adsabs/AstroCLIMB huggingface dataset:
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Evolution of the WFE for JWST generated from WEBBPSF from 2022 October 1 to November 30. Top: the measured WFE for NIRCam Module A3 (NRCA3, yellow) is shown along with that of the general telescope facility (blue). Bottom: the EE of the F200W PSF in 0.″31 and 0.″08 apertures (green and purple, respectively) relative to the median. Relevant control and stability criteria are indicated. behavior during the four UNCOVER visits is effectively unchanged, with ΔEE ≲ 0.1%.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Photometry measured in this work based on corrected 0.″48 apertures compared to that of Paris et al. (2023) from 0.″42 apertures in the seven common HST bands and eight common JWST bands. Format follows that of Figure 13.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Photometry measured in this work based on corrected 0.″7 apertures compared to that of Kokorev et al. (2022) from the apertures of the same diameter in the seven common HST bands and two IRAC bands similar to those in NIRCam. Format follows that of Figure 13.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Photometry measured in this work based on corrected 0.″7 apertures compared to that of Shipley et al. (2018) from the apertures of the same diameter in the seven common HST bands and two IRAC bands similar to those in NIRCam. Format follows that of Figure 13.
Paper: The UNCOVER Survey: A First-look HST + JWST Catalog of 60,000 Galaxies near A2744 and beyond
Authors: John R. Weaver, Sam E. Cutler, Richard Pan, Katherine E. Whitaker, Ivo Labbé, Sedona H. Price, Rachel Bezanson, Gabriel Brammer, Danilo Marchesini, Joel Leja, Bingjie Wang, 冰洁 王, Lukas J. Furtak, Adi Zitrin, Hakim Atek, Iryna Chemerynska, Dan Coe, Pratika Dayal, Pieter van Dokkum, Robert Feldmann, Natascha M. Förster Schreiber, Marijn Franx, Seiji Fujimoto, Yoshinobu Fudamoto, Karl Glazebrook, Anna de Graaff, Jenny E. Greene, Stéphanie Juneau, Susan Kassin, Mariska Kriek, Gourav Khullar, Michael V. Maseda, Lamiya A. Mowla, Adam Muzzin, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, Camilla Pacifici, Casey Papovich, David J. Setton, Alice E. Shapley, Heath V. Shipley, Renske Smit, Mauro Stefanon, Edward N. Taylor, Andrea Weibel, Christina C. Williams
Figure caption: Distribution of z phot (teal) and z spec (purple) shown up to z = 15. The z phot values are derived from super catalog SEDs fit with EA z Y using the SFHz_CORR template set.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-275 (Kepler-129). Left: the best-fit models include one nontransiting planet, although the unusual time sampling is consistent with two different classes of model: either a near-circular, nontransiting giant planet (top) or a slightly longer period, eccentric giant planet with a substantial residual trend (middle). Right: periodograms after removing models of just the transiting planets (top) and a three-planet model in which the shorter, more circular period for the companion is favored (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-273 (Kepler-454). Left: the RVs were taken at Keck-HIRES (black circles) and TNG-HARPS-N (maroon triangles). The best-fit model includes two nontransiting planets, Kepler-454 c at 525 days and Kepler-454 d at 4500 days (see insets in phase-folded panels). Right: the top panel is a periodogram of the RVs after removing the transiting planets only, the middle panel is the periodogram after removing one nontransiting planet at 525 days, and the bottom panel is the periodogram after removing nontransiting planets at 525 and 4500 days.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-283 (Kepler-131). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-282 (Kepler-130). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-292 (Kepler-97). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-281 (Kepler-510). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-274 (Kepler-128). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-277 (Kepler-36). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-285 (Kepler-92). No nontransiting companions are detected.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Left: pie plot of the CMASS NGC data and the light cones of GADGET mock , and COLA  mock with (z init = 29,  da = 1/30), with a thickness of 4° (i.e., decl.  ∈  [28°, 32°]), with R.A.  ∈  [140°, 220°]). All shells represent z ∈ [0.45, 0.55], corresponding to a comoving distance range of r ∈ [1221.5, 1457.1], h −1 Mpc in the fiducial cosmology. Right: redshift slice of the COLA  mock (z init = 29,  da = 1/30) with a mean redshift of z mean = 0.5 and a bin width of Δz = 0.004 in the sky region of 165° < R.A. < 185° and 25° < decl. < 45°. Each side of this region approximately extends for 468 h −1 Mpc based on the fiducial cosmology. The gray points represent the full (sub)halos, and the red crosses (“×”) correspond to the mock galaxies selected using the SHAM procedures.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Contours of the correlation function ξ(r ⊥, r ∥) dependent on the separation parallel (r ∥) and perpendicular (r ⊥) to the LOS direction. The solid contours show the ξ(r ⊥, r ∥) of the CMASS NGC catalog in each panel. Left: comparison of ξ(r ⊥, r ∥) between the GADGET mock (dashed) and CMASS NGC (solid). Right: comparison of ξ(r ⊥, r ∥) between the COLA  mock with (z init = 49, da = 1/50, N step = 50) (dashed) and CMASS NGC (solid). The contours from the outside to the inside correspond to ξ = (0.25, 0.5, 1, 2, 4, 8). It can be observed that the 2PCF of the COLA catalog is very similar to that predicted by GADGET, and both of them are able to accurately reproduce the observational result.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Top panel: redshift-invariant complete SMF ϕ tot (dashed) as described in Section 2.3, along with the observed SMFs of the CMASS NGC catalog in three redshift bins (marked) denoted by ϕ NGC. Bottom panel: downsampling ratio f down for three redshift bins. This ratio is defined as the number density of observed galaxies in a given bin (ϕ NGC) divided by the number density of the full galaxy population (ϕ tot). Since observations are inherently incomplete, the observed catalog in each stellar mass bin represents a subset of the full galaxy population in the same sky region. Note that our analysis in this study specifically focuses on catalogs within the redshift range of 0.45 < z < 0.55 (solid blue).
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of halo mass functions (HMFs) of the simulated halos provided by GADGET and COLA simulations with different settings of (z init, da), respectively. The theoretical Press–Schechter mass function, labeled as PS, is also shown as a black dashed line in each panel. As observed, the HMF derived from COLA agree well with the theoretical prediction and that derived from GADGET. Furthermore, the results from different COLA parameter settings converge. In the low-mass region (M  h  ≲ 2 × 1012 h −1 M ⊙), the simulated HMFs in both and COLA begin to noticeably deviate from the theoretical predication. This deviation is due to the limitations of mass resolution in N-body simulations.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of the monopole of 2PCF for GADGET mock, CMASS NGC and COLA mock with different combinations of (z init, da). We observe a close match between ξ 0(s) of GADGET mock and CMASS NGC within the range of s ∈ [4, 20] h −1 Mpc. When z init is set to 29, 49, and 59, the resulting ξ 0(s) values of the COLA mocks all fall within the 2σ region, indicating a good match with CMASS NGC.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of the sky coverage. The area shaded in blue represents the sky coverage of CMASS NGC. For simplicity, we do not apply the angular selection of CMASS NGC to the mock catalogs (GADGET and COLA mocks) when estimating the two-point or three-point clustering. This means that the sky coverage of the mocks includes the entire region in red. However, when calculating the multipoles of the power spectrum (see Section 4.4), we do apply the angular selection of CMASS NGC to the mock catalogs.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: The χ 2 estimation defined by Equation (14), which is used to quantify the differences between mock catalogs and the observed CMASS NGC galaxies. We employ different COLA settings for comparison.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Distributions of Gaia objects and their APs. The left panel represents the H-R diagram of Gaia DR3 objects. The blue dashed lines provide preliminary bounds for our subsample of “cool dwarfs” based on the position of the vertical and horizontal blue lines at (1.3, 5). The middle panel plots the Kiel diagram (T eff vs. log g) based on parameters assigned using BP/RP spectra of the objects selected by the blue dashed lines in the left panel from Andrae et al. (2023), as well as PARSEC isochrones with an age of 6 Gyr and [M/H] of 0, −0.25, −0.5, and −1.0 dex. The right panel depicts the same Kiel diagram for objects with parameters based on RVS spectra from Recio-Blanco et al. (2023), along with the same isochrones used in the middle panel.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Color–magnitude diagram of Gaia stars and selected stars. Top: the background displays Gaia DR3 objects, while the training sample is plotted as gray contours with logarithmic scaling and fitted with a blue dashed line. The oblique black dashed lines are created by shifting the blue line up and down by 1.0 mag. The two horizontal black lines represent the absolute G magnitudes of 7 and 11 mag, respectively. Bottom: a zoom-in panel of the top panel with M  G  between 4 and 13 mag with the addition of Gaia sources with APs. The green points are the sources with APs from RVS spectra, while the magenta points are the objects with APs from BP/RP spectra that lie within the black dashed selection box.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Example spectra of HD 213893 shown from 0.4 to 5 μm. The top panel shows an optical spectrum observed by SDSS, with RSR lines in the u, g, r, i, and z bands plotted. The bottom panel shows the infrared spectrum from SpeX, which covers the J, H, K, W1, and W2 bands.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Source number comparison between Gaia cool dwarfs (in gray) and those with spectroscopic APs from LAMOST (in blue) for M  G  (top) and G (bottom) photometry.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Kiel diagram of our catalog: log g as a function of T eff color coded by [M/H]. The solid lines indicate PARSEC isochrones with an age of 6 Gyr and various [M/H]s. The left panel shows the H-R diagram of our catalog predicted by RF, plotting four isochrones with the age of 6 Gyr and [M/H] of 0, −0.25, −0.5, and −1.0 dex. The right panel indicates the H-R diagram of our catalog predicted by LGB, with the isochrones the same as in the left panel.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Comparison diagrams of the testing samples for the true and predicted values in terms of T eff (left), [M/H] (bottom), and log g (right). The top panels show the comparisons of the predicted values from RF and the true values, color coded by the number density of the test samples. The bottom panels indicate the difference between the predicted and true values, color coded by the photometric color error of W1 − W2 for T eff and log g and color J − H for [M/H].
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: The upper row shows density plots comparing APs of the LAMOST training sample with those from APOGEE. The histograms inside each plot show the difference between the two samples. The bias (μ) and scatter (σ) are annotated inside each panel. The bottom row shows histogram distributions for the T eff (left), [M/H] (middle), and log g (right) of our training sample.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: AP comparisons between APOGEE DR16 and the RF values for this work for T eff (top), [M/H] (middle), and log g (bottom). The difference histogram between this work and APOGEE is plotted inside each panel. The x-axis represents the residual, and the y-axis represents the number of occurrences.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Density distribution of the uncertainties of T eff (left), [M/H] (middle), and log g (right), along with the distance, color coded by spectra type. Here, the error of the APs is the dispersion of 100 predicted values by repeating modeling using 100 subtraining samples.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: Feature importance graph during model building for T eff (top), [M/H] (middle), and log g (bottom). The color is the feature value, the x-axis is the SHAP value, and the y-axis for each feature is ordered by their contribution to model construction.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: AP comparison between RF values from our work (yellow points) and DR3 APs from BP/RP spectra (gray points) in terms of log g and T eff.
Paper: Stellar Atmospheric Parameters for Cool Dwarfs in Gaia Data Release 3
Authors: Cai-Xia Qu, A-Li Luo, Rui Wang, Hugh R. A. Jones, Bing Du, Xiang-Lei Chen, You-Fen Wang
Figure caption: AP comparison of this work with RVS spectra in terms of log g and T eff. The yellow points represent this work, while the gray points depict RVS spectra.