adsabs/AstroCLIMB huggingface dataset:
Paper: ATLAS Photometry of Interstellar Object 3I/ATLAS
Authors: John L. Tonry, Larry Denneau, Miguel R. Alarcón, Alejandro Clocchiatti, Nicolas Erasmus, Alan Fitzsimmons, Javier Licandro, Karen J. Meech, Robert Siverd, Henry Weiland
Figure caption: These images illustrate the evolution of 3I/ATLAS. From left to right are the c band stack from MJD 60818 to 60826 (May 28), the o band stack from 60817 to 60828 (May 26), the epoch at 60884 (July 27) just before the H band slope change described below, and the epoch at 60905 (August 17) when the eastward, antisolar tail becomes prominent. The fields are 100″ with 2″ pixels, north up and east left, and black indicates surface brightness brighter than 23.2 AB arcsec−2.
Paper: Machine Learning Confirms GW231123 is a “Lite” Intermediate Mass Black Hole Merger
Authors: Chayan Chatterjee, Kaylah McGowan, Suyash Deshmukh, Nicholas Tyler-Howard, Karan Jani
Figure caption: (a) Empirical versus nominal coverage for AWaRe predictive uncertainties, evaluated on the simulated IMBH dataset. The points correspond to the central 10%, 50%, and 90% confidence intervals of the Gaussian predictive distributions. (b) Overlap between reconstructed and true waveforms as a function of the single-detector SNR for the Hanford and Livingston detectors.
Paper: ATLAS Photometry of Interstellar Object 3I/ATLAS
Authors: John L. Tonry, Larry Denneau, Miguel R. Alarcón, Alejandro Clocchiatti, Nicolas Erasmus, Alan Fitzsimmons, Javier Licandro, Karen J. Meech, Robert Siverd, Henry Weiland
Figure caption: The discovery the o band image of 3I/ATLAS from MJD 60957 is shown on the left centered on 3I/ATLAS, and the four difference images from that night are stacked on the right. The 9﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 image on the left has north up and east left with the native 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩86 pixels; the 10′ image on the right has 2″ rebinned pixels; black indicates surface brightness brighter than 21 AB arcsec−2.
Paper: Machine Learning Confirms GW231123 is a “Lite” Intermediate Mass Black Hole Merger
Authors: Chayan Chatterjee, Kaylah McGowan, Suyash Deshmukh, Nicholas Tyler-Howard, Karan Jani
Figure caption: Recovered properties of scattering noise (using ArchGEM) versus injected scattering noise (with GlitchPop, which also includes IMBH signal). The left plot refers to the maximum scattering frequency and the plot on the right shows the frequency of scattering.
Paper: ATLAS Photometry of Interstellar Object 3I/ATLAS
Authors: John L. Tonry, Larry Denneau, Miguel R. Alarcón, Alejandro Clocchiatti, Nicolas Erasmus, Alan Fitzsimmons, Javier Licandro, Karen J. Meech, Robert Siverd, Henry Weiland
Figure caption: Magnitudes of 3I/ATLAS in a 6″ × 6″ aperture are shown on the left as a function of time. Red is o band, blue is c band, and magenta is w band from Teide. On the right the magnitudes are corrected for geometrical illumination and distance, ﹩5{\mathrm{log}}\,(r{\rm{\Delta }})﹩, and the Schleicher HM phase function, i.e., an absolute H magnitude in the observed bandpass that shows the physical evolution of 3I/ATLAS with time.
Paper: Machine Learning Confirms GW231123 is a “Lite” Intermediate Mass Black Hole Merger
Authors: Chayan Chatterjee, Kaylah McGowan, Suyash Deshmukh, Nicholas Tyler-Howard, Karan Jani
Figure caption: Box plots showing the median and interquartile ranges of the overlap distributions between AWARE reconstructions and original waveforms for simulated BBH events with total masses between 100 and 1000 M⊙.
Paper: Quasar Negative Feedback to Surrounding Galaxies Probed with Lyα Emitters and Continuum-selected Galaxies
Authors: Yuta Suzuki, Yoshiki Matsuoka, Satoshi Kikuta, Hisakazu Uchiyama, Haruka Kusakabe, Masatoshi Imanishi
Figure caption: Distribution of MUV of continuum-selected galaxies measured by stacking the 18 quasar fields. The blue/red squares show the distribution inside/outside the quasar proximity region. The error bar shows the 1σ uncertainties calculated by the bootstrap resampling method.
Paper: Quasar Negative Feedback to Surrounding Galaxies Probed with Lyα Emitters and Continuum-selected Galaxies
Authors: Yuta Suzuki, Yoshiki Matsuoka, Satoshi Kikuta, Hisakazu Uchiyama, Haruka Kusakabe, Masatoshi Imanishi
Figure caption: Spectra of our quasars sample.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Similar to Figure 2, time evolution of the surface density (first column), tilt (second column), twist angle (third column), and warp amplitude (fourth column) for temperature perturbation in the form of m = 1, n = 1 with amplitude A0,11 = 1%, without and with exponentially cutoff in the outer disk (HFm1n1R0p01 and HFTm1n1R0p01). The temperature perturbation forms are shown in the insets in the ϕ–z plane.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Residual line-of-sight velocity (vlos − vlos,K) for R30 at ﹩{z}^{{\prime} }/r=0﹩, shown in units of the local sound speed. Top row: iref = 30°. Second row: corresponding iobs(r) (black) with disk tilt β (yellow) for reference. Third row: iref = 60°. Fourth row: corresponding iobs(r). Columns from left to right show PA0 = 0°, 90°, 180°, and 270°. These maps can be directly compared with the first row, fourth column of Figure 5.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Left two panels: density on the warped surface for the i = 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 (HF7R) and m = 1, n = 1 (HFm1n1R0p054) models at t = 90P0. This figure is analogous to Figure 1, but with the z-axis stretched by a factor of 5 to emphasize the disk tilt. Right panel: fractional density residual between the two models, plotted on the warped surface of the m = 1, n = 1 model (HFm1n1R0p054). Only the inner 3r0 part of the disk is highlighted. Three concentric grid lines are at r = 1, 2, and 3r0. Because the warped surfaces are nearly identical, plotting the residual on the i = 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 surface (HF7R) yields an almost identical result.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Density distribution in the ﹩{\phi }^{{\prime} }﹩–﹩{\theta }^{{\prime} }﹩ plane for R30 and R90 at t = 500P0. These are the same density fields shown in the first row of Figure 4, but they are zoomed in to the midplane regions, and displayed with linear ﹩{\phi }^{{\prime} }﹩–﹩{\theta }^{{\prime} }﹩ projections. The solid cyan curve marks an alternative density-weighted definition of the gas scale height (Equation (A1)), while the dashed cyan curve traces the vertical location of maximum density. The ﹩\exp (-1/2)﹩ definition of the scale height is still shown in black curves, as in Figure 4.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Similar to Figure 15, but the residual line-of-sight velocity at ﹩{z}^{{\prime} }/r=0.2﹩. These maps can be directly compared with the second row, fourth column of Figure 5.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Long-term evolution of the tilt (top), twist (middle), and warp (bottom) at r = r0 across all full-disk models (blue: HFm1n1R0p01, orange: HFTm1n1R0p01, green: HFm1n1R0p054, dashed pink: HF7R, and dashed gray: HF30R). The vertical line marks the time corresponding to the snapshots shown in Figures 11 and 20 and the end point of the evolution shown in Figures 10 and 12.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Similar to Figure 3, a comparison of the accretion evolution for the radiation–hydrodynamical model (R30) and pure hydrodynamical model (H30) for a 30° inclined shadow.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Vertical slices of the density and temperature for the R30 model at t = 500P0 (P0 ≈ 253 yr) are shown over the entire simulation domain in unprimed code coordinates, in contrast to Figure 5.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Time evolution of the density (top row), tilt (second row), twist (third row), and warp (bottom row) in the pure hydrodynamical simulations with a 30° inclined shadow. Results are shown for reflecting (left, HF30R) and modified outflow (right, HF30Mo) boundary conditions.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: Variation of orbital parameters and the Cartesian velocity in the z-direction. In each panel, the orange curves represent nongravitational accelerations of 10−5 au day−2, and the green, brown, and navy-blue curves represent nongravitational accelerations of 10−6, 10−7, and 10−8 au day−2. Here, we plotted the behavior of 50 clones to keep the image size manageable.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: Variation of orbital parameters and the Cartesian velocity in the z-direction. In each panel, the gray curves are for the simulation without considering interactions with Mars and Jupiter, whereas the blue curves include these planets. The vertical red and black dashed lines represent the date at which the comet is close to Mars and Jupiter. The vertical dotted lines in indigo represent the time of perihelion. Here, we plotted the behavior of 50 clones to keep the image size manageable.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: Variation of the Cartesian coordinates, x, and z, and the Cartesian velocities, vx, and vy. In each panel, the orange curves represent nongravitational accelerations of 10−5 au day−2, and the green, brown, and navy-blue curves represent nongravitational accelerations of 10−6, 10−7, and 10−8 au day−2. Here, we plotted the behavior of 50 clones to keep the image size manageable.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: Top: Histogram of the minimum distance from Jupiter for simulations with 500 clones in the presence of gravitational forces only. Bottom: Histogram of the minimum distance from Jupiter for simulations with 500 clones in the presence of both gravitational and non-gravitational forces. The different non-gravitational accelerations are marked in the same colours as the previous plots.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: The distances from comet to Juno spacecraft, dJuno, and Jupiter dJupiter, are plotted in blue and red curves, respectively, in log scale. The black dashed line is the time of the interaction with Jupiter. The masked region is for the optimal observation when comet 3I will be at 0.4 au or below from the Juno spacecraft with a solar elongation between 28° and 100°.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: The “cosmic shoreline,” which divides solar system planets into those with and without atmospheres, is not universal across exoplanetary systems. The empirical relation between the estimated cumulative XUV irradiation and escape velocity, ﹩{I}_{\mathrm{XUV}}\propto {v}_{\mathrm{esc}}^{4}﹩ (solid purple line), is in line with predictions of the XUV stellar radiation driving atmospheric escape in planets (K. J. Zahnle & D. C. Catling 2017); see also R. D. Chatterjee & R. T. Pierrehumbert (2024) and X. Ji et al. (2025) for more analytical predictions. The arbitrary envelope around the cosmic shoreline represents uncertainty based on factors like host star type, atmospheric composition, and initial volatile content. The cumulative XUV irradiation for each planet is estimated based on the simple scaling relation (Equation (27)) in K. J. Zahnle & D. C. Catling (2017). Planets marked in colors have measured dayside brightness temperatures from Spitzer or JWST that are consistent with (red) or less than (blue) the maximum dayside brightness temperature (see Figure 3 and Table A2 in Appendix A). The planets are divided into those above (circles) and below (triangles) the expected transition in planet density from rocky to not (just) rocky (∼0.8 in ρ/ρe, the ratio between the density of the planet and the density for the same-mass planet given an Earth-like composition; M. Plotnykov & D. Valencia 2024). Given the high irradiation and low escape velocity of TOI-561 b (the light blue symbol outlined in dark blue), our JWST/NIRSpec evidence for a thick atmosphere is in strong conflict with the empirical “cosmic shoreline” hypothesis.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: The JWST/NIRSpec emission spectrum of TOI-561 b is inconsistent with a zero-albedo bare-rock surface. The black symbols and error bars show the Eureka! (circles), ExoTiC JEDI 1 (squares), and ExoTiC JEDI 2 (triangles) reductions/fits. There is no offset applied between the NRS1 and NRS2 detectors (the gap around 3.75 μm). The gray dashed line shows the expected emission spectrum for a bare rocky surface assuming zero Bond albedo. The colored lines show model spectra simulated using a 1D self-consistent atmospheric model and different chemical compositions (see the legend). We assume no day–night heat redistribution in the rock vapor case and efficient day–night heat redistribution in the cases without rock vapor. Volatile-rich atmospheric compositions are able to reproduce the observed brightness temperature. The points plotted here are in Table 1.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: TOI-561 b’s dayside brightness temperature presents the strongest evidence out of all rocky planets for the presence of an atmosphere. As measured from the ∼3–5 μm G395H emission spectrum, the brightness temperature of TOI-561 b (red star symbols, one for each data reduction/fit) is well below the irradiation temperature expected assuming a zero-albedo, zero-heat-redistribution planet (dashed gray line; see the text). The observed trend in the dayside brightness temperature of the current sample of observed rocky planets suggests that USPs with highly irradiated daysides (Tirr > 2500 K) have atmospheres (that may be rock vapor) evaporated from their molten daysides, although note that wavelength ranges are different depending on the observing mode (e.g., MIRI LRS covers ∼6.5–11.5 μm). The data for this plot are provided in Table A2 in Appendix A.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: Normalized RMS vs. bin size for the Eureka! reduction white-light curves (heavier lines) and spectroscopic light curves (lighter lines). In these plots, NRS1 is in blue, and NRS2 is in red, with panels ((a)–(d)) showing Eclipses 1–4. In the absence of time-correlated noise, the actual lines (shown in colors) would follow the ﹩1/\sqrt{(}n)﹩ lines (shown in black). There is residual correlated noise, primarily in Eclipse 4, which has the least amount of out-of-transit baseline. We show the RMS vs. bin size for the white-light curves as the bold lines, and we color code the RMS vs. bin size of the spectroscopic bins according to the central wavelength. The fourth eclipse shows higher noise, but including it does not actually bias the jointly fit emission spectrum—the spectra with and without the fourth eclipse agree at better than 1.5σ per point, with a median difference of less than 5 ppm for the Eureka! reduction.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: Phase-folded Eureka! (top) and ExoTiC JEDI 2 (bottom) independently normalized white-light curves of secondary eclipses of TOI-561 b. We show the phase-folded eclipses with instrumental noise removed for (a), (c) NRS1 (2.8627040–3.7143560 μm) and (b), (d) NRS2 (3.8199180–5.0627574 μm; see Section 4 for details). The black points with associated errors show the 20 minute binned Eureka! or ExoTiC JEDI 2 data, and the red lines show the best-fit astrophysical model from the joint fit to the four eclipses. From the NRS1 and NRS2 white-light curves, we measure eclipse depths of 25 ± 4 ppm and 46 ± 5 ppm, Eureka! and ﹩{53}_{-4}^{+6}﹩ ppm and ﹩{60}_{-8}^{+7}﹩ ExoTiC JEDI 2, respectively.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: Retrieved blackbody emission spectra (left panels) and corresponding temperature posterior probability distributions (right panels) for the Eureka! (top), ExoTiC JEDI 1 (middle), and ExoTiC JEDI 2 (bottom) reductions. In the left panels, the dark orange lines show the medium retrieved spectrum, while the dark/light shaded regions show the 1σ/2σ contours, respectively. These retrievals assume a single-parameter blackbody-spectrum model.
Paper: A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Authors: Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia, Mark Hammond
Figure caption: White-light curves of secondary eclipses of TOI-561 b ((a)–(d)). The four individual consecutive secondary-eclipse white-light curves with best-fit models from the joint fits to the Eureka! eclipses. In each panel, NRS1 (2.8627040–3.7143560 μm) is in blue, and NRS2 (3.8199180–5.0627574 μm) is in red. The unbinned points are shown in the background, and the 2 minutes binned points are shown with their errors. The best-fit models are shown in black.
Paper: HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen
Authors: Nathalie K. Jones, Jason J. Wang, Eric L. Nielsen, Robert J. De Rosa, Anne E. Peck, William Roberson, Jean-Baptiste Ruffio, Jerry W. Xuan, Bruce A. Macintosh, S. Mark Ammons, Vanessa P. Bailey, Travis S. Barman, Joanna Bulger, Eugene Chiang, Jeffrey K. Chilcote, Gaspard Duchêne, Thomas M. Esposito, Michael P. Fitzgerald, Katherine B. Follette, Stephen Goodsell, James R. Graham, Alexandra Z. Greenbaum, Pascale Hibon, Patrick Ingraham, Paul Kalas, Quinn M. Konopacky, Michael C. Liu, Franck Marchis, Jérôme Maire, Christian Marois, Brenda Matthews, Dimitri Mawet, Stanimir Metchev, Maxwell A. Millar-Blanchaer, Rebecca Oppenheimer, David W. Palmer, Jenny Patience, Marshall D. Perrin, Lisa Poyneer, Laurent Pueyo, Abhijith Rajan, Julien Rameau, Fredrik T. Rantakyrö, Bin Ren, Aniket Sanghi, Dmitry Savransky, Adam C. Schneider, Anand Sivaramakrishnan, Adam J. R. W. Smith, Inseok Song, Remi Soummer, Sandrine Thomas, Kimberly Ward-Duong, Schuyler G. Wolff
Figure caption: Posteriors from the OFTI orbit fit of HD 143811 AB b, based on three epochs of relative astrometry. Orbits with eccentricity ≲0.5 are generally preferred, with semimajor axis of ∼60 au and period of ∼300 yr. Red, blue, and green contours correspond to 1σ, 2σ, and 3σ confidence intervals, respectively.
Paper: XRISM Spectroscopy of the Stellar-mass Black Hole GRS 1915+105
Authors: Jon M. Miller, Liyi Gu, John Raymond, Laura Brenneman, Elena Gallo, Poshak Gandhi, Timothy Kallman, Shogo Kobayashi, Junjie Mao, Daniele Rogantini, Megumi Shidatsu, Yoshihiro Ueda, Xin Xiang, Abderahmen Zoghbi
Figure caption: The XRISM/Resolve spectrum of GRS 1915+105 in its obscured state. The model in red is the best-fit model detailed in Table 1. It consists of a highly obscured disk plus power-law continuum and three photoionized emission zones in the outer accretion disk, weakly shaped by resonant scattering. The strongest lines are from He-like and H-like charge states of Si, S, Ar, Ca, Cr, Mn, Fe, and Ni. Solid vertical lines mark the lab energies of the observed He-like (top row) and H-like transitions (bottom row). A weak, narrow, neutral Fe Kα emission line is clearly detected at 6.4 keV, signaling the presence of cold gas at intermediate disk radii. Several RRC features are marked with triangles, including from He-like and H-like Fe at 8.8 and 9.3 keV, respectively. The data are binned using the “optimal” binning algorithm.
Paper: The Plane Quasar Survey: An Ionized Extension of the Magellanic Stream on the Northern Side of the Galactic Plane
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, Mary E. Putman, Yong Zheng, J. E. G. Peek, Hannah Bish, David Schiminovich
Figure caption: The location of high-ion absorbers near the MS in (panel (a)) Galactic coordinates and (bottom panel (b)) MS coordinates. In this work, we detect C IV absorbers (circles), extending to the northern sky (Galactic latitude of b ∼ 30∘). We also include C IV (squares; A. J. Fox et al. 2014) and O VI (cross symbols; K. R. Sembach et al. 2003) absorbers from previous studies. The LSR velocity of the absorbers is color coded. The all-sky H I map from the HI4PI survey (T. Westmeier 2018) is shown with the same velocity color scale.
Paper: The Plane Quasar Survey: An Ionized Extension of the Magellanic Stream on the Northern Side of the Galactic Plane
Authors: Bo-Eun Choi, Jessica K. Werk, Kirill Tchernyshyov, Mary E. Putman, Yong Zheng, J. E. G. Peek, Hannah Bish, David Schiminovich
Figure caption: UV spectra and fitted Voigt profiles for Si IIλ1527 (left), Si IVλ1394 (center), and C IVλ1548 (right) absorptions in the QSO sight lines. The components associated with the MS are shown in purple. These components have distinct velocity offsets from other HVCs, such as Complex C (green), and are not detected in low ions like Si II.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Slices of the radiation–hydrodynamical simulations at r = 4r0 (160 au) for the i = 30° tilted shadow (R30, left) and i = 90° tilted shadow (R90, right) at t = 500P0 (P0 ≈ 253 yr). Top: density. Middle: temperature. Bottom: tangential velocity (streamlines) overlaid on the radial velocity background. Longitude lines are spaced every 60°, centered at ﹩{\phi }^{{\prime} }=\pi ﹩; latitude lines are spaced every 30°. Although both shadows have the same intrinsic width, the polar shadow appears narrower due to projection effects. The center and edges (i.e., τ = 1 surfaces, at ±0.27 of the midplane) of the shadow lanes in density and velocity plots are marked by white curves. In the density panels, the high-density regions are defined as the regions within the black curves defined as the ﹩\exp (-1/2)﹩ of the maximum density along the ﹩{\theta }^{{\prime} }﹩ direction. In the temperature panels, shock heated regions are marked by black arrows.