adsabs/AstroCLIMB huggingface dataset:
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Comparison between different subimage definitions for a nonrotating black hole. The observer is positioned at i = 17° away from the normal to the midplane, which is shown as a black dashed line. The colored lines represent the α = 0, β < 0 geodesics that reach the observer (see Section 2.2 for more detail). Photons emitted at different points along the same geodesic can contribute to different subimages. We color each point along the geodesics according to whether a photon emitted at that point will contribute to the direct (n = 0; blue) or indirect (n = 1; red) subimage. The colors in the left and right panels are evaluated according to the d θ/ds and dz/ds turning-point definitions, respectively. In both panels, photons emitted along the geodesics in the underlying gray shaded region would be considered direct emission (n  t  = 0) under the time-ordering subimage definition.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Echo delay seen by a face-on observer as a function of black hole spin and midplane emission location. The gray hatched region covers the radii interior to the event horizon. The color map shows the n = 0 → n = 1 echo delay for the emitted material as a function of black hole spin a * and radial position within the midplane r. Blue and red lines show the locations of the innermost stable circular orbit (ISCO) for prograde and retrograde massive particles, respectively. The black shaded region denotes the photon shell, extending from the prograde photon orbit (smaller radius) to the retrograde one (larger radius). The polar photon orbit, i.e., the one visible to a face-on observer, is denoted with a dashed black line. The echo delay period is more sensitive to the emission location than the spin.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: The amplitude of the Fourier transform (visibility amplitude) of the simulated image shown in Figure 1 for the total image and its subimage decomposition. The ringing features become more prominent for higher-order subimages, reflecting the increasingly sharp and regular ring structure seen in the images.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Isodeltachrones for a Schwarzschild black hole. Both the contours and the color map show the time delay between the direct and first-order indirect emission (left), between the first- and second-order indirect emission (second), and so on. The observer is located directly above the black hole at infinity. The zero-time-delay isodeltachrones coincide with the caustics along the z-axis. The isodeltachrone structure quickly converges to a universal pattern that alternatively mirrors across the x-axis for each higher-order pair of subimages.
Paper: Evolution of Semiconvective Staircases in Rotating Flows: Consequences for Fuzzy Cores in Giant Planets
Authors: J. R. Fuentes, Bradley W. Hindman, Adrian E. Fraser, Evan H. Anders
Figure caption: Panel (a): density profile at the beginning of the erosion phase for the nonrotating and rotating cases. Note that in the rotating case, the density is not constant within the convection zone. Instead, there is a positive density gradient due to the thermal structure of the fluid in the convection zone (in nonrotating convection, the temperature becomes isothermal, whereas in rotating convection, the fluid develops a small temperature gradient). Panel (b): evolution of the density contrast between the two layers during the erosion phase. For both cases Δρ decreases linearly with time, but the rotating case decays at a slower rate. Further, the initial density contrast at the beginning of the erosion phase is smaller for the rotating case (likely due to diffusion since it takes longer for the fluid to reach this stage).
Paper: Evolution of Semiconvective Staircases in Rotating Flows: Consequences for Fuzzy Cores in Giant Planets
Authors: J. R. Fuentes, Bradley W. Hindman, Adrian E. Fraser, Evan H. Anders
Figure caption: Horizontally averaged concentration of heavy elements at depth z and time t (normalized by the thermal diffusion time across the box ﹩{\tau }_{T}={L}_{z}^{2}/{\kappa }_{T}﹩). Results are shown for both the nonrotating and rotating cases (panels a and b, respectively). Layer formation occurs in both cases, but layers persist for a longer time in the rotating case. The vertical dashed line in both panels denotes the time at which the nonrotating case becomes fully mixed. Note that the horizontal axis is not the same in both panels.
Paper: Evolution of Semiconvective Staircases in Rotating Flows: Consequences for Fuzzy Cores in Giant Planets
Authors: J. R. Fuentes, Bradley W. Hindman, Adrian E. Fraser, Evan H. Anders
Figure caption: Vertical profiles of the rms velocity for four different phases during the evolution of the convective staircase for the rotating case. From the rms velocity, we have estimated the Rossby number, Ro, of the flow (see main text). As expected, as layers merge the flow velocity increases. Time increases as the system evolves from six to four to two and finally to one layer.
Paper: Evolution of Semiconvective Staircases in Rotating Flows: Consequences for Fuzzy Cores in Giant Planets
Authors: J. R. Fuentes, Bradley W. Hindman, Adrian E. Fraser, Evan H. Anders
Figure caption: Vertical profiles of the convective and diffusive composition fluxes for the nonrotating case (blue) and rotating case (orange). The fluxes are shown at the beginning of the erosion phase of the remaining two layers. The solid and dashed lines denote the contribution to the flux purely due to convection and diffusion, respectively.
Paper: Atmospheric Retrievals Suggest the Presence of a Secondary Atmosphere and Possible Sulfur Species on L98-59 d from JWST Nirspec G395H Transmission Spectroscopy
Authors: Agnibha Banerjee, Joanna K. Barstow, Amélie Gressier, Néstor Espinoza, David K. Sing, Natalie H. Allen, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Carole A. Haswell, Nikole K. Lewis, Stephen R. Lewis, Jingxuan Yang
Figure caption: The retrieved spectra for the two alternate retrievals are shown: the Stellar + Atmosphere scenario with H2S and SO2 removed is plotted in red and the equilibrium chemistry scenario is plotted in blue. The 1σ and 2σ credible intervals are plotted in dark and light shades of the corresponding colors, respectively. The NRS2 points are shifted by the retrieved offset, and the unshifted NRS2 points are shown in gray. Underneath the spectrum, in the first row from left to right, the retrieved posterior distributions for f het, T phot, ΔT het, and offset are shown. In the second row, from left to right, the retrieved posterior distribution for temperature, metallicity, S:O ratio, and C:O ratio are shown.
Paper: Atmospheric Retrievals Suggest the Presence of a Secondary Atmosphere and Possible Sulfur Species on L98-59 d from JWST Nirspec G395H Transmission Spectroscopy
Authors: Agnibha Banerjee, Joanna K. Barstow, Amélie Gressier, Néstor Espinoza, David K. Sing, Natalie H. Allen, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Carole A. Haswell, Nikole K. Lewis, Stephen R. Lewis, Jingxuan Yang
Figure caption: This plot shows the retrieved spectra from the main retrieval scenarios of stellar inhomogeneities with planetary atmospheres and stellar inhomogeneities only extended to the 0.6–12 μm JWST wavelength range. The gas contributions for H2S and SO2 are highlighted. The available wavelength ranges for different JWST instruments are marked at the top of the plot. Several H2S features in the NIRISS SOSS range, combined H2S and SO2 features in the NIRSpec G395H range, and SO2 features in the MIRI LRS range may be detectable in future observations.
Paper: Atmospheric Retrievals Suggest the Presence of a Secondary Atmosphere and Possible Sulfur Species on L98-59 d from JWST Nirspec G395H Transmission Spectroscopy
Authors: Agnibha Banerjee, Joanna K. Barstow, Amélie Gressier, Néstor Espinoza, David K. Sing, Natalie H. Allen, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Carole A. Haswell, Nikole K. Lewis, Stephen R. Lewis, Jingxuan Yang
Figure caption: The retrieved spectra for the retrievals using two different reductions are shown: transitspectroscopy is plotted in red and FIREFLy is plotted in blue. The 1σ and 2σ credible intervals are plotted in dark and light shades of the corresponding colors, respectively. The NRS2 points are shifted by the retrieved offset, and the unshifted NRS2 points are shown in gray. Underneath the spectrum, in the first row from left to right, the retrieved posterior distributions for log(H2S), log(SO2), and temperature are shown. In the second row, from left to right, the retrieved posterior distributions for f het, T phot, and ΔT het are shown.
Paper: Atmospheric Retrievals Suggest the Presence of a Secondary Atmosphere and Possible Sulfur Species on L98-59 d from JWST Nirspec G395H Transmission Spectroscopy
Authors: Agnibha Banerjee, Joanna K. Barstow, Amélie Gressier, Néstor Espinoza, David K. Sing, Natalie H. Allen, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Carole A. Haswell, Nikole K. Lewis, Stephen R. Lewis, Jingxuan Yang
Figure caption: The retrieved spectra for the main retrievals: Stellar + Atmosphere scenario is plotted in red, Atmosphere Only in blue, and Stellar Only in green. The 1σ and 2σ credible intervals are plotted in dark and light shades of the corresponding colors, respectively. The NRS2 points are shifted by the retrieved offset, and the unshifted NRS2 points are shown in gray. Underneath the spectrum, in the first row from left to right, the retrieved posterior distributions for log(H2S), log(SO2), and temperature are shown. In the second row, from left to right, the retrieved posterior distributions for f het, T phot, and ΔT het are shown.
Paper: Atmospheric Retrievals Suggest the Presence of a Secondary Atmosphere and Possible Sulfur Species on L98-59 d from JWST Nirspec G395H Transmission Spectroscopy
Authors: Agnibha Banerjee, Joanna K. Barstow, Amélie Gressier, Néstor Espinoza, David K. Sing, Natalie H. Allen, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Carole A. Haswell, Nikole K. Lewis, Stephen R. Lewis, Jingxuan Yang
Figure caption: The corner plot showing retrieved posterior distributions for each parameter for the main retrieval. The plots on the diagonal show the histograms of retrieved parameters and the inner plots show the pairwise correlations between the parameters. Large abundances for H2S and SO2 can be seen, with upper bounds for all other active gases.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Top half: geometrical representation of the spectral lags. Positive lag is produced within θ out due to the curvature effect, while negative lag is produced due to the late emission of high-energy photons from the region bounded within θ j − θ out, where the energy gain takes place. However, the high-energy photons typically escape from the inner jet region (θ < θ j) at the last scattering. Bottom half: geometry of the last scattering angle. θ  l  is the angle between the radially moving electron and the observer’s location. If the observer is assumed at θ o = 0, then θ  l  = θ.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Distribution of the observed photon energy E over observing time t for the observer situated along the jet axis for parameters L = 1052 erg s−1, θ j = 0.01 rad, p = 4, and Γ0 = 100 (top panel) and L = 1051 erg s−1, θ j = 0.03 rad, and Γ0 = 50 (bottom panel). The photons are injected with energy E  i  = 10−3 m  e  c 2.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Photon map in the E–t plane for L = 1050 erg s−1, θ j = 0.01 rad, Γ0 = 30, p = 4, and ﹩{{\rm{\Gamma }}}_{\min }=1.2﹩. The photons are launched at r inj = R ph/20 following blackbody distribution with corresponding fluid temperature ﹩T^{\prime} ({r}_{i},\theta )﹩.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Spatial relations between X-rays and γ-rays. The dual-band image consists of ROSAT X-ray images of W50 (red) and the significance of H.E.S.S. data in the 0.8–2.5 (a), 2.5–10 (b), and >10 TeV (c) bands (H.E.S.S. Collaboration et al. 2024; cyan). The white contours show the 1.5σ, 3σ, and 4.5σ confidence levels of the TeV emission. The X-ray image is in square-root scale, and the contour levels are 1.5σ, 3.0σ, and 4.5σ. The newly discovered X-ray shell is labeled in green. In the upper panel, the yellow plus signs mark the location of GeV source Fermi J1913+0515 and the “west excess” (J. Li et al. 2020), and the circle stands for the position uncertainty. In the lower panel, the yellow plus signs label LHAASO sources 1LHAASO J1913+0515 (detected by KM2A) and 1LHAASO J1910+0516* (detected by WCDA and KM2A; Z. Cao et al. 2024), with the circles the 1σ extension or 95% extension upper limit of the sources.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Light curves for different energy channels showing positive lag in the low-energy range (upper panel) and negative lag in the high-energy band (lower panel). The light curves are overplotted with the Savitzky–Golay filter (solid lines). The vertical arrows represent the location of the peak of the light curves. The parameters are the same as in Figure 3.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: (a) Average surface brightness evolution of the wind bubble in the region Clump. (b), (c), and (d) Normalized luminosity distribution of the temperature in 20, 90, and 150 kyr, respectively. At 20 kyr, the X-ray emission is completely from the shell, as the shock has not arrived at the cloud. At 90 and 150 kyr, the X-rays are dominated by the clump. The last bin (1.6 keV) represents the temperature range above 1.5 keV.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Variation of spectral lag between different energy channels for Γ0 = 30. Other parameters are the same as in Figure 4.
Paper: An X-Ray Shell Reveals the Supernova Explosion for Galactic Microquasar SS 433
Authors: Yi-Heng Chi, 奕恒 池, Jiahui Huang, 佳辉 黄, Ping Zhou, 平 周, Hua Feng, 骅 冯, Xiang-Dong Li, 向东 李, Sera B. Markoff, Samar Safi-Harb, Laura Olivera-Nieto
Figure caption: Relation between the change in the chi-square (Δχ 2) and the value of the emission measure (in units of cm−5) given by steppar for three models in two regions (blue solid lines). Green dotted lines and orange dashed lines mark the fitting statistics corresponding to the 3σ (Δχ 2 = 9) and 5σ (Δχ 2 = 25) confidence level. With large degrees of freedom, the chi-square distribution can be approximated as the Gaussian distribution.
Paper: Probing the Low-velocity Regime of Nonradiative Shocks with Neutron Star Bow Shocks
Authors: Stella Koch Ocker, Maren Cosens
Figure caption: Ratio of blue- to redshifted broad-line radial velocity ∣V blue/V red∣ vs. shock inclination angle. Negative angles correspond to inclination out of the sky and positive angles into the sky. The horizontal lines and shaded regions show inferred values and 1σ uncertainties of ∣V blue/V red∣ for J0742−2822 (blue), J1741−2054 (green), and J2225+6535 (purple). The expected velocity ratio is estimated for an axisymmetric shock from an isotropic stellar wind (F. P. Wilkin 1996), for different values of α = V */V  w , the ratio of the ISM velocity to stellar wind velocity. We constrain approximate ranges of inclination angle for each shock using the limit α → 0 (solid black curve), as appropriate for a relativistic wind.
Paper: Probing the Low-velocity Regime of Nonradiative Shocks with Neutron Star Bow Shocks
Authors: Stella Koch Ocker, Maren Cosens
Figure caption: KCWI observations of three pulsar bow shocks, J0742−2822 (top), J1741−2054 (middle), and J2225+6535 (the Guitar Nebula; bottom). Images are shown for 12 radial velocity bins centered around the peak shock emission; the spectra have been smoothed from the native resolution of 0.25 Å to show the large velocity range (larger bins are used for the Guitar Nebula due to its wider extension to negative velocities). These slices are continuum subtracted using off-band portions of the data cube; photospheric Hα absorption causes many stars to show negative residuals, centered on different low-velocity channels. Over-subtracted stars are shown by the gray dashed circles and are masked in subsequent analysis. The white tick marks are 5″ apart; each image is about 13″ on a side (≈0.1, 0.02, and 0.04 pc on a side, from top to bottom). The dynamic range of each image is normalized to its peak flux level in order to illustrate shock structure at the lowest and highest velocities.
Paper: Probing the Low-velocity Regime of Nonradiative Shocks with Neutron Star Bow Shocks
Authors: Stella Koch Ocker, Maren Cosens
Figure caption: Heliocentric radial velocity profiles for J0742−2822 (left), J1741−2054 (middle), and J2225+6535 (right). The upper panels illustrate the regions of each shock used to calculate the aperture-averaged velocity profiles shown in the bottom panels, labeled (a, b, c, and d). The images in the upper panels are averaged over the full velocity range of each shock, and the gray dashed circles indicate stars that are subsequently masked. The velocity profiles are each normalized to unity peak flux and shown with an arbitrary offset so that specific velocity features can be compared. Error bars correspond to the standard deviation of flux within each region at a given wavelength. Solid lines indicate the best-fit model for the velocity profile, which is treated as a sum of Gaussian components (Section 3).
Paper: Probing the Low-velocity Regime of Nonradiative Shocks with Neutron Star Bow Shocks
Authors: Stella Koch Ocker, Maren Cosens
Figure caption: Broad-to-narrow line ratio (I b/I n) vs. effective shock velocity for both SNRs (blue) and NS bow shocks (orange). SNR constraints are from the recent literature compilation of J. C. Raymond et al. (2023), and orange points indicate values inferred for the three NS bow shocks in this study and one bow shock from R. W. Romani et al. (2022). All four bow shocks appear to have velocities below the SNR radiative transition, which is shown by the gray dashed line for a nominal energy E = 1051 erg and density n = 1 cm−3 (J. M. Blondin et al. 1998).
Paper: Hedgehog: An Isolated Quiescent Dwarf Galaxy at 2.4 Mpc
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Scott G. Carlsten, Shany Danieli
Figure caption: The SBF measurements for Hedgehog using the IMACS i-band data (top panels) and the Legacy Surveys DR10 i-band data (bottom panels). The left panels show the original image with the mask overlaid in yellow. We fit a Sérsic model to the masked image, subtract the model from the image, and divide the residual by the square root of the model. This normalized residual image is shown in the middle panels. We then calculate the azimuthally averaged power spectrum of the normalized residual, as shown in the right panels. The power spectrum is fit with a combination of the PSF power spectrum and white noise. To account for the contribution from unmasked sources, we measure SBF signals on randomly selected blank fields, whose power spectra are shown as the teal dashed line. After subtracting the background contribution, we calculate the median SBF signal and its standard deviation and convert it to distance using the SBF–color relation in Carlsten et al. (2019). The SBF distances from IMACS and Legacy Surveys DR10 are ﹩{D}_{\mathrm{SBF}}^{\mathrm{IMACS}}=2.40\pm 0.15\ \mathrm{Mpc}﹩, ﹩{D}_{\mathrm{SBF}}^{\mathrm{LS}}=2.45\pm 0.16\ \mathrm{Mpc}﹩. These two independently measured distances are fully consistent.
Paper: Hedgehog: An Isolated Quiescent Dwarf Galaxy at 2.4 Mpc
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Scott G. Carlsten, Shany Danieli
Figure caption: The V-band absolute magnitude and size of Hedgehog, together with other isolated quiescent dwarf galaxies (KKR 25, Makarov et al. 2012; KKs 3, Karachentsev et al. 2015; COSMOS-dw1, Xi et al. 2018; Polzin et al. 2021; Tucana B, Sand et al. 2022) and potential backsplash galaxies in the Local Group and M81 (Cetus, Tucana, And XVIII, Eri II, and Blobby; shown in yellow triangles). The quiescent dwarfs at D < 2 Mpc (McConnachie 2012) and early-type satellites of MW analogs (Carlsten et al. 2022) are shown in gray for reference. Hedgehog agrees with the size–luminosity relation but is on the smaller side.
Paper: Hedgehog: An Isolated Quiescent Dwarf Galaxy at 2.4 Mpc
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Scott G. Carlsten, Shany Danieli
Figure caption: Cutout images of Hedgehog from the Legacy Surveys DR10 (left), the deep and high-resolution Magellan/IMACS i-band data (middle), and the GALEX NUV and FUV data (right). Hedgehog shows significant SBF signals in the Legacy Surveys data and is resolved into individual stars in the IMACS data. There is also no significant UV emission associated with Hedgehog.
Paper: Hedgehog: An Isolated Quiescent Dwarf Galaxy at 2.4 Mpc
Authors: Jiaxuan Li, 嘉轩 李, Jenny E. Greene, Scott G. Carlsten, Shany Danieli
Figure caption:  ArtPop models of Hedgehog at different distances. We generate these mock galaxies assuming an SSP with an age of 6 Gyr and metallicity of [Fe/H] = −1.75 and place them at different distances but fix the shape and surface brightness. The mock galaxy at 2.4 Mpc visually reproduces both the SBF signal and the integrated color of Hedgehog very well. The two galaxies at 1.8 Mpc and 3.0 Mpc show too strong and too weak SBF signals.
Paper: Unified Theory of Negative and Positive Spectral Lags in the Gamma-Ray Burst Prompt Phase due to Shear Comptonization from a Structured Jet
Authors: Mukesh Kumar Vyas, Asaf Pe'er, Shabnam Iyyani
Figure caption: Photospheric radius for viewing angles θ o = 0 (top left), 0.05 (top right), and 0.10 (bottom) with p = 2.0, θ j = 0.10 rad , Γ0 = 50, and L = 1052 erg s−1.