adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Example Bayesian KLIP-FM Astrometry (BKA) results for the F410M filter, corresponding to the photometry and astrometry recorded in Table 2.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Following Figure 5, calibrated 5σ contrast curves and measured contrasts for each filter across the HR 8799 observations.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Post-starlight subtraction image library by filter, for F300M, F250M (LW detector) and F210M, F200W, and F182M (SW detector).  >5σ detections are labeled according to Table 2.
Paper: JWST-TST High Contrast: Living on the Wedge, or, NIRCam Bar Coronagraphy Reveals CO2 in the HR 8799 and 51 Eri Exoplanets’ Atmospheres
Authors: William O. Balmer, Jens Kammerer, Laurent Pueyo, Marshall D. Perrin, Julien H. Girard, Jarron M. Leisenring, Kellen Lawson, Henry Dennen, Roeland P. van der Marel, Charles A. Beichman, Geoffrey Bryden, Jorge Llop-Sayson, Jeff A. Valenti, Joshua D. Lothringer, Nikole K. Lewis, Mathilde Mâlin, Isabel Rebollido, Emily Rickman, Kielan K. W. Hoch, Rémi Soummer, Mark Clampin, C. Matt Mountain
Figure caption: Post-starlight subtraction image library by filter, for F460M through F335M.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: 1D radial profiles of Hα, [N II], and [S II] emission-line fluxes. Data points located within 6rPDR are represented as black crosses in each panel. The ID number is labeled in the upper left corner, and typical 1σ observational uncertainties are shown in the upper right corner. For each panel, the data are binned into 10 equally spaced intervals along the x-axis. The median value of each bin, after removing outliers, is represented by magenta filled circles, with error bars indicating the scatter. The solid magenta line represents the fitting result of the binned data points. The default order of the polynomial fit is set to 4, except for H II-03, H II-04, and H II-06, where it is set to 2. The detailed coefficients and corresponding errors are provided in Table A1. The red vertical solid line indicates rHα, derived from the 1D radial profile of Hα flux, representing the radius at which the Hα flux decreases to the background value. The green vertical solid line denotes rPDR.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: 1D radial profiles of the line flux ratios [N II]/Ha, [S II]/Ha, and [S II]/[N II]. Data points located within 6rPDR are represented as black crosses in each panel. The ID number is labeled in the upper left corner, and typical 1σ observational uncertainties are shown in the upper right corner. For each panel, the data are binned into 10 equally spaced intervals along the x-axis. The median value of each bin, after removing outliers, is represented by magenta filled circles, with error bars indicating the scatter. The solid magenta line represents the fitting result of the binned data points. The default order of the polynomial fit is set to 4, except for H II-03, H II-04, and H II-06, where it is set to 2. The detailed coefficients and corresponding errors are provided in Table A1. The red vertical solid line indicates rHα, derived from the 1D radial profile of Hα flux, representing the radius at which the Hα flux decreases to the background value. The green vertical solid line denotes rPDR.
Paper: Spatially Resolved Galactic H II Regions Observed by the LAMOST Medium-resolution Spectroscopic Survey of Nebulae (LAMOST MRS-N)
Authors: Wei Zhang, Yunning Zhao, Lin Ma, Shiming Wen, Chaojian Wu, Juanjuan Ren, Jianjun Chen, Yuzhong Wu, Zhongrui Bai, Yonghui Hou, Yongheng Zhao, Hong Wu
Figure caption: 1D radial profiles of VLSR for Hα, [N II], and [S II] emission lines. Data points located within 6rPDR are represented as black crosses in each panel. The ID number is labeled in the upper left corner, and typical 1σ observational uncertainties are shown in the upper right corner. For each panel, the data are binned into 10 equally spaced intervals along the x-axis. The median value of each bin, after removing outliers, is represented by magenta filled circles, with error bars indicating the scatter. The solid magenta line represents the fitting result of the binned data points. The default order of the polynomial fit is set to 5, except for H II-03 and H II-04, where it is set to 2, and for H II-06, where it is set to 3. The detailed coefficients and corresponding errors are provided in Table A2. The red vertical solid line indicates rHα, derived from the 1D profile of Hα intensity, representing the radius at which the Hα flux decreases to the background value. The green vertical solid line denotes rPDR.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Examples of the initial data products. For the top image and the bottom-left image, the y-direction is the cross-dispersion (spatial) direction and the x-direction is the spectral direction. Top: a UVIS flt file, where the zeroth order is imprinted in the center of the image, with the  ±1  orders spread to the left and right, respectively. Bottom: an IR ima file on the left and the acquisition image on the right. Color scales differ between images and are optimized to illustrate the spectra. In all images, all three stars in the system can be seen, with B and C much closer together than A. Notably, C is now the farthest star from A, instead of B as was the case with 2003 HST/NICMOS data shown in J. G. Winters et al. (2019).
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: UVIS (G280) white light curves for all three observed transits. The + 1 and  –1 orders are fitted separated and are shown on the top and bottom rows in red and blue, respectively. The raw light-curve data are shown in dark gray, with the light gray points in the + 1 order being the outlier points excluded in the white light-curve fits. The model fits to the data are shown as red and blue points, and their residuals are shown individually below each plot. The full phase model, along with the systematics-removed points, are shown offset above the raw data, seen as a solid line and black points, respectively.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Stellar contamination forward models based on D. K. Sing et al. (2011), assuming different spot temperatures and dimming fraction (variability) for time-averaged spots that are always present on the stellar disk. Top: blue lines represent a 3000 K cold-spot scenario, with the solid line representing the level of variability that can be rejected to 5σ and the dashed line the level of variability rejected to 2σ. Red lines are the analogous version for a 3600 K hot-spot scenario. Bottom: models rejected at 2σ are shown extrapolated out to JWST wavelengths, demonstrating that the change in transit depth due to cold/hot spot contamination that can be expected is on the order of 30–40 ppm. Mean transit depth is shown as a gray dashed line.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Top: comparison between the primary IR reduction detailed in this paper (WRECS), shown in purple, and the comparison ExoTiC-ISM reduction (offset by 148 ppm), shown in orange. A flat line, representing no atmosphere, is shown as a gray dashed line. The ﹩{\chi }_{\nu }^{2}﹩ value and σ rejection between the model and a flat line is shown in the legend for each reduction. Bottom: agreement between reductions, shown as the σ difference between the two. The reductions largely agree within 1σ.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Combined UVIS and IR spectrum, shown alongside the ground-based Magellan data from H. Diamond-Lowe et al. (2023). Mean depths and their corresponding 1σ errors are shown as solid lines and shaded regions, respectively. The HST mean depths for each instrument agree well.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: The IR (G141) white light-curve fits, with systematics removed, for both the forward (blue, on the left) and reverse (green, on the right) scans. The unbinned data are overplotted with the best-fit model, and the residuals for each fit are shown below. There is good agreement between the Rp/Rs values calculated from each fit (see Table 3.)
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: UVIS transmission spectrum for all three visits, with an offset of 2500 ppm applied between each visit to visually separate the spectra. + 1 and  −1 orders are shown separately in red and blue, respectively, allowing a comparison within each visit. The orders agree well, with all but two points agreeing within 2σ.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Best-fit stellar retrieval models using exoretrievals assuming the spectrum is due entirely to stellar contamination. The cases of cold spots only, hot spots only, and both cold and hot spots are shown in blue, red, and green, respectively. While all three scenarios are consistent with the UVIS data, none of them are well fit to the IR data.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Allan variance plot for the NIR spectroscopic data. This depicts (normalized) rms scatter versus bin size, where the data are binned in time. The solid red line represents the expected decrease in scatter as ﹩\sqrt{N}﹩ assuming Poisson statistics. Each gray line is a spectroscopic bin. One can see that there is negligible correlated noise.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: UVIS transmission spectrum for all three visits, showing the weighted mean of the + 1 and  −1 orders for each visit. The visits agree very well.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Top: stellar spectrum and light curve of LTT 1445C, showing a flare occurred in the fourth exposure of the third UVIS observation. The light curve is integrated from 0.2 to 0.4 μm, the region where the flare shows flux enhancement. Colored points in the light curve match their corresponding spectra. The post-flare spectra shown (in green) also demonstrate slightly increased flux in the same region. There also appears to be a second, smaller flux in the second orbit. Bottom: the flux ratio between the flare and quiescent state (red), the post-flare elevated state and a quiescent state (green), and two quiescent states (blue). The flare shows a flux enhancement factor of  ~2.25, but the Mg II emission line does not follow this trend. There are also chromospheric optical emission lines seen in the flare and even more so in the post-flare environment.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: Best-fit retrieval on combined UVIS and IR data using POSEIDON. CLR priors are used to allow for a high-mean-molecular-weight atmosphere. In purple is the atmosphere retrieval, compared to a flat line. 1 and 2σ confidence on the retrieval is shown in dark and light shaded regions, respectively. Histograms from the retrieved abundances of N2 and ﹩{\rm{HCN}}﹩ are shown on the right. ﹩{\rm{HCN}}﹩ is weakly favored but not detected at statistical significance.
Paper: An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Katherine A. Bennett, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Zafar Rustamkulov, Natalie H. Allen, Joshua D. Lothringer, Ryan J. MacDonald, Nathan J. Mayne, Guangwei Fu
Figure caption: 10×, 100×, and 1000×  solar metallicity forward models generated by TRIDENT assuming thermochemical equilibrium and C/O = 0.55. Each forward model is uniquely vertically shifted to find the minimum possible ﹩{\chi }_{\nu }^{2}﹩. This ﹩{\chi }_{\nu }^{2}﹩ value, along with the corresponding σ rejection, is reported in the legend. 1000×  solar metallicity is favored over lower-metallicity atmospheres.
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: Spectroscopic light curve fits for HST STIS G430L (visit 13 and visit 14, phased together). Left panel: detrended light curves (darker points), raw data from visit 13 (circles) and visit 14 (squares), and the best-fit transit model (solid lines). Each wavelength bin is offset vertically by an arbitrary constant for clarity and the binning wavelength range is shown above the posttransit baseline. Right panel: corresponding residuals in parts per million (ppm). The standard deviation of the residuals is reported in the residuals plot, we report two values that correspond to the two different visits.
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: HAT-P-26b retrieval posterior showing the distribution of the retrieved parameters from the HST + Spitzer transmission spectrum using ATMO for the best-fitting model (haze-only scenario). Contours corresponding to 1, 1.5 and 2σ are shown (blue). The 1D histograms show the parameters’ mean value and 1σ range (red).
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: Top: the raw and and detrended white light curves for each HST visit in the STIS G430L (green and orange) and STIS G750L gratings (purple). The best-fit light curve model is overplotted. Bottom: corresponding residuals from the white light curve fit are shown in the colored circles. The solid lines correspond to one times the standard deviation.
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: Broadband transmission spectrum of HAT-P-26b from HST STIS + WFC3 + Spitzer IRAC with the best-fitting model (black line) derived using the retrieval code ATMO. The work presented here is colored in orange using STIS G430L and G750L while the data from H. R. Wakeford et al. (2017) is shown in blue corresponding to WFC3 G102 and G141, and Spitzer IRAC. The best-fitting model is cloud-free and includes haze opacity. We show the results for model with hazes only with 1σ, 2σ and 3σ uncertainty in the dark to light gray shaded regions.
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: Same as Figure 2, but for one visit with the G750L grating.
Paper: HST SHEL: Revealing Haze and Confirming Elevated Metallicity in the Warm Neptune HAT-P-26b
Authors: Lakeisha M. Ramos Rosado, David K. Sing, Natalie H. Allen, Hannah R. Wakeford, Mercedes López-Morales, Nikolay K. Nikolov, Kevin B. Stevenson, Munazza K. Alam, Thomas M. Evans-Soma
Figure caption: Transmission spectrum comparison of HAT-P-26b from HST STIS G750L grating. The data points shown in purple correspond to the work done here and the ones in light blue to the analysis from H. R. Wakeford et al. (2017).
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: Likelihood distributions of absolute magnitude in the 2MASS K band for a randomly selected star from LAMOST DR10 with observation ID 116242. The top panels show the likelihood distributions calculated using Teff, ﹩{\rm{log}}\,g﹩, [Fe/H], and their associated uncertainties. The star’s parameters are Teff = 4427.28 K, ﹩{\rm{log}}\,g﹩ = 4.70 dex, and [Fe/H] = 0.04 dex, with respective uncertainties of 86.74 K, 0.14 dex, and 0.09 dex. The bottom left panel represents the selection function, while the bottom right panel shows the total likelihood (﹩{{ \mathcal L }}_{\,\rm{tot}\,}﹩), which is obtained by combining all the likelihoods from the top panels with the selection function. Only the likelihood distributions for the absolute magnitude in the 2MASS K band are shown, as the Gaia G band distribution is similar.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The distribution of uncertainties in effective temperature (﹩{\sigma }_{{T}_{{\rm{eff}}}}﹩), surface gravity (﹩{\sigma }_{\mathrm{log}\,g}﹩), and metallicity (σ[Fe/H]) for stars in the LAMOST DR10. Contour lines indicate the number density of stars, while the histograms on the top and right of each panel illustrate the frequency distribution of the atmospheric parameters and their uncertainties. The panels cover the entire range of values present in the LAMOST data, with typical values at the distribution peak being approximately 5600 K for Teff, 4.2 dex for ﹩{\rm{log}}\,g﹩, and −0.2 dex for [Fe/H], and typical uncertainties being approximately 40 K for Teff, 0.06 dex for ﹩{\rm{log}}\,g﹩, and 0.04 dex for [Fe/H].
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The interpolated isochrones grids, illustrating Teff and ﹩{\rm{log}}\,g﹩ as functions of absolute magnitudes in the 2MASS K band (ranging from −8 to 8 mag) and Gaia G band (ranging from −4 to 12 mag), with a step size of 0.001 mag. The [Fe/H] ranges from −3.0 to 0.5 dex, with steps of 0.01 dex. For each metallicity bin, 13 age steps are included, with ages ranging from ﹩{\mathrm{log}}_{10}(\,\rm{age}\,)=9﹩ to 10.2 dex, progressing in alignment with increasing metallicity.
Paper: A Catalog of Distance Determinations for 5 Million Stars in LAMOST DR10
Authors: Chengqun Yang, Xiang-Xiang Xue, Chao Liu, Hao Tian, Ling Zhu, Lan Zhang
Figure caption: The interpolation of MIST isochrones with [Fe/H] = 0.0 dex and an age of 1.0 Gyr, showing Teff and ﹩{\rm{log}}\,g﹩ plotted against absolute magnitudes in the 2MASS K band (MK, top panels) and Gaia G band (MG, bottom panels). Thick colored lines represent the original MIST isochrone, with different colors indicating different monotonic ranges. Red dots represent the results of a direct interpolation, which fails to capture nonmonotonic regions accurately. Black dots, obtained from multiple interpolations based on monotonic segments, align closely with the original isochrone.