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: Left: total redshift success rate (the number of good redshift measurements divided by the number of ELG targets) as a function of the distance of the fiber to the focal center. The filled circles represent the results without any correction, and the error bars demonstrate there is a 3σ difference in success rate for fibers close to the center and those in the outskirts. The shaded region is the weight-corrected success rate. Right: per fiber ELG success rate for both the Berkeley Automated Supernova Search/MzLS survey and DECals survey after the correction for the focal plane location (normalized to one).
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 1.
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: Spectroscopic redshift distribution for different data sets: (a) the WISE and SDSS data set; (b) the WISE and SkyMapper data set with galaxies, quasars, and stars.
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 fiber can be seen bowing out of the edge of the positioner. This is due to the ferrule being fixed into the ferrule arm and the Hytrel tubing adding electrostatic stickiness on the fiber and causing it to be pushed, inchworm style, into the positioner. This issue was remedied by shortening the amount of Hytrel tubing on the fiber.
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: Contrast learning model architecture. Three loss functions are used to optimize the mode conversion and the final photo-z mixture density network for pdf estimation. (L1 loss: contrast loss; L2 loss: adversary loss; L3 loss: CRPS loss.)
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: Comparison of retrieval results of alternative models for YSES 1 b. Blue represents the baseline model, orange shows the enforced (optically thick) cloud model, green represents the model with veiling effect, and gray is the model with GPs accounting for correlated noise. The upper right-hand panel shows the retrieved T–P profiles. Different color saturations indicate the envelopes of 1σ, 2σ, and 3σ intervels. The red dashed line is the self-consistent T–P profile (T eff = 1900 K,log g = 4.0) from the Sonora Bobcat model grid. The dotted curve shows the flux-weighted emission contribution of each model. The corner plots show the posteriors of free parameters, including surface gravity, C/O ratio, metallicity, vertical mixing parameter, settling parameter, mass fraction of clouds at the cloud base, and carbon isotope ratio. We note the correlation between surface gravity and metallicity, while C/O and 12CO/13CO are less model dependent.
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: Detection of 13CO and HF molecules in CRIRES+ observations of YSES 1 b. The top three panels show the 2.32-2.37 μm observational residuals, where the main H2O and 12CO spectral features have been removed from the data. The best-fit 13CO and HF model spectra are overplotted in red and blue lines, demonstrating the detection of individual lines in the data. The bottom panels display CCFs of observational residuals with 13CO and HF models. The gray dashed line is each molecular model’s ACF.
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: One spectral order of CRIRES+ observations of YSES 1 b from 2.32 to 2.37 μm. The observations are shown in black data points with error bars. Overplotted is the best-fit model obtained with retrieval analyzes. We annotated the positions of absorption features from H2O and CO with short bars on the top of each panel. The observational residuals (data minus model) are shown with scattered dots in gray.
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: Posterior distribution of retrieved parameters for YSES 1 c, including surface gravity, effective temperature, C/O ratio, metallicity, and quenching pressure. The vertical dashed lines denote the medium and 1σ intervals. The upper right-hand panel shows the retrieved 1σ, 2σ, and 3σ envelope of the T–P profile. The dotted line is the flux-weighted emission contribution. The dashed line is the condensation curve of MgSiO3 clouds, located below the region of the main emission contribution.
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: Comparison of the CRIRES+ (orange) and SINFONI (blue) data and retrieval results on YSES 1 b. The left-hand and middle panels show the posteriors of the T–P profile, C/O, and 12CO/13CO ratios. The right-hand panel compares the observational residuals of the SINFONI data and the down-convolved CRIRES+ data in solid lines and their best-fit 13CO models in dashed lines. The two bottom panels show the observational residuals of the CRIRES+ data, like in Figure 4, overplotted with the retrieved best-fit 13CO models from both CRIRES+ (orange) and SINFONI (blue) data.
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: Spectral analysis of the YSES 1 primary to retrieve the stellar carbon isotope ratio. Left-hand panels show a portion of the CRIRES+ spectra in black, the best-fit PHOENIX stellar model in orange, and the residuals in gray (with an offset by 0.5). The right-hand panel shows the posterior distribution of the retrieved 12CO/13CO ratio, disk temperature T  d , and the veiling amplitude r 0.
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: Rotation velocities (assuming isotropic inclination distribution) as a fraction of break-up velocities for super-Jovian companions. Our measurements of YSES 1 b and c are denoted with red diamonds. The measurements of other companions are adopted from the literature, including M. L. Bryan et al. (2020b), J. J. Wang et al. (2021), and. W. Xuan et al. (2024a). The data are color-coded by the companion masses. The blue data points show the spin of Jupiter and Saturn in the solar system.
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: Cross-correlation detection of H2O and CO in CRIRES+ observations of YSES 1 c. The detection S/N of H2O, CO, and combined models are 7, 4, and 7.8, respectively. The gray dashed line shows the ACF of each molecular template.
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: RV and ﹩v\sin i﹩ of the primary YSES 1 and its companions b and c as constrained by CRIRES+ observations. The vertical dashed lines represent the median and 1σ values of the posterior distribution.
Paper: Potential Chromospheric Evaporation in the M Dwarf’s Flare Triggered by Einstein Probe Mission
Authors: J. Wang, X. Mao, C. Gao, H. Y. Liu, H. L. Li, H. W. Pan, C. Wu, Y. Liu, G. W. Li, L. P. Xin, S. Jin, D. W. Xu, E. W. Liang, W. M. Yuan, J. Y. Wei
Figure caption: Panel left: differential profile sequence of the Hα emission-line (the solid lines) sorted with time from top to bottom, along with the line profile obtained from the quiescent spectrum (the dashed line). See main text for the details of the generation of the differential line profile. The spectra are shifted vertically by an arbitrary amount for clarity. Panels right: modeling of the Hα differential profile by a linear combination of two Gaussian functions. The modeled local continuum has already been removed from the original differential spectrum. In each panel, the observed and modeled line profiles are plotted by the black and red solid lines, respectively. Each Gaussian function is shown by a dashed line. The curves underneath each line spectrum present the residuals between the observed and modeled profiles.
Paper: Potential Chromospheric Evaporation in the M Dwarf’s Flare Triggered by Einstein Probe Mission
Authors: J. Wang, X. Mao, C. Gao, H. Y. Liu, H. L. Li, H. W. Pan, C. Wu, Y. Liu, G. W. Li, L. P. Xin, S. Jin, D. W. Xu, E. W. Liang, W. M. Yuan, J. Y. Wei
Figure caption: Multiband light curves of 2MASS J12184187−0609123 obtained in 2024, May 7th. The two black downward arrows mark the start and end of our time-resolved spectroscopic monitors. The vertical dashed line shows the trigger time of the corresponding X-ray transient triggered by the EP/WXT. Inset panel: Modeling of the late r-band light curve by an exponential decay. See the main text for the details.
Paper: Potential Chromospheric Evaporation in the M Dwarf’s Flare Triggered by Einstein Probe Mission
Authors: J. Wang, X. Mao, C. Gao, H. Y. Liu, H. L. Li, H. W. Pan, C. Wu, Y. Liu, G. W. Li, L. P. Xin, S. Jin, D. W. Xu, E. W. Liang, W. M. Yuan, J. Y. Wei
Figure caption: The X-ray light curves and temporal evolution of the spectral parameters measured from the X-ray spectra of the two transients detected by EP/WXT. The top panel shows the light curves in 0.5–4.0 KeV. The middle and bottom panels present the temporal variations of temperature and emission measure of the plasma component, respectively. All the errors plotted in the figure are at a significance level of 1σ.
Paper: Potential Chromospheric Evaporation in the M Dwarf’s Flare Triggered by Einstein Probe Mission
Authors: J. Wang, X. Mao, C. Gao, H. Y. Liu, H. L. Li, H. W. Pan, C. Wu, Y. Liu, G. W. Li, L. P. Xin, S. Jin, D. W. Xu, E. W. Liang, W. M. Yuan, J. Y. Wei
Figure caption: An illustration of the modeling for the X-ray light curves of the Flare 1 (left panel) and Flare 2 (right panel). The best-fit exponential decay models are over plotted by the red solid lines in both panels. The black dashed lines mark the corresponding quiescent flux determined from the eROSITA survey.
Paper: Potential Chromospheric Evaporation in the M Dwarf’s Flare Triggered by Einstein Probe Mission
Authors: J. Wang, X. Mao, C. Gao, H. Y. Liu, H. L. Li, H. W. Pan, C. Wu, Y. Liu, G. W. Li, L. P. Xin, S. Jin, D. W. Xu, E. W. Liang, W. M. Yuan, J. Y. Wei
Figure caption: Illustration for the fitting of the X-ray spectrum of Flare 2 observed at 2024-05-07UT08:14:10 with the apec model. The bottom panel underneath the spectrum shows the deviations.
Paper: A Radio Technosignature Search of TRAPPIST-1 with the Allen Telescope Array
Authors: Nick Tusay, Sofia Z. Sheikh, Evan L. Sneed, Wael Farah, Alexander W. Pollak, Luigi F. Cruz, Andrew Siemion, David R. DeBoer, Jason T. Wright
Figure caption: Frequency coverage (x-axis) by day (y-axis) of the TRAPPIST-1 system observations using the ATA at HCRO in fall 2022. The standard radio frequency bands are shaded in the background and labeled. These observations covered a continuous 0.9–9.3 GHz in radio frequency, over two weeks in 2022 October–November.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Expectations for WASP-121 b’s atmosphere via solar composition 1D-RCTE. Left: output high-resolution spectra from the solar composition 1D-RCTE model as described in Section 3, in units of stellar contrast. A model spectrum with all expected opacity sources over the IGRINS wavelength range is shown in black, while the colored spectra contain subsets of gases. Right: the output vertical thermal structure and gas VMRs as predicted by the 1D-RCTE model. Also shown is the wavelength integrated contribution function (blue shading), indicating which pressures IGRINS is most sensitive to. These pressures include thermal dissociation of several O-bearing molecules and ionization of atomic gases, indicating WASP-121 b may have muted spectral features. As these gases dissociate, much of the total O inventory transfers to atomic O, which does not have any spectral features IGRINS is sensitive to. This can challenge efforts to estimate the total volatile inventory of UHJs (see, e.g., M. Brogi et al. 2023).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios
Authors: Peter C. B. Smith, Jorge A. Sanchez, Michael R. Line, Emily Rauscher, Megan Weiner Mansfield, Eliza M.-R. Kempton, Arjun Savel, Joost P. Wardenier, Lorenzo Pino, Jacob L. Bean, Hayley Beltz, Vatsal Panwar, Matteo Brogi, Isaac Malsky, Jonathan Fortney, Jean-Michel Désert, Stefan Pelletier, Vivien Parmentier, Sai Krishna Teja Kanumalla, Luis Welbanks, Michael Meyer, John Monnier
Figure caption: Top: to-scale schematic of the WASP-121 system from a top down perspective. Bottom: observing conditions during each of the two sequences.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Invisible cloud detected with our all-sky image from PASO (left) and the corresponding cloud mask obtained with CLOWN (right). The telescope would still operate under these conditions, as it does not reach 75% blocked sky.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: All-sky image taken from the OPD with cloudy conditions (LNA 2022; left) and corresponding cloud mask obtained with CLOWN (right).
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Visible cloud detected with our all-sky image from PASO (left) and corresponding cloud mask obtained with CLOWN (right).
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Clear-sky image obtained with our all-sky image from PASO (left) and corresponding cloud mask obtained with CLOWN (right).
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: In these images we can see a theoretical planned one-night survey in the optical telescope where the rectangles indicate the observing areas of 6.°9 × 6.°9 corresponding to the telescope FoV of 2.°3 × 2.°3 plus 1 FoV of margin. Yellow and dark blue boundaries reveal areas with and without clouds, respectively. This information is then passed onto the telescope, enabling it to point to a cloudless area. Right and left images show the change in cloud conditions within a 5 minute interval.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: ZenithPointCalculator.py illustration. The zenith point is drawn in the center and the coordinates given in the AltAz file are drawn, so the user can visually see if the correspondence is correct or what error might be causing the mismatch.
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Graphical representation of the image (top left), detected objects, expected stars and matched stars (top right), the output of the first analysis step (bottom left), and final output (bottom right).
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: Different projections and respective linear approximations (left) and the percentage error (right).
Paper:  CLOWN: The PASO Cloud Detection for Optimization of Automatic Optical Surveys
Authors: Luís Gonçalves, Bruno Coelho, Domingos Barbosa, Miguel Bergano, Vitor Bonifácio, Dalmiro Maia
Figure caption: CheckPoint.py illustration: showing the area being checked.
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 cumulative distribution ﹩\hat{F}(c)﹩ of threshold credible intervals for the whole sample, r ≥ 21.5 subsample and r < 21.5 subsample of the KST sample. The left-hand panel shows the data before uncertainty calibration, while the right-hand panel shows the data after calibration.
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 z phot vs. z spec and Δz(norm) distribution by EAZY for the KST (Q  z  < 1) sample. In the left-hand panel, the red dashed line represents Δz(norm) = ± 0.3 separately. In the right-hand panel, red line shows the real distribution, green dotted line is the Gaussian distribution.
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 workflow of photometric redshift estimation.
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:  σ NMAD, MSE, O as a function of r magnitude and spectroscopic redshift for the KST sample.
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 the Δz(norm) distribution by CatBoost.