adsabs/AstroCLIMB huggingface dataset:
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: Fourier spectra of the OB-type pulsating stars with high-frequency (HF).
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: Fourier spectra of the OB-type pulsating stars with pure low-frequency (LF).
Paper: Infrared Galaxies Detected by the Atacama Cosmology Telescope
Authors: Ece Kilerci, Tetsuya Hashimoto, Tomotsugu Goto, Ersin Göğüş, Seong Jin Kim, Simon C.-C. Ho, Yi Hang Valerie Wong
Figure caption: The log (F 90 μm/F 98 GHz) (top left), log (F 90 μm/F 150 GHz) (top right), log (F 98 GHz/F 150 GHz) (bottom left), and log (F 98 GHz/F 220 GHz) (bottom right) color distributions of our sample. The black distribution represents the radio-loud AGNs, the gray one represents the radio-quiet AGNs, the brown one represents the SF radio galaxies, and the cyan one represents the dust emission. These color distributions are extremely useful for estimating the origins of the millimeter radiation, based only on the observed color, without any redshift requirement.
Paper: Infrared Galaxies Detected by the Atacama Cosmology Telescope
Authors: Ece Kilerci, Tetsuya Hashimoto, Tomotsugu Goto, Ersin Göğüş, Seong Jin Kim, Simon C.-C. Ho, Yi Hang Valerie Wong
Figure caption: Examples of spatially extended sources at 150 GHz. Left: image of the isolated source matched with AKARI ID 1105490-000224. Middle: image of the merging system matched with AKARI ID 0540584+202203. The white circles indicate the aperture sizes adopted in our analysis. Right: the total flux density within the aperture as a function of the aperture size for sources matched with AKARI IDs 1105490-000224 and 0540584+202203. The solid and dashed lines correspond to 1105490-000224 and 0540584+202203, respectively. The adopted aperture size for 1105490-000224 (0540584+202203) is shown by the solid (dashed) vertical line.
Paper: Infrared Galaxies Detected by the Atacama Cosmology Telescope
Authors: Ece Kilerci, Tetsuya Hashimoto, Tomotsugu Goto, Ersin Göğüş, Seong Jin Kim, Simon C.-C. Ho, Yi Hang Valerie Wong
Figure caption: The total IR luminosity (top) and the AGN luminosity (bottom) vs. the millimeter-band luminosities measured from the SED model at 98 GHz (left), 150 GHz (middle), and 220 GHz (right) for the 43 galaxies with AGN radio emission (red circles) and the 16 SF radio galaxies (blue squares). These relationships can be used to estimate the AGN and total IR luminosities from the millimeter-band luminosities. The solid lines represent the relationships for the AGN radio emission, while the dashed lines show the relationships for the SF radio emission.
Paper: Infrared Galaxies Detected by the Atacama Cosmology Telescope
Authors: Ece Kilerci, Tetsuya Hashimoto, Tomotsugu Goto, Ersin Göğüş, Seong Jin Kim, Simon C.-C. Ho, Yi Hang Valerie Wong
Figure caption: The physical parameters L dust and L(IR)TOTAL measured from the SEDs vs. the F 98 GHz /F 150 GHz color. The red squares represent the AGNs and the black circles represent the SF galaxies. The Spearman rank correlation coefficient values r  s  are listed, with significances of 0.002 (left) and 0.0003 (right).
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Left: the smoothed probability density function of the SNR diameters. The red solid line is the arithmetic mean (30.5 ± 1.7 pc) and the vertical black dashed line is the geometric mean of the diameter (21.9 pc) of the Galactic SNRs. The histogram is in the background (in green). Right: the cumulative distribution function of SNR diameters of galaxies. The black solid line shows SNR diameters from this work (sample size 214), The red dashed line shows M31 from Lee & Lee (2014) (sample size 156), The blue dashed–dotted line shows M33 from Long et al. (2010) (sample size 137). The green dotted line shows M83 from Dopita et al. (2010) (sample size 47). The magenta solid line shows the LMC from Bozzetto et al. (2017) (sample size 59) and the cyan dotted line shows the SMC from Filipović et al. (2005) (sample size 21).
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: A comparison between the literature distances and distances obtained using the Σ–D relation. The red circles denote the literature distances to SNRs from Ranasinghe & Leahy (2022). The distances obtained from the Σ–D relation presented by Case & Bhattacharya (1998) and Pavlović et al. (2014) are denoted by blue crosses and green diamonds, respectively. The numbers in the x-axis labels correspond to SNR numbers from Table 1.
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Distribution of Galactic SNRs in the Σ–D plane for a sample of 139 shell-type SNRs. The color bar denotes the ages of the SNRs in kiloyears.
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Left: histogram of literature SNR ages (red) and all SNR ages in our sample (gray). Right: the cumulative distribution of SNR ages (180 youngest sources). The best-fit lines: one SN in 164 yr (for ages <50 kyr, red dotted line, sample size 180), one SN in 87 yr (for ages <14 kyr, black dashed–dotted line, sample size 125) and one SN in 58 yr (for ages <2 kyr, blue dashed line, sample size 31). The orange line is the SN rate of one SN in 40 ± 10 yr presented by Tammann et al. (1994) with the uncertainty shown by the orange shaded region.
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Left panel: The PDF of the spectral index (α) distribution. SNRs (all types; 270 SNRs in the sample) in red (histogram and PDF) and shell-type SNRs (sample size 208) in blue (histogram and PDF). The vertical lines show the mean spectral index for each SNR type. Right panel: The spectral index vs. age (175 SNRs in sample). The horizontal lines show the mean spectral index for each SNR type (same as the left panel).
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Galactic SNR diameters and their age distribution for a sample of 80 shell-type SNRs. The best-fit line (black curve) is D = (9.52 ± 0.92) t 0.44±0.04 pc. The green dashed line is the r ∝ t 4/5 ejecta-dominated stage, the red dotted line is the r ∝ t 2/5 adiabatic stage, and the magenta dashed–dotted line is the r ∝ t 2/7 radiative stage.
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: Left panel: Venn diagram showing the number of SNRs with distances (Ranasinghe & Leahy 2022) and the number of SNRs with distances estimated using the Σ–D relation (Case & Bhattacharya 1998 and Pavlović et al. 2014). Right panel: histogram of the percentage differences between the literature distances and the Σ–D distances.
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: The Galactic height distribution (z) of SNRs (sample size of 214). The best-fit exponential distribution, N = 38.8 exp(−∣z∣/48.1), is the black solid curve. The blue curve is the best-fit normal distribution, N = 23.9 exp(−0.5(x/57.3)2).
Paper: A Statistical Analysis of Galactic Radio Supernova Remnants
Authors: S. Ranasinghe, D. Leahy
Figure caption: The Galactic radio SNR diameters, D, vs. Galactic height, z, for the sample of 214 radio SNRs.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A series of logarithmic scatterplots showing correlations between individual coronal-line fluxes and the WISE 2 band fluxes of the host galaxy. Each panel has identical vertical and horizontal scales. Best-fit power laws are plotted with dashed lines over the data, and the best-fit parameters are shown in the legend of each plot as a function of F W2, the W2 flux. The points are colored according to the WISE 1 − WISE 2 color (in magnitudes). Each panel lists the Spearman correlation coefficient r and corresponding p-value of the distribution.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: Distributions of each coronal line over the luminosity (L), FWHM, and velocity shift (v off) organized by the critical density in cm−3. The luminosity is in ergs per second, and FWHM and v off are in kilometers per second. Each line is annotated on the right side of the corresponding ﹩\mathrm{log}\rho ﹩ bin. The colors also indicate the critical density, with more saturated purples corresponding to higher ρ. Note that the vertical axes are not scaled logarithmically; each critical density is shown categorically.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: Distributions of each coronal line over the luminosity (L), FWHM, and velocity shift (v off) organized by the IP in eV. The luminosity is in ergs per second, and FWHM and v off are in kilometers per second. Each line is annotated on the right side of the corresponding IP bin. The colors also indicate the IP, with more saturated purples corresponding to higher IPs. Note that the vertical axes are not scaled linearly; each IP is shown categorically.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: Redshift distribution of the MPA/JHU catalog and CLASS, normalized such that the maximum is 1. The normalization constants for both distributions are shown in the legend.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Ne V] λ λ 3346, 3426 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe V] λ λ 3839, 3891 and [Fe VII] λ3759 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A selection of [Fe VII] λ4893 and [Fe V] λ4181 detections from our subsample. The raw flux, corrected for redshift and Galactic extinction, is plotted in black. The BADASS model and each of its components (emission lines, host galaxy, AGN power law) are plotted in colors indicated by the legend. Each coronal line is labeled, and the spectra’s coordinates and SDSS Spec Object ID are given in the plot titles.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Fluxes and energies of the corresponding indirect and direct beams in the spacecraft-inertial reference frame as a function of the IMAP spin angle, for the cases listed in Table 1. The upper subpanels show the absolute fluxes for the corresponding indirect and direct beams, for three different ionization rates: that obtained for photoionization of ISN He from Sokół et al. (2019a), marked as “β × 1.0,” and the rates increased or reduced by 30% (“β × 1.3” and “β × 0.7,” respectively). The DOY numbers for the indirect- and direct-beam pairs are listed in the upper subpanels. The lower subpanels show the corresponding energies of the direct and indirect beams, with the purple color used for the direct beams, and green for the indirect beams. Note that the spin-angle range adopted for flux integration is 72°–102°, i.e., it is much more narrow than that shown in the figure.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Contribution to the relative uncertainty of the ionization rate derived from pairs of beams of ISN He: indirect and direct in the left panel, and two direct beams in the right panel. The plots present decimal logarithm of the middle term in Equation (A1). The color scale is logarithmic; details are shown in the color bars. The dark color marks a low value, i.e., best suitable for determination of the ionization rate. The horizontal scale marks the DOYs for the first beam, and the vertical scale those for the second beam. The yellow dots mark the selected pairs of DOYs, listed in Table 1. The contributions in the right panel are symmetric relative to the equal DOYs. For identical DOYs for the direct beam, the contribution features singularity because determining the ionization rate from observations of one beam from one vantage point is impossible. See Appendix A.1.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Ratios of the spin-angle-integrated direct/indirect fluxes (the ﹩{ \mathcal F }﹩ ratios) of ISN He, simulated for the ionization model (2) (β ph × 1.0) and the ﹩{ \mathcal F }﹩ ratios for the ionization models (3), i.e., with the rate increased (β ph × 1.3) and decreased (β ph × 0.7) by 30%, are shown in the upper panel for the (indirect, direct) DOY pairs listed in Table 1. The lower panel presents the ratios of the β ph × 1.3 and β ph × 0.7 lines to the line β ph × 1.0 (solid lines). The dashed lines in this panel represent the corresponding cold-model-derived ratios defined in Equation (22) for α = ±0.3.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Upper panel: the ﹩{ \mathcal F }﹩ ratios for the ionization rates characteristic for the maximum of the solar activity, i.e., for the sum of photoionization and electron-impact rate (β 2015) and for the photoionization rate only, with electron-impact ionization neglected, for the solar maximum conditions (β ph,2015). At 1 au, the electron-impact ionization rate contributes ∼14% to the photoionization rate, and more than that with a decreasing distance from the Sun. The line marked as β ph,2015  × 1.14 presents the ﹩{ \mathcal F }﹩ ratio simulated for the ionization model where the photoionization rate is increased by 14% consistently for all distances, and electron-impact ionization is neglected. Lower panel: ratios of the respective ﹩{ \mathcal F }﹩ ratios shown in the upper panel.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Fluxes of the primary and secondary populations of ISN He, direct and indirect beams (upper panel), and the corresponding beam energies (lower panel) for a pair of the (direct, indirect) DOYs (case (3) in Table 1). In the lower panel, the blue line represents the energies for the indirect and direct beams of the primary population, and the green line those of the secondary population.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Relative uncertainties of the ionization rate of ISN He obtained from pairs of (indirect, direct) beams listed at the vertical and horizontal axes, respectively, due to the uncertainty of the inflow parameters of ISN He. The color code is provided in the adjacent color bar. The yellow dots mark the selected pairs of DOYs, listed in Table 1 and used in the analysis in Section 4. Note that these uncertainties are negligibly small as compared with those due to uncertainties in the measured flux ratios, and that their amplitude is small.
Paper: Determining the Ionization Rates of Interstellar Neutral Species Using Direct-sampling Observations of Their Direct and Indirect Beams
Authors: M. Bzowski, M. A. Kubiak, E. Möbius, N. A. Schwadron
Figure caption: Upper panel: distance from the Sun r(t) of indirect atoms inside 1 au as a function of days before detection. The DOYs of detection, listed in the panel, correspond to the indirect DOYs in Table 1. Lower panel: corresponding functions of radial modulation of the electron-impact ionization rate ﹩{\hat{\beta }}_{\mathrm{el}}(r(t))﹩, defined in Equation (2).
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The values of Δ λ(R) (red squares) and Δ N(R) (black circles) as a function of the angular separation R. Our choice of R assoc is marked by the vertical dashed line. It occurs when Δ λ(R) ≃ Δ N(R). Uncertainties on the average λ(R) values obtained by the crossmatches with mock catalogs were computed from their distributions at each R. The correspondent chance probability of having spurious associations at R = R assoc is then reported in the lower panel. Left panels correspond to the G4Jy catalog, used to extract the G4Jy-3CRE sample, while, for comparison, in the right panels we show the results of the same procedure applied to the 3CR sample. In the latter case we used NVSS coordinates similar to those adopted in the G4Jy catalog to estimate the brightness-weighted radio centroids at declinations above −39.°5. Considering that in the Southern Hemisphere the source sky density (i.e., number of sources per square degree) of mid-IR potential counterparts is ∼10% larger than that correspondent to the 3CR, results on these two different catalogs are in agreement.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Same as the left panel of Figure 3, but for G4Jy 171. The blue plus sign marks the position of the brightness-weighted radio centroid, while the red one marks that of the mid-IR and optical counterpart, associated with the radio core. The location of the radio core was identified thanks to the NVAS archival radio map at 1.4 GHz used also to draw radio contours overlaid to the mid-IR image. The radio core is not clearly detected in archival images of the TGSS, NVSS, and SUMSS. The angular separation between the two plus signs is ∼49″.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The DSS optical image, in the red filter, of the field including the two radio sources G4Jy 1748 and G4Jy 1749, the former one harbored in a galaxy cluster at z = 0.0281 and lying at an angular separation of ∼3.″6 (i.e., corresponding to ∼120 kpc at its redshift) from G4Jy 1749. Radio contours from the SUMSS at 843 MHz are overlaid in black, while those obtained from the GLEAM radio maps between 171 and 230 MHz are reported in cyan; the former ones start at a level of 0.1 Jy beam−1, while the latter ones start at 0.4 Jy beam−1, and both increase by a factor of 4.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: Left and middle panels: radio maps of G4Jy 513 at 1.4 and 4.9 GHz, respectively, retrieved from the NVAS. The frequency of each radio map from which radio contours were drawn is reported together with the intensity of the first level and the binning factor indicating how they increase. Right panel: the r-band optical image collected from one of the surveys used in our analysis, with three levels of radio contours drawn from the radio map at 4.9 GHz starting at 4.9 mJy and increasing by 0.5 mJy. No clear detection of the radio core and of a potential optical counterpart is reported for this radio source showing diffuse radio emission.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The redshift distribution obtained from our literature search for those 157 radio sources listed in the G4Jy-3CRE catalog with a z estimate. The red histogram includes also 12 radio sources with uncertain values, in comparison with that of radio sources with firm z measurements shown in gray.
Paper: Powerful Radio Sources in the Southern Sky. I. Optical Identifications
Authors: F. Massaro, S. V. White, A. García-Pérez, A. Jimenez-Gallardo, A. Capetti, C. C. Cheung, W. R. Forman, C. Mazzucchelli, A. Paggi, N. P. H. Nesvadba, J. P. Madrid, I. Andruchow, S. Cellone, H. A. Peña-Herazo, R. Grossová, B. Balmaverde, E. Sani, V. Chavushyan, R. P. Kraft, V. Reynaldi, C. Leto
Figure caption: The two radio galaxies G4Jy 1677 and G4Jy 1678 (aka NGC 7016 and NGC 7018) harbored in the galaxy cluster A374 and lying at an angular separation of ∼190″ (i.e., corresponding to ∼150 kpc at the galaxy cluster redshift). Radio contours from the TGSS and the VLASS archival images at 150 MHz and 3 GHz are overlaid, in blue and black, respectively, on the optical image in r band available in the Pan-STARRS database.
Paper: Observational Properties of 155 O- and B-type Massive Pulsating Stars 
Authors: Xiang-dong Shi, 相东 施, Sheng-bang Qian, 声帮 钱, Li-ying Zhu, 俐颖 朱, Liang Liu, 亮 刘, Lin-jia Li, 临甲 李, Lei Zang, 蕾 臧
Figure caption: The comparison between the temperature of Gaia ESP-HS and that of LAMOST derived by Guo et al. (2021) (LAMOST_Guo). Most of these targets give consistent results.