adsabs/AstroCLIMB huggingface dataset:
Paper: Black Hole Polarimetry I. A Signature of Electromagnetic Energy Extraction
Authors: Andrew Chael, Alexandru Lupsasca, George N. Wong, Eliot Quataert
Figure caption: Left column: histograms of snapshot values of β 2 in the complex plane for images from nine MAD GRMHD simulations ray traced with M87* parameters. Prograde models (a * > 0) are shown in the top row, and retrograde models (a * < 0) in the bottom row. The histograms include all snapshot images at different simulation time slices between 50,000 t g and 100,000 t g. Simulation images were blurred to the EHT resolution of 20 μas before computing β 2. The histograms cover six different models for the low-magnetization ion-to-electron temperature ratio R high. Right column: histograms of ∠β 2 from the same simulation images. With a few exceptions for predominantly low-spin, retrograde simulation snapshots, nearly all MAD GRMHD snapshots have ∠β 2 < 0, corresponding to energy outflow in the simple picture of Figure 1. The range of ∠β 2 values consistent with EHT observations of M87* in 2017 is shown in the blue band (EHTC VII).
Paper: Black Hole Polarimetry I. A Signature of Electromagnetic Energy Extraction
Authors: Andrew Chael, Alexandru Lupsasca, George N. Wong, Eliot Quataert
Figure caption: Top: the sign of B  ϕ /B  r  for three MAD GRMHD simulations averaged in time and azimuth. From left to right, the GRMHD simulations correspond to a retrograde accretion disk around a spinning black hole (a * = −0.5), a Schwarzschild disk (a * = 0), and a prograde disk (a * = +0.5). Middle: the angular frequency of the magnetic field lines Ω F  in the same simulations in natural units of ﹩{t}_{{\rm{g}}}^{-1}﹩. (Bottom) The averaged radial Poynting flux ﹩\sqrt{-g}{{ \mathcal J }}_{{ \mathcal E }}^{r}﹩ in BL coordinates in the same simulations. In the bottom panel, all three panels are independently normalized and are not plotted in the same units; the energy flux in the a * = 0 simulation (driven by the accretion disk) is an order of magnitude smaller than in the a * = ±0.5 simulations (driven by black hole spin). In all plots, the cyan contour indicates the surface where the magnetization σ = 1. White contours show surfaces of constant vector potential ψ ≡ A  ϕ .
Paper: Black Hole Polarimetry I. A Signature of Electromagnetic Energy Extraction
Authors: Andrew Chael, Alexandru Lupsasca, George N. Wong, Eliot Quataert
Figure caption: Left column):∠β 2 as a function of image radius in time-averaged images of M87* from MAD GRMHD simulations. The top row shows the time-averaged image for a * = −0.5, the middle row for a * = 0, and the bottom row for a * = 0.5. All images use R high = 1 to set the electron temperature in radiative transfer. The vertical magenta line shows the outermost radius of the “inner shadow,” or the lensed image of the equatorial event horizon; the cyan band shows a range of radii corresponding to the n = 1 photon ring. Right column: the time-averaged images used in computing ∠β 2 in the left panels. Images are displayed in a gamma color scale and are not blurred to EHT resolution. The black hole shadow/critical curve is indicated by the cyan contour, and the inner shadow with the magenta contour. The image-average value of ∠β 2 is displayed on each panel. A version of the top row of this plot was first produced in Ricarte et al. (2022), Figure 8.
Paper: On the Optical Transients from Double White-dwarf Mergers
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, C. Guidorzi, J. A. Rueda
Figure caption: Different populations of fast transients observed with the ZTF Bright Transient Survey (Perley et al. 2020). The shaded box highlights where we expect most DWD mergers should lie. Figure adapted from Perley et al. (2020).
Paper: On the Optical Transients from Double White-dwarf Mergers
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, C. Guidorzi, J. A. Rueda
Figure caption: Emission from the expanding, cooling ejecta at early times (solid lines) in the visible (r band) and in the infrared (i and K  s  bands). We refer to Appendix for details on the theoretical model.
Paper: On the Optical Transients from Double White-dwarf Mergers
Authors: M. F. Sousa, J. G. Coelho, J. C. N. de Araujo, C. Guidorzi, J. A. Rueda
Figure caption: Emission spectra from the expanding, cooling ejecta at selected postmerger times. We refer to Appendix for details on the theoretical model.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Disk with high initial eccentricities (e = 0.99) with an in-plane recoil kick. Top: the postkick distribution of the z-component of the angular momentum (normalized by the circular angular momentum at a given radius) as a function of semimajor axis, with the color bar showing the y-component of the eccentricity vector. Second from top: the y-component of the mean eccentricity vector, 〈e  y 〉, binned by semimajor axis and separated into prograde (j  z  > 0) and retrograde (j  z  < 0) stars. The mean for prograde orbits is shown by the blue solid line whereas the mean for retrograde orbits is shown by the orange dashed line. The shaded noise floor shows the maximum expected deviation from 0 (at the 3σ level) if the distribution were isotropic. Second from bottom: the eccentricity profile as a function of semimajor axis with the inclination color coded. Bottom: the retrograde fraction of the disk at a given semimajor axis range. Two antialigned ENDs create a linear, bar-like structure with a ≳40% retrograde fraction at most semimajor axis ranges. The eccentricity gradient, de/da, is negative inward of a ∼ 3 and positive outward of a ∼ 5.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Parameter study of an initially thin disk with varying eccentricities and kick directions. Top: the mean y-component of the eccentricity vector, 〈e  y 〉. Bottom: the mean first component of the tilt vector, 〈t 1〉, which measures roll, as a function of the initial eccentricity, with different lines showing different out-of-plane kick components. We show 〈e  y 〉 and 〈t 1〉 because they dominate the mean eccentricity vector and the mean tilt vector, respectively. The other components, 〈e  x 〉, 〈e  z 〉, 〈t 2〉, and 〈t 3〉, are all ∼0. α = 0° is a completely out-of-plane recoil kick whereas α = 90° is a completely in-plane kick. The solid lines are analytic expectations and the “x” markers show the numerical results. We omit the analytic expectation for the purely in-plane tilt vector, since the longitude of ascending node is not well defined for a two-dimensional orbit in the x–y plane. The eccentricity vector alignment becomes weaker with increasing initial eccentricities and larger out-of-plane kick components. Tilt vector alignment happens in all cases except when the kick is purely in plane.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. Top: distribution of the postkick eccentricity as a function of semimajor axis with the inclination on the color bar. Bottom: two measures of ω-clustering: the magnitude of the mean tilt vector (blue solid line), ∣〈 t 〉∣, and the mean unit tilt vector (orange dashed line), ﹩| \langle \hat{t}\rangle | ﹩, where the tilt vector is defined in Equation (5), binned by semimajor axis. The shaded noise floor region shows the maximum expected deviation from 0 (within 3σ) if the distribution were isotropic. Both eccentricity and inclination monotonically increase with semimajor axis, and tilt vector alignment is statistically significant at most semimajor axes.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. The line-of-sight velocity maps in the frame comoving with the recoiling black hole (“o” marker) in the face-on (top) and edge-on (bottom) orientations at t = 0 (left), t = 0.1 Myr (center), and t = 0.35 Myr (right). In each orientation, the color bar is adjusted such that approaching velocities are blue and receding velocities are red. The recoil kick direction is marked and labeled as v kick for each row. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The strong correlation in anomalies and arguments of periapsis causes clear, circular patterns in the line-of-sight velocities for the face-on orientation. The edge-on orientation shows that the dome-shaped structure maintains coherent rotation.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. The edge-on, postkick distribution of stars at t = 0 (top left), t = 0.15 Myr (bottom left), and t = 0.75 Myr (right). Bound and unbound stars are shown with blue triangle markers and green dots, respectively. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The recoil is applied in the direction indicated by the arrow labeled v kick. All positions are computed in the galactic center frame of reference. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The postkick distribution is a large ball of trailing stars with the bound stars forming a distinct dome shape behind the recoiling black hole.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. A histogram of the postkick mean anomaly, ﹩{ \mathcal M }﹩, and argument of periapsis, ω. The mean anomalies are strongly clustered around 0 since every star begins its new orbit at periapsis, and the ω values are strongly clustered around π since the new periapsis corresponds to the orbit’s descending node for all orbits.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an in-plane recoil kick. The line-of-sight velocity maps in the frame comoving with the recoiling black hole (“o” marker) in the x–y plane (top), x–z plane (center), and y–z plane (bottom) at t = 0 (left), t = 0.1 Myr (center), and t = 0.35 Myr (right). In each orientation, the color bar is adjusted such that approaching velocities are blue and receding velocities are red. The recoil kick direction is marked and labeled as v kick for each row. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The edge-on orientations clearly show the presence of a retrograde disk at large radii: there exists a mix of blueshifted and redshifted stars on either side of the black hole.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. The face-on, postkick distribution of stars at t = 0 (left), t = 0.15 Myr (center), and t = 0.75 Myr (right). Bound and unbound stars are shown with blue triangle markers and green dots, respectively. The “x” marker shows the center of the galaxy and the “o” marker shows the recoiling black hole. The recoil kick direction is out of the plane, marked and labeled as v kick. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The distribution is always axisymmetric, but an underdensity seems to emerge between the central region and the surrounding ring which both radially expand over time.
Paper: Anisotropic Star Clusters around Recoiling Supermassive Black Holes
Authors: Tatsuya Akiba, Ann-Marie Madigan
Figure caption: Circular disk with an out-of-plane recoil kick. The postkick surface density distribution of bound stars in the face-on (top) and edge-on (bottom) orientations at t = 0 (left), t = 0.01 Myr (center), and t = 0.04 Myr (right). The “o” marker shows the recoiling black hole, and these density contours are calculated in the frame comoving with the black hole. In each orientation, the recoil kick direction is marked and labeled as v kick. The length scale and time units assume a black hole mass of M • = 4 × 106 M ⊙ and a kick of v kick = 100 km s−1. The face-on orientation reveals the evolution of the central region and the surrounding ring overdensity. The edge-on orientation shows the development of the characteristic dome shape.
Paper: A Simple Method for Predicting N H Variability in Active Galactic Nuclei
Authors: Isaiah S. Cox, Núria Torres-Albà, Stefano Marchesi, Xiurui Zhao, Marco Ajello, Andrealuna Pizzetti, Ross Silver
Figure caption: The FPR as a function of N H for three different threshold ﹩{\chi }_{{\rm{c}}}^{2}﹩ values and different count levels. The details are described in Figure 9.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: An illustrative example of our process for measuring a galaxy’s MDF from HST imaging. This case study is for CVn II. The upper left panels show the CMDs of CVn II, with members shown in red and stars in common with other studies highlighted in blue. The upper right panels show the scatter and bias in the ASTs for each filter. The bottom left panel shows the CaHK diagram with member stars plotted in red and select metallicity tracks as lines. The high-opacity lines are the convolution of the intrinsic models low-opacity with the ASTs. The lower right panel shows the MDF of CVn II. The shaded red regions are well-constrained metallicity fits for individual stars, while the unshaded regions reflect stars with poorly constrained fits (e.g., off the metallicity grid, truncated probability density functions (PDFs)). The blue line shows a Gaussian fit to all stars on the histogram.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Example posterior distribution functions of stars in CVn II. (Upper left) Position of example stars in CaHK space, plotted against the MIST monometallic tracks used to infer metallicities in this work. (Upper right) Example of a star with a well-constrained PDF. (Lower left) Example of a star with a well-constrained PDF peak that is truncated at the metal-poor end; we also designate this star as an extremely metal-poor candidate. (Lower right) Example of a star for which we only constrain an upper limit is also an extremely metal-poor candidate.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: A gallery of F606W–F814W CMDs for our galaxies in order of decreasing luminosity from the top left to the bottom right. We color code stars by their F395N S/N for F395N S/N >5 and have not yet applied any membership selection or removed spurious detections.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: A comparison of metallicities for stars in common with our example galaxies CVn II, Grus I, and Dra II. The top row shows a 1:1 comparison of stars common in both studies. Our metallicities and those in the literature generally agree to ∼1.5σ. The lower panels show a comparison between our MDFs (gray) and all MDFs in the literature for each galaxy. The histogram bins are 0.4 dex wide.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Same as Figure 3 only for Dra II, which has no RGB stars. The monometallic tracks shown in the bottom left panel are for MSTO and MS stars. Accordingly, the MDF is entirely based on stars from these evolutionary phases.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: The same as Figure 1 only for F475W–F814W CMDs. The broader CMD features are partially driven by the lower S/N of the F475W data and the increased metallicity sensitivity of F475W–F814W vs. F606W–F814W.
Paper: Metallicity Distribution Functions of 13 Ultra-faint Dwarf Galaxy Candidates from Hubble Space Telescope Narrowband Imaging
Authors: Sal Wanying Fu, Daniel R. Weisz, Else Starkenburg, Nicolas Martin, Alessandro Savino, Michael Boylan-Kolchin, Patrick Côté, Andrew E. Dolphin, Alexander P. Ji, Nicolas Longeard, Mario L. Mateo, Ekta Patel, Nathan R. Sandford
Figure caption: Same as Figure 3 only for the fainter, less populated system, Grus I.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Example Quaver output panel for Pictor A in Sector 5. Top: corrected light curve created with the simple hybrid method. Bottom left: additive and multiplicative components removed by the hybrid method. Different colors correspond to different PCA components. Bottom right: Postage stamp of the TESS Target Pixel File. The source is well detected in the center of the image, and the extraction region is cross-hatched in red. The pixel scale is 21″ pixel−1.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Fit output diagrams for Sector 5 for each of the three methods. Top: PCA fitting only. Middle: simple hybrid model, with subtracted background light curve (scaled to match the median flux of the raw light curve) shown with the original in the top panel, and the background-subtracted light curve shown with the corrected multiplicative model in the lower panel. The amplitude of the subtracted background can be estimated by comparing the raw and background-subtracted curves. Bottom: fully hybrid model.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Cycle 1 light curves of three non-variable reference stars extracted by the Quaverpipeline. Each panel shows the light curves of stars 1–3, as labeled in Figure 1, from top to bottom. In each panel, all three Quaver methods are used, with colors given in the legend. Light curves have been arbitrarily offset for visible distinction. Differences in the noise spread of the light curves is due to the different apertures used to extract the stars and variable level of background light from sector to sector.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: Comparison of the three Quaver reduction methods (colored light curves as indicated in legend) and ground-based light curves from ZTF (black). Light curves have been rescaled to have similar normalizations for comparison of long-term behavior. Conversion of TESS counts to standard magnitude systems is not straightforward due to its unusual bandpass; instead, ZTF magnitudes have been converted to generic flux counts via f = 10 m/−2.5 and rescaled to a similar normalization as the TESS light curves; see the text for details.
Paper: The Rapid Optical Variability of the Nearby Radio-loud AGN Pictor A: Introducing the Quaver Pipeline for AGN Science with TESS
Authors: Krista Lynne Smith, Lia F. Sartori
Figure caption: TESS target pixel file image of the Pictor A field of view, with contours from the DSS overlaid. The three reference stars extracted by the pipeline are labeled in red circles; their light curves are shown in Figure 3. The scale is 21″ per pixel. Pictor A is the galaxy at the center of the frame.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The hydrogen column density along the line of sight (﹩\mathrm{log}{N}_{{\rm{H}}}^{\mathrm{LOS}}/{\mathrm{cm}}^{-2}﹩) as a function of the inclination angle (i) based on the parsec-scale radiation-driven fountain model. (b) ﹩\mathrm{log}{N}_{{\rm{H}}}^{\mathrm{LOS}}/{\mathrm{cm}}^{-2}﹩ as the function of i based on the sub-parsec-scale radiation-driven fountain model. Here we assumed that the logarithmic initial disk density was ﹩\mathrm{log}d/{\mathrm{cm}}^{-3}=13﹩.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The distribution of the hydrogen number density (﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩) based on the parsec-scale radiation-driven fountain model (Wada et al. 2016). (b) The distribution of ﹩\mathrm{log}{n}_{{\rm{H}}}/{\mathrm{cm}}^{-3}﹩ based on the sub-parsec-scale radiation-driven fountain model (Kudoh et al. 2023). Here we assumed that the logarithmic initial disk density was ﹩\mathrm{log}d/{\mathrm{cm}}^{-3}=13﹩.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The dependence of the Stokes parameter I on the inclination angle (i). (b) The dependence of the Stokes parameter Q on i. (c) The dependence of the Stokes parameter U on i. (d) Comparison of the degree of polarization obtained from our simulation with that of the Circinus galaxy observed with the IXPE (red region). The blue region represents a range of inclination angles of the Circinus galaxy suggested by observations (see Section 3.1). Here errors correspond to a 1σ credible interval.
Paper: Circumnuclear Multiphase Gas in the Circinus Galaxy. V. The Origin of the X-Ray Polarization in the Circinus Galaxy
Authors: Atsushi Tanimoto, Keiichi Wada, Yuki Kudoh, Hirokazu Odaka, Ryosuke Uematsu, Shoji Ogawa
Figure caption: (a) The dependence of the Stokes parameter I on the time. (b) The dependence of the Stokes parameter Q on the time. (c) The dependence of the Stokes parameter U on the time. (d) Comparison of the degree of polarization obtained from our simulation with that of the Circinus galaxy observed with the IXPE (red region). The blue region represents a range of observational suggested inclination angles of the Circinus galaxy (see Section 3.1). Here errors correspond to a 1σ credible interval.