adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of an Extremely Large Impact Flash on Jupiter by High-cadence Multiwavelength Observations
Authors: Ko Arimatsu, Kohji Tsumura, Fumihiko Usui, Jun-ichi Watanabe
Figure caption: PONCOTS V-band image and spectral-system response for the three PONCOTS bands. (a) The left panel is an example of the PONCOTS V-band image of Jupiter obtained during the flash; the right panel is as for the left but shown with a different surface brightness range. An artifact ghost image appears in the field of view. The bright spot on the left in the image corresponds to Io, a satellite of Jupiter. (b) Relative spectral responses of the three PONCOTS bands. Blue, green, and red lines indicate the efficiency for the PONCOTS V, Gh, and CH4 bands, respectively. Spectral responses for the V and CH4 bands were estimated by convolving quantum efficiencies of CMOS sensors with the filter response and transmittance or reflectance of the dichroic mirrors is provided by manufacturers. The Gh band response was obtained from signal values of artifact images of the spectrophotometric standard stars at each wavelength, using narrowband filters.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: Panel (a): Radial magnetization profiles of the jets with σ 0 = 15, calculated by taking the weighted-average magnetization over the radial energy flux excluding the rest-mass energy flux and fluid elements with u ∞ < 1. The profiles at different times indicate that the magnetization in the jets does not change over time and remains at 〈σ〉 ∼ 10−2 after breakout. Panel (b): Profiles of the weighted averages of σ (blue), proper velocity u (green), and asymptotic proper velocity u ∞ (black), shown for jets with σ 0 = 15 (thick lines) and σ 0 = 200 (thin lines) when the jet head is at r ≈ 2.5 × 1011 cm (t = 10 s). The jets are launched with high magnetization (σ ≫ 1), but the magnetic energy is efficiently converted into kinetic energy until r ≈ 109.5 cm, maintaining a constant 〈u ∞〉. After this point, the mixing between the jets and the star increases, thereby reducing 〈σ〉 further, and 〈u ∞〉 as well, as seen by their correlated values. The jets become mildly magnetized at r ≈ 1010 cm. Panel (c): Profiles of the maximum values of the quantities in (b) for the jet with σ 0 = 15 at t = 18 s. It shows that some jet elements reach Γ ∼ 10 after breakout with a maximum σ ∼ 0.3.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: The energy distribution of matter at r >  R ⋆, excluding the rest-mass energy, is shown according to various parameters. For the simulation with σ 0 = 15, we show the distribution at three different times: t = 6 s (purple), t = 12 s (maroon), and t = 18 s (gray). The blue line represents the distribution of energy in the jet with σ 0 = 200 at t = 10 s. Panel (a): The angular energy distribution integrated over the azimuthal angle of the outflow can be modeled by a flat core and a moderate power law followed by an exponential decay. Panel (b): The energy distribution per logarithmic asymptotic proper velocity is quasi-uniform irrespective of the choice of σ 0. Both angular and radial distributions are consistent with those of hydrodynamic jets (Gottlieb et al. 2021b). Panel (c): The fraction of energy in matter with magnetization larger than σ out of the total energy. It can be seen that a significant amount (∼20%) of the outflow energy is carried by plasma with σ ≳ 10−2 (σ ≳ 10−1) when σ 0 = 15 (σ 0 = 200).
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: 3D rendering in the simulation with σ 0 = 15 shows the logarithm of u ∞ (top) and σ (middle) in the jet (yellow)/cocoon (blue) structure when the jet head reaches r = 0.5 R ⋆ at t ∼ 1.5 s. It shows that at this radius the jet magnetization is already σ ≲ 0.1. Bottom: The postbreakout outflow after 18 s, when the head of the intermittent jet (red) is at ∼12 R ⋆ and the cocoon (green blue) explodes the star (yellow) entirely. The color coding is a combination of the mass density with u ∞ in order to show both the jet and the cocoon. Movies showing the full evolution of the outflow are available at http://www.oregottlieb.com/collapsar.html.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: The radiative efficiency at r = 2 R ⋆ for the jet with σ 0 = 15. The jet’s wobbling motion is responsible for two features in the signal: (i) long quiescent times at all viewing angles and (ii) observers far from the polar axis, at θ  t  + θ  j , can detect high radiative efficiency. However, we find that in general, the efficiency decreases with angular distance from the axis.
Paper: Inferring Late-stage Enrichment of Exoplanet Atmospheres from Observed Interstellar Comets
Authors: Darryl Z. Seligman, Juliette Becker, Fred C. Adams, Adina D. Feinstein, Leslie A. Rogers
Figure caption: The ratio of accreted to outward-scattered comets, given by Equation (13), as a function of the Safronov number of the interacting planet. The (i) dashed and (ii) solid lines correspond to comets with perihelia (i) much less than (Λ = 3, Γ = 1) and (ii) approximately equal to (Λ = 0.18, Γ = 1) the semimajor axis of the scattering planet. The blue, yellow, and red regions indicate where σ A/σ C = 100%, 10% < σ A/σ C < 100%, and σ A/σ C < 10% for Λ = 3. The top x-axis shows the semimajor axis corresponding to the Safronov number on the bottom axis, for a planet with a Jovian mass and radius, orbiting a solar-type star. The positions of WASP-77 Ab, Jupiter, and HR 8799 b are indicated by vertical white lines.
Paper: Inferring Late-stage Enrichment of Exoplanet Atmospheres from Observed Interstellar Comets
Authors: Darryl Z. Seligman, Juliette Becker, Fred C. Adams, Adina D. Feinstein, Leslie A. Rogers
Figure caption: The cometary accretion efficiency for every detected exoplanet. The x-axis shows the orbital semimajor axis, and the y-axis shows the mass or m sin i for each planet. The color of each point indicates the efficiency with which the planet accretes comets, as given by the ratio of the accretion to the outward-scattering cross section. We calculate this quantity using Equation (13) with Λ = 1 and Γ = 1.
Paper: Black Hole to Photosphere: 3D GRMHD Simulations of Collapsars Reveal Wobbling and Hybrid Composition Jets
Authors: Ore Gottlieb, Matthew Liska, Alexander Tchekhovskoy, Omer Bromberg, Aretaios Lalakos, Dimitrios Giannios, Philipp Mösta
Figure caption: The time evolution of the jet-tilt angle θ  t  in the simulation with σ 0 = 15. Top: The tilt angle deep inside the star (blue) and upon breakout (purple) shows that θ  t  is attenuated as the jet propagates in the star and its orientation is focused toward the stellar rotation axis. Bottom: Colormap of the jet-tilt angle shows that it varies significantly inside the star but is conserved after breakout along light-like streamlines. The asymptotic jet-tilt angle is θ  t  ≲ 0.2 rad.
Paper: Inferring Late-stage Enrichment of Exoplanet Atmospheres from Observed Interstellar Comets
Authors: Darryl Z. Seligman, Juliette Becker, Fred C. Adams, Adina D. Feinstein, Leslie A. Rogers
Figure caption: The accretion efficiency for exoplanets that will be observed with JWST. Because most targets are susceptible to cometary enrichment, this process should be considered when interpreting forthcoming observations of these exoplanetary atmospheres. We calculate this using Equation (13) with Λ = 1 and Γ = 1. Note that the following JWST targets are not included in the figure: TOI-836 b TOI-836 c, TOI-175 b, GJ 341 b, GJ 4102 b, and TOI-134 b.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: The velocity structure from the cavity wall B0 to shocks B1 and B2 (the same for both cases with or without pb correction). The three left columns show the velocity structure maps of the (2,2) and (3,3) lines. The background in each panel shows the velocity map V  p , where the line intensity peaks (the first column), V  b , where the blueshifted wing extends to (the second column), and the peak-to-bluest velocity offset V  p  − V  b  (the third column). All maps are naturally weighted. The black contours are the same continuum emissions as those in Figure 1. The purple contour indicates the 5σ emission from the (1,1) integrated intensity toward the flattened envelope around the protobinary system, which is perpendicular to the outflow direction. The gray dashed contours and the labeled clumpy substructures are the same as shown in Figure 1, and the synthesized beam is plotted in the bottom-left corner. The pb-corrected line emissions with < 5σ rms are blank in each panel. The black curve guides the path of the precessing jet from L1157-mm as modeled by Podio et al. (2016). The last column shows the (2,2) and (3,3) line profiles extracted from clumpy substructures along the jet path. The gray dashed vertical line indicates the system velocity of the cloud Vsys  = 2.7 km s−1, and the red dashed vertical line indicates the velocity where the main component of each line blueward V lsr = −10 km s−1. The line intensity Jy beam−1 is converted to the brightness temperature T  B , and the horizontal cyan line indicates the baseline (T  B  = 0 K). A narrow feature appears toward the protobinary system mm on the spectrum, probably tracing the quiescent and cold gas in the flattened envelope.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: The outline of the southern (blueshifted) outflow lobe from the Class 0 compact protobinary system L1157-mm. Color maps show the naturally weighted (r = 2.0) intensity maps of NH3 (1,1)–(7,7) integrated over the velocity range of −25 to +25 km s−1 (without pb correction). Line emissions with <5σ rms are blank in each panel. The red contours, starting from 8σ (σ = 0.27 Jy beam−1) and increasing with a step of 8σ, show the CO (1–0) emission, obtained from the NOEMA and IRAM-30 m combination (Gueth et al. 1996). The black contours, starting from 4σ (σ = 0.01 mJy beam−1) and increasing with a step of 4σ, show the naturally weighted continuum emission at 1.3 mm (without pb correction). The gray circle in each panel indicates the largest recoverable scale at the corresponding line rest frequency, and the angular resolution is plotted at the bottom-left of each panel. In the panel of the (1,1) line, the black curve guides the path of the precessing jet from the driving source L1157-mm as modeled by Podio et al. (2016). The black squares indicate the shock knots B0, B1, and B2. In the panels of the (2,2)–(7,7) lines, nine clumpy substructures are labeled.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: Left column: the V  p  map of the main hyperfine component of the (1,1) and (2,2) lines toward the flattened envelope around the marked protobinary system, which should elongate in the direction shown as the gray two-headed arrow (Chiang et al. 2010), perpendicular to the outflow. In each panel, the black contours indicate the integrated intensity (with pb correction), starting from 5σ and increasing by 3σ. The gray dashed contours, starting from 4σ (σ = 0.27 Jy beam−1) and increasing with the step of 5σ, show the CO (1-0) emission (Gueth et al. 1996), and the synthesized beam is plotted in the bottom-left corner. The pb-corrected (1,1) line emissions with <5σ rms are blank in each panel. Right column: beam-averaged line profiles extracted from the protobinary system and two positions perpendicular to the outflow direction in the flattened structure (labeled as α and β on the V  p  map). The gray dashed vertical line indicates the Vsys  = 2.7 km s−1 of the cloud. The line intensity Jy beam−1 is converted to the brightness temperature T B , and the horizontal cyan line indicates the baseline (T  B = 0 K).
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: Beam-averaged line profiles (the line intensity Jy beam−1 is converted to the brightness temperature T  B ), with the center toward nine clumpy substructures (Table A1) in the plane of the sky. The HfS fit is shown in red overlying each spectrum. All lines are extracted from images smoothed to the same pixel size (0.″5), and their velocity resolutions are listed in Table 1. In each panel, two red vertical lines at ‒25 and + 25 km s−1 indicate the velocity range within which we integrate the intensity; the gray dashed vertical line indicates the Vsys  = 2.7 km s−1 of the cloud. The horizontal cyan line indicates the baseline (T  B  = 0 K).
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: Kinetic temperature maps and column density maps for o- and p-NH3, derived from LVG MultiNest best fitting, by assuming a single component (with an FWHM line width of 4 km s−1) and two filling factors (1 for (1,1)–(3,3) lines and 0.1 for (4,4)–(7,7) lines) toward each position. Panels from left to right in the upper row show the relative ratio and the mean of T kin from o-/p-NH3, as well as the total column density and the OPR of NH3. Panels in the lower row show the uncertainty with respect to the value of the above parameters. The pixels where the pb-corrected NH3 (5,5) and (6,6) lines < 5σ emission and CO(1–0) < 8σ emission are blank. The gray dashed contours and the labeled clumpy substructures are the same as shown in Figure 1. The black curve guides the path of the precessing jet from L1157-mm as modeled by Podio et al. (2016). These maps are derived by smoothing all lines to the same pixel size and angular resolution, i.e., 4.″90 × 3.″81, shown as the synthesized beam in the bottom left of each panel.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: The outline of the southern (blueshifted) outflow lobe from the Class 0 compact protobinary system L1157-mm (images with different weightings are given in different rows). Color maps show the intensity maps of NH3 (1,1)–(7,7) integrated over the velocity range of −25 to + 25 km s−1 (with pb correction). The black contours, starting from 4σ (σ = 0.03 mJy beam−1) and increasing with a step of 4σ, show the continuum emission with the same weighting as the line emissions (with pb correction). The rest of the contours and all the labels are the same as in Figure 1. The solid gray circle indicates the largest recoverable scale and the dashed gray circle indicates the primary beam.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: The best fit of the kinetic temperature maps and column density maps for o- and p-NH3, derived from LVG MultiNest, by assuming a single component and unity filling factor for all lines toward each position. The results assuming the line width as 4 km s−1 and 9 km s−1 are shown in the upper and lower rows, respectively. The pixels where the NH3 (5,5) and (6,6) lines show <5σ emission and CO(1–0) show < 8σ emission are blank for p- and o-NH3, respectively. The gray dashed contours and the labeled clumpy substructures are the same as shown in Figure 1. These maps are derived by smoothing all lines to the same pixel size and angular resolution, i.e., 4.″90 × 3.″81, shown as the synthesized beam in the bottom left of each panel.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: The PDF of o/p-NH3 parameters toward B1a, derived by using RADEX and the MultiNest algorithm. A line width of 4 km s−1 is adopted for all lines, and the beam-filling factor is assumed to be unity for the (1,1)–(3,3) lines while to be 0.1 for the (4,4)–(7,7) lines. The fitting parameters, including the H2 volume density (n), o/p-NH3 column density N(o/p-NH3) and the gas kinetic temperature (T kin), are listed.
Paper: A Detailed Temperature Map of the Archetypal Protostellar Shocks in L1157
Authors: S. Feng, 思轶 冯, H. B. Liu, P. Caselli, A. Burkhardt, F. Du, R. Bachiller, C. Codella, C. Ceccarelli
Figure caption: Optical depth τ  m  maps of the (1,1)–(6,6) lines. The gray dashed contours and the labeled clumpy substructures are the same as shown in Figure 1. The integrated intensity of the line within the red solid contour shows >4σ emissions. The pixels where lines show <4σ emissions or uncertainty 1 dex higher than the value of τ  m  are blank.
Paper: Jansky Very Large Array Detections of CO(1–0) Emission in H I-absorption-selected Galaxies at z ≳ 2
Authors: B. Kaur, N. Kanekar, M. Rafelski, M. Neeleman, J. X. Prochaska, M. Revalski
Figure caption: The ratio of the CO(J → J − 1) line luminosity to the CO(1–0) line luminosity, plotted as a function of the upper-state rotational quantum number, J. The dashed black line indicates the value of unity for thermal excitation. The red symbols represent the H I-selected galaxies at z ∼ 2 (Kanekar et al. 2020; Klitsch et al. 2022, this work). For comparison, we have plotted the median value of the above ratios for main-sequence galaxies at z ≈ 1.5 (green crosses; Daddi et al. 2015), main-sequence galaxies at z > 2 (blue pentagons; Riechers et al. 2010; Brisbin et al. 2019; Boogaard et al. 2020; Henríquez-Brocal et al. 2021), and submillimeter galaxies at z > 2 (inverted black triangles; Sharon et al. 2016; Calistro Rivera et al. 2018; Birkin et al. 2021). The gray diamonds indicate the CO SLED of the inner disk of the Milky Way (Fixsen et al. 1999).
Paper: Jansky Very Large Array Detections of CO(1–0) Emission in H I-absorption-selected Galaxies at z ≳ 2
Authors: B. Kaur, N. Kanekar, M. Rafelski, M. Neeleman, J. X. Prochaska, M. Revalski
Figure caption: JVLA CO(1–0) integrated emission (red contours) overlaid on the ALMA CO(3–2) emission (white contours) and the HST WFC3 F105W image (in color) for (A) DLA B1228-113 at z = 2.1933 and (B) J0918+1636 at z = 2.5848, respectively. The left and right insets in each panel show, respectively, the JVLA (red) and ALMA (gray) synthesized beams. The CO(1–0) contours are at (−3.0, 3.0, 4.0, 5.0) × σ significance (note that there are no negative contours with ≥3σ significance), while the outermost CO(3–2) contour is at 6σ significance, with successive later contours increasing by factors of ﹩\sqrt{2}﹩.
Paper: Jansky Very Large Array Detections of CO(1–0) Emission in H I-absorption-selected Galaxies at z ≳ 2
Authors: B. Kaur, N. Kanekar, M. Rafelski, M. Neeleman, J. X. Prochaska, M. Revalski
Figure caption: JVLA CO(1–0) spectra from (A) DLA B0551-366 at z = 1.9615, (B) DLA B1228-113 at z = 2.1933, and (C) DLA J0918+1636 at z = 2.5848. The vertical gray bands indicate the edges of the digital subbands of the WIDAR correlator, which have significantly lower sensitivity. The blue dashed curves in each panel indicate the ±1σ error at each velocity channel.
Paper: The Origin of Weakened Magnetic Braking in Old Solar Analogs
Authors: Travis S. Metcalfe, Adam J. Finley, Oleg Kochukhov, Victor See, Thomas R. Ayres, Keivan G. Stassun, Jennifer L. van Saders, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Marc H. Pinsonneault, Klaus G. Strassmeier, Pascal Petit
Figure caption: Dependence of activity cycle period on rotation, showing two distinct sequences (solid lines). Points are colored by effective temperature, indicating F-type (blue triangles), G-type (yellow and orange circles), and K-type stars (red squares). Schematic evolutionary tracks are shown as dashed lines (Metcalfe & van Saders 2017 and references therein), leading to stars with constant activity that appear to have shut down their global dynamos (arrows along the top).
Paper: The Origin of Weakened Magnetic Braking in Old Solar Analogs
Authors: Travis S. Metcalfe, Adam J. Finley, Oleg Kochukhov, Victor See, Thomas R. Ayres, Keivan G. Stassun, Jennifer L. van Saders, Catherine A. Clark, Diego Godoy-Rivera, Ilya V. Ilyin, Marc H. Pinsonneault, Klaus G. Strassmeier, Pascal Petit
Figure caption: Stokes V circular polarization profiles for 18 Sco (left) and 16 Cyg A  and B (right) from LBT observations in 2021 May. Mean profiles are shown as black lines, while uncertainties are indicated with gray shaded areas. Colored lines show axisymmetric model profiles assuming dipole (blue), quadrupole (red), or octupole (magenta) geometry with fixed inclination.
Paper: Two Candidate KH 15D–like Systems from the Zwicky Transient Facility
Authors: Wei Zhu, 伟 祝, Klaus Bernhard, Fei Dai, 飞 戴, Min Fang, 敏 房, J. J. Zanazzi, Weicheng Zang, 伟呈 臧, Subo Dong, 苏勃 东, Franz-Josef Hambsch, Tianjun Gan, 天君 干, Zexuan Wu, 泽炫 吴, Michael Poon
Figure caption: Bernhard-1 light curves. The upper panel shows the available data from the ZTF survey and the archival Pan-STARRS (PS) data release 2. The out-of-occultation magnitudes have been subtracted to align the different bandpasses. The lower-left panel shows the period-folded and flux-normalized ZTF g and r light curves on top of the model light curve. The lower-right panel is the Pan-STARRS data folded by the same period. The shaded regions in the lower panels indicate the durations of ingress and egress. The best-fit model based on the ZTF data cannot match the Pan-STARRS data, suggesting the breakdown of the simplified model or the evolution of the occultation profile, potentially due to a precessing circumbinary disk.
Paper: Two Candidate KH 15D–like Systems from the Zwicky Transient Facility
Authors: Wei Zhu, 伟 祝, Klaus Bernhard, Fei Dai, 飞 戴, Min Fang, 敏 房, J. J. Zanazzi, Weicheng Zang, 伟呈 臧, Subo Dong, 苏勃 东, Franz-Josef Hambsch, Tianjun Gan, 天君 干, Zexuan Wu, 泽炫 吴, Michael Poon
Figure caption: SEDs of both Bernhard objects, suggesting the presence of a cold disk component. The measurements used here are from Pan-STARRS (g, r, i, z, y), 2MASS (J, H, K  s ), and WISE (W1–4). SED measurements are also available in Table 2 in terms of magnitude values.
Paper: Two Candidate KH 15D–like Systems from the Zwicky Transient Facility
Authors: Wei Zhu, 伟 祝, Klaus Bernhard, Fei Dai, 飞 戴, Min Fang, 敏 房, J. J. Zanazzi, Weicheng Zang, 伟呈 臧, Subo Dong, 苏勃 东, Franz-Josef Hambsch, Tianjun Gan, 天君 干, Zexuan Wu, 泽炫 吴, Michael Poon
Figure caption: LCOGT observations in g and i bands on the Bernhard-2 object. The light curves are folded in the same way as the ZTF data in the lower-left panel of Figure 3. The shaded region marks the egress according to the one-sided screen model. The LCOGT observations are available as data behind the figure.(The data used to create this figure are available.)