adsabs/AstroCLIMB huggingface dataset:
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: A spectrograph spool box tray populated with bare looped fiber. A clear Perspex lid is installed, which allows the fiber technician to ensure that all fibers are able to move freely inside the cassette before building the next bundle.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: Left: a sintered Nylon part can be placed around the AR window and held in place with screws. Fine-threaded screws adjust the six fingers on this jig. Right: adjusting the finger positions (and retains during the slow curing process), the window in place in x, y, and tilt.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: A polished V-block is held upright beneath the digital microscope using a 3D-printed vacuum jig. Strain relief for the PTFE fiber bundles and Venturi pump air line is provided. Six fingers adjusted with fine-thread screws can place (and, crucially, retain during the epoxy cure time) the AR-coated window.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: V-blocks are held in place by a vacuum. The cover lid is positioned and retained with two removable arms. Fibers are inserted into the V-grooves beneath the cover lid. Double-sided adhesive tape restrains the fibers. The vacuum can be terminated, and the PTFE brace and cover lid arms removed once the block is bonded and cured.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: A bare fiber is inserted from the rear of the V-block into its respective V-block channel. The cover lid is held on top of the fibers. Once bonded, the front face of the block/fibers/lid is optically polished before an AR-coated window is attached.
Paper: Overview of the Fiber System for the Dark Energy Spectroscopic Instrument
Authors: Claire Poppett, Luke Tyas, J. Aguilar, Christopher Bebek, D. Bramall, T. Claybaugh, J. Edelstein, P. Fagrelius, H. Heetderks, P. Jelinsky, S. Jelinsky, Robin Lafever, A. Lambert, M. Lampton, Michael E. Levi, P. Martini, C. Rockosi, J. Schmoll, Ray M. Sharples, Martin Sirk, Edward Wishnow, Jiaxi Yu, S. Ahlen, A. Bault, S. BenZvi, D. Brooks, S. Cole, A. de la Macorra, Arjun Dey, P. Doel, K. Fanning, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, C. Hahn, K. Honscheid, J. Jimenez, S. Juneau, D. Kirkby, A. Kremin, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, J. Nie, G. Niz, N. Palanque-Delabrouille, W. J. Percival, F. Prada, D. Rabinowitz, M. Rezaie, G. Rossi, E. Sanchez, Edward F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B. A. Weaver, R. Zhou
Figure caption: A to-scale paper template is used to set the appropriate lengths for the bare and PTFE-clad fiber bundles. Each bundle had a unique length to conform to the “race track” slots of the slit assembly.
Paper: Photometric Redshift Estimation of Quasars by a Cross-modal Contrast Learning Method
Authors: Chen Zhang, Wenyu Wang, Meixia Qu, Bin Jiang, YanXia Zhang
Figure caption: The CRPS and PIT distribution plots corresponding to the seven experimental results in Table 2.
Paper: Photometric Redshift Estimation of Quasars by a Cross-modal Contrast Learning Method
Authors: Chen Zhang, Wenyu Wang, Meixia Qu, Bin Jiang, YanXia Zhang
Figure caption: Confusion matrix by means of our probabilistic model based on the WISE and SkyMapper data set.
Paper: Photometric Redshift Estimation of Quasars by a Cross-modal Contrast Learning Method
Authors: Chen Zhang, Wenyu Wang, Meixia Qu, Bin Jiang, YanXia Zhang
Figure caption: Photometric redshifts vs. spectroscopic redshifts with three different methods for the SDSS data set: (a) the result of our probabilistic model; (b) the result of D’Isant’s method; (c) the result of Yao’s method.
Paper: Photometric Redshift Estimation of Quasars by a Cross-modal Contrast Learning Method
Authors: Chen Zhang, Wenyu Wang, Meixia Qu, Bin Jiang, YanXia Zhang
Figure caption: Photometric redshifts vs. spectroscopic redshifts for three different methods on the WISE and SkyMapper data set: (a) the result of our probabilistic model; (b) the result of D’Isant’s method; (c) the result of Yao’s method.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: Posterior distributions for the Bond albedo A B and heat redistribution parameter ε (top row of the corner plots, as defined in Equation (7) and Equation (4) of N. B. Cowan & E. Agol 2011), which determine the dayside effective temperature for the 3.6 and 4.5 μm channels. The purple shaded regions show the range in Bond albedos predicted by the radiative-convective models described in Section 3.3. On the bottom row are the corresponding posterior distributions for the dayside temperature (as defined in Equation (7)).
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: The dayside temperatures T d vs. Bond albedos A B for HD 202772 A b in the 3.6 μm (light blue) and 4.5 μm (red). The purple shaded region is the range of Bond albedos calculated from the radiative-convective models described in Section 3.3, and listed in Table 4. Also plotted in green are the same quantities for other TESS-observed hot Jupiters, calculated from their Spitzer 4.5 μm phase curves as analyzed in T. J. Bell et al. (2021), listed in Table 8 of I. Wong et al. (2021). The calculated Bond albedos for HD 202772 A b are consistent with the generally flat behavior of close-in giants with dayside temperature, with the notable exception of HAT-P-7 b, whose negative albedo is due to it having a significantly brighter dayside than would be expected from purely thermal emission.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: Distributions of heat redistribution efficiency values (ε), as calculated from the nested sampling results, that fall within the range of Bond albedos derived from the effective temperatures of the 1D radiative-convective climate models. The values from the 3.6 μm channel are in light blue, and those from the 4.5 μm channel are in red. The two distributions are distinct, with a distribution for the 3.6 μm channel that suggests a heat redistribution much more even (i.e., much closer to 1) than that for the 4.5 μm channel, which suggests virtually no heat flow to the nightside.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: The rms residuals in our eclipse model fits to the data, as a function of the bin size used in the process described in Section 3.1. The solid line represents the residuals, and the dashed line represents the “ideal” expectation of pure photon noise (i.e., no correlated noise), which should follow a −1/2 slope in the log–log space of log bin size vs. rms residuals. For the 3.6 ﹩\mu ﹩m channel, a Gaussian process regression is added to the original (red) noise profile, yielding the result shown in black. The timescale of the radial basis function (﹩\tau \approx 29.7﹩ minutes ﹩=\,27.8﹩ bins in Equation 2) is shown as a vertical blue dashed line. One caveat of this approach is that the final fit suffers from some over-subtraction of noise at bin sizes longer than the timescale ﹩\tau ﹩, as the kernel function becomes undersampled.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: The T–P profile and emission contribution function calculated by the radiative-convective model described in Section 3.3, for the case of C/O = 2× solar, ﹩\left[\mathrm{Fe}/{\rm{H}}\right]=1﹩, which is nominally closest to the measured eclipse depths. However, our constraints on the albedo and heat redistribution efficiencies imply that the 3.6 μm eclipse data are not well described by a 1D dayside-only model that does not account for heat flow to the nightside.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: The setup and fits to the pixel-level decorrelation (PLD) technique used to reduce the Spitzer data for observations of HD 202772 A in the channel centered at 3.6 μm. The raw light curve is shown in black on the top two subplots, with the model fit from PLD in red. The green shaded region shows when we predict in time the planet will be in secondary eclipse. The lower two subplots show the residuals and detrended eclipse light curve after accounting for systematics via PLD. The data points in orange are binned to 30 minutes intervals, with the 68% confidence interval of the binned and detrended light curve in blue.
Paper: Modeling Spitzer 3.6 and 4.5 μm Eclipse Depths for the Inflated Hot Jupiter in the Evolved Binary System HD 202772
Authors: Arthur D. Adams, Kimberly Bott, Paul A. Dalba, Tara Fetherolf, Stephen R. Kane, Ian Crossfield, Drake Deming, Diana Dragomir, Varoujan Gorjian, Laura Kreidberg, Farisa Y. Morales, Michael W. Werner
Figure caption: The setup and fits to the PLD technique used to reduce the Spitzer data for observations of HD 202772 A in the channel centered at 4.5 μm. The raw light curve is shown in black on the top two subplots, with the model fit from PLD in red. The green shaded region shows when we predict in time the planet will be in secondary eclipse. The lower two subplots show the residuals and detrended eclipse light curve after accounting for systematics via PLD. The data points in orange are binned to 30 minutes intervals, with the 68% confidence interval of the binned and detrended light curve in blue.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: High-contrast imaging data for all targets. In each panel, we show the achieved 5σ contrast limit as a function of angular separation from the host star for each high-contrast data set. We also plot 1.″4 × 1.″4 postage stamps of the reconstructed ﹩z^{\prime} ﹩-band NESSI images (right-hand inset in each panel) for all targets and the AO images (left-hand insets) for TOI-5414, TOI-5616, and TOI-5634A and TOI-6034.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: (Top left) RV time series for K2-419A, where the dashed line denotes the planet model, whereas the blue line and shaded region depict the best model fit (and 16%–84% uncertainties) after including the RV offsets and trends. (Top right) RVs phase folded at the best-fit period, including the model and uncertainty. The gray error bars behind the points show the errors when including the RV jitter that is estimated during the joint fit. (Bottom) Phase-folded photometry for K2-419A, including TESS (shown in red), where the dilution term is allowed to float owing to its large pixel size. The model and uncertainties follow the usual definitions. The TESS and K2 data, (a), (b), (c), are shown after subtracting the median trend as estimated after masking the planet transits. We also include the representative median statistical uncertainty at −0.07 day.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: (Top left) RV time series for TOI-6034. (Top right) Phase-folded RVs. (Bottom) The phase-folded light curves. Note the varying TESS depths due to contamination. The plot styling and definitions are similar to Figure 1.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: ZTF photometry phase folded to the best-fit planetary ephemeris, where the model is shown with a black line, and the ZTF observations in red-filled triangles (ZTF r) and green-filled circles (ZTF g). Top: observations for TOI-6034. Bottom: observations for TOI-5616.
Paper: Searching for GEMS: Characterizing Six Giant Planets Around Cool Dwarfs
Authors: Shubham Kanodia, Arvind F. Gupta, Caleb I. Cañas, Lia Marta Bernabò, Varghese Reji, Te Han, Madison Brady, Andreas Seifahrt, William D. Cochran, Nidia Morrell, Ritvik Basant, Jacob Bean, Chad F. Bender, Zoë L. de Beurs, Allyson Bieryla, Alexina Birkholz, Nina Brown, Franklin Chapman, David R. Ciardi, Catherine A. Clark, Ethan G. Cotter, Scott A. Diddams, Samuel Halverson, Suzanne Hawley, Leslie Hebb, Rae Holcomb, Steve B. Howell, Henry A. Kobulnicky, Adam F. Kowalski, Alexander Larsen, Jessica Libby-Roberts, Andrea S. J. Lin, Michael B. Lund, Rafael Luque, Andrew Monson, Joe P. Ninan, Brock A. Parker, Nishka Patel, Michael Rodruck, Gabrielle Ross, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Aubrie Thoms, Andrew Vanderburg
Figure caption: (Top left) RV time series for TOI-5218. (Top right) Phase-folded RVs. (Bottom) The phase-folded light curves. The plot and definitions are similar to Figure 1.
Paper: The ESO SupJup Survey. III. Confirmation of 13CO in YSES 1 b and Atmospheric Detection of YSES 1 c with CRIRES+ 
Authors: Yapeng Zhang, Darío González Picos, Sam de Regt, Ignas A. G. Snellen, Siddharth Gandhi, Christian Ginski, Aurora Y. Kesseli, Rico Landman, Paul Mollière, Evert Nasedkin, Alejandro Sánchez-López, Tomas Stolker, Julie Inglis, Heather A. Knutson, Dimitri Mawet, Nicole Wallack, Jerry W. Xuan
Figure caption: CRIRES+ observations and best-fit model spectrum of YSES 1 c. The observations in gray are convolved with the rotational broadening kernel for better visualization. The typical uncertainties of the data are shown in gray error bars on the left-hand side. The planetary signal is buried in the noise in individual channels.
Paper: The ESO SupJup Survey. III. Confirmation of 13CO in YSES 1 b and Atmospheric Detection of YSES 1 c with CRIRES+ 
Authors: Yapeng Zhang, Darío González Picos, Sam de Regt, Ignas A. G. Snellen, Siddharth Gandhi, Christian Ginski, Aurora Y. Kesseli, Rico Landman, Paul Mollière, Evert Nasedkin, Alejandro Sánchez-López, Tomas Stolker, Julie Inglis, Heather A. Knutson, Dimitri Mawet, Nicole Wallack, Jerry W. Xuan
Figure caption: Similar as Figure 3 but for other spectral orders of CRIRES+ observations of YSES 1 b.
Paper: The ESO SupJup Survey. III. Confirmation of 13CO in YSES 1 b and Atmospheric Detection of YSES 1 c with CRIRES+ 
Authors: Yapeng Zhang, Darío González Picos, Sam de Regt, Ignas A. G. Snellen, Siddharth Gandhi, Christian Ginski, Aurora Y. Kesseli, Rico Landman, Paul Mollière, Evert Nasedkin, Alejandro Sánchez-López, Tomas Stolker, Julie Inglis, Heather A. Knutson, Dimitri Mawet, Nicole Wallack, Jerry W. Xuan
Figure caption: Figure 12 continued.