jonathan P. Gardner, Eric Gawiser, Nimish P. Hathi, Matthew J. Hayes, Rolf A. Jansen, Zhiyuan Ji, David C. Koo, Ray A. Lucas, Nir Mandelker, Vihang Mehta, Bahram Mobasher, Kalina V. Nedkova, Joel Primack, Swara Ravindranath, Brant E. Robertson, Michael J. Rutkowski, Zahra Sattari, Emmaris Soto, L. Y. Aaron Yung
Figure caption: Example galaxies (rows) from our clump-detection algorithm. The respective columns show (from left to right) each galaxy in the H-band filter, NUV filter, smoothed (F275W), residual (F275W − smoothed), and original F275W cutout with detected clumps marked. Each galaxy center is marked with a cyan “x” and our clump-detection size limit of r ≤ 3 × R  e  indicated by black dashed circles. The detected clumps that pass (fail) our fiducial selection criterion are marked with green (red) circles. Our selection criterion removed one clump from both IDs 8008 and 15209 due to their proximity to the host galaxy’s center. Additionally, another clump was removed from ID 8008 due to its radial distance being greater than 3 R  e , which suggests a probable association with an external galaxy.