adsabs/AstroCLIMB huggingface dataset:
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Left: similar to Figure 2, [O III]-to-UV ratio ﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩ versus transverse distance Δr for galaxies near the quasar redshift (z ≈ 6.3, red), in the foreground (z ≈ 6.2, green), and in the background overdensity (z ≈ 6.8, orange). Only data points with >50% completeness are shown here. Solid, dotted, and dashed curves show completeness-matched median fits for the three slices, with shaded bands indicating the 16%–84% ranges. Binned averages (five galaxies per bin) with bootstrap uncertainties are overplotted. Right: cumulative distributions (CDFs) of ﹩{\mathrm{log}}_{10}({L}_{5008}/{L}_{1500})﹩ for galaxies within Δr < 7 cMpc of the quasar, comparing z ≈ 6.3 (red), z ≈ 6.2 (green), and z ≈ 6.8 (orange). The background sample shows higher ratios than the z ≈ 6.3 sample (K–S p = 0.017), while the foreground is more similar (p = 0.167), consistent with the visual impression from the left panel.
Paper: Quasar Radiative Feedback May Suppress Galaxy Growth on Intergalactic Scales at z = 6.3
Authors: Yongda Zhu, Eiichi Egami, Xiaohui Fan, Fengwu Sun, George D. Becker, Christopher Cain, Huanqing Chen, Anna-Christina Eilers, Yoshinobu Fudamoto, Jakob M. Helton, Xiangyu Jin, Maria Pudoka, Andrew J. Bunker, Zheng Cai, Jaclyn B. Champagne, Zhiyuan Ji, Xiaojing Lin, Weizhe Liu, 刘伟哲, Hai-Xia Ma, Zheng Ma, Roberto Maiolino, George H. Rieke, Marcia J. Rieke, Pierluigi Rinaldi, Yang Sun, Wei Leong Tee, Feige Wang, Jinyi Yang, Minghao Yue, Junyu Zhang
Figure caption: Sky map of the J0100+2802 field, combining NIRCam F356W mosaics from SAPPHIRES (top) and EIGER (bottom). Galaxies at z ≈ 6.3 (near the quasar redshift; red circles), z ≈ 6.2 (foreground; green hexagon), and z ≈ 6.8 (background overdensity; orange squares) are shown with symbol sizes scaled by their observed [O III] λ5008 luminosities. The black cross marks the quasar position. We also show other galaxies with transverse distance from the quasar Δr < 7 cMpc on the sky map just for reference. The inset shows the projected distribution along the line of sight, with transverse separation Δr plotted against line-of-sight distance Δd from the quasar.
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, shown in 2 keV segments. The model in red is the best-fit model detailed in Table 1. Solid vertical lines mark the lab energies of the observed He-like and H-like lines, as well as neutral Fe. The redshift of the bulk of the emitting gas relative to lab wavelengths is evident, especially in the strongest Fe XXV and Fe XXV lines. RRC features are marked with triangles.
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 the band containing He-like and H-like lines from Cr, Mn, Fe, and Ni. The model in red is the best-fit model detailed in Table 1. Solid vertical lines mark the lab energies of the observed He-like (top row) and H-like transitions (bottom row). RRC features are marked with triangles.
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 the vicinity of the strongest emission-line complexes (He-like Fe XXV, centered at 6.7 keV, and H-like Fe XXVI centered at 6.97 keV). The total best-fit model is shown in red, with individual photoionized components shown in blue (pion1), cyan (pion2), and orange (pion3). In these and other lines from adjacent charge states, it is clear that multiple components are needed to describe He-like and H-like line fluxes and detailed line shapes. It is evident that the lines are redshifted with respect to their laboratory energy values, marked in gray at the top of the frame. Note that the component colors adopted in this plot are not connected to the elemental color scheme in other plots.
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 the band containing Fe XXV and Fe XXVI RRC features (marked with triangles). The best-fit model in other figures is now shown in blue. The Fe XXVI RRC is clearly not smooth, as expected if recombining electrons are thermally distributed; instead, oscillatory structure with a spacing of 30 eV is evident. This structure is nominally consistent with recombination from Landau levels in a highly magnetized corona (B = 2.5 × 109 G; this model is shown in red). Alternatively, the lines could arise in a v = 0.34c flow wind, wherein iron retains intermediate charge states. Both explanations are unsatisfactory.
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: The top panel displays the Q-transform visualization of the GW231123 event and scattered-light glitches observed at the Livingston Observatory. The middle panel displays the scattered-light glitches propagating in an Alignment Sensing and Control auxiliary channel. The bottom panel is the ARCHGEM output highlighting the software’s capability to recognize scattered-light morphologies and extract them for further analysis using a dual methodology ML approach.
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: Top: reconstructions of (a) Livingston and (b) Hanford data of GW231123 using AWARE. The red dashed curves show the AWARE mean reconstructions. The red bands show the associated reconstruction uncertainties. Reconstructions from cWB, Bilby, and BayesWave are shown in green, blue, and purple, respectively. The whitened noisy strains are shown in gray. Bottom: residuals obtained by subtracting the AWARE mean reconstructions from the whitened strains.
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: Predicted class label probabilities from 8 s around GW231123 using GW-WHISPER in Livingston (left) and Hanford (right). The top row shows the whitened strains from the respective detectors with the segment containing the event highlighted green. The bottom row contains the probabilities for each label in each segment. The model predicts “No Glitch” for all segments around the event and “GW” in the segment that contains the event.
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: A diagram of a warped disk geometry that might lead to the spectrum observed from GRS 1915+105 with Resolve. Position 1 sees the central engine, only obscured by disk winds. At Position 2, the central engine is blocked by the warp in the outer disk, but emission from the inner face of the warp is visible. At Position 3, the central engine and irradiated face of the disk are both blocked. Note that the warp period is much slower than the orbital period of the system; it is not locked in orbital phase.
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: (a) Observed ion column density ratios, NSiIV/NCIV (black hatched) and NOV I/NCIV (blue hatched), and comparison with ionization models. We present ion ratio predictions from photoionization (gray), collisional ionization equilibrium (CIE; black), radiative cooling (olive and brown), and TRML models (black plus signs). (b) The expected C IV fraction from collisional ionization models (O. Gnat & A. Sternberg 2007), CIE (black), and time-dependent radiative cooling at constant pressure (isobaric; olive) and at constant volume (isochoric; brown). We present subsolar metallicity (0.1 Z⊙) for radiative cooling models. The shaded temperature ranges are derived from observed ion column density ratios, NSiIV/NCIV (black) and NOV I/NCIV (blue), respectively.
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 ion column density ratios of Si IV and C IV along the MS. (Left) QSO sight lines with detected C IV absorption, shown in MS coordinates and color coded by the Si IV/C IV column density ratio. Filled circles represent measurements from this work, and open circles are from A. J. Fox et al. (2014). Triangles denote sight lines where only upper limits on Si IV are available. (Right) Si IV/C IV column density ratios, along with MS latitude (BMS).
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: Radial number density profile of galaxies measured by stacking the 18 quasar fields, normalized at r/rprox = 3.0. The color shaded region shows the 1σ error calculated by the bootstrap resampling method. The dashed line and gray shaded region show the median proximity radius and its 1σ error of the present quasar sample. Left: comparison of LAEs (blue) and continuum-selected galaxies (red). Middle: comparison of the continuum-selected galaxies, high-EW LAEs (light blue) and low-EW LAEs (orange). Right: comparison of the LAEs, bright continuum-selected galaxies (green), and faint continuum-selected galaxies (purple).
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: Radial number density profile measured by stacking the 18 quasar fields and continuum-selected galaxy fields, normalized at 20′. The halo masses of the central continuum-selected galaxies are comparable to that of quasars. The shaded region shows the 1σ uncertainties calculated by the bootstrap resampling method. (Top) Comparison of the density of continuum-selected galaxies around the control continuum-selected galaxies (magenta circles) and around quasars (red stars). (Bottom) Comparison of the density of LAE around the control continuum-selected galaxies (cyan circles) and around quasars (blue stars).
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 EW0 of LAEs measured by stacking the 18 quasar fields. The blue/red circles 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: Distribution of LAEs and continuum-selected galaxies with all quasar fields rescaled and stacked. The central cross shows the quasar. The circle shows the median proximity region size. The blue/orange dots show the distribution of LAEs/continuum-selected galaxies.
Paper: Shadow-induced Warps in Protoplanetary Disks
Authors: Shangjia Zhang, Zhaohuan Zhu, Callum W. Fairbairn
Figure caption: Various quantities on the rotated surfaces for the full-disk pure hydrodynamical simulations with a 20% temperature perturbation. Top: i = 30° (HF30R). Bottom: i = 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 (HF7R). The layout is similar to Figure 5. The arrows indicate the azimuthal locations of the local maxima in the velocity perturbations (﹩{v}_{r}^{{\prime} }﹩ and ﹩{v}_{\theta }^{{\prime} }﹩), highlighting the dominant Fourier mode (m = 1, 2, and 3) at each layer. Similar to Figure 5, some of the grid-like patterns arise from the nearest-neighbor interpolation used in the coordinate transformation.
Paper: Dynamical Simulation of the Interstellar Comet 3I/ATLAS
Authors: Goldy Ahuja, Shashikiran Ganesh
Figure caption: Left: close encounters between interstellar comet 3I/ATLAS and Mars at epoch JD 2460951.5 (2025 October 3). Right: close encounters between interstellar comet 3I/ATLAS and Jupiter at epoch JD 2461115.5 (2026 March 16). For clarity, we show only the planets’ orbits (up to Jupiter), whereas in the simulation, we have also considered the three other planets (Saturn, Uranus, Neptune), the four big asteroids (Ceres, Pallas, Juno, Vesta) in the asteroid belt, and five KBOs (Pluto, Makemake, Haumea, Quaoar, Sedna).
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Top: 0.5–8 keV X-ray surface brightness map and temperature map from Chandra. In the surface brightness map, XRISM pixels are overlaid in transparent white. Weak-lensing contours (S. Mandal et al. 2019) are overlaid on the surface brightness (temperature) map in white (black). Regions from which ICM temperatures are measured are shown as white boxes on the temperature map, with their respective temperatures labeled. We also plot the locations of the BCGs as a black star/pentagon. Bottom: simulated X-ray surface brightness and emissivity-weighted temperature map, projected along the line of sight. DM density contours are plotted in black.
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Top: 5.6–6.2 keV Resolve spectrum of A1914 from the full FOV (gray crosses), showing Fe Heα and Lyα lines. The spectrum is binned such that each energy bin is detected at 4σ significance. The best-fit one-component model is shown as a dashed black line. The best-fit two-component model is shown in solid black, with individual ICM components shown in blue and red. Residuals from the two-component model, calculated as (data model)/error, are plotted below the spectrum. Inset: 2–8 keV Chandra image of A1914, with the Resolve FOV (a simplified ﹩{3}^{{\prime} }\times {3}^{{\prime} }﹩ square) overlaid in white. Bottom: best-fit bulk velocity separation between the red and blue ICM components, plotted as color against the velocity dispersions of the two components. The 1/2/3 σ constraints on σred and σblue are plotted as solid white contours. Global/local minima are labeled with a star/triangle marker, respectively.
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Top: spatially resolved maps of the red/blue flux ratio (left), bulk velocity (center), and velocity dispersion (right), derived from the nine-region (left) and north–south–central binnings (center and right). Contours from the Chandra image of A1914 are shown in gray. Bottom: simulated maps of X-ray fluxes from the red and blue subclusters (left) and emissivity-weighted bulk velocity/velocity dispersion (center/right). Surface brightness contours are shown in black. Merger shocks are denoted in white in the center and right panels.
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Left: map of X-ray emission from the simulated red and blue subclusters, viewed perpendicular to the merger plane. Center: simulated X-ray-weighted temperature map in the same projection. Here we additionally plot black contours showing the DM mass distribution and red/blue arrows showing the trajectory of the corresponding subclusters during the merger. The white arrow indicates the projected line of sight presented in Figure 3. The line of sight is inclined to the x–y-plane by ≃70°. Right: redshift distribution of cluster member galaxies from R. Barrena et al. (2013), between z = 0.16 and 0.18. Red and blue ICM redshifts from XRISM are shown as colored vertical lines. BCG redshifts are shown as dotted black lines.
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Binned spectra used to map the bulk velocity and velocity dispersion in Figure 2. The total model is plotted as a dashed black line. ICM emissions from each of the three sky regions (north, center, and south) are plotted in colored lines (red, green, and blue). Spectra are binned such that each energy bin is detected at >3σ significance.
Paper: A Yin-yang Galaxy Cluster Merger in A1914 Revealed by XRISM
Authors: Annie Heinrich, Congyao Zhang, Irina Zhuravleva, Eugene Churazov, Hannah McCall, Reinout J. van Weeren, William R. Forman
Figure caption: Predicted distributions of the tSZ (left) and kSZ (right) effects at 150 GHz in the line-of-sight projection equivalent to Figure 2. Both maps have been smoothed with a 8″ Gaussian. Black contours show DM matter distribution.
Paper: The Rotation Dip in the Envelope–Disk Transition of HH 111: Evidence for Magnetic Braking
Authors: Jyun-Heng Lin, Chin-Fei Lee, Zhi-Yun Li, Yueh-Ning Lee, Ya-Lin Wu, J. A. López-Vázquez
Figure caption: In each row, from left to right, the panels display the model velocity profiles, the model–observation comparison, and the residual map, respectively. In the velocity setup (a), (d), and (g), the red line represents the specific angular momentum ℓ, with its values shown on the right-hand y-axis. The blue and green lines indicate the rotation velocity vϕ and infall velocity vr, respectively. Two vertical black dashed lines divide the diagram into three parts: from the outer to the inner regions, they represent the envelope, the transition region, and the Keplerian disk. In the PV diagrams (b), (e), and (h), the color scale shows the observational data and the red contours the model, while in the residual maps (c), (f), and (i), the color scale and white contours show the observation-model residuals. The red and white contours start at 4σ and increase in steps of 10σ (σ = 4.8 × 10−3 Jy beam−1). An apparent asymmetry between the redshifted and blueshifted sides in the model is present, which is primarily due to self-absorption (see Section 3.2).
Paper: Projections of Earth’s Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Authors: Jacob Haqq-Misra, Ravi K. Kopparapu, George Profitiliotis
Figure caption: Albedo spectra of different scenarios from Table 1 compared to the present-day-Earth scenario (R1). Distinct absorption features from industrial activity—such as NO2, in the short-wavelength region, and CO2, in the near-infrared—are noticeable. Scenarios S5, S9, and S10 are omitted because they are spectrally identical to preagricultural Earth (R0; see Figure 1).
Paper: Projections of Earth’s Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Authors: Jacob Haqq-Misra, Ravi K. Kopparapu, George Profitiliotis
Figure caption: Total integration time required for the Square Kilometre Array to observe a radio beacon from scenarios S1 or S5 at a distance of 10 pc (following Equation (2)). The results are shown using a 10 Hz bandwidth analogous to the Arecibo message and a 0.01 Hz bandwidth comparable to radar science (see S. Z. Sheikh et al. 2025). The dashed lines show the comparable EIRPmin values for the Deep Space Network and Voyager spacecraft. The maximum transmission at 1011 W would correspond to ∼0.1% of the scenario civilization’s total power use, which could be detectable with 50 ms of observation time at 10 Hz. Lower-power transmissions, comparable to the Deep Space Network, would need 8.5 minutes, while transmitters comparable to Voyager would require over a year of integration time.
Paper: The Rotation Dip in the Envelope–Disk Transition of HH 111: Evidence for Magnetic Braking
Authors: Jyun-Heng Lin, Chin-Fei Lee, Zhi-Yun Li, Yueh-Ning Lee, Ya-Lin Wu, J. A. López-Vázquez
Figure caption: The left panel shows the flux-weighted velocity map (moment 1) of C18O (J = 2–1) in HH 111, integrated over the velocity range from 7 to 12 km s−1. The contours represent the total intensity map (moment 0), starting at 2σ and increasing in steps of 3σ (σ = 28 mJy beam−1 km s−1) up to 25σ. The magenta line indicates the PV cut, taken along the disk major axis at a P.A. of ∼6﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7, as determined from the observed disk orientation. The middle panel illustrates the structural distribution of an edge-on protostellar system, and the right panel shows a schematic of the simplified flattened envelope model; a detailed description is given in Section 3.3.
Paper: Projections of Earth’s Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Authors: Jacob Haqq-Misra, Ravi K. Kopparapu, George Profitiliotis
Figure caption: Mid-infrared spectra as observed by LIFE of preagricultural Earth (R0) and present-day Earth (R1) (left), scenarios S1, S2, and S3 (middle), and scenarios S4, S6, S7, and S8 (right). Scenarios S5, S9, and S10 are spectrally identical to R0. The calculations assume a 10 days integration period and a 10 pc distance to the planet. Some distinguishing features can be seen that result from differences in industry (CO2, NO2, CFC-11, and CFC-12) and large-scale agriculture (N2O, NH3, and CH4).
Paper: Projections of Earth’s Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Authors: Jacob Haqq-Misra, Ravi K. Kopparapu, George Profitiliotis
Figure caption: Summary of technosignature detectability with future missions for each scenario. The darker colors indicate where multiple technosignatures in a scenario are observable by a mission.