adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: The three-dimensional distribution of clusters in the richest supercluster of our catalog (SCl 2), the CB supercluster. The colors represent the mass of the clusters, with blue representing the less massive clusters and yellow the most massive ones. The red spheres represent the Abell clusters; their Abell IDs are written next to them. There are a total of 57 clusters in SCl 2.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: (a) Normalized histograms of the masses of clusters within superclusters (red histogram) and in the field (blue histogram). (b) Median masses (red dots) of the member clusters of superclusters as a function of their total mass. The blue error bars denote the quartile values of the member cluster masses above and below the median values, and the solid black line is the running mean of the red dots.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Number of candidate superclusters as a function of unweighted comoving linking length l  o  (in blue). The red line shows the position l  o  = 20.65 Mpc where the number of candidate superclusters is maximum.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: (a) Mass functions of WHL clusters and mock clusters (HR4 halos) within 0.05 ≤ z ≤ 0.366. n is the number density of the clusters/halos. (b) Number density as a function of the redshift of the WHL and mock clusters (HR4 halos) within 0.05 ≤ z ≤ 0.366.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: The blue histogram represents the redshift distribution of the entire sample of 158,103 WHL clusters, and the red line represents the selected sample of 85,686 clusters within the redshift range of 0.05 ≤ z ≤ 0.42.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Sky plane distribution of the superclusters within 0.26 ≤ z ≤ 0.29. The dots represent the WHL clusters within the redshift slice. The gray dots are not a part of any supercluster, and the other colored dots represent the member clusters of 93 superclusters within the redshift slice.
Paper: Identification of Superclusters and Their Properties in the Sloan Digital Sky Survey Using the WHL Cluster Catalog
Authors: Shishir Sankhyayan, Joydeep Bagchi, Elmo Tempel, Surhud More, Maret Einasto, Pratik Dabhade, Somak Raychaudhury, Ramana Athreya, Pekka Heinämäki
Figure caption: Number density ϕ(z) of WHL clusters as a function of redshift within 0.05 ≤ z ≤ 0.42. Inset: corresponding weights w  f,i  of the clusters as a function of redshift.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: (a)–(d) Time evolutions of SXR fluxes in 1–8 Å (pink line) and 0.5–4 Å (dark blue line), volume emission measure (green line) and temperature (orange line), radiative loss rate of SXR-emitting plasma (magenta line), and SXR flux derivative (cyan line) of the X1.4 flare, respectively. (e) Time evolutions of the radio fluxes at 0.72 GHz (purple line) and 1.40 GHz (blue line) during the impulsive phase of the flare. The red dotted line denotes the time (10:40:30 UT) when v HC reaches the linear speed of the CME.
Paper: Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST
Authors: Jie Song, GuanWen Fang, Zesen Lin, Yizhou Gu, Xu Kong
Figure caption: Difference between M *,resolved and M *,unresolved as a function of (a) redshift and (b) the reddest rest-frame wavelength included in the SED fitting for M *,resolved estimates. M *,unresolved is estimated using all available data (i.e., from F435W to F444W). The cyan, lime, orange, violet, and red curves represent the median differences between M *,resolved and M *,unresolved when the reddest filters used are F150W, F200W, F277W, F356W, and F444W for M *,resolved estimates, respectively, while the colored regions are the corresponding 1σ uncertainties. The vertical gray line in the left panel indicates z = 0.5, below which there is no significant difference between M *,resolved and M *,unresolved, while the similar line in the right panel marks a rest-frame wavelength of 10000 Å, beyond which the differences in M * are negligible.
Paper: Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST
Authors: Jie Song, GuanWen Fang, Zesen Lin, Yizhou Gu, Xu Kong
Figure caption: (a) Direct comparison between M * estimated with and without LW bands color-coded by redshift. The gray dashed line is the one-to-one relation. (b) The difference between them (i.e., ﹩\mathrm{log}({M}_{* ,\mathrm{without}\,\mathrm{LW}}/{M}_{* ,\mathrm{with}\,\mathrm{LW}})﹩) as a function of redshift. The solid black line and red shaded area represent the median and 1σ uncertainty, respectively.
Paper: Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST
Authors: Jie Song, GuanWen Fang, Zesen Lin, Yizhou Gu, Xu Kong
Figure caption: Distributions of stellar age (left) and A  V  (right) for galaxies at z ∼ 2, with blue and red representing the distributions from the fittings with and without LW bands, respectively. The median values are denoted by bars at the top of the figure. The stellar age and A  V  are indeed overestimated when rest-frame NIR data are not included in the SED fitting.
Paper: Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST
Authors: Jie Song, GuanWen Fang, Zesen Lin, Yizhou Gu, Xu Kong
Figure caption: Similar to Figure 2 but for the comparison between M *,resolved and M *,unresolved. It is evident that there is no significant difference between M *,resolved and M *,unresolved.
Paper: Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST
Authors: Jie Song, GuanWen Fang, Zesen Lin, Yizhou Gu, Xu Kong
Figure caption: Images from different bands and the estimated stellar mass maps of a few example galaxies. The stellar mass maps are derived using the pixel-by-pixel SED fitting method.
Paper: Energetics of a Solar Flare and a Coronal Mass Ejection Generated by a Hot Channel Eruption
Authors: Qingmin Zhang, Weilin Teng, Dong Li, Jun Dai, Yanjie Zhang
Figure caption: Time–distance diagrams of S1 in 131 and 94 Å. The s = 0 and s = 206.6 Mm denote the west and east endpoints of S1, respectively.
Paper: A Lack of 9 s Periodicity in the Follow-up NuSTAR Observation of LS 5039
Authors: Oleg Kargaltsev, Jeremy Hare, Igor Volkov, Alexander Lange
Figure caption: Plot of flux and photon index (Γ) as a function of phase for the 2016 and 2022 NuSTAR observations. NuSTAR is jointly fitted with Suzaku XIS data in both cases. Black and red error bars are the flux values (in 3–70 keV) for the 2016 and 2022 NuSTAR data, respectively. Blue and orange error bars correspond to the photon index (shown on the right vertical axis) obtained using 2016 and 2022 NuSTAR data, respectively. The data points that use 2016 NuSTAR data are adopted from V+21.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: The correlations between ﹩{J}_{P}\left(\mathrm{AIA}\right)﹩ (J s) and F107 (SSN). The results showed that the SWM changes at different wavelengths from from 094 to 335 Å showed high correlation with F107 (SSN), but 1600 and 1700 Å shows no correlation.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: Comparison among J  s (094–335 Å). It reads that the SWM derived variations at different wavelengths from 094 to 335 Å show a generally similar trend.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: A case analysis on the time variation of ﹩{J}_{P}\left({AIA}\right)﹩ and F107, when the solar index R remains at zero during the period of 2021 January. The images (top two panels) are the AIA EUV images at AIA 193 Å.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: The result of modified SWM (with a Savitzky–Golay filter) for nine AIA EUV channels.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: The AIA EUV images at 171 and 193 Å (panels 1 and 3 from top), as well as the derived J  s  indices (panels 2 and 4) around a coronal mass ejection event.
Paper: A New Index to Describe the Relationship between Solar Extreme Ultraviolet Variation and Solar Activity
Authors: Zhou Chen, Kecheng Zhou, Jing-Song Wang, Qiao Song, Zhihai Ouyang, Haimeng Li, Meng Zhou, Xiaohua Deng
Figure caption: Comparison between ﹩{J}_{{lP}}\left({AIA}\right)﹩ and F107 as well as SSN.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The HH 80 field observed in 2018 with HST showing [S II] (red) and [O III] (blue and white). The features identified by Heathcote et al. (1998) are marked at their 2018 locations.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The HH 81 field observed in 2018 with HST showing [S II] (red) and [O III] (blue and white). The features identified by Heathcote et al. (1998) are marked.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: The full field observed in 2018 with HST showing HH 80/81 in Hβ.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 81 in [S II]. Red shows 1995 epoch Hα observed with WFC2's PC channel. Red shows the 1995 epoch. Cyan shows the 2018 epoch.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 81 in hydrogen. Red shows the 1995 epoch Hα observed with WFC2's PC channel. Cyan shows the 2018 epoch Hβ.
Paper: HH 80/81: Structure and Kinematics of the Fastest Protostellar Outflow
Authors: John Bally, Bo Reipurth
Figure caption: Proper motions of features in HH 80 in hydrogen. Red shows the 1995 epoch Hα observed with WFC2's WF channel. Cyan shows the 2018 epoch Hβ.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: Composite maps of M82. In all panels, the teal rectangle shows the fully sampled region of the upGREAT [C II] map of the disk (3 kpc × 1 kpc). The footprints of the upGREAT single pointing along the southern outflow are shown as the teal circles, where the size of each circle is the upGREAT beam size (14.″1). Top left: an r-band image of M82 from the SINGS Survey (Kennicutt et al. 2003). Top right: the H I integrated intensity is shown by orange–purple filled contours, with values linearly spanning 4–1500 K km s−1 (Martini et al. 2018). The missing H I data in the center reflect where accurate H I information cannot be obtained due to strong absorption against the continuum; this region fully covers the region detected with signal-to-noise ratio (S/N) >2 in the [C II] map. The CO integrated intensity is shown by grayscale contours, with values logarithmically spanning 20–600 K km s−1 (Krieger et al. 2021). The FWHM beam sizes of the H I and CO data are shown in the lower right corner in magenta and black respectively. Bottom left: a zoom-in, showing the [C II] integrated intensity in green–blue, with values logarithmically spanning 200–1200 K km s−1. The H I integrated intensity is shown by the orange–purple filled contours over the same range of values as in the top right panel. The FWHM beam sizes of the H I and [C II] data are shown in the lower right corner in magenta and teal respectively. The numbers in each of the teal circles give the pixel numbers of the LFA. The white × marks the galaxy center. Bottom right: the same as the bottom left, but showing the CO integrated intensity (as grayscale contours over the same range of values as in the top right panel) instead of the H I.
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: The upGREAT [C II] maps of the central 3 kpc × 1 kpc of M82, showing the [C II] peak intensity (top left), integrated intensity (moment 0; top right), mean velocity (moment 1; bottom left), and line width (moment 2; bottom right). Spaxels with S/N < 2 (relative to the rms noise of the cube) are masked out of the 3D cube before the 2D maps are made. The black rectangle shows the boundaries of the fully sampled map. The black-outlined circles below the maps show the same values for the single pointings along the outflow. The numbers in each of the circles in the upper left panel give the pixel numbers of the LFA. The solid black circles in the lower left corners show the 14.″1 (≈250 pc) beam. The black × marks the galaxy center (Martini et al. 2018). In the lower left panel, the gray horizontal line in the color bar marks the systemic velocity (V sys) of M82 (210 km s−1; Krieger et al. 2021).
Paper: [C II] Spectral Mapping of the Galactic Wind and Starbursting Disk of M82 with SOFIA
Authors: Rebecca C. Levy, Alberto D. Bolatto, Elizabeth Tarantino, Adam K. Leroy, Lee Armus, Kimberly L. Emig, Rodrigo Herrera-Camus, Daniel P. Marrone, Elisabeth Mills, Oliver Ricken, Juergen Stutzki, Sylvain Veilleux, Fabian Walter
Figure caption: SOFIA upGREAT [C II] spectra in the southern outflow of M82, with 10 km s−1 channels (teal filled). The panels are arranged as shown in Figure 1, where the pixel number is shown in the top left of each panel. The distance from the center of each LFA pixel to the galaxy center is shown in the top right corner. The panels all have the same axis scaling, as shown in the lower left panel. Scaled versions of the CO (dark gray) and H I (magenta) profiles are overplotted. The CO and H I spectra are simply normalized to the peak of the [C II] spectrum, and the values by which the CO and H I spectra are scaled are listed in each panel.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: Left: the Chandra temperature profiles from this work (red) and found by Sanderson et al. (2005; blue). Right: the XMM-Newton temperature profiles from this work (yellow), Pointecouteau et al. (2004; red), de Plaa et al. (2004; blue), and Sanderson et al. (2005; black). Our XMM-Newton profile is cooler than found in other works; this is likely due to the application of the applyabsfluxcorr correction (see Appendix C).
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: Corner plot of the Chandra MCMC simulations (see Section 3.7). The parameters are the double-β density parameters and the temperature parameters excluding T cool. The simulation was only run for 1000 iterations with 50 walkers, making the contours fairly rough. The NuSTAR and XMM-Newton corner plots are similar. This plot was made with the python package corner.py (Foreman-Mackey 2016).
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The joint (red), ACIS-S (blue), and ACIS-I (green, dashed) Chandra temperature fits. The outermost annulus is not included for the individual ACIS-S and ACIS-I fits because the signal-to-noise was too low to constrain the temperature.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: Left: the Chandra temperatures used in this work (red) as well as the Chandra temperatures with N H fixed at the XMM-Newton best-fit values (yellow). Right: the XMM-Newton spectra fitted with N H fixed to the Chandra best-fit values.
Paper: The Hydrostatic Mass of A478: Discrepant Results from Chandra, NuSTAR, and XMM-Newton
Authors: Cicely Potter, Ayşegül Tümer, Qian H. S. Wang, Daniel R. Wik, Ben J. Maughan, Gerrit Schellenberger
Figure caption: The XMM-Newton temperature profiles with applyabsfluxcorr=yes (yellow) and applyabsfluxcorr=no (green).
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: The intrinsic mean axis ratios μ B/A and μ C/A inferred for subsamples with different stellar mass (rows) and concentration indices C 95 (columns). In each panel, the filled contours, represent the central 68% and 95% inter-percentile range of the Bayesian posterior distributions of μ B/A and μ C/A. The black dashed line indicates the B = C line. The inset plot at the bottom of each panel shows the central 68% and 95% inter-percentile range of the posterior distributions of σ B/A (x-axis) and σ C/A (y-axis). The inset plot at the top of each panel shows the observed axis ratio q distribution (filled gray histogram) and a model distribution obtained by randomly sampling viewing angles of ellipsoids characterized by the most likely mean intrinsic axis ratios and standard deviations (open blue histogram). The number of galaxies in each subsample is indicated at the upper right corner of each panel. The p-values of K-S test for the q distributions of the highest-C 95 (panels (a), (d), and (g)) and lower-C 95 subsamples in each mass interval are also indicated at the top right corner of each panel.
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Histogram of the observed axis ratios of red dwarfs with different C 95. Filled histogram is for high-concentration red dwarf subsample, and open histogram is for low-concentration red dwarf subsample. Note that the distribution of low-C 95 red dwarfs is skewed toward larger average axis ratios. The K-S test p-value (=0.006) for the two subsamples is indicated in the figure.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Color–mass diagram for our sample of dwarf galaxies analyzed in this work that do not host an AGN (gray crosses) and those analyzed in Kimbrell et al. (2021) that do host an AGN, demonstrating that both samples span a similar mass and color range. The AGN sample of Kimbrell et al. (2021) is color coded by bulge-to-total (B/T) light ratio. Yellow stars indicate the irregular galaxies in the AGN sample.
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Same as Figure 3 but for dwarfs in different local environments (rows) and with different concentration indices C 95 (columns).
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Same as Figure 3 but for blue dwarfs in different environments (rows) with different concentration indices C 95 (columns).
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Same as Figure 3 but for for blue dwarfs with different concentration indices C 95.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Size–mass diagram for our sample of dwarf galaxies analyzed in this work that do not host an AGN (gray crosses) and those analyzed in Kimbrell et al. (2021) that do host an AGN (red dots), demonstrating that both samples span a similar mass and size range.
Paper: Dwarf Galaxies with the Highest Concentration Are Not Thicker than Ordinary Dwarf Galaxies
Authors: Lijun Chen, Hong-Xin Zhang, Zesen Lin, Guangwen Chen, Bojun Tao, Zhixiong Liang, Zheyu Lin, Xu Kong
Figure caption: Same as Figure 3 but for red dwarfs (left) and blue dwarfs (right).