adsabs/AstroCLIMB huggingface dataset:
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: Histograms showing the distribution of KL modes for all parameter combinations (choice of weights for image quality metrics and choice of KL modes for combination) where the four quantitative measures of similarity between parameter explorer heat map structures for true and injected companions (described in detail in the text) were among the top 10% (left) and top 12% (right) of values according to all four measures. In the top 10% of reductions, 5 KL modes was chosen most frequently. In the top 12% of reductions, 20 KL modes was chosen most frequently.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: S/N maps showing the effect of high-pass filtering on the HD 142527 2013 April 11 data set. The left S/N map shows no high-pass filtering (highpass = False) and has a peak companion S/N of 4.1. The middle S/N map shows a default high-pass filter width of 0.1 × the image size (highpass = True) and has a slightly higher peak S/N of 4.6. The right S/N map shows a more aggressive high-pass filter width of 1 × FWHM and has a peak S/N of 8.1.
Paper: The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Jéa I. Adams Redai, Katherine B. Follette, Jason Wang, 劲飞 王, Clare Leonard, William Balmer, Laird M. Close, Beck Dacus, Jared R. Males, Katie M. Morzinski, Joseph Palmo, Laurent Pueyo, Elijah Spiro, Helena Treiber, Kimberly Ward-Duong, Alex Watson
Figure caption: A schematic representation of the optimization process applied in this work, with images drawn from optimization of the HD 142527 2013 April 11 data set.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: The RV time series and orbit models for TOI-1669's AIC-preferred circular model (left) and our preferred model including eccentricity (right). Although the circular model has a lower AIC, we adopt the more general model including eccentricity, and emphasize that our limited RV sample contributes to model selection uncertainty. In both figures, (a) shows our full Keck/HIRES RV time series (black points) with the fitted model in blue. The residuals to the fit are given in (b). Each subsequent panel shows the time series phase-folded to a particular model planet period. Both models recover consistent periods and masses for the giant TOI-1669 b, as well as a long-term linear trend, suggesting that these parameters are not highly sensitive to our choice of model. By contrast, our eccentric model shows that TOI-1669 b’s orbit may deviate from circular. Future observations will resolve this disagreement. The existence of TOI-1669.01 is known from TESS photometry, so we include it in our model despite its low RV amplitude.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: Observations of the Distant Giants sample between its official start in 2020 August and late 2022. Red squares are HIRES RVs and gray circles are APF RVs. Targets are ordered by R.A., shown in the right margin. The typical target in our sample is inaccessible from Keck Observatory for about three months out of the year, which is reflected in the bands of decreased observation density that run diagonally through the plot. During their observing seasons, all targets generally meet or exceed the prescribed monthly cadence.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: The RV time series of TOI-1694, together with orbit models assuming a circular (left) or eccentric (right) outer planet. In both figures, (a) shows our full Keck/HIRES RV time series (black points) with the fitted model in green. The residuals to the preferred fit are shown in (b). Each subsequent panel shows the time series phase-folded to a particular model planet period. For consistency with our treatment of TOI-1669, we include two models that differ only in the eccentricity of the outer planet. However, in contrast to TOI-1669, the eccentric model we adopted for TOI-1694 is also formally preferred by the AIC. TOI-1694 b’s mass and orbital separation identify it as a hot Neptune.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: Stellar and transiting planet parameters of the TKS survey. Filled points show targets selected for the Distant Giants sample. Panels (a) through (c) show stellar parameters. TOI-1775 and TOI-2088 are not shown in panel (b) because they lacked measured ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ values when we finalized our sample. Panel (d) shows parameters of the transiting planets. For multitransiting Distant Giants systems, we checked planet radii in order of ascending TOI number, and show the first planet to pass our survey filters.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Excess absorption, in percent, as a function of time and wavelength in the stellar rest frame. Clockwise from upper left: TOI 560b (first published in Zhang et al. 2022c), 1430.01, 2076b, and 1683.01. The color bars and wavelengths are matched, but the y-axes are not. The red lines show the wavelengths of the helium triplet in the planet rest frame. The horizontal dashed and solid lines show the beginning of white-light ingress and end of white-light egress, respectively.(The data used to create this figure are available.)
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Stellar spectra in the vicinity of the helium triplet (in red) before and after correction for tellurics. Unlike in the rest of the paper, the wavelengths are in Earth’s frame, not the stellar rest frame, leading the telluric lines to have the same wavelengths for every target. The telluric lines do not overlap with the helium line for any target except TOI 560, for which we were lucky to have had an exceptionally dry night.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: A 2048 × 515 CUTE CCD image with the slit fully illuminated with a diffuse, uncollimated Hg light source, obtained during thermal vacuum testing. The projected image of the slit is shown at several mercury lines, including 2536 Å, 2967 Å, and a doublet at 3125 and 3131 Å. The exposure time for this image was set to sample the fainter spectral features of the light source; as a result, many pixels in the 2536 Å line reached saturation levels and some side effects of this saturation can be seen in the image.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Left: 2048 × 515 CCD image of Castor’s spectra with the background subtracted. The spectrum is the bright green line in the image’s center. Below the spectrum is residual background subtraction noise, and above the spectrum is residual spectral light as the CCD is read out while the shutter remains open. CCD register clocking moves charges to the right and vertical clocking moves the charges down. Right: one-dimensional cross-section of the frame to illustrate the readout streak. The vertical dashed line marks the median value of the readout residual exposure at 2.2% of the normalized counts cross-section.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Top: a 2048 ×515 CUTE spectral image of Castor with background effects removed to show the spectrum. Middle left: zoom of a blue portion of the CUTE spectrum to highlight the out-of-focus lobes. Middle right: zoom of a red portion of the CUTE spectrum to highlight the less-out-of-focus lobes. Bottom: one-dimensional cross-sections of the middle panels.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: CAD renderings of the CUTE telescope and spectrograph. Top: front view of the Cassegrain telescope. Middle: view of the spectrograph internals. Bottom: view of the fully closed-out spectrograph, including the detector and the thermal strap attached to the spacecraft radiator.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Flux-calibrated spectrum of ζ Pup. A CUTE spectrum is in black, plotted over the blue IUE spectrum. Black vertical tick marks note the spectral features used to calculate CUTE's wavelength solution. IUE sensitivity falls off beyond 3100 Å, so a model was fit to the IUE data in order to calculate CUTE's effective area and flux spectrum.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: Effective area of the CUTE instrument as proposed (blue), estimated with laboratory measurements (orange), and calculated in-flight and smoothed (black). The in-flight effective area beyond λ ≈ 3100 Å is estimated based on a model fit to the IUE ζ Puppis one-dimensional spectrum.
Paper: The On-orbit Performance of the Colorado Ultraviolet Transit Experiment Mission
Authors: Arika Egan, Nicholas Nell, Ambily Suresh, Kevin France, Brian Fleming, Aickara Gopinathan Sreejith, Julian Lambert, Nicholas DeCicco
Figure caption: The CUTE spacecraft with solar panels fully deployed and communication cables attached. Solar cells are opposite the telescope boresight. The telescope is visible in the left 2/3 of the spacecraft and the star tracker and avionics are contained in the right 1/3. The star tracker has a red “remove before flight” panel covering its aperture. The UHF antenna is deployed on the bottom left of the spacecraft chassis and is noted with the yellow arrow.
Paper: The Colorado Ultraviolet Transit Experiment Mission Overview
Authors: Kevin France, Brian Fleming, Arika Egan, Jean-Michel Desert, Luca Fossati, Tommi T. Koskinen, Nicholas Nell, Pascal Petit, Aline A. Vidotto, Matthew Beasley, Nicholas DeCicco, Aickara Gopinathan Sreejith, Ambily Suresh, Jared Baumert, P. Wilson Cauley, Carolina Villarreal D'Angelo, Keri Hoadley, Robert Kane, Richard Kohnert, Julian Lambert, Stefan Ulrich
Figure caption: Initial CUTE light curves of WASP-189b, showing three independent NUV (approximately 2540–3300 Å) light curves (black points) and the best-fit transit models in gray. The plots compare the NUV band light curves with the optical light curve (in red) from CHEOPS (Lendl et al. 2020). The NUV transits are significantly deeper than their broadband optical counterparts, indicating an effective planetary radius increase of R  P,NUV ≈ 1.5R  P,opt.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Probability density distribution of solutions for mass m 2 of the third component in the V907 Sco system. The available data set of photometric observations was used. The nonzero values correspond to the projection of five-dimensional parameter-space zone ﹩{ \mathcal V }﹩ containing all admissible solutions within 90% confidence limit. The vertical dashed line is the median value of the distribution. Should the eccentricity e 2 of the outer orbit be smaller/larger than the nominal value 0.467 used here, the distribution would shift toward larger/smaller values as shown by the arrows.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Probability density distribution of solutions for precession period P  ν  and mutual inclination J of inner and outer orbits of the V907 Sco system. The available data set of photometric observations was used. The nonzero values correspond to the projection of five-dimensional parameter-space zone ﹩{ \mathcal V }﹩ containing all admissible solutions within 90% confidence limit. The vertical solid line is the median value of the distribution.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Predicted increase in the primary eclipse depths for the V907 Sco inner binary in the next decade. The effect is due to the increasing inclination i 1 of the orbital plane (Figure 6). The red line is adjusted to the actual measurements in 2022 reported in Section 2. The abscissa gives the phase of the P 1 ≃ 3.776 day cycle; the ordinate is the magnitude.
Paper: V907 Sco Switched to the Eclipsing Mode Again
Authors: Petr Zasche, David Vokrouhlický, Brad N. Barlow, Martin Mašek
Figure caption: Predicted value of ETVs (ΔT) for the primary component in the V907 Sco. The abscissa is the cycle count of the eclipsing binary (period P 1 = 3.776 day; the whole time span shown is therefore little more than two years), the ordinate is in minutes. The red line is the dynamical (physical) delay due to the third-star perturbations of the mean motion of the binary, and the blue line is the light-time (Roemer) effect due to motion of the binary center of mass about the barycenter of the whole system. Both are expressed analytically (e.g., Rappaport et al. 2013). Symbols show the dynamical delay determined numerically for sake of comparison. The perihelion of the outer-orbit motion occurs where the gradient of the dynamical effect change is the largest.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: Masses and periods of known exoplanets discovered by RVs (blue circles) and transits (red circles). Transiting planet masses are estimated from their radii using the mass–radius relation of Weiss & Marcy (2014). Transiting/resolved Distant Giants companions are overlaid as red/blue squares. Inner and outer companions in the resolved systems, HD 219134, HD 75732, TOI-1669 and TOI-1694, are connected with black lines. We also plot estimated parameters of HD 191939 f, though our analysis of this planet’s RV signal is still preliminary. TOI-1669 b and TOI-1694c have masses and periods typical of cold Jupiters. The red arrows indicate planetary periods shorter and longer than the current ∼2 yr survey baseline. HD 75732 d and HD 219134 g have orbits well beyond three years, and are only resolved due to their extensive observing histories.
Paper: TESS-Keck Survey. XIV. Two Giant Exoplanets from the Distant Giants Survey
Authors: Judah Van Zandt, Erik A. Petigura, Mason MacDougall, Gregory J. Gilbert, Jack Lubin, Thomas Barclay, Natalie M. Batalha, Ian J. M. Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Lauren M. Weiss, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Christopher E. Henze, Michelle L. Hill, Lea A. Hirsch, Rae Holcomb, Steve B. Howell, Jon M. Jenkins, David W. Latham, Andrew Mayo, Ismael Mireles, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex S. Polanski, George R. Ricker, Lee J. Rosenthal, Ryan A. Rubenzahl, S. Seager, Nicholas Scarsdale, Emma V. Turtelboom, Roland Vanderspek, Joshua N. Winn
Figure caption: Distribution of eccentricity vs. orbital separation for confirmed exoplanets between 0.01 and 30 au with σ  e  ≲ 0.1 (blue points). The four resolved giants in our sample are shown in orange. TOI-1669 b and HD 219134 g have eccentricities consistent with zero, and each is represented by an arrow, the base of which shows the 84% upper eccentricity limit. It is not obvious that the distribution from which these planets’ eccentricities are drawn is distinct from that of the underlying population.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Band-integrated light curves, integrated within 1.5 Å of the main peak of the helium triplet, at 10833.3 Å. The wavelength range is defined with respect to the stellar frame in order to give an accurate picture of stellar variability in the helium line. The y-axes are matched, but the x-axes are not. Dashed and solid vertical lines represent the beginning and end of the white-light transit, respectively.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Four mini-Neptunes in context, with the size of each point inversely proportional to the planetary radius. The y-axis shows δ Rp/H eq, the ratio of the increase in apparent radius at 1083 nm to the scale height at equilibrium temperature. For all of our planets (red filled circles), the y-axis error bars are dominated by the uncertainty in mass. In particular, planets other that TOI 560 have no mass measurement. Data for published planets (black filled circles) are taken from Kasper et al. (2020), with updates from Orell-Miquel et al. (2022; GJ 1214b, tentative) and Kirk et al. (2022; WASP-52b). Photometric detections are excluded because they are not comparable. Breaking with precedent, upper limits are excluded to reduce clutter.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Left: X-ray spectrum of TOI 1430 (top) and TOI 1683 (bottom), measured by XMM-Newton’s three EPIC cameras. Note that both the throughput and the line-spread profile are heavily dependent on wavelength. Right: theoretical model that best explains the measurements. The model consists of two components (top; TOI 1430) or one component (bottom; TOI 1683) of optically thin, collisional plasma in equilibrium.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: The TTVs computed with the above ephemeris. The shaded regions are the model predictions from the low-mass (left) or high-mass (right) nested sampling runs.
Paper: Detection of Atmospheric Escape from Four Young Mini-Neptunes
Authors: Michael Zhang, Heather A. Knutson, Fei Dai, Lile Wang, George R. Ricker, Richard P. Schwarz, Christopher Mann, Karen Collins
Figure caption: Average in-transit excess absorption spectrum. Note that we only have the last third of the transit for TOI 2076, making it difficult to directly compare to the other full-transit observations.