adsabs/AstroCLIMB huggingface dataset:
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: H-R diagram with the 1σ T eff–L error box of TIC 400562821 and evolutionary tracks calculated with varying masses and metallicities. Seismic models that best reproduce the three observational frequencies with χ 2 < 0.07 are marked with diamonds. The three frequencies create two branches in terms of possible evolutionary phases: in the left panel, the best-fitting seismic models are in the post-main-sequence (Post-MS) phase of evolution; in the right panel, they are in the overall contraction (OC) phase and close to the terminal-age main sequence (TAMS).
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: Amplitude variation during 10,000-cycle (∼710 days) integrations of TIC 400562821 RSP model.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: The stability parameter η of the pulsation modes of ℓ = 0. The stellar model is with M = 1.38 M ⊙ and Z = 0.008. For clarity, the observed Fourier spectrum is overplotted.
Paper: Asteroseismology of Triple-mode Radial δ Scuti Star: TIC 400562821
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Mariel Lares-Martiz, Zhi Li, Zhao Guo
Figure caption: The Petersen diagram for the model with mass M = 1.38 M ⊙ and Z = 0.008. Here is shown the effect of the mixing-length parameter on the frequency ratios of F/F1 and F/F2.
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Top row: photoemission rate of SPEs per H (left), fraction of SPEs to total photoelectrons as a function of grain alignment size (middle), and SPE photoemission yield (SPE per UV photon; right). The dashed horizontal line shows the results produced by the smallest grains of a < a align. Perfect alignment of large grains of a > a align with ﹩{f}_{\max }=1﹩ is considered. Middle row: the same as the top row but for the variation of the photoemission rate for different maximum alignment degrees. The ratio of SPE increases with grain growth and could reach 15% for ﹩{a}_{\min }=0.01\,\mu {\rm{m}}﹩. Bottom row: the same as the top row but for the variation of the photoemission rate for the minimum size of the grains. The ratio of SPE increases with grain growth and could reach 15% for ﹩{a}_{\min }=0.01\,\mu {\rm{m}}﹩. Perfect alignment of large grains of a > a align with ﹩{f}_{\max }=1﹩ is considered.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: PSB sizes (top) and central densities (bottom) relative to quiescent galaxies vs. the time since quenching as defined in Section 2.1. PSBs are subdivided into small (f 1 Gyr < 0.2, left) and significant bursts (f 1 Gyr > 0.2, right). The PSB median properties, errors on the medians (thick error bars), and population scatter (thick error bars) in each t  q  bin are shown in dark green. Typical error bars are included in the upper left corners. The scatter of quiescent galaxies around the best-fitting M *–R  e  or M *–Σ1 kpc quiescent relation is shown as a shaded region in light red.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Upper left: comparison between between the R  e  measured directly through pysersic and the R  e  corrected with residuals. In addition, we show the systematic differences in the measured R  e  (upper right), axis ratios (lower left), and derived Σ1 kpc (lower right) that are obtained with GALFIT and pysersic.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Left panel: axis ratio vs. stellar mass for PSBs (green), 3D-HST quiescent galaxies (red), and star-forming galaxies (blue). The star symbols mark the PSBs with merger features (interacting) while the circle symbols mark the ones that are not disrupted (isolated). Right panel: running median and 16th–84th quantile population distributions for each galaxy population. With some notable exceptions, the PSBs in this sample are round in projection, suggesting that they are predominantly round spheroids.
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Enantiomer excess due to CDRC on the grain surface by SPEs as a function of the grain temperature for different magnitudes of SOC (V SO).
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Photoelectric yield of neutral silicate grains as a function of photon energy for the different grain sizes. The yield is larger for smaller grains.
Paper: Magnetically Aligned Grains as a Ubiquitous Source of Spin-polarized Electrons and Chiral-symmetry-breaking Agents
Authors: Thiem Hoang
Figure caption: Illustration of the magnetization of an irregularly shaped grain by rotation (Barnett effect) and photoemission of SPEs. Electron spins are random in the nonrotating grain (left) but are aligned along the rotation axis for the rotating grain (right). UV irradiation on the aligned rotating grain will produce spinup or right-handed electrons.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Selected HST/WFC3 F110W image cutouts of PSBs in this sample. Each field of view is centered on the object.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Maximum outflow velocity (left), mass outflow rate (middle), and kinetic energy outflow rate (right) as a function of bolometric AGN luminosity for the extended outflow in our object J1007+2115 (red star) in comparison with the outflows discovered in two z ∼ 6.8 quasars (blue triangles) from M. A. Marshall et al. (2023) and other AGN-driven outflows at z < 4 compiled by F. Fiore et al. (2017). In the middle and right panels, for J1007+2115, we also show the total rates for both the nuclear and extended outflows combined (orange star). For the z ∼ 6.8 quasars, we only quote the [O III] emission-line-based results for consistency. For our object and the z ∼ 6.8 quasars, the error bars are not shown when their sizes are smaller than the symbol sizes. For sources from F. Fiore et al. (2017), no formal errors were reported for individual objects. The uncertainties caused by the electron density (n  e  = 1000–100 cm−3) and extinction (A  V  = 0–1) are indicated, respectively, by the blue and orange bars at the bottom right corners of the middle and right panels.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Quasar spectrum extracted from an r = 0.″25 aperture centered on the brightest spaxel of the IFU data cube. Top: data (black) and best-fit quasar continuum (orange), iron emission (cyan), and overall emission-line model (blue). The individual Balmer and [O III] emission-line components are shown in red and green, respectively. The locations of major emission lines at the systemic velocity are indicated by the vertical dotted lines. The residual from the best fit is shown in the dotted, light gray line. The spectral windows adopted for the quasar pseudocontinuum fit are marked in thick gray bars. Bottom: zoom-in view of the emission-line-only spectrum for the Hβ and [O III] region. The color coding is the same as the top panel.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Flux, velocity dispersion σ, and velocity v 50 maps of the [O III] λ5007-emitting gas in J1007+2115, after the quasar PSF has been subtracted. The spatial scales are in units of kpc. The location of the quasar is indicated by the black cross. As stated in Section 4.1, only spaxels with a peak flux density above 2σ and passing visual inspection are kept and shown in these figures.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Spectrum stacked over the spaxels with [O III] λ5007 detections shown in Figure 3 from the quasar PSF-subtracted data cube. The expected locations of the [O III] λλ4959, 5007 and Hβ emission lines from the outflow at −870 km s−1 with respect to the systemic velocity are indicated by the green vertical dashed lines. The orange vertical dashed lines indicate the expected line locations at the systemic velocity. The red dashed line represents the error from the original data cube before PSF subtraction.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Example best-fit Hβ and [O III] λλ4959, 5007 emission-line profiles from a single spaxel. Top: the data are in black, the overall best fit is in red, the best-fit scaled quasar template (i.e., the quasar PSF contribution in this spaxel) is the blue dashed line, and the individual Gaussian components for the host galaxy Hβ and [O III] emission lines (from left to right) are shown as the green dashed line. The y-axis has arbitrary flux density units. The locations of the Hβ and [O III] emission lines at the systemic velocity are indicated by the vertical dashed lines. Bottom: shown in brown is the difference between the data (black) and the overall best-fit model (red) in the top panel. Shown in blue is the spectral error. The black horizontal dashed line indicates y = 0.
Paper: Fast Outflow in the Host Galaxy of the Luminous z = 7.5 Quasar J1007+2115
Authors: Weizhe Liu, 伟哲 刘, Xiaohui Fan, Jinyi Yang, Eduardo Bañados, Feige Wang, Julien Wolf, Aaron J. Barth, Tiago Costa, Roberto Decarli, Anna-Christina Eilers, Federica Loiacono, Yue Shen, Emanuele Paolo Farina, Xiangyu Jin, Hyunsung D. Jun, Mingyu Li, Alessandro Lupi, Madeline A. Marshall, Zhiwei Pan, Maria Pudoka, Ming-Yang Zhuang, 明阳 庄, Jaclyn B. Champagne, Huan Li, Fengwu Sun, Wei Leong Tee, Andrey Vayner, Haowen Zhang
Figure caption: Left: reconstructed PSF from q3dfit results of J1007+2115. The image is integrated over the wavelength range of 4.0–4.5 μm. Right: comparison of the azimuthally averaged surface brightness (SB) radial profiles between the reconstructed PSF in the left panel and the empirical PSF constructed from the IFU observation of the PSF star associated with J1007+2115.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: Panels (a), (b), and (c): The Lomb–Scargle periodogram of EPIC 248705247. Horizontal lines (in red) denote the significance threshold of 5.4σ. The vertical short segments indicate the independent frequencies, while the red segments indicate the triplets. Panels (d)–(i): Complete and incomplete triplets indicating frequency splittings.
Paper: Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Jiayi Zhang, Jianning Fu, Tianqi Cang, Jie Su, Yanhui Chen, Xiaoyu Ma, Gang Meng
Figure caption: The finding chart and the optimal aperture masked for EPIC 248705247 provided by the open code tpfi.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: The detection results of the QPO signal corresponding to the γ-ray light curve in the upper panel of Figure 1. The solid purple line shows the best-fit underlying PSD with a power-law model. Left panel: the left subpanel shows the color profile of the weighted wavelet z-transform (WWZ) power spectrum, where the horizontal yellow patches indicate a possible QPO signal. For the right subpanel, the black curve and the green dashed curve indicate the LSP power spectrum and the corresponding 4.0σ significance level, respectively; the red curve and the blue dashed curve represent the time-averaged WWZ power spectrum and the corresponding 4.0σ significance level, respectively. Right panel: the WWZ and LSP are plotted with higher frequency resolution in the vicinity of the claimed period (frequencies 0.003–0.0004).
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: Analysis results of PDM algorithms with N  b  = 4 for the period search. The red dashed line represents the 3.5σ significance level.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: AIC maps from ARIMA and SARIMA model analysis of light curves. (a) Results of the ARIMA(p, d, q) model analysis. We can see that there is a minimum value of the AIC in the ARIMA(1, 0, 6) (the box marked with a red square). (b) Results of the SARIMA(0, 1, 2) × (P, 1, Q) model analysis. We find a global minimum AIC value at SARIMA(0, 1, 2) × (0, 1, 2) (the box marked with a red square) considering a period (season of 660 days). In the uncolored boxes, either the fit is not converging, or the AIC is greater than a specified threshold. (c) The SARIMA(0, 1, 2) × (0, 1, 2) model is the basis for the consideration of different periods. We observe the global minimum AIC value at 660 days. (d) The resulting mean PSD of the simulated light curves and the corresponding 68% confidence interval (bright color region). A slightly protruding peak appeared around 650 days.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: Left panel: the meaning indicated by the subpanels is the same as in Figure 3, but here for the results of the analysis of the V-band data over the period from MJD 53587 to 58384. The yellow shaded area represents the half-width at half-maximum of the γ-ray QPO signal. Right panel: the results of the correlation between the different bands obtained with the DCF method. The top subpanel displays the analysis results between γ-ray and the V band during MJD 54600–58400, while the bottom subpanel displays the analysis results between γ-ray and the G band during MJD 56900–57900.
Paper: The Detection of Possible Quasiperiodic Oscillations in the BL Lac 4FGL J2139.4−4235
Authors: Yunlu Gong, Quangui Gao, Xiaopan Li, Min Yuan, Tingfeng Yi, Huaizhen Li, Longhua Qin, Haitao Yang, Haiyan Yang, Pengfei Zhang, Jun Fang, Li Zhang
Figure caption: Comparison of model results with the observed light curves (0.3–300 GeV) of 4FGL J2139.4−4235. The upper panel indicates a steady injection of proton, and the bottom panel represents the temporal injection of proton.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Test showing whether past starbursts can be recovered from SED fitting. We generate mock photometry and a mock spectrum using FSPS with a PSB-like SFH pushed by 0.0, 0.5, 1.0, and 2.0 Gyr, presented from the top to the bottom rows. The first column shows the mock photometry in circles. The same HST/ACS+WFC3 (blue circles) and JWST/NIRCam filters (green circles) are used for mock photometry. The best-fit SED model is shown with the red line. The second column shows the noise-added mock spectrum generated with each SFH, and the red line shows the best-fit SED model. The blue line in each panel in the third and fourth columns is the input SFH, and the light-weighted age of the stellar population is shown in the right corner. The reconstructed SFHs from Prospector fitting are shown in the third (using the continuity prior) and the fourth (using the bursty prior) columns. The stellar ages inferred from SED fitting are also given in the right corner. The green and yellow–green shades in the third column include 1σ and 2σ of the posteriors at each SFH time bin. The green line shows the 50th percentile of the posteriors at each time bin, and the dashed black line shows the SFH from MAP. The same format is used with a magenta color for the reconstructed SFHs using the bursty prior in the fourth column. We find that the continuity prior does not seem to well reproduce the past starburst events. The past starburst events are much better reproduced when the bursty prior is used. However, even the bursty prior cannot perfectly reproduce the exact moment and intensity of the past starbursts that happened more than 2 Gyr ago.
Paper: Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Song Wang, Xue Li, Henggeng Han, Jifeng Liu
Figure caption: Left panel: ratio of photospheric NUV emission to total NUV emission. The orange contours represent the number distribution of F to K stars, while the violet contours represent the number distribution of M stars. The blue points and their data are from B. Stelzer et al. (2013). The red squares and green triangles represent young and old M dwarfs, respectively, from A. C. Schneider & E. L. Shkolnik (2018). The dotted horizontal lines (from top to bottom) mark ratios of 1, 0.5, and 0.1, meaning 100%, 50%, and 10%, respectively, of the UV emission is from the photosphere. The color bars indicate the number of stars. Histograms are included as the subplot to show the distributions of the ratios for F, G, K, and M stars, with sample sizes of 183867, 499829, 112779, and 5797, respectively. For clarity, the bin sizes differ across stellar types: 0.001 for F stars, 0.0005 for G stars, 0.00125 for K stars, and 0.05 for M stars. Right panel: ratio of FUV photospheric emission to total emission. Histograms are included as the subplot to show the distributions of the ratios for F, G, K, and M stars, with sample sizes of 21603, 5397, 1157, and 448, respectively. For clarity, the bin sizes differ across stellar types: 0.006 for F stars, 0.06 for G stars, 0.12 for K stars, and 0.24 for M stars.