adsabs/AstroCLIMB huggingface dataset:
Paper: A Photometric Redshift Catalogue of Galaxies from the DESI Legacy Imaging Surveys DR10
Authors: Changhua Li, Yanxia Zhang, Chenzhou Cui, Shirui Wei, Jingyi Zhang, Yongheng Zhao, Xue-Bing Wu, Yihan Tao, Shanshan Li, Youfen Wang, Zihan Kang
Figure caption: Accuracy and F1 as a function of ratio in SMOTE. The red line represents F1 for the high-redshift subsample while the green-dashed line represents F1 for the low-redshift subsample.
Paper: A Photometric Redshift Catalogue of Galaxies from the DESI Legacy Imaging Surveys DR10
Authors: Changhua Li, Yanxia Zhang, Chenzhou Cui, Shirui Wei, Jingyi Zhang, Yongheng Zhao, Xue-Bing Wu, Yihan Tao, Shanshan Li, Youfen Wang, Zihan Kang
Figure caption: The scatter figure of estimated photometric redshifts vs. spectroscopic redshifts and Δz(norm) distribution for the KST sample by the optimal model group.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: The uncertainty map derived for the α Cyg PSF-subtracted Vega image. The uncertainty was computed by measuring the pixel-wise standard deviation for the full stack of de-rotated PSF-subtracted images to estimate temporal variations. This standard deviation map was then replicated and rotated to match the azimuthal coverage of the Vega data set. Multiple rotations coupled with several point sources in the Vega FOV lead to azimuthally symmetric artifacts.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Radial profiles for each of the 32 orbits in this program prior to PSF subtraction. Vega orbits are displayed in blue and α Cyg orbits are shown in red. We display a percent difference from the median α Cyg orbit to highlight the features. Color-mismatch effects are apparent inside of ∼5″, while a broad peak in the Vega orbits is visible out to 30″. The top panel uses a uniform scale factor for the α Cyg orbits to illustrate the variability. The middle panel corrects for the variability by normalizing to orbit 63, while the bottom panel inflates these scale factors by 1%.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Here we present the final cRDI PSF-subtracted image using ζ Aql as the science target and α Cyg as the reference PSF. Left: the cRDI-subtracted image shown on a linear scale. Middle: the uncertainty map generated using the same technique as shown in Figure 12 shown on a logarithmic scale. Right: the S/N map for this reduction. In all cases, the images are rotated north up. The PSF-subtracted image shows strong negative residuals inside of 10″, consistent with the minor color mismatch between ζ Aql α Cyg. The S/N map shows no detection of extended signal outside of this region.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: The impact of the relative scaling between the α Cyg and Vega orbits on the final reduction. The left panel shows the α Cyg − Vega reduction using the variability-corrected α Cyg orbit scale factors (equivalent to the middle panel of Figure 8). The right panel shows the α Cyg − Vega reduction assuming a 1% increase in the α Cyg scale factors, showing a strong oversubtraction in the central region. The middle panel represents a 0.5% increase to the variability-corrected α Cyg scale factors and is equivalent to the right panel of Figure 2. In all cases the disk is visible outside of ∼10″, though the integrated flux is impacted.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: The radial profile of a quick image subtraction of HD 88981 – HD 141653 shown on a log–log scale. For each target, all images obtained at the STIS WEDGEA1.0 position were median combined, normalized to the peak, and centered using the diffraction spikes prior to subtraction. The observations show the close-in features characteristic of a color-mismatched PSF: a strong negative ring close to the inner working angle, followed by a positive “corona” with a negative power-law slope of ∼3 (black dashed line). Outside of 10″, no evidence for color-induced PSF subtraction artifacts exists, however this may be a sensitivity limitation.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: The 3σ median absolute deviation (MAD) contrast for the Vega − α Cyg reduction (purple). The 32 orbits of the science target, Vega, enable among the lowest achieved MAD contrasts to date. Image sensitivities are shown on the left. For comparison, we also include the image sensitivities associated with the radial profile of the empirically estimated uncertainty map for the Vega − α Cyg reduction shown in Figure 12 (green).
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Here we show the radial profile for each of the 25 median-averaged Vega orbits divided by the median radial profile. This provides a color-independent estimation of the impacts of breathing on these observations. The telescope PSF appears stable over the ∼year of observations. Inside of 30″, variations between orbits are <1%, with no clear curvature that could mimic a scattered-light dust halo.
Paper: Deep Search for a Scattered Light Dust Halo Around Vega with the Hubble Space Telescope
Authors: Schuyler G. Wolff, András Gáspár, George H. Rieke, Jarron M. Leisenring, Kate Su, David J. Wilner, Luca Matrà, Marie Ygouf, Nicholas P. Ballering
Figure caption: Cumulative pixel counts for the Vega − α Cyg reduction. There is generous coverage inside of 30″.
Paper: A Submillisecond Fourier and Wavelet-based Model to Extract Variable Candidates from the NEOWISE Single-exposure Database
Authors: Matthew Paz
Figure caption: Sample of synthetically generated light curves. Rows 1–2 are null stars and rows 3–4 are novae. Light curves in row 5 are pulsators, with their phase-folded waveforms directly below in row 6. Row 7 is transits, with their phase-folded counterparts directly below.
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: Panel (a)—The splicing proved to be the most unreliable step of the fusion process. Failure modes included divots, misalignments, and hotspots. A good splice is shown at the bottom of this panel. Panel (b)—One cassette of a splice box. The cassette holds 50 fibers and ensures the spliced area remains straight while guaranteeing that the minimum bend radius of the extra fiber is not violated. The spliced area is held between two pieces of foam to reduce stress.
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: The panel on the left shows the first petal loaded onto the sled prior to insertion. The sled ensures that the petal is well aligned before it is inserted in order to reduce the risk of damage to the fiber positioners. The panel in the middle shows the back of the focal plane with 8/10 petals installed. The panel on the right shows the cable management structure that ensured that the bend radius of the cables would not be exceeded and that each cable could be moved without affecting any other cable.
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: Final measurements of all 5000 fibers in the fully integrated fiber system prior to shipment to Kitt Peak. The FRD performance had a median value of 2° FWHM for f/3.9 input, and the absolute throughput, including these contributions, was measured as 91.1%, meeting the requirement imposed by DESI.
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: Slit metrology for one of the slit assemblies. The three histograms show the measured focus residual in z (determined by block position on the datum pins and AR window glue layer thickness), the gaps between fibers (determined by the V-groove spacing), and the interblock spacing (determined by the plate bonding spacer wire). For this assembly, the mean fiber spacing was 229.5 ± 2.3 μm (meeting the requirement of 230+−10), and the mean block spacing was 570.8 ± 20.0 μm (meeting the requirement of 556+−50).
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: The fibers at the focal plane are routed to different areas on the spectrograph for each petal. This randomized mapping allows analyses to break degeneracies between effects that are correlated on the focal plane vs. effects that are correlated on the spectrograph slit (and thus on the spectrograph CCDs). The mapping has the following distribution of fibers on the focal plane, color coded by fiber location on the slithead (first column on the detector = dark blue through last column on the detector = dark red).
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: Panel (a)—The petalbot is used to inject a collimated beam mounted on motorized x–y stages into focal plane fibers. Panel (b)—The slitbot has two cameras mounted on motorized stages that follow the curve of the spectrograph slit. One camera is used to determine the mapping between the focal plane and the slit. The second camera is used to measure the FRD performance of the fiber.
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: The wire-eroded datum jig is removed, and the paper target is exchanged for a three-axis stage carrying a microscope and camera. The camera scans the slit determining the x and y locations of the illuminated fiber output faces, as well as their focus in z, using centroiding and image sharpness algorithms. Each scan is repeated several times and takes around 4 hr to complete.
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: The fiber cables and slits were stored on their shipping carts during the focal plane installation and handled by an expert team of NOIRlab engineers during cable routing. The middle and right panels show the NOIRLab team, each person managing one fiber cable and spectrograph spool box with slitheads as the fiber cables are installed to the telescope.
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: Panel (a) shows a schematic of the custom, ergonomic splicing station. Panel (b) shows the custom ergonomic splicing station in use during production.
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: Position of the CRIRES+ slit at one nodding position and wavelength-averaged PSF along the slit in one order (2.32–2.34 μm) of the CRIRES+ observations. The red box in the upper panel marks the slit position aligning the two YSES 1 companions. The background SPHERE image is adapted from A. J. Bohn et al. (2020b). In the lower panel, the in-slit light from the primary is largely reduced because of the slit offset from the stellar center.
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: Stellar background removal around the spectral trace of YSES 1 b. The upper and lower panels show the cuts of a single order on the detector image before and after removing stellar backgrounds using polynomials.
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: We show a sample of planets with host star T eff < 7200 K, and planetary radii between 8 and 15 R ⊕. In (a) and (b), we highlight systems with T eff < 4300 K to focus on the cooler host stars. In all these plots, the systems discovered as part of the Searching for GEMS are circled in red, while the TOIs confirmed here with triangles in green (upright for TOIs with mass measurements) and purple (inverted for TOIs with mass upper limits).
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-5616. (Top right) Phase-folded RVs. (Bottom) The phase-folded light curves. The plot styling and definitions are similar to Figure 1.