adsabs/AstroCLIMB huggingface dataset:
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Left: the evolution of the observed number density at M UV = −20. The red circles show the observed number density at this absolute magnitude from CEERS (connected by the light-red shaded region; the small stars show the DPL fit values at this magnitude). The dark-blue region shows the measured value from Finkelstein & Bagley (2022), and the lighter-shaded region shows the extrapolation of the Finkelstein & Bagley (2022) results to higher redshift. While prelaunch expectations were that the number densities at z > 9 would either continue the observed trend at z = 3–9 or evolve more rapidly downward with increasing redshift, we find that the number density of bright galaxies surprisingly flattens at z > 9, where we measure a change in slope ﹩d\mathrm{log}\phi ﹩/dz between z < 9 and z > 9 at 2.1σ significance. Right: the evolution of the integrated specific UV luminosity density, obtained by integrating DPL fits to our observed luminosity functions to M UV = −17. The evolution here is less clear, with increased uncertainties (particularly at z ∼ 14, which is shown faded to represent its large uncertainty), making it less clear whether this quantity also has a flatter evolution at higher redshift.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Our measured UV luminosity functions at z ∼ 9, 11, and 14 are shown by the large symbols (circles for our CEERS results, and squares for NGDEEP from Leung et al. 2023). The shaded regions are the same as in Figure 9, showing the extrapolated UV luminosity functions from Finkelstein & Bagley (2022). The inset panel likewise shows the same ﹩{ \mathcal P }(z)﹩ curves from Figure 9, here plotted on the same scale. The thin curves show the median DPL fit to the data at each redshift. This figure highlights that brighter galaxies (M UV ≲ −20) have higher number densities than the extrapolated luminosity functions would predict. While there is a known overdensity at z ∼ 8.7 (Larson et al. 2022; Whitler et al. 2024) that could affect our lowest-redshift bin, there is no evidence for such overdensities at higher redshifts.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The evolution of the FUV color ﹩{{ \mathcal C }}_{\mathrm{FUV}}﹩ with redshift, color-coded by M UV. The large squares show median values in bins of redshift and magnitude (error bars show the 1σ spread), for bins with ≥5 sources. While reddened galaxies exist at z ∼ 7–8, the median colors are still fairly blue. Notably, the median FUV color for M UV = −20 galaxies is similar at z ∼ 8 to z ∼ 11, suggesting that a significant drop in dust attenuation is unlikely to explain the high abundance of bright z ∼ 11 galaxies.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Cutout images, 5″ on a side, of objects originally selected, but identified via visual inspection as being diffraction spikes.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Same as Figure 14, but for objects identified as oversplit portions of nearby brighter galaxies.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Same as Figure 14, but for objects identified as being associated with chip edges.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Same as Figure 14, but for objects identified as bad pixels.
Paper: The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5
Authors: Steven L. Finkelstein, Gene C. K. Leung, Micaela B. Bagley, Mark Dickinson, Henry C. Ferguson, Casey Papovich, Hollis B. Akins, Pablo Arrabal Haro, Romeel Davé, Avishai Dekel, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Nor Pirzkal, Rachel S. Somerville, L. Y. Aaron Yung, Ricardo O. Amorín, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Volker Bromm, Caitlin M. Casey, Óscar A. Chávez Ortiz, Yingjie Cheng, Katherine Chworowsky, Nikko J. Cleri, M. C. Cooper, Kelcey Davis, Alexander de la Vega, David Elbaz, Maximilien Franco, Adriano Fontana, Seiji Fujimoto, Mauro Giavalisco, Norman A. Grogin, Benne W. Holwerda, Marc Huertas-Company, Michaela Hirschmann, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Rebecca L. Larson, Ray A. Lucas, Bahram Mobasher, Alexa M. Morales, Caroline V. Morley, Sagnick Mukherjee, Pablo G. Pérez-González, Swara Ravindranath, Giulia Rodighiero, Melanie J. Rowland, Sandro Tacchella, Anthony J. Taylor, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Same as Figure 14, but for objects identified as being affected by bad photometry.
Paper: M17 MIR: A Massive Star Is Forming via Episodic Mass Accretion
Authors: Wei Zhou, 威 周, Zhiwei Chen, 志维 陈, Zhibo Jiang, 治波 江, Haoran Feng, 浩然 冯, Yu Jiang, 禹 蒋
Figure caption: (a) PV diagram of the CO J = 2–1 line emission along the outflow axis. The yellow vertical dashed lines indicate the velocity range 13–27 km s−1. The black horizontal dashed line denotes the position of M17 MIR on the slice. The red and blue solid curves represent the integrated intensity in the slice with 3″ width varying with the slice offset. The d represents the axial offset between the blue- and redshifted components of the N2 knot. The positions of the CO knots, from which the distances of the CO knots to the central source are measured, are marked by the black dots overlaid on the vertical black segments (the lengths of the CO knots). (b) Integrated intensity of the red- and blueshifted CO J = 2–1 emission with ∣V − V sys∣ > 7 km s−1 are displayed as the red and blue contours, respectively, overlaid on the ALMA 1.3 mm continuum map. The synthesized beam of the 1.3 mm continuum is drawn in the lower right corner. The red/blue contours start from 30% of the red-/blueshifted integrated emission peak (∼1.6/2.2 Jy km s−1 beam−1), with steps of 20% of the red/blue integrated emission peak. The white cross indicates the position of M17 MIR. (c) Zoomed-in map of Figure 2(b), depicting the EHV components of the red- and blueshifted outflows (∣V − V sys∣ > 30 km s−1). The blue and red contours both start from 5σ level with a step of 3σ level, where σ ≈ 15 mJy km s−1 beam−1.
Paper: Indefinitely Flat Circular Velocities and the Baryonic Tully–Fisher Relation from Weak Lensing
Authors: Tobias Mistele, Stacy McGaugh, Federico Lelli, James Schombert, Pengfei Li
Figure caption: The circular velocities from weak lensing (circles) compared with those from gas kinematics (diamonds). The individual galaxies illustrated here have among the most extended 21 cm rotation curves in their mass bins; the lensing data continue to much larger radii still. The error bars show the statistical error, while the gray band indicates the systematic uncertainty from converting ESD profiles to radial accelerations (Section 3.1). Symbol colors are as in Figure 1. Open symbols at large radii indicate where lenses are not sufficiently isolated. The solid green lines indicate the circular velocities of NFW halos and baryonic point masses appropriate for each mass bin. Green crosses indicate each NFW halo’s virial radius. The light green band adds a qualitative estimate of a two-halo term contribution to the NFW halo, which may become important at large radii in case our isolation criterion is imperfect there.
Paper: Indefinitely Flat Circular Velocities and the Baryonic Tully–Fisher Relation from Weak Lensing
Authors: Tobias Mistele, Stacy McGaugh, Federico Lelli, James Schombert, Pengfei Li
Figure caption: Circular velocities implied by weak lensing for four baryonic mass bins (most to least massive from the top row to the bottom) for the whole sample (left column), for LTGs (middle column), and for ETGs (right column). The lowest ETG mass bin is not shown because it contains too few lenses. Instead we show results for lenses with spectroscopic redshifts from GAMA, without splitting by mass or type due to the small sample size (gray and white symbols). For comparison, we also show results for KiDS without splitting by mass or type (small yellow symbols). Open symbols at small radii indicate where lenses are not yet effective point masses. Light-colored symbols (not-outlined) at large radii indicate data points that may still be reliable but where the isolation criterion is less certain. The error bars show the statistical errors. Horizontal lines and the corresponding shaded regions indicate the inferred V flat values and uncertainties that we use for the BTFR. The extent of the horizontal lines indicates the radial range we consider when calculating V flat.
Paper: Indefinitely Flat Circular Velocities and the Baryonic Tully–Fisher Relation from Weak Lensing
Authors: Tobias Mistele, Stacy McGaugh, Federico Lelli, James Schombert, Pengfei Li
Figure caption: Left: stacked ESD profiles for four stellar mass bins from the G-11P’ ΛCDM simulation from Wang et al. (2016; see their Figure 4). We ignore data points with negative ΔΣ in the lowest-mass bin. Right: the circular velocities implied by these ESD profiles according to our deprojection formula Equation (5). Colored bands indicate the systematic uncertainty from converting ESD profiles to accelerations (Section 3.1). Solid gray lines indicate the circular velocity of an NFW halo and a baryonic point mass as in Figure 2. Light gray bands additionally take into account contributions due to the local environment around not perfectly isolated lenses according to Equation (C2). In particular, the gray bands show the ±0.1 dex range around b  e  values of 0.3, 0.57, 0.95, and 1.25, respectively, for the four stellar mass bins.
Paper: M17 MIR: A Massive Star Is Forming via Episodic Mass Accretion
Authors: Wei Zhou, 威 周, Zhiwei Chen, 志维 陈, Zhibo Jiang, 治波 江, Haoran Feng, 浩然 冯, Yu Jiang, 禹 蒋
Figure caption: Channel maps of 12CO J = 2–1 for the eight velocity ranges from −20 to 60 km s−1. The velocity range and the relative velocity to V sys are shown in the upper left corner of each map. The red and blue solid lines illustrate wide parabolic cavity walls carved by the red- and blueshifted outflow, respectively. The black horizontal line in the 24–30 km s−1 channel represents the extension of N2 perpendicular to the outflow axis. The two vertical dotted lines 3″ apart outline the areas for generating the PV diagram in Figure 2(a). The outflow knots are marked within the dashed rectangle. The black cross indicates the position of M17 MIR.
Paper: Indefinitely Flat Circular Velocities and the Baryonic Tully–Fisher Relation from Weak Lensing
Authors: Tobias Mistele, Stacy McGaugh, Federico Lelli, James Schombert, Pengfei Li
Figure caption: The baryonic Tully–Fisher relation implied by weak lensing for the entire sample (yellow symbols, left column) and for ETGs and LTGs separately (red and blue symbols, right column). The V flat values are weighted averages of the V  c  values shown in Figure 1 for 50 kpc < R < 300 kpc (first row) and 50 kpc < R < 1000 kpc (second row). Vertical error bars represent a 0.1 dex systematic uncertainty on M */L. For comparison, we also show the best fit to the kinematic data from Lelli et al. (2019; solid gray line) and the corresponding binned kinematic data (white diamonds).
Paper: M17 MIR: A Massive Star Is Forming via Episodic Mass Accretion
Authors: Wei Zhou, 威 周, Zhiwei Chen, 志维 陈, Zhibo Jiang, 治波 江, Haoran Feng, 浩然 冯, Yu Jiang, 禹 蒋
Figure caption: The diagram illustrates the geometry of knot N2. The outflow orientation is bottom up, denoted by the black arrow. The blueshifted component is slightly closer to the central source than the redshifted component. d represents this axial offset between them and is depicted in Figure 2(a). D denotes the extension of knot N2 perpendicular to the outflow axis (the black horizontal line in the 24–30 km s−1 channel of Figure 1).
Paper: A JWST Project on 47 Tucanae: NIRSpec Spectroscopy of Multiple Populations among M Dwarfs 
Authors: A. F. Marino, A. P. Milone, A. Renzini, E. Dondoglio, E. Bortolan, M. G. Carlos, G. Cordoni, A. Dotter, S. Jang, E. P. Lagioia, M. V. Legnardi, F. Muratore, A. Mohandasan, M. Tailo, T. Ziliotto
Figure caption: NIRSpec spectra for the two stars #32620 and #25862 marked with large starred symbols in the ChM from Marino et al. (2024; right panel). Based on the location on the ChM, the two stars have different values both in ΔF606W,F814W and Δ C F606W,F814W,F322W2, with #32620 being a 1P star, and #25862 a 2P one. The similar values of the atmospheric parameters for the plotted stars have been reported in the inset of the left panel. The shaded regions indicate the spectral range spanned by the H2O bands.
Paper: A JWST Project on 47 Tucanae: NIRSpec Spectroscopy of Multiple Populations among M Dwarfs 
Authors: A. F. Marino, A. P. Milone, A. Renzini, E. Dondoglio, E. Bortolan, M. G. Carlos, G. Cordoni, A. Dotter, S. Jang, E. P. Lagioia, M. V. Legnardi, F. Muratore, A. Mohandasan, M. Tailo, T. Ziliotto
Figure caption: Examples of two spectral syntheses. The displayed observed spectra (gray crosses) are relative to stars #25862 and #34657, which have different locations on the chromosome map. Overall, the analyzed spectral regions of star #34657, photometrically classified as a 1P star, are deeper than those of #25862, which is associated with the most polluted 2P population. This is in spite of the lower temperature of the latter, which acts in the direction of deeper H2O features (see Figure 2). The best-fit synthetic spectrum is shown in red. Both the observed and the simulated spectra have been normalized at the same pseudo-continuum, and the difference of the simulated−observed (Δ(Flux)) is shown in the bottom panels.
Paper: A JWST Project on 47 Tucanae: NIRSpec Spectroscopy of Multiple Populations among M Dwarfs 
Authors: A. F. Marino, A. P. Milone, A. Renzini, E. Dondoglio, E. Bortolan, M. G. Carlos, G. Cordoni, A. Dotter, S. Jang, E. P. Lagioia, M. V. Legnardi, F. Muratore, A. Mohandasan, M. Tailo, T. Ziliotto
Figure caption: Synthetic spectra computed at different O abundances, keeping all the other chemical abundances and stellar parameters fixed, are shown in the top left panel. As indicated in the inset, the simulations have been computed for [O/Fe] ranging from −0.3 to +0.5 dex, with a step of 0.10 dex. The other panels illustrate the impact of changing temperatures (top right) up to 300 K (in steps of 100 K), log g by 1 dex (bottom left), and C abundances (bottom right) by 1 dex.
Paper: A JWST Project on 47 Tucanae: NIRSpec Spectroscopy of Multiple Populations among M Dwarfs 
Authors: A. F. Marino, A. P. Milone, A. Renzini, E. Dondoglio, E. Bortolan, M. G. Carlos, G. Cordoni, A. Dotter, S. Jang, E. P. Lagioia, M. V. Legnardi, F. Muratore, A. Mohandasan, M. Tailo, T. Ziliotto
Figure caption: ChM diagram of M dwarfs in 47 Tucanae from JWST-HST photometry (gray dots). Spectroscopic targets observed with NIRSpec at JWST are represented with filled colored circles. Targets with no available m F322W2 from NIRCam at JWST are plotted with Δ C F606W,F814W,F322W2 = 0.00 as empty circles. Different colors have been used for stars associated with different stellar populations on the ChM, specifically: first population (1P) stars are colored in red, second population ones have been colored in orange (2Pa), cyan (2Pb), and blue (2Pe). The [O/Fe] abundance vs. the ΔF606W,F814W and Δ C F606W,F814W,F322W2 values are shown in the upper and right panels, respectively. For each population, we plot the average values and the associated error.
Paper: High-velocity Blue-shifted Fe XXV Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg
Authors: Shun Inoue, Wataru Buz Iwakiri, Teruaki Enoto, Hiroyuki Uchida, Miki Kurihara, Masahiro Tsujimoto, Yuta Notsu, Kenji Hamaguchi, Keith Gendreau, Zaven Arzoumanian, Takeshi Go Tsuru
Figure caption: (a) 0.3−4 keV light curve (same as the one in Figure 1(b)). (b) Time evolution of the electron temperature calculated from the 5−9 keV continuum. (c) Best-fit normalization (K gauss1, K gauss2) of the two Gaussians. (d) Lyα/Heα ratio calculated using the two Gaussian best-fit normalizations (K gauss2/K gauss1). (e) Doppler velocity of the line center of the Fe XXV Heα line. The negative sign corresponds with blueshift.