adsabs/AstroCLIMB huggingface dataset:
Paper: Spin Doctors: How to Diagnose a Hierarchical Merger Origin
Authors: Ethan Payne, Kyle Kremer, Michael Zevin
Figure caption: The complementary cumulative distribution function (1–CDF) of detectable 1G1G (shaded; purple) and hierarchical BBH mergers (lines) as a function of the logarithmic likelihood ratio, ﹩\mathrm{ln}\,\mathrm{LR}﹩, defined in Equation (3). The three different line styles correspond to different threshold choices (﹩{\chi }_{\mathrm{thres}}=0.2,0.3,0.4﹩), and shadings correspond to simulated signals detected in the first half of the LVK's third observing period (O3) sensitivity (dark), or a three-detector LIGO-Virgo network at design sensitivity (light). The top and bottom panels correspond to the complementary cumulative distribution functions for χ  p  and χ eff, respectively. Finally, the observed values of ﹩\mathrm{ln}\,\mathrm{LR}﹩ at the different thresholds for three gravitational-wave observations made during O3—GW190521 (purple), GW191109_010717 (pink), and GW200129_065458 (yellow)—are marked. A significantly larger fraction of the hierarchical population possesses a confidently measurable value of χ  p , whereas only the most relaxed threshold at design sensitivity can lead to a confident negative χ eff measurement in a single event.
Paper: Spin Doctors: How to Diagnose a Hierarchical Merger Origin
Authors: Ethan Payne, Kyle Kremer, Michael Zevin
Figure caption: Two-dimensional distribution of spin parameters, χ eff and χ  p , for detectable low-spinning first-generation BBHs (1G1G; purple), and hierarchically formed BBHs (yellow). The one-dimensional marginal cumulative distribution functions (CDFs) are shown in the top and right panels. The spins of the low-spinning population are drawn uniformly and isotropically with spin-magnitudes from 0 to 0.2 in postprocessing. All black hole masses are determined from the cluster simulations. We have selected for signals that are detectable by enforcing a signal-to-noise ratio threshold of 10 across the three detector LIGO-Virgo network at the LVK's sensitivity during their third observing period. The threshold of ﹩{\chi }_{\mathrm{thres}}=0.2﹩ used throughout the manuscript is indicated by the black lines for χ eff and χ  p . A significantly greater fraction of the hierarchical systems possess χ  p  >0.2 than χ eff < − 0.2.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: Color–magnitude distribution, (g − r) − M  r , of observed galaxies from the NSA (black) and simulated galaxies from CAMELS-TNG (blue). Overall, the distributions of NSA and CAMELS-TNG galaxies are in good agreement. The distribution for CAMELS-TNG is significantly broader because its galaxies are simulated using a wide range of cosmological and baryonic feedback parameters. We mark the 95th percentile contour of the NSA subsample of 22,338 galaxies analyzed in this work (orange dotted–dashed; Section 2) along with three arbitrarily selected galaxies from this sample (crosses).
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: Graphical representation of our hierarchical approach that illustrate the relationship among the parameters of our model. White circles are inferred random variables, and dark shaded circles are observed quantities. The physical properties of galaxies, ﹩{\theta }_{i}^{g}﹩, are determined from the cosmological and hydrodynamical parameters Ω and ﹩{ \mathcal B }﹩ through CAMELS-TNG. Then the noisy optical photometry, ﹩{\hat{X}}_{i}﹩, is derived from ﹩{\theta }_{i}^{g}﹩ using SPS and our noise model.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: SBC plot of ﹩{q}_{\phi }({\rm{\Omega }},{ \mathcal B }\,| \,{{\boldsymbol{X}}}_{i})﹩ using 10% of the CAMELS-TNG data reserved for testing. The histogram in each panel represents the distribution of the rank statistic of the true value within the marginalized posterior (solid blue) for each parameter. We plot the rank distributions for k = 5-folds of the test data to illustrate the uncertainties (light blue). The rank distribution is uniform for the true posterior (black dashed). The rank distribution of q  ϕ  is nearly uniform for all Ω and ﹩{ \mathcal B }﹩ parameters. Therefore, it provides unbiased and accurate estimate of the true posterior.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: The posterior of Ω m  and σ 8 inferred from the observed photometry of 22,338 NSA galaxies. The contours mark the 68th and 95th percentiles. We include the posterior from the Amon et al. (2022) DES Year 3 cosmic shear analysis for comparison (black dashed). We place significant cosmological constraints from the photometry of galaxies alone.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: The cosmological information, p(Ω ∣ θ  g ), of a star-forming galaxy with M * ∼ 109.5 M ⊙ and SFR = 10−0.3 M ⊙ yr−1 from TNG (blue) and from SIMBA (orange). The contours mark the 68th and 95th percentiles. Specific galaxy populations, such as intermediate-mass star-forming galaxies contain consistent cosmological information across different galaxy formation models.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: DRP coverage test validating the accuracy of our ﹩{q}_{\phi }({\rm{\Omega }},{ \mathcal B }\,| \,{{\boldsymbol{X}}}_{i})﹩ posterior estimate (solid blue). The DRP test is calculated using 10% of the CAMELS-TNG data reserved for testing. We plot the coverage tests for k = 5-folds of the test data to illustrate the uncertainties (light blue). The black dashed line represents an optimal estimate of the posterior. The DRP test demonstrates that q  ϕ  provides a near-optimal estimate of the true posterior.
Paper: Cosmology with Galaxy Photometry Alone
Authors: ChangHoon Hahn, Francisco Villaescusa-Navarro, Peter Melchior, Romain Teyssier
Figure caption: Estimated marginalized posteriors of the cosmological and hydrodynamical parameters (Ω, ﹩{ \mathcal B }﹩) from photometry, ﹩{q}_{\phi }({\rm{\Omega }},{ \mathcal B }\,| \,{{\boldsymbol{X}}}_{i})﹩, for three arbitrarily selected NSA galaxies. The posteriors correspond to the galaxies marked in Figure 1. The photometry of a single galaxy contains limited cosmological information.
Paper: Cascade Radiations of e ± from γγ-annihilation Process as an Extra Component of the Early Optical/X-Ray Afterglows of Gamma-Ray Bursts
Authors: Ren-Jie Xiong, Xiao-Li Huang, Ze-Rui Wang
Figure caption: Temporal evolution of the opacity of 0.1, 1, and 10 TeV gamma-ray photons within the afterglow jet (left panel), the broadband SEDs of afterglows at 100 s after the GRB trigger (middle panel), and the theoretical X-ray and optical lightcurves of the emission primary electron population and cascade emission of the e ± from the γ γ annihilation process (right panel). The model parameter values used are E k,iso = 1 × 1052 erg, n 0 = 1.0 cm−3, ϵ  e  = 0.01, ϵ  B  = 1.0 × 10−4, p = 2.4, Γ0 = 100, θ  j  = 5°, and z = 1. The line styles for different components are marked in each panels.
Paper: Cascade Radiations of e ± from γγ-annihilation Process as an Extra Component of the Early Optical/X-Ray Afterglows of Gamma-Ray Bursts
Authors: Ren-Jie Xiong, Xiao-Li Huang, Ze-Rui Wang
Figure caption: The observed optical/X-ray/TeV lightcurves (dots) of GRB 221009A and the theoretical fits (solid lines) with our model. The primary and cascade emission components are marked with dotted and dashed lines, respectively. The model parameter values used are E k,iso = 2.82 × 1055 erg, A * = 0.022, ϵ  e  = 0.2, ϵ  B  = 1.0 × 10−4, p = 2.4, Γ0 = 320, θ  j  = 0.°8, and z = 0.1505.
Paper: Cascade Radiations of e ± from γγ-annihilation Process as an Extra Component of the Early Optical/X-Ray Afterglows of Gamma-Ray Bursts
Authors: Ren-Jie Xiong, Xiao-Li Huang, Ze-Rui Wang
Figure caption: The observed optical/X-ray lightcurves (dots) of GRB 050801 (left panel) and GRB 080310 (right panel) and the theoretical fits (solid lines) with our model. The primary and cascade emission components are marked with dotted and dashed lines, respectively.
Paper: Cascade Radiations of e ± from γγ-annihilation Process as an Extra Component of the Early Optical/X-Ray Afterglows of Gamma-Ray Bursts
Authors: Ren-Jie Xiong, Xiao-Li Huang, Ze-Rui Wang
Figure caption: The same as Figure 1 but for adopting the parameter values as E k,iso = 1 × 1055 erg, n 0 = 1.0 cm−3, ϵ  e  = 0.1, ϵ  B  = 1.0 × 10−4, p = 2.4, Γ0 = 1000, θ  j  = 5°, and z = 1.
Paper: Cascade Radiations of e ± from γγ-annihilation Process as an Extra Component of the Early Optical/X-Ray Afterglows of Gamma-Ray Bursts
Authors: Ren-Jie Xiong, Xiao-Li Huang, Ze-Rui Wang
Figure caption: The same as Figure 1 but for n 0 = 100.0 cm−3 and ϵ  e  = 0.1.
Paper: Evidence for Plasmoid-mediated Magnetic Reconnection during a Small-scale Flare in the Partially Ionized Low Solar Atmosphere
Authors: Guanchong Cheng, Lei Ni, Zehao Tang, Yajie Chen, Yuhao Chen, Jialiang Hu, Jun Lin
Figure caption: Overview of the ROI. (a): tricolor image; the red, purple, and green components are AIA 304, 131, and 171 Å images, respectively. (b): the VIS Hα observation of the reconnection region; the field of view (FOV) is indicated by the box in (a). (c): the NLFFF extrapolation of the ROI; the FOV is the same with (a). (d): the zoom-in of (c). (f): the composite image; the yellow and gray components are two VIS Hα+0.8 Å images at two different time, while the red is the AIA 171 Å image. The FOV of (f) is indicated by the box in (b).
Paper: Evidence for Plasmoid-mediated Magnetic Reconnection during a Small-scale Flare in the Partially Ionized Low Solar Atmosphere
Authors: Guanchong Cheng, Lei Ni, Zehao Tang, Yajie Chen, Yuhao Chen, Jialiang Hu, Jun Lin
Figure caption: Time-series plot of DEM analysis, where color indicates the distribution of radiative intensity, the x-axis represents the timeline of the reconnection event, and the y-axis represents lg T. The white vertical line highlighted in the plot signifies the moment when the plasmoid-like structures collide with the PRL.
Paper: Evidence for Plasmoid-mediated Magnetic Reconnection during a Small-scale Flare in the Partially Ionized Low Solar Atmosphere
Authors: Guanchong Cheng, Lei Ni, Zehao Tang, Yajie Chen, Yuhao Chen, Jialiang Hu, Jun Lin
Figure caption: General view of simulation results at different moments. Columns (1), (2), (3), and (4) display the temperature, density, current density (J  z ), and v  y  distributions for three different times, respectively. The black solid lines in column (3) represent the magnetic field lines. The white arrows in column (4) represent the velocity fields.
Paper: Evidence for Plasmoid-mediated Magnetic Reconnection during a Small-scale Flare in the Partially Ionized Low Solar Atmosphere
Authors: Guanchong Cheng, Lei Ni, Zehao Tang, Yajie Chen, Yuhao Chen, Jialiang Hu, Jun Lin
Figure caption: The cartoon of the reconnection event. The bottom plane symbolizes the photospheric layer, with black and red blocks denoting regions of differing magnetic polarities. Magnetic field lines of corresponding polarities are illustrated by black and red lines, respectively. Black arrows indicate the heights of these regions. The light green plane represents the area covered by the 2.5D MHD simulation.
Paper: Mid-infrared Spectrum of the Disk around the Forming Companion GQ Lup B Revealed by JWST/MIRI
Authors: Gabriele Cugno, Polychronis Patapis, Andrea Banzatti, Michael Meyer, Felix A. Dannert, Tomas Stolker, Ryan J. MacDonald, Klaus M. Pontoppidan
Figure caption: Best fits for the different models considered in this work (left) and schematic representation of the models (right). In the left panels, orange data points represent MUSE and SINFONI data, red squares show VLT/NaCo photometries (Seifahrt et al. 2007; Stolker et al. 2021), and circles beyond 5 μm show the spectrum extracted from the MRS data (1A–2C). The gray line shows the atmospheric contribution from GQ Lup B, the dashed blue line shows the contribution from the disk, and the thick black line shows the overall SED model. Each panel reports the reduced ﹩{{\rm{\chi }}}_{\mathrm{MRS}}^{2}﹩. Panel (a): best-fit model when no disk emission is considered. For the fit, we only used data points shortward of 5 μm, as including the MRS spectra resulted in an unphysical result. Atmospheric emission is not able to account for the strong radiation at λ > 5 μm. Panels (b)–(e): best-fit results for the models that take into account disk emission (model reported on the top right of each panel). In the right panels, the considered scenarios are illustrated. The size of the cavity is reported in each panel, even though the illustration is not to scale. For comparison, the Galilean moons around Jupiter have semimajor axes between 5.9 and 26.3 R J. Brown dwarf artist impression credit: NASA.
Paper: Mid-infrared Spectrum of the Disk around the Forming Companion GQ Lup B Revealed by JWST/MIRI
Authors: Gabriele Cugno, Polychronis Patapis, Andrea Banzatti, Michael Meyer, Felix A. Dannert, Tomas Stolker, Ryan J. MacDonald, Klaus M. Pontoppidan
Figure caption: Wavelength-combined images before (first column; only channels 1A and 2A shown) and after (second to fourth columns; channels between 1A and 2C) PSF subtraction. The band is reported on the top left corner of each panel. The corresponding wavelength range is shown on the bottom left corner of each panel, while the S/N of the detection is indicated on the top right corner. The color scale is the same in every image, and the spatial axes follow the MRS integral field unit internal coordinates. A scale is provided for channels 1 and 2 in the panels of the second column, while arrows pointing north and east in the sky coordinate are reported on panels in the third column. The central dashed circle represents the FWHM of the stellar PSF. With increasing wavelength, the size of the PSF increases and the companion separation falls to ∼1.5 λ/D.
Paper: Mid-infrared Spectrum of the Disk around the Forming Companion GQ Lup B Revealed by JWST/MIRI
Authors: Gabriele Cugno, Polychronis Patapis, Andrea Banzatti, Michael Meyer, Felix A. Dannert, Tomas Stolker, Ryan J. MacDonald, Klaus M. Pontoppidan
Figure caption: Detection limits of the MRS for bands 1A–2C. Thin gray lines show the limits for each individual MRS wavelength, while thick black lines indicate the median across the channel. For each channel, we report the atmospheric flux of GQ Lup B inferred from the NIR spectra as a white star and the measured flux (atmosphere+CPD) from our MRS observations as a red star. Without the contribution from the CPD, GQ Lup B would have been detected at only some wavelengths in channels 1A and 1B. In addition, we report MIR fluxes for other known young companions for reference.
Paper: Mid-infrared Spectrum of the Disk around the Forming Companion GQ Lup B Revealed by JWST/MIRI
Authors: Gabriele Cugno, Polychronis Patapis, Andrea Banzatti, Michael Meyer, Felix A. Dannert, Tomas Stolker, Ryan J. MacDonald, Klaus M. Pontoppidan
Figure caption: Comparison of the best-fit models of the SED of GQ Lup B. Red squares show VLT/NaCo photometries (Stolker et al. 2021), while circles beyond 5 μm show the spectrum extracted from the MRS data (1A–2C). In black and violet, the best-fit models for flat and vertically extended disks, respectively, are shown with different line styles. λ = 2–4 μm and λ > 12 μm observations can break the degeneracy and indicate the best-suited set of models to describe the observations. The MRS spectra are available as the data behind this figure.(The data used to create this figure are available.)
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Tidal disruption radius R  T  (scaled by the BH gravitational radius R  g ) of Pop III stars and a solar-type star as a function of BH mass M BH. The red and blue solid or dashed lines represent Pop III stars of mass 300M ⊙ (M 300) and 30M ⊙ (M 30), respectively, with metallicity Z = 10−5 (Z −5) or 10−9 (Z −9). The black solid line shows a solar-type star for comparison. It can be seen that a Pop III star, depending on its metallicity, has a R  T  similar to or a few times larger than that of the Sun. The green dotted line indicates R  T  = R  g , which gives the maximum mass of M BH for a star to be disrupted inside the MBH event horizon.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Left panel: debris mass fallback time t fb for tidal disruption of 300M ⊙ (M 300, red) and 30M ⊙ (M 30, blue) Pop III stars with Z = 10−5 (Z −5, solid lines) and Z = 10−9 (Z −9, dashed lines) compared to a regular 1M ⊙ star (black solid line). Right panel: Eddington ratio of the peak debris mass fallback rate ﹩{\dot{M}}_{\mathrm{fb},\mathrm{peak}}﹩ for the same stars as in the left panel. Pop III stars have shorter fallback times and much higher peak mass fallback rates compared to Pop I star TDEs.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Average density (ρ ⋆) of Pop III stars with Z = 10−5 (red solid line) and Z = 10−9 (red dashed line) in the mass range of 30–300M ⊙ compared to Pop I stars (black solid line) in the mass range of 0.1–300M ⊙. All stars are in their main-sequence stages. Pop III stars typically have ρ ⋆ ∼ 0.01–1 ρ ⊙ and those with lower metallicities or lower masses are denser. The stellar density of 1ρ ⊙, 0.1ρ ⊙, and 0.01ρ ⊙ are marked with green dotted lines.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: A wide-field DECaLS grz image showing the galaxies in the vicinity of BC6 and the H I complex. Contours showing H I emission from ALFALFA are overlaid (same contour levels as Figure 3). Each source identified by SoFiA is plotted separately, and the color of the contours corresponds to the flux-weighted mean velocity of each the source. Velocities for undetected sources are included as numerical values (from Cappellari et al. 2011; Albareti et al. 2017). We note that although NGC 4445 is weakly detected by ALFALFA (Haynes et al. 2018), it was not recovered in our automated extraction with SoFiA, as it has lost most of its H I.
Paper: Dark No More: The Low-luminosity Stellar Counterpart of a Dark Cloud in the Virgo Cluster 
Authors: Michael G. Jones, Steven Janowiecki, Swapnaneel Dey, David J. Sand, Paul Bennet, Denija Crnojević, Catherine E. Fielder, Ananthan Karunakaran, Brian R. Kent, Nicolas Mazziotti, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: NGVS ugi image of an additional blue blob candidate cospatial with H I cloud C4 (Figure 3) identified in our citizen science search. However, this candidate appears to be background galaxies.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: Schematic diagram of Pop III TDEs. In a galaxy at z ≳ 10, a Pop III star is scattered by other stars and gets tidally disrupted by the MBH. A large fraction of the fallback debris material is converted to a powerful wind with outflowing mass rate ﹩{\dot{M}}_{\mathrm{out}}={f}_{\mathrm{out}}{\dot{M}}_{\mathrm{fb}}﹩, which produces a luminous optical/UV flare. At z = 0, the flare emissions are redshifted to the NIR wavelength and can be detected by JWST and Roman.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The differential Pop III star TDE volumetric rates as a function of M BH for the three different BHMFs in Figure 12. One can see that the BHMF through the merger-driven growth channel overall produces the highest TDE volumetric rate.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The fallback time t fb and peak debris mass fallback rate ﹩{\dot{M}}_{\mathrm{fb},\mathrm{peak}}﹩ as functions of the MBH mass using both the GR13 model and the B24 model. The solid and dashed lines are the same as Figure 3 (based on the GR13 model). The cyan dotted line in the left panel represents the fallback time using the B24 model. The black, blue, and red dotted lines in the right panel correspond to ﹩{\dot{M}}_{\mathrm{fb},\mathrm{peak}}﹩ in the TDEs of a solar-type Pop I star, a 30M ⊙ Pop III star, and a 300M ⊙ Pop III star, respectively, using the B24 model.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The fallback time t fb and peak debris mass fallback rate ﹩{\dot{M}}_{\mathrm{fb},\mathrm{peak}}﹩ as functions of stellar mass using both the GR13 model and the B24 model. The magenta solid and dashed lines represent the TDEs of Pop III stars with Z = 10−5 and Z = 10−9, respectively. The solid black line represents the TDE of Pop I stars. All of the lines mentioned above adopt the GR13 model. The cyan solid line represents the results from B24 for Pop I stars (in the stellar mass range of 0.2–5M ⊙). The yellow shaded regions denote the estimated uncertainties of the B24 model.
Paper: Detecting Population III Stars through Tidal Disruption Events in the Era of JWST and Roman
Authors: Rudrani Kar Chowdhury, Janet N. Y. Chang, Lixin Dai, Priyamvada Natarajan
Figure caption: The observed flux of a Pop III TDE (M ⋆ = 300M ⊙,  Z = 10−5,  M BH = 106 M ⊙) at z = 10 using the ZEBRA model.
Paper: High-resolution Spectroscopic Reconnaissance of a Temperate Sub-Neptune
Authors: Samuel H. C. Cabot, Nikku Madhusudhan, Savvas Constantinou, Diana Valencia, Johanna M. Vos, Thomas Masseron, Connor J. Cheverall
Figure caption: Top: molecular inferences from cross-correlating the detrended spectra with our model templates. Results are shown for three species (CH4, NH3, and H2O). Bright regions in these maps correspond to peaks in the CCF. For species in the atmosphere of the exoplanet, a positive signal is expected at the true orbital parameters, i.e., K  p  ≈ 68 and V sys ≈ 0 km s−1 (Nowak et al. 2020; Bonfanti et al. 2024; indicated by the black plus sign). The standard deviation across other velocity combinations serves as a proxy for noise when deriving the S/N of the signal. Note that each panel spans the same S/N color range (−3 to +4). The grayscale arrays at the top of each panel depict the CCFs for each exposure. These CCFs are Doppler shifted by the planet’s velocity under an assumed (K  p , V sys) pair and subsequently stacked, which produces the color-scale S/N maps. Middle: same as the top row, except an artificial transmission spectrum was multiplied into the spectra at the start of data analysis. The injection assumes an orbit specified by K  p  = 68 and V sys = 80 km s−1, as indicated by the dotted white boxes in each panel. Bottom: same as the middle row, except the injection is specified by K  p  = − 68 and V sys = 0 km s−1 so as to more closely mimic the statistical properties of the observed signal.