adsabs/AstroCLIMB huggingface dataset:
Paper: Energetic Protons in the Inner Heliosphere Exhibit Consistent ∼1 MeV Temperatures
Authors: H. A. Farooki, M. E. Cuesta, L. Y. Khoo, G. Livadiotis, D. J. McComas, J. S. Rankin, M. M. Shen, J. R. Szalay
Figure caption: Time series observations by PSP and STA of the 2023 July 17 event. The first panels show the magnetic field measurements from FIELDS (S. D. Bale et al. 2016), (obtained from Berkeley SSL https://research.ssl.berkeley.edu/data/psp/data/sci/fields/l2/mag_RTN_1min) for PSP and IMPACT/MAG for STA (obtained from SPDF https://spdf.gsfc.nasa.gov/pub/data/stereo/ahead/l1/impact/rtn/mag). The second panels show the intensities from each spacecraft’s LET and HET instruments color-coded by energy. The third panels show the total count across all energies and telescopes in each 60 s interval for LET and HET. The remaining panels show the values of the thermodynamic parameters (κEP, nEP, TEP) derived from both methods (direct fit and tail fit) plotted together (in black and red, respectively). Flagged points are left blank.
Paper: Energetic Protons in the Inner Heliosphere Exhibit Consistent ∼1 MeV Temperatures
Authors: H. A. Farooki, M. E. Cuesta, L. Y. Khoo, G. Livadiotis, D. J. McComas, J. S. Rankin, M. M. Shen, J. R. Szalay
Figure caption: Example fits to the spectra from each spacecraft in the same 30 minute window. Both the energy and intensity axes are in log scale. Each energy has multiple intensities: one for each point in time within the window times the number of apertures that measure intensities at that energy. The blue/purple points are measured by the LET/HET instrument on each spacecraft. The fitted parameters for both methods are included in the bottom left of each panel. The red/black solid lines are the model distribution with the fitted parameters from the tail-/direct-fit methods. The dashed lines are the analytic power-law tail of the model distributions extrapolated to low energies, such that the solid and dashed lines converge at high energies. All uncertainties represent standard errors (1σ uncertainties).
Paper: Energetic Protons in the Inner Heliosphere Exhibit Consistent ∼1 MeV Temperatures
Authors: H. A. Farooki, M. E. Cuesta, L. Y. Khoo, G. Livadiotis, D. J. McComas, J. S. Rankin, M. M. Shen, J. R. Szalay
Figure caption: Histograms of thermodynamic parameters based on both methods for each spacecraft. Points that did not meet the goodness criteria are not included in the histograms. The y-axes show the probability density for the values on the x-axes. The left, central, and right dashed vertical lines represent the 5th percentile, median, and 95th percentile, respectively.
Paper: Energetic Protons in the Inner Heliosphere Exhibit Consistent ∼1 MeV Temperatures
Authors: H. A. Farooki, M. E. Cuesta, L. Y. Khoo, G. Livadiotis, D. J. McComas, J. S. Rankin, M. M. Shen, J. R. Szalay
Figure caption: Average output TEP estimated by the direct-fit method as a function of true TEP based on simulated data. The green box shows the approximate range of output TEP that can be trusted.
Paper: The Mid-infrared-emitting Jet in the Black Hole V404 Cygni in Quiescence
Authors: E. S. Borowski, R. I. Hynes, Q. Hunt, A. J. Tetarenko, R. M. Plotkin, T. Shahbaz, P. Gandhi, T. J. Maccarone, J. C. A. Miller-Jones, C. O. Heinke, A. W. Shaw, T. D. Russell, G. R. Sivakoff, P. A. Charles, E. V. Palaiologou, P. Reig
Figure caption: The radio to MIR average SED of V404 Cyg, including the Spitzer observations from 2006 for comparison. The MIR flux densities have been corrected for interstellar extinction as described in the main text. The solid gray line is a model stellar atmosphere representing the secondary star (adopted from R. I. Hynes et al. 2009). The error bars represent statistical uncertainties only, and in most cases are smaller than the data points. The dotted line and shaded region indicate the best-fit simultaneous radio/millimeter/MIR spectral index and 90% confidence region, respectively. An additional 5% calibration uncertainty was added in quadrature with the statistical uncertainties to generate the confidence region (based on R. A. Perley & B. J. Butler 2017 for VLA, P. Cortes et al. 2025 for ALMA, and estimated based on aperture correction uncertainties for JWST). The approximately flat spectrum is consistent with that expected from a jet.
Paper: The Mid-infrared-emitting Jet in the Black Hole V404 Cygni in Quiescence
Authors: E. S. Borowski, R. I. Hynes, Q. Hunt, A. J. Tetarenko, R. M. Plotkin, T. Shahbaz, P. Gandhi, T. J. Maccarone, J. C. A. Miller-Jones, C. O. Heinke, A. W. Shaw, T. D. Russell, G. R. Sivakoff, P. A. Charles, E. V. Palaiologou, P. Reig
Figure caption: Light curves from our multiwavelength observational campaign. (a) JWST group-level light curve showing a detailed view of the large MIR flare. (b) VLA light curve. (c) ALMA light curve. (d) JWST integration-level light curve. (e) Skinakas Observatory and GTC HiPERCAM light curves. (f) XMM-Newton and Chandra light curves. Correlated variability is present throughout, particularly during the large MIR flare and about halfway through the second JWST exposure.
Paper: A Two-stage Kick Scenario for the Peculiar Low-mass X-Ray Binary GX 1+4
Authors: Xiangyu Ivy Wang, 翔煜 王, Shi-Jie Gao, Xiang-Dong Li
Figure caption: Toomre diagram for GX 1+4 and its local comparison sample. Stars from Gaia DR3 are plotted as gray points for comparison. GX 1+4 is marked with a red star, while the sample median is indicated by a purple star. The solid black, brown, and gray ellipses enclose 68%, 90%, and 95% of the comparison sources, respectively.
Paper: A Two-stage Kick Scenario for the Peculiar Low-mass X-Ray Binary GX 1+4
Authors: Xiangyu Ivy Wang, 翔煜 王, Shi-Jie Gao, Xiang-Dong Li
Figure caption: Probability distribution of systems achieving an eccentricity e < 0.15 as a function of vroc derived from rocket kick simulations, assuming a post-AIC eccentricity of eAIC = 0.1, 0.3, 0.6, and 0.99.
Paper: A Two-stage Kick Scenario for the Peculiar Low-mass X-Ray Binary GX 1+4
Authors: Xiangyu Ivy Wang, 翔煜 王, Shi-Jie Gao, Xiang-Dong Li
Figure caption: The simulated eAIC-﹩{v}_{{\rm{sys}}}^{{\rm{nat}}}﹩ distribution for various natal kick velocities (ω).
Paper: A Two-stage Kick Scenario for the Peculiar Low-mass X-Ray Binary GX 1+4
Authors: Xiangyu Ivy Wang, 翔煜 王, Shi-Jie Gao, Xiang-Dong Li
Figure caption: The vpec–Porb distribution of LMXBs in Y. Zhao et al. (2023)’s catalog. The red star represents GX 1+4.
Paper: A Two-stage Kick Scenario for the Peculiar Low-mass X-Ray Binary GX 1+4
Authors: Xiangyu Ivy Wang, 翔煜 王, Shi-Jie Gao, Xiang-Dong Li
Figure caption: Allowed ω–vroc parameter space for forming systems like GX 1+4.
Paper: RIOJA. JWST and ALMA Unveil the Inhomogeneous and Complex Interstellar Medium Structure in a Star-forming Galaxy at z = 6.81
Authors: Mitsutaka Usui, Ken Mawatari, Javier Álvarez-Márquez, Takuya Hashimoto, Yuma Sugahara, Rui Marques-Chaves, Akio K. Inoue, Luis Colina, Santiago Arribas, Carmen Blanco-Prieto, Yurina Nakazato, Naoki Yoshida, Tom J. L. C. Bakx, Daniel Ceverino, Luca Costantin, Alejandro Crespo Gómez, Masato Hagimoto, Hiroshi Matsuo, Wataru Osone, Yi W. Ren, Yoshinobu Fudamoto, Takeshi Hashigaya, Miguel Pereira-Santaella, Yoichi Tamura
Figure caption: Comparison of the velocity profiles of the [O III] 5008 and [O III] 88 emission lines. The blue and red lines represent the profiles of [O III] 5008 and [O III] 88, respectively, normalized to their peak intensities.
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Top row: magnetic-energy dissipation over time in 2D (panel (a)) and 3D (panel (b)) during ion–electron reconnection for different σi,0. Bottom row: evolution of magnetic energy stored in the (initially absent) By component in 2D (panel (c)) and 3D (panel (d)).
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Evolution of the spectral power in selected wavenumbers of By(x) (top row) and Bx(z) (bottom row) at the location of the current sheet, for σi,0 = 0.1, 0.4, 10 (from left to right columns). Each line corresponds to a different value of k, with darker lines representing smaller k.
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Volume rendering (covering the entire simulation domain) of the total (ion and electron) plasma density in the current sheet during subsequent reconnection phases (from top to bottom) and for increasing magnetization (from left to right).
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Fraction of nonthermally accelerated electrons (top row) and ions (bottom row) at the end of each run (﹩t\,=\,2000{\omega }_{{\rm{p}},i}^{-1}﹩), for different magnetizations in 2D (diamonds) and 3D (squares). This is obtained by fitting a Maxwell–Jüttner distribution to each spectrum and then subtracting the thermal part.
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Energy distributions of electrons (top row) and ions (bottom row) at the end of each run (﹩t=2000{\omega }_{{\rm{p}},i}^{-1}﹩) in 2D (left column) and 3D (right column). Dashed lines indicate the initial distribution. Dotted lines show reference spectral slopes.
Paper: Three-dimensional Dynamics of Strongly Magnetized Ion–Electron Relativistic Reconnection
Authors: Fabio Bacchini, Gregory R. Werner, Camille Granier, Jesse Vos
Figure caption: Evolution of the average current-sheet thickness δ, defined as the region where σi ≤ 3σi,0/4, for selected initial magnetizations.
Paper: A Supermassive Black Hole in a Diminutive Ultracompact Dwarf Galaxy Discovered with JWST/NIRSpec+IFU
Authors: Matthew A. Taylor, Behzad Tahmasebzadeh, Solveig Thompson, Eugene Vasiliev, Monica Valluri, Michael J. Drinkwater, Patrick Côté, Laura Ferrarese, Joel Roediger, Holger Baumgardt, Misty C. Bentz, Kristen Dage, Eric W. Peng, Drew Lapeer, Chengze Liu, Zach Sumners, Kaixiang Wang, Vivienne Baldassare, John P. Blakeslee, Youkyung Ko, Tyrone E. Woods
Figure caption: Summary of black hole modeling results. Top panel: M/L vs. ﹩{{ \mathcal M }}_{{\rm{BH}}}﹩ χ2 confidence contours of the JAM (blue), Schwarzschild (red), and DF (yellow) modeling results. Curves are shown at 1σ, 2σ, and 3σ confidence levels. Middle panel: σlos radial profile shown for the modeling results, with colors representing the same models as the top panel. The observed profile is indicated by the gray dashed line, bounded by gray shading corresponding to the 1σ kinematic uncertainties, while the black dashed line shows the no black hole scenario in the Schwarzschild modeling. Bottom panel: h4 radial profile shown for the DF (yellow) and Schwarzschild (red) modeling results, with the gray dashed line and shading representing the observed profile and 1σ uncertainties. Horizontal gray lines indicate the extent of the radial bins.
Paper: A Supermassive Black Hole in a Diminutive Ultracompact Dwarf Galaxy Discovered with JWST/NIRSpec+IFU
Authors: Matthew A. Taylor, Behzad Tahmasebzadeh, Solveig Thompson, Eugene Vasiliev, Monica Valluri, Michael J. Drinkwater, Patrick Côté, Laura Ferrarese, Joel Roediger, Holger Baumgardt, Misty C. Bentz, Kristen Dage, Eric W. Peng, Drew Lapeer, Chengze Liu, Zach Sumners, Kaixiang Wang, Vivienne Baldassare, John P. Blakeslee, Youkyung Ko, Tyrone E. Woods
Figure caption: Signal-to-noise ratio map and PPXF fits to central pixel and radius 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 of UCD736. The left panel shows the signal-to-noise ratio per resolution element for each pixel considered in the NIRSpec/IFU field of view, where we find a central maximum of ≳75 with a rapid decline to zero beyond the extent of UCD736. Pixels are azimuthally binned to increase signal-to-noise prior to determining the kinematic profile. The right panels show PPXF fits to the center-most pixel (top), with data shown in black, kinematic fit in purple, and residuals shown by blue points. Below is a similar fit to the azimuthally averaged pixels centered at a projected distance of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 from the center. In both panels we indicate the number of IFU pixels contributing to the spectrum, and measured signal-to-noise ratio.
Paper: Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds
Authors: Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm, Edward D. Young
Figure caption: Comparison between the accreted and equilibrated water mass fractions of sub-Neptunes. The black dashed line indicates the 1:1 correlation; in the absence of chemistry, all planets would lie along this line. The gray shaded region denotes the 10–90 wt% water mass fraction range proposed for Hycean planets by N. Madhusudhan et al. (2021). All planets in our sample exhibit significant water depletion following equilibration and fall well below the Hycean threshold.
Paper: A Supermassive Black Hole in a Diminutive Ultracompact Dwarf Galaxy Discovered with JWST/NIRSpec+IFU
Authors: Matthew A. Taylor, Behzad Tahmasebzadeh, Solveig Thompson, Eugene Vasiliev, Monica Valluri, Michael J. Drinkwater, Patrick Côté, Laura Ferrarese, Joel Roediger, Holger Baumgardt, Misty C. Bentz, Kristen Dage, Eric W. Peng, Drew Lapeer, Chengze Liu, Zach Sumners, Kaixiang Wang, Vivienne Baldassare, John P. Blakeslee, Youkyung Ko, Tyrone E. Woods
Figure caption: The M59/M60 complex with UCD736 and SMBH-hosting UCDs of previous studies. The main panel shows an NGVS ﹩{g}^{{\prime} }﹩-band image with the location of UCD736 between M59 and M60 indicated by the yellow zoom-in inset. The top right-hand panel shows UCD736 imaged with HST’s ACS/WFC in the F850LP filter used for our light-profile modeling, while the bottom panel shows a JWST/NIRSpec+IFU white-light image reconstructed from the 1.74 μm < λ < 3.03 μm wavelength slices. Physical scale bars are presented in the main and HST panels for context.
Paper: Observational Evidence of Dust Evolution in Supernova Remnants: Size Redistribution toward Larger Grains in the Early Sedov Phase
Authors: He Zhao, 赫 赵, Bingqiu Chen, 丙秋 陈, Jun Li, 军 李
Figure caption: RV values as a function of SNR radii RSNR. The upper panel shows the SNR RV (colored squares) and the ISM RV (white squares) for 14 SNRs whose widely used names are marked as well. The lower panel shows the differences between the SNR and ISM RV. The colors represent the different methods of determining SNR distances: red: extinction; blue: kinematics; orange: association with known objects. The SNR ages are also indicated in the top of each panel, estimated by a simple age–diameter relation in the Sedov phase (Equation (39.9); B. T. Draine 2011). The dashed black lines indicate RV  =  3.1 and ΔRV  =  0, respectively.
Paper: Observational Evidence of Dust Evolution in Supernova Remnants: Size Redistribution toward Larger Grains in the Early Sedov Phase
Authors: He Zhao, 赫 赵, Bingqiu Chen, 丙秋 陈, Jun Li, 军 李
Figure caption: Comparison of ΔRV = SNR RV − ISM RV with ISM RV derived from different regions relative to the SNRs. Red square: an annular region with dynamic ranges (see Section 2.3) at the SNR distance; blue circle: a bigger annulus (4–5 θSNR) at the SNR distance; orange triangle: a ring (θSNR) in front of the SNR (in a foreground distance bin in the 3D RV map); purple plus: a ring (θSNR) behind the SNR (in a background distance bin in the 3D RV map); black hexagons: an annular region of 3 − 4 θSNR for ISM with an expanded region (ER) for SNR (1.6 θSNR).
Paper: Observational Evidence of Dust Evolution in Supernova Remnants: Size Redistribution toward Larger Grains in the Early Sedov Phase
Authors: He Zhao, 赫 赵, Bingqiu Chen, 丙秋 陈, Jun Li, 军 李
Figure caption: Examples of deriving RV in SNRs and their vicinity for SNRs DA 495 (upper) and Puppis A (lower). The red circles and black pluses indicate the SNR angular sizes (θSNR) and centers. The rhombuses represent the HEALPixels of the used 3D RV map (Nside  =  128). The HEALPixels with centers in the SNR region or the ISM annulus (dashed purple circles) are colored and marked by their RV values. Empty HEALPixels are marked as “NaN” and colored in white. External HEALPixels are colored in silver.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Top: the normalized residuals (i.e., data minus model, divided by noise) for three different lens model best fits to the F814W image (from left to right, corresponding to the no subhalo, dark subhalo, and luminous subhalo cases, respectively. The dashed blue squares in the left panel highlight regions with large residuals. Middle: the best-fit source reconstructions of the three different subhalo models. The white lines mark the caustic lines on the source plane. Bottom: comparison between the lensed source light and the subhalo light of the best-fit luminous subhalo model. On the left is the lensed source emission, in the middle is the subhalo light, and on the right is the emission combining these two together. The images shown in this row have been convolved with the realistic PSF.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Projections of the posterior distribution for the subhalo parameters from both our dark subhalo (blue) and luminous subhalo (green) fits to the F814W image of SDSS J0946+1006. The top right panel shows the M200–c projection of the posterior, with previous measurements of the perturber’s properties overlaid. Our dark subhalo model leads to an inferred mass and concentration for the subhalo in reasonable agreement with previous work (B24; D25; E25; M25). The L16 band shows the expected concentration–mass relation in a CDM Universe, taken from A. D. Ludlow et al. (2016). In N24, the perturber was forced to lie on the L16 relation. Our luminous model decreases the concentration values required to explain the data.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Normalized residuals for three different lens models fit to our mock data. Left: the normalized residual of the best-fit no subhalo model. The dashed blue squares highlight the localized residuals corresponding to the subhalo. Middle: the normalized residuals of the dark subhalo model. Right: the normalized residuals of the best-fit luminous subhalo model.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Posteriors of the subhalo model parameters of the mock test. The blue and green contours show the results of the dark and luminous subhalo models, respectively. The red dashed lines mark the true input values of the mock image. Similarly, in the top right corner, we plot a zoom-in figure to show our constraints on the subhalo’s mass and concentration in detail.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Comparison between our measurement of the SDSS J0946+1006 subhalo’s mass (M1kpc)/luminosity and those of subhalos in TNG50-1. The green contours indicate our measurement, while the gray points represent the subhalos in the simulation with M1kpc > 107M⊙. The dashed black contours enclose 75%, 85%, and 95% of those simulated subhalos.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Posteriors of the parameters of the luminous subhalo model. The units of X, Y, and Re are arcseconds, the unit of Ie is e− pix–1, and the unit of ϕ is degrees. The dark and light green colors indicate the 68% and 95% credible intervals, respectively.
Paper: Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
Authors: Qiuhan He, Andrew Robertson, James W. Nightingale, Aristeidis Amvrosiadis, Shaun Cole, Carlos S. Frenk, Samuel C. Lange, Shubo Li, Ran Li, Xiaoyue Cao, Leo W. H. Fung, Xianghao Ma, Richard Massey, Kaihao Wang, Maximilian von Wietersheim-Kramsta
Figure caption: Similar to Figure C1 but showing the mock test results. The red dashed lines mark the true input values.
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: Cumulative frequencies, as a function of [Fe/H], for our full sample of CEMP (black), CEMP-s (red), and CEMP-no (blue) stars, along with their associated error bars. The orange, green, and magenta symbols represent the frequency of each category from the HR sample. The HR sample includes stars with [Fe/H] < −2.5. The error bars are the 1σ binomial Wilson score confidence intervals (see the main text).
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: Logarithmic number-density plot of our final SDSS/LAMOST sample in the [C/Fe]–[Fe/H] plane, after smoothing with a Gaussian kernel, coded as shown in the bar at the top. The blue-solid line is at [C/Fe] = 0. The red dots are taken from the high-resolution spectroscopic determinations in various literature (see the main text). Each bin has a size of 0.05 × 0.05 dex in [Fe/H] and [C/Fe], respectively.
Paper: A New Subclass of Carbon-enhanced Metal-poor Stars at Extremely Low Metallicity
Authors: Young Sun Lee, 영선 이, Timothy C. Beers, Yutaka Hirai, Jihye Hong, Miji Jeong, Changmin Kim, Young Kwang Kim
Figure caption: Distribution of A(C) for the high-quality spectra (S/N ≥ 30) of stars with [Fe/H] < −2.5. The red and blue curves are fits to a Gaussian mixture model for the low and high-A(C) stars, respectively. The green curve is the sum of the two Gaussian curves. The vertical dashed line at A(C) = 7.15 separates CEMP-no stars from CEMP-s stars.