adsabs/AstroCLIMB huggingface dataset:
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Spectrum of CR protons at the disk for the different diffusion prescriptions. Model 1 gives negligible contribution from the GWTS component, while model 2 is capable of accelerating CRs up to 40 PeV, an order-of-magnitude energy gain compared to the CRs produced within the disk.
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Sketch of the problem under consideration. The wind geometry is shown as a magnetic flux tube. CRs produced by Galactic sources in the disk travel with the wind up to the Galactic wind termination shock (GWTS), where they get reaccelerated to higher energies. The gray line is a schematic of a CR trajectory originating at the disk, crossing the GWTS, and propagating back to the disk.
Paper: Reacceleration of Galactic Cosmic Rays beyond the Knee at the Termination Shock of a Cosmic-Ray-driven Galactic Wind
Authors: Payel Mukhopadhyay, Enrico Peretti, Noémie Globus, Paul Simeon, Roger Blandford
Figure caption: Fluxes of CRs escaping out into the IGM for different elements. The plot shows that reacceleration at the GWTS can be a source of seeding the IGM with intermediate-energy CRs, reaching up to O(1 EeV) for iron.
Paper: Physical Evolution of Dark Matter Halo around the Depletion Boundary
Authors: Hongyu Gao, Jiaxin Han, Matthew Fong, Y. P. Jing, Zhaozhou Li
Figure caption: Two-dimensional joint dependence of the depletion radius and density contrast on halo mass and other properties at z = 0. Only the bins with more than 50 halos are displayed. The four rows from top to bottom represent the joint dependence of r cd, r id, Δ(<r cd), and Δ(<r id), respectively. The values of r cd, r id, Δ( < r cd), and Δ(<r id) are shown on each pixel. Here r cd and r id have been scaled by r vir.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: Bar graph comparing the photochemical yield at a fluence of 13.1 × 1017 cm−2 with respect to the initial NH3.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The growth curves for the imine and nitrile produced during the irradiation of NH3:C2H6 (a), NH3:C2H4 (b), (d), and NH3:C2H2 (c), (e). The scatter plot shows the photochemical yield of the imine after 1, 2, 3, 4, 5, and 6 h of irradiation.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The steps taken for the analysis of our irradiation experiments. A representative experiment has been chosen to depict the steps of the analysis (NH3:C2H2 at 10 K). (1) We compare the initial and final spectra to look for new peaks and morphology changes due to the irradiation; (2) once the new peak has been attributed to its parent molecule, we look at its growth over the irradiation period. In order to do so, we fit the spectrum with a Gaussian curve and we calculate the area underneath it; (3) the area under the curve can be converted into column density and then MLs (Equation (3)). This allows us to calculate a photochemical yield and plot a growth curve.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: Ethylamine TPD traces following irradiation of NH3:C2H4 ices: (a) mass 30 (﹩{{\mathrm{CH}}_{2}{\mathrm{NH}}_{2}}^{+}﹩), (b) mass 44 (﹩{{\mathrm{CH}}_{3}{\mathrm{CHNH}}_{2}}^{+}﹩), and (c) mass 45 (﹩{{\mathrm{CH}}_{3}{\mathrm{CH}}_{2}{\mathrm{NH}}_{2}}^{+}﹩). The TPD for the irradiation of pure ethylamine is shown in each panel to confirm our detection. The pure ethylamine QMS current has been divided by 103, so as not to drown out the significantly weaker signal detected in our experiments.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The main TPD traces for the main m/z masses associated with CH3CH=NH and CH3CN for each ice mixture. Masses 39–43 are associated with the imine, whereas masses 39–42 are associated with the production of acetonitrile.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The initial spectra (dashed line) and the subtracted spectra (final spectrum minus initial) for each of the irradiation temperatures of the C2H6 experiments. We observe the formation of a new peak at 1650 cm−2 during the irradiation of these ice mixtures at 50 K, which we assigned to ethanimine.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: The evolution of the imine peak at 1650 cm−1 during TPD in three representative experiments for the three kinds of ice mixtures. Note that desorption is complete at 120 K for the C2H6 mixture, and at 160 K for the C2H4 and C2H2 mixtures.
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: Evolution of the nitrile peak at 2252 cm−1 during heating for NH3:C2H2 and NH3:C2H4 ice mixtures at 10 and 30 K, respectively (the experiments with the highest yield of nitrile).
Paper: The Formation of Imines and Nitriles during VUV Photoirradiation of NH3:C2H x  Ice Mixtures
Authors: Alessandra Canta, Karin I. Öberg, Mahesh Rajappan
Figure caption: Close-up of the regions where we would expect the formation of CN bonds. The dashed lines show the pre-irradiation spectra, whereas the solid lines show the region after 6 h of irradiation.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Comparison of the Sérsic index (left) and effective radius (right) for the distribution between stars and gas measured from r-band and Hα images, respectively. The ratios of these measurements between stars and gas are plotted as scatter diagrams (middle) and histograms (bottom). SF-ETGs and SF-LTGs are represented in red and blue. The histograms for SF-ETGs are multiplied by a factor of 10 on the left and 20 on the right for an easy comparison with the SF-LTGs distribution. The p-values from the K-S and A-D tests for the ratio between SF-ETGs and SF-LTGs are shown in the top right of the bottom panels. The dashed lines on all panels indicate a one-to-one relation.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Distributions of galaxies on the plane of the stellar mass ﹩\mathrm{log}({M}_{* }/{M}_{\odot })﹩ and the environmental parameter ρ 20/〈ρ〉 (c), with 20% of galaxies for each type represented by different colors: SF-ETGs (red), SF-LTGs (blue), q-ETGs (gray), and q-LTGs (green). The fractions ((a) and(e)) and the normalized histograms ((b) and (d)) are plotted as functions both of the stellar mass (upper panels) and of the environmental parameter (right panels). These quantities are calculated for the entire sample galaxies. The uncertainties are estimated from the confidence interval of the fraction for a beta distribution.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Radial profiles of age (top) and stellar metallicity (bottom) for four different types of galaxies. The radial profiles are determined by calculating the median value at each binned radius after stacking the data for all of the galaxies in each type. The four types of galaxies are indicated by different colors. The age and metallicity estimates are influenced by whether they are weighted by mass (left) or light (right). The error bars are estimated by the bootstrap method.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Fractions of different stellar populations in the total stellar mass. The four different types of galaxies, divided by their morphology and star-forming status, are represented by different colored lines: star-forming early-type (SF-ETG) and late-type (SF-LTG) galaxies, and quiescent early-type (q-ETG) and late-type (q-LTG) galaxies are shown in red, blue, gray, and green, respectively. The ages are estimated using two different methods: mass-weighted (left) and light-weighted (right). The errors are estimated from the confidence interval of the fraction for a beta distribution.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Global gas and dust properties estimated by H I gas (left) and Balmer decrement (right) as a function of stellar mass. The four types of galaxies are represented by red (SF-ETGs), blue (SF-LTGs), gray (q-ETGs), and green (q-LTGs), respectively. We only display 10% (left) and 1% (right) of the data, respectively, for clarity. The median values at each mass bin are displayed as solid lines with errors, which are estimated by the bootstrap method. These quantities are calculated for the entire sample galaxies.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Radial profiles of stellar age for four types of galaxies in different mass bins. These profiles are measured in the same way as in Figure 4 but are displayed by the three mass bins. The different colors represent different types. The age is estimated by mass-weighted (top) and light-weighted (bottom) ways, respectively. The errors are measured by the bootstrap method.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Example spectra (left) and images (right) of SF-ETGs (top three rows) and q-ETGs (bottom row). The spectra and images are sourced from SDSS/DR17. The three SF-ETGs are arranged in ascending order of stellar mass: above 109 M ⊙, 1010 M ⊙, and 1011 M ⊙, from top to bottom. The example galaxy of q-ETG is selected with a stellar mass exceeding 1011 M ⊙, which falls within the common mass range of q-ETGs.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Fractions of position angle (PA) offsets of the rotation axes between stars and gas for three different types of galaxies: SF-ETGs (left), SF-LTGs (middle), and q-LTGs (right). Galaxies with ΔPA > 30° are classified as misalignments, and galaxies with ΔPA > 150° are selected as counterrotators.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Normalized histograms of four types of galaxies as a function of the large-scale environment ρ 20/〈ρ〉, with the three panels representing galaxies in different mass ranges from lower mass (top) to higher mass (bottom). The four types are represented by different colors, SF-ETGs (red), SF-LTGs (blue), q-ETGs (gray), and q-LTGs (green). The uncertainties are estimated using the confidence interval of the fraction for a beta distribution.
Paper: Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection
Authors: Bingkun Yu, Yutian Chi, Mathew Owens, Christopher J. Scott, Chenglong Shen, Xianghui Xue, Luke Barnard, Tielong Zhang, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Zhenpeng Su, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Xiankang Dou, Mike Lockwood
Figure caption: Perturbations in the Martian upper atmosphere caused by the ICME. Both the associated IMF and high-speed solar winds can remarkably influence planetary electrons and heavy ions (O﹩{}_{2}^{+}﹩ and O+). The top panel shows the dynamic pressure of upstream solar wind out of the bow shock at Mars (﹩{P}_{{\mathrm{dyn}}_{\mathrm{sw}}}﹩) as a red-shaded area, the thermal pressure of the nightside ionopause (﹩{P}_{{\mathrm{th}}_{i}}﹩) as yellow circles, the magnetic pressure of the nightside ionopause (﹩{P}_{{B}_{i}}﹩) as blue squares, and the magnetic pressure of the dayside ionopause as blue diamonds. The bottom panel shows the variations in column abundance density of electrons (blue), ﹩{{\rm{O}}}_{2}^{+}﹩ (yellow), and O+ (red) for the nightside ionosphere measured by MAVEN integrated between 185–500 km, with the corresponding altitude of the ionopause as circles from density profiles for electrons, ﹩{{\rm{O}}}_{2}^{+}﹩, and O+ respectively. The blue vertical-dashed line represents the uncertainty of the column abundance density of electrons because the altitude of the ionopause cannot be precisely defined due to a data gap. The red vertical-dashed line and the gray color band are the arrival time of the ICME-driven shock and the interval of the ICME. The occurrence of reduction in the column abundance of ionospheric plasma occurred shortly after the arrival of the ICME.
Paper: Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection
Authors: Bingkun Yu, Yutian Chi, Mathew Owens, Christopher J. Scott, Chenglong Shen, Xianghui Xue, Luke Barnard, Tielong Zhang, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Zhenpeng Su, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Xiankang Dou, Mike Lockwood
Figure caption: The spacecraft and planet positions on the solar equatorial plane, the orbits of Tianwen-1 and MAVEN, and the in situ solar wind observations. (a) The solar wind speed as simulated by the HUXt model with the positions of Mars and the BepiColombo spacecraft in the heliocentric Earth equatorial (HEEQ) coordinate on 2021 December 6, at 18:25 UT. (b) Trajectories of Tianwen-1 (red line) and MAVEN (blue line) in a cylindrical coordinate system for the time interval from 00:00 UT on 2021 December 8 to 00:00 UT on 2021 December 13, color-coded by distance from the Mars surface. The outer black line denotes the average location of the bow shock and the interior dashed-black line denotes the average location of the magnetic pileup boundary. (c) Magnetic observations by the BepiColombo magnetometer, showing total field strength (B total) and components (B  r , B  t , and B  n ) in the Radial-Tangential-Normal coordinate. (d) The magnetic field, solar wind velocity, density by MAVEN, and the magnetic field by Tianwen-1. The black-vertical line represents the arrival time of the possible shock observed from the enhanced plasma density in solar wind. The purple-shaded region represents the interval of the ICME.
Paper: Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection
Authors: Bingkun Yu, Yutian Chi, Mathew Owens, Christopher J. Scott, Chenglong Shen, Xianghui Xue, Luke Barnard, Tielong Zhang, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Zhenpeng Su, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Xiankang Dou, Mike Lockwood
Figure caption: In situ observations from MAVEN at altitudes of 185–500 km on the nightside of Mars (X MSO < 0) during 2021 December 6–15. From top to bottom: (a) MAVEN/LPW electron density, (b) MAVEN/NGIMS ﹩{{\rm{O}}}_{2}^{+}﹩ density, (c) MAVEN/NGIMS O+ density, (d) MAVEN/LPW electron temperature, and (e) MAVEN/MAG magnetic filed in the Martian nightside ionosphere. MAVEN = Mars Atmosphere and Volatile Evolution; LPW = Langmuir Probe and Waves; NGIMS = Neutral Gas and Ion Mass Spectrometer; and MAG = Magnetometer.
Paper: Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection
Authors: Bingkun Yu, Yutian Chi, Mathew Owens, Christopher J. Scott, Chenglong Shen, Xianghui Xue, Luke Barnard, Tielong Zhang, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Zhenpeng Su, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Xiankang Dou, Mike Lockwood
Figure caption: Daily altitude profiles of electron density in the Martian nightside ionosphere using MAVEN. The top six panels show the background ionospheric profiles of electron density before the ejecta of the ICME arrived at Mars. The black line represents the daily mean electron density, with the error bar representing the standard deviation in this mean. The middle six panels show the ionospheric profiles of electron density during and after the interval of the ICME by comparison with the background ionospheric profiles. The bottom six panels show the relative changes in the electron density during and after the ICME interval, ΔN  e /N  e  (%), with the shaded area representing the standard deviation.
Paper: Tianwen-1 and MAVEN Observations of the Response of Mars to an Interplanetary Coronal Mass Ejection
Authors: Bingkun Yu, Yutian Chi, Mathew Owens, Christopher J. Scott, Chenglong Shen, Xianghui Xue, Luke Barnard, Tielong Zhang, Daniel Heyner, Hans-Ulrich Auster, Ingo Richter, Jingnan Guo, Beatriz Sánchez-Cano, Zonghao Pan, Zhuxuan Zou, Zhenpeng Su, Zhiyong Wu, Guoqiang Wang, Sudong Xiao, Kai Liu, Xinjun Hao, Yiren Li, Manming Chen, Xiankang Dou, Mike Lockwood
Figure caption: Illustration of Tianwen-1, MAVEN, and BepiColombo in situ measurements of the response of Martian upper atmosphere and ionosphere to an interplanetary coronal mass.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Mass distribution comparison for sdB/sdOB stars in Group 3 with sdB stars in Schaffenroth et al. (2022). Left panel: mass distribution for sdB+dM/BD (black solid curve) and sdB+WD systems (black dashed curve) in Schaffenroth et al. (2022) are plotted separately. Right panel: both sdB+dM/BD and sdB+WD systems in Schaffenroth et al. (2022) were put together to plot the mass distribution (black solid curve). In each panel, the magenta dashed–dotted curve denotes the mass distribution for sdB/sdOB stars in Group 3. All distributions were normalized to the maximum values for a better comparison.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Mass distribution for the selected hot subdwarfs with different spectral classifications in three groups. In each group, the mass distributions for all samples, sdB/sdOB stars, He-rich stars, and sdO stars are denoted by black solid, magenta dashed–dotted, blue dashed, and green dotted histograms, respectively. The bin size is the same as in Figure 7.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Mass distribution comparison between sdB/sdOB stars in Group 3 and the results predicted by Han et al. (2003). From the upper left to bottom right panel, the mass distribution predicted by 12 sets of simulation in Han et al. (2003) are denoted separately by black solid, dashed, and dotted curves (see legend box) in each panel, while the mass distribution for sdB/sdOB stars in Group 3 of this study is presented by the magenta dashed–dotted curve. Bin numbers for sdB/sdOB stars in Group 3 were normalized to the maximum bin number of Han et al. (2003) in each panel.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Mass distributions for all types of hot subdwarf stars in three groups. Left panel: absolute numbers in each bin. Right panel: numbers in each group were normalized to the maximum. Black solid, blue long-dashed, and red short-dashed histograms denote the mass distribution for hot subdwarf stars in Groups 1, 2, and 3, respectively. The bin size is set to 0.035 M ⊙, and 26 bins are present in the mass range of 0.1–1.0 M ⊙.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Relationship between mass and atmospheric parameters for the selected hot subdwarfs. From upper left to bottom right, it shows mass–T eff plane, mass–﹩\mathrm{log}g﹩ plane, mass–﹩\mathrm{log}(n\mathrm{He}/n{\rm{H}})﹩ plane, and mass–luminosity plane, respectively. The labels with different colors denote the spectral classification of hot subdwarfs from Lei et al. (2018, 2019b, 2020). Parameter errors are not shown for clarity.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption:  T eff–luminosity plane for the hot subdwarf stars selected in this study. The labels with different colors denote the same spectral classifications as in Figure 2. The two brown dashed lines denote the ZAHB and TAHB positions for HB stars with [Fe/H] = −1.48 from Dorman et al. (1993).
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Mass–radius plane for the hot subdwarf stars selected in this study. The color bar on the right denotes different ﹩\mathrm{log}g﹩ values, while the black dashed curves from top to bottom denote constant ﹩\mathrm{log}g﹩ values of 5.0, 5.45, 5.85, 6.0, and 6.3 dex, respectively.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Left panel: mass comparison between this study and Schaffenroth et al. (2022). Right panel: mass comparison between this study and Fontaine et al. (2012).
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Radius and luminosity comparison between this study and Schaffenroth et al. (2022).