adsabs/AstroCLIMB huggingface dataset:
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption:  ﹩\overline{E(B-V)}﹩ values in bins of voff. Error bars are the standard error of the mean in each bin. Note that at voff  <  5000 km s−1 we have drawn samples every 200 km s−1, whereas at voff  >  5000 km s−1 they are drawn every 500 km s−1. Black lines are overlaid at voff = 0 km s−1 and voff = 3500 km s−1.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: Histogram of fit color excess values for all 50,674 spectra in both our sample of absorbed QSOs and our control sample of QSOs with no detected Mg II absorbers. Bins are 0.01 mag of extinction wide.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: Histogram of absorber redshift values for the 50,674 absorption-line systems in our sample. Bins are 0.1 redshift wide.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Effect of star-spot water vapor on CC detections of exoplanetary water. Three CC functions are shown, for no spots, and 2% and 5% spot filling fractions. The CC functions are displaced in velocity (and also in the Y-axis) to illustrate them without overlap, and the star-spot velocity is set at –70 km s–1 relative to the planet, so that their CC peaks do not overlap. (In the case of most real M-dwarf stars, the CC peaks from the planet and star spot would be closely coincident). Triangles mark the signal from water in the exoplanet, and the magenta lines mark the signal from water in the star spot. This is for the M6V case, with star spots 600 K cooler than the photosphere.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Simulated CC detections of methane in a temperate planet orbiting an M4V star 12 pc from Earth, using the 39 m E-ELT. The upper panel shows the CC functions with observational photon noise turned off, and varying coverage of unocculted spots having ΔT = −400 K. The CC functions are displaced in velocity for clarity (avoiding overlap), and the triangles mark their centers. In the absence of star spots and photon noise (blue curve), the S/N for the methane detection (=145) is limited by overlap with other molecules in the exoplanetary atmosphere. When limited by unocculted star spots, the S/N is 36 and 18 for 10% and 20% spot coverage, respectively. The lower panel adds photon noise to the unspotted case, using the E-ELT (978 m2 collecting area with 10% efficiency), and 100 transits. The S/N for that detection is 12.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Effect of alternate normalization to reduce the noise and contamination from star spots in a CC detection of water vapor for an M6V host star. In this example, photon noise has been turned off, and the noise in the CC is due to the star. The 6.7% average degree of spottedness produces a large amount of noise that prevents detection of the dip in the CC due to the planet, and the spots also produce their own dip, that we moved to –50 km s–1 (marked by magenta line) to avoid confusion with the exoplanet dip. The result from alternate normalization shows a factor of 6 reduction in noise, and contamination of the exoplanetary signal is less by a factor of 9 (at 3σ significance).
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Ratio of noise from unocculted star spots to the photon noise when averaged over 100 transits. These are for detection of carbon dioxide in a temperate planet transiting M3V, M6V, and M8V stars using the E-ELT, as a function of the filling fraction of the spots. The different curves are for different temperature differences between the photosphere and star spots.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: V – K photometric color (in magnitudes) of an M6V star vs. the filling fraction of star spots, adopting that the spots are all 600 K cooler than the quiet photosphere, and varying their filling fraction randomly from 0.0 to 0.15.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Simulated CC detections of molecular oxygen in a temperate rocky planet orbiting an M4V star, 12 pc from Earth, using the 39 m E-ELT. This is the same as Figure 6, but for the case of molecular oxygen. In the absence of unocculted star spots (blue curve) and with photon noise turned off, the S/N for the detection is 43, limited by overlap between the template and other molecules present in the exoplanetary atmosphere. With 10% unocculted spot area, the S/N is 9, and when considering only photon noise for 200 transits (lower panel) the S/N for the detection is 4.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: The same calculations as in Figure 8, but for the case of water vapor.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: The same calculations as in Figure 8, but for the case of molecular oxygen.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: The same calculations as in Figure 8, but for the case of methane.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: The ratio between Cp and ﹩{C}_{{\rm{\max }}}﹩ for all stars, as a function of planetary orbital radius. The error bars represent the lower limit of prediction, derived from predicted contrasts with errors. Blue points indicate targets observed by both missions, while red points refer to those exclusive to HWO.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Stellar properties of HWO targets from C. K. Harada et al. (2024) and astrometric and imaging signals contours. The orange, red, blue circle, and black points represent stars with known planets, binary stars, single stars, and common targets of CHES, respectively. Left panel: stellar luminosity vs. distance of all targets. The olive solid, green dashed, and red dashed–dotted lines represent α = 1.0, 0.3, and 0.1 μas, respectively, in the scenario of a planet with 1 M🜨 located at the the center of the habitable zone; the logarithmic relation between stellar mass and luminosity is adopted for drawing the curves (Z. Eker et al. 2015). Right panel: effective temperature vs. luminosity, and the horizontal lines corresponds to different imaging contrasts.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Left panel: histogram of expected number of detected planets vs. planetary semimajor axis based on the low frequency and optimistic habitable zone model. The orange crosshatched and blue bars represent the expected yields by direct imaging alone and imaging + astrometry, respectively. Right panel: planet yields from synergistic observations of terrestrial planets in the conservative habitable zone as a function of stellar effective temperature. The blue, orange, green, and red points represent F, G, K, and M stars, respectively. The size of each point indicates the position of the habitable zone for the corresponding star.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Contrast fluctuation vs. with orbital eccentricity and inclination. The eccentricity range is 0–0.8, and the inclination range is 0°–90°. The color bar presents logarithmic fluctuations between maximum and minimum contrast.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Left panel: the overall completeness of every target. The bottom-left subpanel shows a comparison of completeness by direct imaging alone (x-axis) and imaging + astrometry (y-axis). The top-left and bottom-right subpanels give histogram of completeness in the two scenarios. Right panel: a comparison of the benefit-to-cost ratio by imaging alone and imaging with astrometry. The orange points and blue crosses indicate targets of HWO only and common targets, respectively. The sizes of the points represent the distance of the center of the habitable zone.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Detection map for HD 100623 A in two observational scenarios. Left panel: results based solely on the direct imaging method are derived from five observations, each with a single exposure time of 4 hr. Right panel: results for the synergy between direct imaging and astrometry. Contour lines in different colors represent detection efficiencies ranging from 20% to 95%, calculated based on the S/N criterion.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Instrumental performance curves used in our simulations. The red solid, blue dashed, and green dashed–dotted lines represent core contrast, core throughput, and coronagraphic transmission, respectively. The black lines shows the base contrast value 4 × 10−11 of HWO.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Simulated motion and contrast of τ Cet e for 200 days. The solid, dashed, and dashed–dotted lines represent planet’s position for I = 0°, 60°, and 90°, respectively. The color bar indicates logarithmic contrast, while the blue region marks the area within the IWA, where detection is not possible.
Paper: Closeby Habitable Exoplanet Survey (CHES). IV. Synergy between Astrometry and Direct Imaging Missions of the Habitable World Observatory for Detecting Earth-like Planets
Authors: Chunhui Bao, Jianghui Ji, Dongjie Tan, Guo Chen, Xiumin Huang, Su Wang, Yao Dong
Figure caption: Planet occurrence rate vs. corresponding host star effective temperature. The blue, orange, and green regions represent the occurrence rates of planets in the optimistic habitable zone, conservative habitable zone, and Earth-like planets, respectively. The data are based on the planet occurrence model of S. Bryson et al. (2021).
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and ∣v0∣/Δv for simulated mutual approximations of set B. The condition of set B is shown in Table 5. The Pearson coefficient is 0.82 with the p-value of 0.
Paper: Observation and Simulation of Mutual Approximations between Five Main Uranian Satellites
Authors: Jian Chen, 健 陈, Hao-Ran Song, 浩冉 宋, Ye Yuan, 烨 袁, Fan Li, 凡 李, Yan-Ning Fu, 燕宁 傅, Tian-Rui Sun, 天瑞 孙, Yu-Xi Jiang, 雨汐 蒋
Figure caption: Relation between the ﹩{\mathop{\sigma }\limits^{\unicode{x00304}}}_{{\rm{eq}}}﹩ and ∣v0∣/Δv for simulated mutual approximations of set A. The condition of set A is shown in Table 5. The Pearson coefficient is 0.80 with the p-value of 0.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The variation of metallicity with RGC in M31. Red dots are for bins within 30 kpc, and blue dots are for bins greater than 30 kpc. The dashed gray line is −0.008 dex kpc−1 derived in the RGC range of 7–45 kpc given by C. H. Lee et al. (2013), the solid gray line is −0.020 dex kpc−1 derived in the RGC range of 4–20 kpc by D. Gregersen et al. (2015), and the dotted gray line is −0.038 dex kpc−1 derived in the RGC range of 0–30 kpc by B. Chen et al. (2016).
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The variation of metallicity with RGC in M33. Red dots are for bins within 9 kpc, and green dots are for bins greater than 9 kpc. The solid gray line is −0.078 dex kpc−1 derived in the RGC range of 0–9 kpc by M. R. L. Cioni (2009), the dashed gray line is −0.070 dex kpc−1 derived in the same RGC range by Vivian U et al. (2009), and the dotted gray line is −0.29 dex kpc−1 derived within RGC < 4.5 kpc by M. A. Beasley et al. (2015).
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Comparison of metallicity gradients among different galaxies. Circles indicate metallicity gradients from the literature, while triangles represent this work and Paper I. The metallicity gradient is expressed in units of dex ﹩{R}_{25}^{-1}﹩.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Metallicity distribution in M33 for different extinction corrections. The dots present the [M/H] of each bin.
Paper: Metallicity Distribution in M31 and M33 Based on the Tip of the Red Giant Branch Near-infrared Color
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Metallicity distribution in M31 for different extinction corrections. The dots present the [M/H] of each bin.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: Histogram distributions of voff values, drawn every 100 km s−1 and shown in light orange, overlaid with ﹩\overline{E(B-V)}﹩ values, drawn every 1000 km s−1 and shown in dark purple, as calculated using redshift subsamples of associated absorbers. The redshift range of each panel is indicated in the upper right and the 50th percentile value of the voff distribution, as well as the difference to the 16th and 84th percentile, is given in the upper left and these percentiles are displayed as light orange vertical lines. Note that the ﹩\overline{E(B-V)}﹩ values are calculated in seven 1000 km s−1 bins from −3500 km s−1 to +3500 km s−1 as indicated by the light gray boxes and are only shown if the corresponding voff bin has at least 30 entries, error bars on these points are the standard error of the mean. The top axis of each panel has been converted from voff to a difference in redshift using the mean redshift of each panel’s redshift range.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: A recreation of Figure 7 using voff values as calculated from the zQSO values found when masking Mg II absorption lines. The voff histogram and vertical lines indicating the 16th, 50th, and 84th percentile of each panel are now shown in light purple. Note that the ﹩\overline{E(B-V)}﹩ values, shown in dark purple, are calculated in seven 1000 km s−1 bins from −3500 km s−1 to +3500 km s−1 as indicated by the light gray boxes and are only shown if the corresponding voff bin has at least 30 entries, error bars on these points are the standard error of the mean. The top axis of each panel has been converted from voff to zQSO - zAAS using the mean redshift of each panel’s redshift range.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Upper panel: Transit spectroscopy signal ﹩{R}_{p}^{2}/{R}_{s}^{2}﹩ (minus the minimum value, and given in parts-per-million) for a temperate planet orbiting an M2V star, and adopting the “preindustrial Earth” planetary model from M. H. Currie et al. (2023). Lower panel: Template of line strengths for water vapor used in our CCs.
Paper: DESI Mg II Absorbers: Extinction Characteristics and Quasar Redshift Accuracy
Authors: Lucas Napolitano, Adam D. Myers, Victoria A. Fawcett, Jessica Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Shaun Cole, Axel de la Macorra, Biprateep Dey, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Aaron Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Hu Zou
Figure caption: The difference in redshift between the catalog values and the values found when the Mg II lines are masked. Δz is calculated in redshift bins 0.1 units wide and the 50th percentile value is plotted with the surrounding colored envelope showing the 16th and 84th percentiles of the distribution. Results for systems initially at voff  > 0 km s−1 are shown in blue and systems initially at voff  < 0 km s−1 in red.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Comparison of our calculated S/Ns for CC detections with those of M. H. Currie et al. (2023), showing four different planetary host star/atmospheric molecule combinations. In each case, the S/N for the detection of the molecule in question is plotted vs. the number of transits (solid blue and red lines), and S/N increases as the square root. Our S/Ns are calculated using multiple Monte Carlo trials, and the dashed red lines give the ±1σ bounds on our calculations. The bottom X-axis is only for the bottom panel, and the top X-axis is for the remaining panels. The distance of each system is adopted to be 12 pc, and the results from M. H. Currie et al. (2023) are from their Figure 13.
Paper: Minimizing Star-spot Contamination of Exoplanet Transit Spectroscopy Using Alternate Normalization
Authors: Drake Deming, Miles H. Currie, Victoria S. Meadows, Sarah Peacock
Figure caption: Effects of star spots on Sλ for the case of a temperate planet orbiting an M8V star 12 pc from Earth, with 5% area coverage of an unocculted star spot having ΔT = −800 K. The upper panel shows the median-subtracted unspotted case and the effect of spots is shown in the lower panel, where the Y-axis is the median-subtracted Sλ as per Equation (4). The effect on the CC function will be smaller than this effect on Sλ because the star-spot spectrum is not highly correlated with the molecular templates.