adsabs/AstroCLIMB huggingface dataset:
Paper: A Measurement of the Kuiper Belt’s Mean Plane From Objects Classified By Machine Learning
Authors: Ian Matheson, Renu Malhotra
Figure caption: Kuiper Belt mean plane and its confidence ellipses in the (q, p) plane, by semimajor axis bin. Semimajor axis bins are (a) the classical belt from 42 to 48 au, (b) the entire belt from 35–150 au, and (c) the entire belt minus the classical region. The best-fit mean plane is the dark green +. The mean planes of 40,000 Monte Carlo samples are in light green, and the 68.2%, 95.4%, and 99.7% covariance ellipses for them are in dark green. The J2000 ecliptic/equinox pole is at the origin. The invariable plane is the black x. The theoretical prediction (from linear secular theory) for the Laplace surface as a function of semimajor axis is plotted in blue. More details are given in the main text.
Paper: A Measurement of the Kuiper Belt’s Mean Plane From Objects Classified By Machine Learning
Authors: Ian Matheson, Renu Malhotra
Figure caption: Kuiper Belt mean plane and 68.2% confidence intervals by semimajor axis bin. The mean planes and confidence intervals from this work are in green, and those from VM17 are in magenta. For the sake of readability, the vertical magenta and green lines have been slightly offset from each other in semimajor axis when they would otherwise overlap. The theoretical prediction for the Laplace surface as a function of semimajor axis is plotted in blue. The invariable plane is indicated by the horizontal black line.
Paper: A Measurement of the Kuiper Belt’s Mean Plane From Objects Classified By Machine Learning
Authors: Ian Matheson, Renu Malhotra
Figure caption: Semimajor axis, inclination, and eccentricity of the 931 nonresonant KBOs with well-determined orbits from 35 < a < 150 au from VM17 (red +), and the sample of 1812 nonresonant KBOs with well-determined orbits from 35 < a < 150 au, with q > 30.34 au, in this study (blue dots). Orbital elements for the 1812 nonresonant KBOs are from JPL Solar System Dynamics Group (2022) as explained in Section 5.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Theoretical (red) and observable (black) metastable He transmission spectra of GJ 436 b assuming a substellar escape rate of 108 g s−1 and an outflow temperature of 3000 K.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption:                       ﹩{\rm{\Delta }}{\chi }^{2}\equiv {\chi }_{\min }^{2}-{\chi }^{2}﹩ values associated with each of the n e solutions (Equation (5)) found to be consistent with the most probable solution (n e = 51, P e ≈ 46.8 days) at the ≈4σ level; lower n e values, which decrease monotonically toward ﹩{\chi }_{\min }^{2}-{\chi }^{2}\lt -90﹩ at n e = 1, are not shown for visual clarity. The 2σ, 3σ, and 4σ confidence intervals are indicated by the horizontal dashed lines. Under the assumption of circular orbits, all longer periods with P e > 55.4 days are rejected at the 3σ level in favor of the n e = 51 solution, while seven shorter period solutions with 43.3 < P e/d < 55.4 (n e = 43, 46, 47, 50, 51, 54, and 55) are consistent within 3σ.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Best fit to the HARPS and CARMENES RV measurements (left panels) and the MAROON-X red and blue measurements (right panels) using the n e = 51 (P e ≈ 46.8 days) solution (n.b., the MAROON-X measurements are plotted with a time offset for better visibility). The top panels show the GP fit to the observed RVs with the planetary component removed, the middle panels show the total planetary component with the GP fit removed, and the bottom panels show the residuals. The STELLA and HERMES measurements, which are included in our analysis, are not shown due to their comparatively large uncertainties.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption:  O − C values for the derived transit times measured with respect to each planet’s 〈P〉; the break in the x-axis separates the K2 measurements (BJD – 2454833 < 2300) from the TESS measurements (BJD – 2454833 > 4640). The white points are those measurements that may be biased due to overlapping transits or partial event coverage.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Best fit to the K2 light curve using the n e = 51 (P e ≈ 46.8 days) solution. The top panel shows the observed flux measurements compared with the GP model. The middle panel shows the transit models compared with the detrended measurements (i.e., with the GP model removed). The bottom four panels show the phased transits for planets b, c, d, and e; individual transits are shown in Figure 4.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Selected individual transits observed in the TESS light curve.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Selected individual transits observed in the K2 light curve.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Same as Figure 3 but for the TESS light curve. Individual transits are shown in Figure 6.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Masses and radii of V1298 Tau’s four transiting planets derived for the most probable P e and assuming circular orbits (squares; upper mass limits correspond to 2σ) where the colors correspond to the equilibrium temperature. Five planets with mass constraints from three other young systems (<100 Myr) are plotted for comparison (circles): DS Tuc A b (Benatti et al. 2021), AU Mic b and c (Gilbert et al. 2022; Zicher et al. 2022), and TOI-942 b and c (Carleo et al. 2021). The dark-gray and light-gray lines are the theoretical planet mass–radius relations published by Fortney et al. (2007) at an age of 20 Myr and 5 Gyr, respectively. These models are computed for 50/50 ice-rock cores with H/He envelopes that are irradiated by a Sun-like host star at a distance of 0.1 au. The dashed–dotted curve is a model published by Zeng et al. (2019) composed of an Earth-like rocky core (47.5% by mass) with an H2O layer (47.5%) and an H2 envelope (5%) at T eq = 1000 K.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Marginalized posterior distributions derived for the RV semiamplitudes of planets c, d, b, and e for the seven most probable n e solutions—those that are consistent with the most probable n e = 51 solution (P e ≈ 46.8 days) within the 3σ confidence interval. The thicker line indicates the n e = 51 solution.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Marginalized planet mass posteriors derived for the most probable n e = 51 solution assuming circular orbits (black contours). The dynamical stability probability (P(Stable)) estimated for each sample using SPOCK is also shown. The blue contours show the posteriors obtained after after applying rejection sampling to the calculated P(Stable) values.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Same as Figure 12 but for noncircular orbits where the eccentricity distributions are also plotted.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Individual planetary contributions to the stellar reflex RV phased by orbital period for the median solution fit (Table 1) assuming P e ≈ 46.8 days. Filled circles correspond to the detrended observed RVs and the red dashed lines indicate the model fits. For visual clarity, the STELLA and HERMES measurements are not plotted.
Paper: Updated Planetary Mass Constraints of the Young V1298 Tau System Using MAROON-X
Authors: James Sikora, Jason Rowe, Saugata Barat, Jacob L. Bean, Madison Brady, Jean-Michel Désert, Adina D. Feinstein, Emily A. Gilbert, Gregory Henry, David Kasper, Déreck-Alexandre Lizotte, Michael R. B. Matesic, Vatsal Panwar, Andreas Seifahrt, Hinna Shivkumar, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Injected vs. recovered planetary RV signatures. Note the differing axis scales.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Integrated intensity map of 12CO, 13CO, and C18O within the velocity range of [−20, 70] km s−1. The intensity is integrated according to the 12CO cloud catalog boundary in PPV space that comes from the DBSCAN algorithm (Section 3.1). The circles symbolize SNRs (Green 2019) and H II regions (for more information on H II see Sharpless 1959; Anderson et al. 2014). The asterisk represents open cluster NGC 2264 (Herbig 1954). The triangles represent Lynds dark clouds (Lynds 1962). Some well-known MCs are also shown on the map. The newly discovered CO-dark hole (named “MWISP Hole”) is marked with a rectangle in the upper left corner.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Spectral noise distribution of 12CO, 13CO, and C18O in the total 250 deg2 region.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Spatial distribution of 12CO, 13CO, and C18O noise in the total 250 deg2 region.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The spatial distribution of all 7069 clouds. The background is the 12CO integrated intensity map within the velocity ranges of [−20, 0], [0, 20], [20, 40], and [40, 70] km s−1, respectively. The boundaries of the MC are outlined with different colored lines and are shown in four velocity intervals depending on the peak velocity of the cloud.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: Longitude–velocity map of 12CO emissions. The latitude integration range is between −5.°25 and 5.°25. There is a bright stripe along the Galactic longitude in the figure, which is caused by a bad channel at the velocity of 34 km s−1.
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: (a) The average spectrum of 32 clouds considered containing C18O emission. Different colors and line types represent different CO isotopologues. The spectra of different isotopologues are averaged for all pixels in the cloud. (b) Continuation of panel (a).
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption:  13CO and C18O percentage rates of clouds with different parameters (peak intensity, projected area, and total flux).
Paper: The Molecular Clouds in a Section of the Third Galactic Quadrant: Cloud Catalog
Authors: Chen Wang, Haoran Feng, Ji Yang, Xuepeng Chen, Yang Su, Qinq-Zeng Yan, Fujun Du, Yuehui Ma, Jiajun Cai
Figure caption: The left panel shows 13CO vs. C18O integrated intensity of the cloud MWISP G217.942−02.083+034.45; the C18O intensity is integrated within the channels selected by the 12CO velocity distribution range pixel by pixel. The right panel also shows 13CO vs. C18O integrated intensity for the same cloud, but the C18O intensity is integrated with the channels selected by 13CO intensity greater than 2 × rms. The dashed lines represent the average value of triple integrated rms of 13CO and C18O, and the solid lines represent two typical ratios of 13CO to C18O in the cloud.
Paper: Spectral Energy Distributions for 258 Local Volume Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Jordan A. Turner, Daniela Calzetti, Robert C. Kennicutt, Janice C. Lee
Figure caption: Comparison of global star-formation rates and stellar masses for the LVL sample (filled red/black/green circles) with the “z0MGS” z = 0 Multiwavelength Galaxy Synthesis catalog (blue dots) of Leroy et al. (2019). The star-forming main-sequence linear relation from Peng et al. (2010) is shown as a black line; our best-fit relation for the LVL sample is provided as a red line. LVL star-formation rates are based on the Hao et al. (2011) FUV+TIR calibrations for 216 galaxies (red circles), the Hao et al. (2011) NUV+TIR calibrations for 11 galaxies without (GALEX) FUV observations (black circles), and the Kennicutt et al. (2009) Hα+24 μm calibration for 17 galaxies with neither (GALEX) NUV nor FUV observations (green circles). Stellar masses are based on 3.6 μm fluxes using the prescription outlined in Appendix A.4 of Leroy et al. (2019).
Paper: Spectral Energy Distributions for 258 Local Volume Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Jordan A. Turner, Daniela Calzetti, Robert C. Kennicutt, Janice C. Lee
Figure caption: Left: dust-to-stellar mass as a function of stellar mass. Filled circles indicate our results for the LVL sample, the open red triangles are from the CIGALE SED fits for the KINGFISH sample from Hunt et al. (2019), and the open blue squares represent the SED-based values from the Dwarf Galaxy Sample presented in Rémy-Ruyer et al. (2015). Right: dust-to-stellar mass as a function of star-formation rate averaged over the past 100 Myr, as inferred from the SED fitting (the star-formation rates for the DGS sample are based on Hα+TIR).
Paper: Spectral Energy Distributions for 258 Local Volume Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Jordan A. Turner, Daniela Calzetti, Robert C. Kennicutt, Janice C. Lee
Figure caption: Top: the reduced χ 2 values as a function of SED-derived stellar mass. The points are color coded according to best-fit stellar metallicity. Bottom: The distributions of the best-fit metallicities as a function of stellar mass using the same color scheme as in the top panel.
Paper: Spectral Energy Distributions for 258 Local Volume Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Jordan A. Turner, Daniela Calzetti, Robert C. Kennicutt, Janice C. Lee
Figure caption: Example CIGALE fits for three LVL galaxies, one a massive spiral galaxy (NGC 3031 = M 81) and two lower-luminosity irregular galaxies (NGC 4214 and UGC 6900). The blue, red, green, and black lines represent the intrinsic stellar continuum, dust continuum, nebular, and total modeled emission, respectively. The filled red circles represent the model flux densities in the 25 possible broadband bandpasses whereas the open magenta circles are the observed flux densities (upper limits are open magenta triangles).
Paper: Spectral Energy Distributions for 258 Local Volume Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Jordan A. Turner, Daniela Calzetti, Robert C. Kennicutt, Janice C. Lee
Figure caption: Comparison of CIGALE SED-based stellar masses with those derived from 3.6 μm infrared photometry. The 3.6 μm—based stellar masses are computed using a mass-to-light ratio that depends on the specific star-formation rate following Appendix A.4 of Leroy et al. (2019). The horizontal dotted line indicates unity for the mass ratio.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Final transmission spectrum in the planetary rest frame centered on the 10831–10835 Å range. Planetary absorption would be seen as a negative value, so this flat spectrum shows no indication of helium absorption. One example of the 1D Parker wind model is overplotted with the spectrum. This example depicts various mass-loss rates (﹩\dot{M}={10}^{9}\mbox{--}{10}^{11}\ {\rm{g}}\ {{\rm{s}}}^{-1}﹩) with a thermosphere temperature of 9500 K. The absorption signature increases with the mass-loss rate at this thermosphere temperature.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Example spectrum from 2019 May 19 08:08 UT in the topocentric rest frame. The rest wavelengths of the HITRAN-derived OH and H2O features are shown with vertical green and yellow dashed lines, respectively. These coincide with the emission lines seen in the spectrum, confirming that they are telluric features originating in the Earth’s atmosphere. The expected location of the stellar silicon feature and any planetary helium feature is also plotted. Note that the location of the predicted helium feature varies across exposures due to changing barycentric and planetary velocity corrections.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Science fiber in the topocentric rest frame, both before (light blue line) and after (dark blue line) sky flux subtraction. This exposure is from 2019 May 19 08:08 UT. We have zoomed in to see that the sky subtraction has successfully removed the OH emission lines and revealed a stellar helium line underneath the small OH doublet.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Number of standard deviations between the transmission spectrum and model in the range 10831–10835 Å, measured across the full range of parameter space. A line is drawn around the 3σ contour to show that anything higher than this value (red on the plot) can be rejected. The apparent decrease in absorption at high mass-loss rates may be a model artifact due to the fact that our model does not take into account helium that exists beyond the Hill radius.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Final transmission spectrum in the planetary rest frame. Same as Figure 4 but with varying thermosphere temperatures (T = 7000–10,000 K) at a constant mass-loss rate of ﹩\dot{M}={10}^{10}\ {\rm{g}}\ {{\rm{s}}}^{-1}﹩. At this mass-loss rate, helium absorption increases with decreasing temperature.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: Final version of EMC showing absorption depth at the 10833 Å helium line across randomly selected subsets of in-transit and out-of-transit exposures. The solid and dotted black lines depict the calculated absorption depth and error from the transmission spectrum. The corresponding magenta lines show the average absorption and standard deviation calculated in the EMC. The lines are within 0.1σ of each other, suggesting that we have correctly accounted for systematic errors in the analysis.
Paper: Nondetection of Helium in the Hot Jupiter WASP-48b
Authors: Katherine A. Bennett, Seth Redfield, Antonija Oklopčić, Ilaria Carleo, Joe P. Ninan, Michael Endl
Figure caption: In-versus-out of transit spectrum in the stellar rest frame. The individual spectra have been interpolated and undergone a weighted sum with their inverse variances used as weights. No planetary helium signal is visible.