adsabs/AstroCLIMB huggingface dataset:
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the flux intensities for the emission lines derived using the nonparametric (NP_ELINES) and parametric (PM_ELINES) procedures described in Section 3.1, for the ad hoc realistic simulations described in Section 4.2 (left panel) and the Orion data discussed in Section 5. Contours, symbols, and lines in each panel have the same meaning as those in Figure 7.
Paper: The SDSS-V Local Volume Mapper: Data Analysis Pipeline
Authors: Sebastián F. Sánchez, Alfredo Mejía-Narváez, Oleg V. Egorov, Kathryn Kreckel, Niv Drory, Guillermo A. Blanc, J. Eduardo Méndez-Delgado, Jorge K. Barrera-Ballesteros, Hector Ibarra-Medel, Dmitry Bizyaev, Pablo García, Aida Wofford, Alejandra Z. Lugo-Aranda
Figure caption: Comparison between the recovered and simulated nonlinear parameters of the stellar component: v⋆ (left panel), σ⋆ (middle panel), and AV,⋆ (right panel). Contours, symbols, and lines in each panel have the same meaning as those in Figure 7.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. I. Generalized Ambartsumian (1937) Approach and the Family of Power-law Distributions of Eccentricity
Authors: Valeri V. Makarov
Figure caption: Empirical distribution (histogram) of the projected separations between the components of resolved binary systems in Gaia DR3 from the catalog by K. El-Badry et al. (2021) after additional filtering. The blue line represents the properly scaled PDF of the best-fitting analytical distribution, which is a {0.78, 0.22} mixture distribution of Gamma [2.1, 487] and LogNormal [8.68, 0.83] distributions. The peculiar sample PDF is not adequately represented by any available analytical forms, having a concave ascending slope, a sharp peak, and an exponentially descending heavy tail.
Paper: Extinction Distributions in Nearby Star-resolved Galaxies. I. M31
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Comparison between the extinction distributions derived in this work and that inferred from B. T. Draine et al. (2014). Left panel: extinction distribution calculated from the dust-mass surface density map based on infrared emission (B. T. Draine et al. 2014), with the same resolution as Figure 4. Right panel: Pixel-by-pixel comparison between AV values derived in this work (x-axis) and the resolution-matched ﹩{A}_{{V}_{{\rm{emission}}}}﹩ values from the emission-based map (y-axis). The red line shows the linear regression fit forAV > 0.5 mag, given by the equation ﹩{A}_{{V}_{{\rm{emission}}}}=1.28{A}_{V}-0.40﹩.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. I. Generalized Ambartsumian (1937) Approach and the Family of Power-law Distributions of Eccentricity
Authors: Valeri V. Makarov
Figure caption: Observed (gray color) and Monte Carlo simulated (yellow color) distributions of the cosine motion angle ﹩\cos \vartheta ﹩, Equation (17).
Paper: Extinction Distributions in Nearby Star-resolved Galaxies. I. M31
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Left panel: distribution of the stellar number in each pixel. Right panel: extinction distribution in M31 with a resolution of approximately 50″.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. I. Generalized Ambartsumian (1937) Approach and the Family of Power-law Distributions of Eccentricity
Authors: Valeri V. Makarov
Figure caption: CDF (left panel) and PDF (right panel) of power-law marginal eccentricity distribution for different values of ﹩\alpha ^{\prime} ﹩ per Equation (13).
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Stellar radius vs. stellar effective temperature for all confirmed transiting planet hosts. TESS discoveries are shown in black and discoveries from other telescopes are shown in gray. Systems discovered by the GTG survey are marked by orange circles, with TOI-7041 indicated by the filled orange point.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: (a) Phase-folded TESS light curve, centered on the transit of TOI-7041 b. Light gray points show the TESS observations, dark gray points show TESS data binned to 1 hr, and the orange line shows the best-fit transit model. (b) RV measurements obtained with CHIRON (light gray), FEROS (dark gray), and PFS (black), phase folded to the period of the transit signal. The orange line shows our best-fit orbital model, with random draws from the posterior distribution of the model shown by the fainter orange lines. The RV and transit models were fit simultaneously using the exoplanet Python package.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Frequency echelle diagram of the smoothed power spectrum. Orange points indicate the identified ℓ = 0 modes and blue points indicate the ℓ = 2 modes. Uncertainties on the identified mode frequencies are shown by the error bars; some uncertainties are smaller than the point size. The shading shows the SNR at each frequency.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Planet radius shown as a function of incident flux the planet receives from its star. Point color indicates the planet mass. The dashed vertical line shows the inflation threshold from B.-O. Demory & S. Seager (2011). The estimated main-sequence incident flux received by TOI-7041 b is indicated by the white circle.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Planetary orbital semimajor axis (a) shown as a function of stellar radius (R⋆) for all confirmed exoplanet (gray) and TOI-7041 b (orange). The solid black line shows the 1:1 relation where a = R⋆.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Full RV time series for TOI-7041 with our two-planet model shown in orange. In addition to the signal in phase with the transit ephemeris (shown as a phase-folded RV curve in Figure 4, right), we identify a periodic trend with a period of ∼150 days.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Contrast curve of TOI-7041 in the 562 nm and 832 nm passbands. The inset figure shows a high-contrast speckle image reconstruction centered on TOI-7041.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Planet radius vs. planet mass for all known exoplanets are shown in gray. The position of TOI-7041 b is marked by the orange point. Solar system planets Earth, Neptune, Saturn, and Jupiter are marked by their initials.
Paper: TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star 
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, J. M. Joel Ong, 加冕 王, Kevin C. Schlaufman, Daniel Hey, Yaguang Li, 亚光 李, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, Samuel N. Quinn, Samuel W. Yee, Rafael Brahm, Trifon Trifonov, Andrés Jordán, Thomas Henning, David K. Sing, Meredith MacGregor, Catherine A. Clark, Colin Littlefield, Sarah Deveny, Steve B. Howell, Emma Page, David Rapetti, Ben Falk, Alan M. Levine, Chelsea X. Huang, Michael B. Lund, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Joint posterior distributions from our isochrone grid modeling of TOI-7041.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: A summary of different problems in astronomy that can be solved with different machine learning techniques. Each example is illustrated with an example Uniform Manifold Approximation and Projection (UMAP) plot (see Section 4.4), which is a low-dimensional embedding of a high-dimensional data space where each point represents a different image or sample in the dataset.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Examples of sources with their human-assigned score. Each image has been normalized using an asinh scaling with a threshold at 90% of the maximum brightness to highlight faint features. The beam size for each image (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is indicated with a bar in the lower left.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: High-level flowchart of the full methodology with references to relevant Sections. The section of the flowchart indicated by “a” outlines the procedure for extracting features from the raw data and is further expanded in Figure 3. After feature extraction, the analysis is divided in two, making use of a fully labeled subset of the data to evaluate performance and optimize algorithm hyperparameters and subsequently applying the methodology to the full dataset to locate and follow up high-scoring sources. In both cases, PROTEGE is used with the same settings and is described in more detail in Figure 8.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Comparison between the two lead authors’ scoring for a random sample of 100 sources. The error bars represent the standard deviation of author L.R.’s scores for a given value of M.L.’s scores.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Examples of sources author L.R. scored high while M.L. scored low. The images have been normalized with asinh scaling.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Flowchart of the preprocessing and feature extraction process.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Spectral index for source 237 (left) and 255 (right), only including pixels with flux density at least 10 times higher than the rms for the image (4.00 μJy beam−1 and 7.36 μJy beam−1, respectively) and for which σα/α < 0.2. The spectral index is estimated in-band using least-squares fitting applied to the 12 sub-band images. Contours are drawn at five evenly spaced flux density levels between the minimum and the maximum flux, with background sources excluded.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Highest-ranked sources according to PROTEGE. Images have been normalized using an asinh scaling with a threshold at 90%, and the beam size (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is indicated with a bar in the lower left. Known sources that have published Figures from K. Knowles et al. (2022) and related literature are highlighted with a yellow border, while new recommendations discussed in the text have a red border.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: X-shaped radio galaxies scored highly by PROTEGE. The flux density in these images is truncated to 99% of maximum for the left and right images and 95% for the central image, to highlight faint features. The potential host, where one is identified, is shown as a white circle, and the synthesized beam (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is shown as a gray circle in the lower left of each image.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Sources detected by PROTEGE that are similar to odd radio circles (ORCs). Source 37 (left) is SAURON, and source 146 (middle) is a morphologically similar source discovered by PROTEGE. While not a candidate ORC, source 3 (right) is an unusually rounded source. The flux density in these images is truncated to 99% of maximum to highlight faint features, and the potential host galaxy (where identified) is indicated with a white circle. The synthesized beam (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is shown as a gray circle in the lower left of each image.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: A zoomed-out image of source 3 revealing it as the likely lobe of a large (possibly giant) radio galaxy. The flux density in this image is truncated to 99% of maximum to highlight faint features, and the synthesized beam (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is shown as a gray circle in the lower left.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: Flowchart describing the original approach taken in M. Lochner & B. A. Bassett (2021) as applied to the MGCLS data. In contrast to the method described in the main text, features are extracted by fitting ellipses to isophotes (contours of constant brightness), and the standard machine learning algorithm isolation forest is used to indicate anomalies. The active learning process to refine the anomaly scores is a reweighting by combining the isolation forest score, predicted human labels, and an uncertainty penalty term. The process is fundamentally different to PROTEGE, which is trained to focus on regions of interest rather than first filtering through an anomaly detection algorithm.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: UMAP plot of the BYOL features for the full dataset, colored by the predicted score from PROTEGE. Candidate XRGs (source 237, 255, and 110) and unusually circular sources (37, 146, and 3) are highlighted. The remarkable diversity even within a single “class” of “interesting” source type is reflected by the large distance between them in feature space. Nonetheless, they all lie in regions of interest to PROTEGE.
Paper: Astronomaly Protege: Discovery through Human-machine Collaboration
Authors: Michelle Lochner, Lawrence Rudnick
Figure caption: A random sample of sources from the full dataset. Images have been normalized using an asinh scaling with a threshold at 90%, and the beam size (∼7﹩\mathop{.}\limits^{^{\prime\prime} }﹩6) is indicated with a bar in the lower left.
Paper: JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-776 b
Authors: Lili Alderson, Sarah E. Moran, Nicole L. Wallack, Natasha E. Batalha, Nicholas F. Wogan, Anne Dattilo, Hannah R. Wakeford, Jea Adams Redai, Munazza K. Alam, Artyom Aguichine, Natalie M. Batalha, Anna Gagnebin, Peter Gao, James Kirk, Mercedes López-Morales, Annabella Meech, Johanna Teske, Angie Wolfgang
Figure caption: Forward model fits to the ExoTiC-JEDI (top, pink shades) and Eureka! (bottom, blue shades) transmission spectra for Visits 1 (left) and 2 (right), accounting for the offset in Visit 2 (see Section 5.1). Note the differing y-axis limits between visits due to differing baselines (see Table 3). We show models from 100 to 1000×  solar metallicity for each visit with a putative 1-bar opaque pressure. The χ2/N and confidence (in σ) by which we can rule out each model are listed next to each model. There are slight differences in the model limits achieved between the ExoTiC-JEDI and Eureka! reductions, with the Eureka! reduction able to rule out higher metallicities in both visits.
Paper: Ground-based Reconnaissance Observations of 21 Exoplanet Atmospheres with the Exoplanet Transmission Spectroscopy Imager
Authors: Ryan J. Oelkers, Luke M. Schmidt, Erika Cook, Mary Anne Limbach, D. L. DePoy, J. L. Marshall, Jimmy Ardoin, Mitchell Barry, Evan Batteas, Alexandra Boone, Brant Conway, Silvana Delgado Adrande, John D. Dixon, Enrique Gonzalez-Vega, Alexandra Guajardo, Landon Holcomb, Christian Lambert, Shravan Menon, Divya Mishra, Jacob Purcell, Zachary Reed, Nathan Sala, Noah Siebersma, Nhu Ngoc Ton, Raenessa M. L. Walker, Z. Franklin Wang, Kaitlin Webber
Figure caption: A visual comparison of transmission spectra measured for various planets during transit (red points) and out of transit (black points). The p-value of the Anderson–Darling test comparing the two measurements is shown in the title of each subfigure. The out-of-transit measurements were generated via 1000 bootstrap simulations where the white-light transit signal (see Table 3) was injected at various times of midtransit and measured the same way as the in-transit data. The top row of planets have a calculated p-value of p < 0.05 indicating the in-transit and out-of-transit data are statistically different from one another. The bottom row of planets have p-values of p > 0.05 indicating they are not statistically dissimilar to the bootstrap simulations. For these planets we additionally compared previous measurements from the Exoplanet Archive with a flat line using the R2 metric. We find the previous measurements all have an R2 < 0.54, which suggests the atmospheric signal is likely consistent with a flat line and the consistency between the in-transit and out-of-transit observations may be because the spectrum is naturally featureless.
Paper: JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-776 b
Authors: Lili Alderson, Sarah E. Moran, Nicole L. Wallack, Natasha E. Batalha, Nicholas F. Wogan, Anne Dattilo, Hannah R. Wakeford, Jea Adams Redai, Munazza K. Alam, Artyom Aguichine, Natalie M. Batalha, Anna Gagnebin, Peter Gao, James Kirk, Mercedes López-Morales, Annabella Meech, Johanna Teske, Angie Wolfgang
Figure caption: Allowed parameter space in terms of opaque pressure level (either a cloud-top or surface pressure, bars) vs. log metallicity for the ExoTiC-JEDI (top, pink shades) and Eureka! (middle, blue shades) reductions for Visits 1 (left) and 2 (right). In all cases, we are able to rule out metallicities of at least 100×  solar (i.e., mean molecular weights of  ∼5.5) with an opaque pressure of 1 mbar by 3σ. The exact limits of each reduction and visit differ (see Table 4). Bottom: the 3σ limits for each reduction and each visit are shown on the same axis for better comparison.
Paper: Ground-based Reconnaissance Observations of 21 Exoplanet Atmospheres with the Exoplanet Transmission Spectroscopy Imager
Authors: Ryan J. Oelkers, Luke M. Schmidt, Erika Cook, Mary Anne Limbach, D. L. DePoy, J. L. Marshall, Jimmy Ardoin, Mitchell Barry, Evan Batteas, Alexandra Boone, Brant Conway, Silvana Delgado Adrande, John D. Dixon, Enrique Gonzalez-Vega, Alexandra Guajardo, Landon Holcomb, Christian Lambert, Shravan Menon, Divya Mishra, Jacob Purcell, Zachary Reed, Nathan Sala, Noah Siebersma, Nhu Ngoc Ton, Raenessa M. L. Walker, Z. Franklin Wang, Kaitlin Webber
Figure caption: A comparison of the brightnesses of transiting hot Jupiters and their transit depths for a sample of hot Jupiters observable from McDonald Observatory (δ > −15°) with an orbital period of P < 15 days, and a mass of M > 0.05 MJ (black points). The sample observed as part of this work is shown with red points. Data with diamond shapes represent targets with previous transmission measurements. The majority of the observed targets in this survey have the largest transit depths for their magnitudes. Objects selected in the middle of the distribution typically have previous transmission measurements, allowing for comparison.