adsabs/AstroCLIMB huggingface dataset:
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Color–magnitude diagram of the primary sample of M dwarfs. The error bars represent the average values and the 1σ uncertainties of G magnitudes with a color step of 0.5 mag, and the black dashed line is the first-order polynomial fit to the average values. The oblique red-dashed lines are created by shifting the black line up and down by 1σ uncertainty on G magnitude. The objects lying within the red-dashed box are selected.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Histograms of differences between ASPCAP and StarHorse (top row), and Qiu23 and StarHorse (bottom row). The red-dashed curves are Gaussian fits to the distributions, and the mean and dispersion of the Gaussian fits to the mean and standard deviation values of the differences.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The sky distribution of the “footprints” of the 671,654 M-type stars selected from LAMOST DR11, indicated by red for giants and blue for dwarfs. The map is projected using equatorial coordinates.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Color–magnitude diagram of the sample of 160 added stars, color coded by the logg values.
Paper: The Statistical Analysis of GeV Spectral Breaks in Bright Gamma-Ray Flat-spectrum Radio Quasars
Authors: K. R. Zhu, J. M. Chen, L. Zhang
Figure caption: The fitting results of the 15 yr average gamma-ray spectra for 87 bright FSRQs. Red line and red area: best-fit line and its 1σ confidence region for LP model. Green line and green area: best-fit line and its 1σ confidence region for the BPL model. Black dashed line: extension line for the low-energy power-law component of the BPL model. Black (blue) dots: real SED data significant at 5σ (3σ). Gray area: spectrum break energy range. Blue area: fractional difference between the two model fit lines.
Paper: The Statistical Analysis of GeV Spectral Breaks in Bright Gamma-Ray Flat-spectrum Radio Quasars
Authors: K. R. Zhu, J. M. Chen, L. Zhang
Figure caption: Distribution of part BPL fitting parameter: (a) the spectral break energy and the redshift; (b) the low-energy spectral index and the high-energy spectral index; (c) the redshift and the change in spectral index. The black points represent 87 bright FSRQs in this study; the red points show A. A. Abdo et al. (2010)'s fitting results for 12 bright FSRQs; the blue points represent J. Poutanen & B. Stern (2010)'s fitting results for nine bright FSRQs; green points are J. Harris et al. (2012)'s fitting results for nine bright FSRQs.
Paper: The Statistical Analysis of GeV Spectral Breaks in Bright Gamma-Ray Flat-spectrum Radio Quasars
Authors: K. R. Zhu, J. M. Chen, L. Zhang
Figure caption: The normalized energy spectra of 87 bright FSRQs in the observed frame (left panel) and their rest frames (right panel). The gray lines represent the normalized gamma-ray spectra of individual samples, the red lines represent the average gamma-ray spectra estimated through Monte Carlo sampling, and the red dashed lines indicate the 1σ confidence region. The blue dashed lines represent the spectral break energy range.
Paper: The Statistical Analysis of GeV Spectral Breaks in Bright Gamma-Ray Flat-spectrum Radio Quasars
Authors: K. R. Zhu, J. M. Chen, L. Zhang
Figure caption: The distribution of ΔAIC in 87 bright FSRQs. The black dashed line represents the Gaussian fitting line.
Paper: Ultra-long-period Cepheids as Standard Candles from Gaia to Rubin-LSST
Authors: Ilaria Musella, S. Leccia, R. Molinaro, M. Marconi, F. Cusano, M. Di Criscienzo, G. Fiorentino, V. Braga, V. Ripepi, G. De Somma, M. Gatto, E. Luongo, T. Sicignano
Figure caption: The effect of a 10% (left panels), 30% (center panels), and 50% (right panels) blending on the recovered magnitude (upper panels) and amplitudes (bottom panels) for the model C (see Table 3) located in the galaxy NGC 55. The differences plotted correspond to the model value (mag T  and Amp T ) minus the recovered one for each considered blend (magrec  X  and Amprec  X ). The color code is the same as in Figure 10.
Paper: Ultra-long-period Cepheids as Standard Candles from Gaia to Rubin-LSST
Authors: Ilaria Musella, S. Leccia, R. Molinaro, M. Marconi, F. Cusano, M. Di Criscienzo, G. Fiorentino, V. Braga, V. Ripepi, G. De Somma, M. Gatto, E. Luongo, T. Sicignano
Figure caption: The effect of a blending of 10%, 30%, and 50% on the recovered light curves for the model C (see Table 3) located in the galaxy NGC 55. See text for details.
Paper: Six Maxims of Statistical Acumen for Astronomical Data Analysis
Authors: Hyungsuk Tak, Yang Chen, Vinay L. Kashyap, Kaisey S. Mandel, Xiao-Li Meng, Aneta Siemiginowska, David A. van Dyk
Figure caption: Upper panel: Comparison of the power (i.e., the probability of rejecting the null hypothesis when it is false) of a conditional (dashed curve) and unconditional (solid curve) goodness-of-fit test based on the C-statistic. We compare the uniform null model given in Equation (1) with s  i ( θ ) = λ to a particular alternative model with s  i ( θ ) varying linearly between 2 and 9. The power obtained from the conditional test is uniformly higher than that of the unconditional test. The dotted–dashed vertical line indicates the significance level of the 3σ threshold (i.e., 0.0027), while the dotted vertical line represents the 2σ threshold (0.05). Bottom panel: Percentage improvement in power as a function of the statistical significance level. With the 3σ threshold, indicated by the dotted–dashed vertical line, the power improves by 31.4%. At the 2σ threshold, denoted by the dotted vertical line, the power improves by 16.4%.
Paper: Six Maxims of Statistical Acumen for Astronomical Data Analysis
Authors: Hyungsuk Tak, Yang Chen, Vinay L. Kashyap, Kaisey S. Mandel, Xiao-Li Meng, Aneta Siemiginowska, David A. van Dyk
Figure caption: A simulation study where the posterior mass accumulates near the boundary of a uniform prior distribution. The uniform prior distribution of the second parameter is bounded between −0.2 and 0.2, and the posterior mass clearly concentrates on the upper bound. In general, when a uniform prior distribution is used, it is important to check the sensitivity of the resulting posterior distribution to the choice of hard bound on the prior, unless there is a specific scientific justification for the choice of bound.
Paper: Six Maxims of Statistical Acumen for Astronomical Data Analysis
Authors: Hyungsuk Tak, Yang Chen, Vinay L. Kashyap, Kaisey S. Mandel, Xiao-Li Meng, Aneta Siemiginowska, David A. van Dyk
Figure caption: The posterior distribution of the time delay under the microlensing model. The top panel is based on the uniform (−1178.939, 1178.939) prior distribution for the time delay parameter, while the bottom panel is based on the uniform (430, 1178.939) prior distribution. In the bottom panel, the posterior mass accumulates near the lower bound, which may be evidence of misspecification of the prior distribution.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Right panel: the Kiel diagram of the empirical sample. The color is coded by the metallicity [M/H]. The dashed lines represent the isochrones from the PARSEC model with different metallicities at the same age of 3 Gyr, i.e., −0.6, −0.2, and 0.2 dex for the red, blue, and black lines, respectively. Left panel: histograms of logg for [M/H] values less than −0.5 dex.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Left column: histograms showing the differences between the derived parameters (T eff, [M/H], and logg) in the internal cross-validation process and their stellar labels. Right column: black points indicate the stellar labels, while red lines point to the derived parameters in the internal cross-validation process.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Examples of spectra clusterings for eps values of 1.0 (top panel) and 2.0 (bottom panel). The gray lines show all the spectra in the parameter bin of T eff: 3550–3600 K, logg: 4.7–4.8 dex, and [M/H]: −0.3 to 0.4 dex, while the red lines show the spectra that form a cluster.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Surface gravity comparison between dwarf and giant spectra of the same metallicity and temperature for the entire spectrum. The black (red) line shows the dwarf (giant) spectrum. The Na-line pairs around 7680 and 8190 Å, which are sensitive to logg, are labeled.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Effective temperature variations for the same surface gravity and metallicity. The different colors of lines represent different T eff values. The T eff-sensitive TiO bands around 7050 and 8430 Å are labeled.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Comparison diagrams of the testing set between the true and predicted values for T eff (top panels), logg (middle panels) and [M/H] (bottom panels). The left column shows one-to-one comparison diagrams and the right column shows the histograms of differences.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The LASPM-derived Kiel diagram of LAMOST DR11. The color is coded by the metallicity [M/H]. The dashed lines represent the isochrones from PARSEC model with different metallicities at the same age of 3 Gyr, i.e., −0.6, −0.2, and 0.2 dex for the red, blue, and black lines, respectively.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Metallicity comparison between spectra of the same surface gravity and temperature for the entire spectrum. The different colors of lines represent different [M/H] values.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The loss function of the fifth training session with a sampling interval of 100.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The left column shows density plots comparing the LASPM results with those from StarHorse for M dwarf stars. The right column shows histograms of differences: no systematic shift was noticed. The correlation coefficient between LASPM and StarHorse [M/H], omitting data points with errors exceeding one standard deviation (1σ), is presented.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The left column shows density plots comparing the LASPM results with those from StarHorse for M giant stars. The right column shows histograms of differences: no systematic shift was noticed. The correlation coefficient between LASPM and StarHorse [M/H], omitting data points with errors exceeding one standard deviation (1σ), is presented.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Histograms of ϵ for T eff (left), logg (middle), and [M/H] (right). The unbiased estimator, ϵ, was derived from parameter estimates of multiple observations with a spectral S/N greater than 10.0 for the same M-type stars. The histogram is fitted by a Gaussian shown as the red-dashed curves. The parameter precision (1σ uncertainty) for the three parameters is labeled.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Comparison of the stellar parameters derived from LASPM to the adjusted parameters of ASPCAP for M giants, where adjusted_T eff = T eff − 156 (K), adjusted_logg = logg − 0.16 (dex), and adjusted_[M/H] = [M/H] + 0.17 (dex). The left column shows one-to-one comparison diagrams and the right column shows the histograms of differences.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Comparison of the stellar parameters derived from LASPM to the adjusted parameters of ASPCAP for M dwarfs, where adjusted_T eff = T eff − 87 (K), adjusted_log g = log g + 0.05 (dex), and adjusted_[M/H] = [M/H] + 0.02 (dex). The left column shows one-to-one comparison diagrams and the right column shows the histograms of differences.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Kiel diagram of all stars of LAMOST DR9 (upper) and DR11 (lower), color coded by the density. The stellar parameter catalog for M-type stars has been updated in DR10, which is a subset of DR11.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: The parameter errors at different S/Ns in terms of T eff (top), logg (middle), and [M/H] (bottom). The error bars in red represent the parameter errors in different S/N bins, with a step of 5.0.
Paper: An Empirical Sample of Spectra of M-type Stars with Homogeneous Atmospheric-parameter Labels
Authors: Bing Du, A-Li Luo, Song Wang, Yinbi Li, Cai-Xia Qu, Xiao Kong, Yan-xin Guo, Yi-han Song, Fang Zuo
Figure caption: Comparison of the metallicity derived from LASPM to the metallicity of Qiu24. The upper panel shows density plots of direct comparison diagrams and the lower panel shows the histograms of differences.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The fitting parameters of SLF variability, α 0, ν char, and γ as a function of various stellar parameters including mass, radius, fractional main-sequence age (τ age), and wind mass-loss rate (log ﹩\dot{M}﹩). Each star is represented as a circle and color coded by spectroscopic luminosity. The data sets of individual stars observed in different sectors are connected by red lines.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The locations of stars in our sample are represented as gray circles in the spectroscopic Hertzsprung–Russell diagram. The size of each circle is directly proportional to ν char (left panel) and ﹩\mathrm{log}({\alpha }_{0}\,[\mu \mathrm{mag}])﹩ (right panel). Evolutionary tracks are depicted as gray solid lines. Additionally, the simulation results of ν char and ﹩\mathrm{log}({\alpha }_{0}\,[\mu \mathrm{mag}])﹩, computed by M. Cantiello et al. (2021), are illustrated as black contour lines in the spectroscopic Hertzsprung–Russell diagrams.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: Correlation between the fitting parameters of SLF and spectroscopic measured of v macro. Each star is depicted as a circle and color coded based on spectroscopic luminosity. The data sets of individual stars observed in different sectors are connected by red lines. The Spearman’s rank correlation coefficient (denoted as R) and the corresponding two-sided p-value (obtained from a t-test) are presented in each panel.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: Dependence of the fitting parameters of SLF variability on the log(﹩{ \mathcal L }/{{ \mathcal L }}_{\odot }﹩) (top panels) and T eff (bottom panels). Each star is represented as a circle and color coded by v macro in kilometers per second. The data sets of individual stars observed in different sectors are connected by red lines.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The significant linear correlation between the ν char and stellar radius for stars with M ≥ 30 M ⊙. Each star is represented as a circle, color coded according to its age τ age. The data sets of individual stars observed in different sectors are connected by red lines. The circle size is directly proportional to the stellar mass. The Spearman’s rank correlation coefficient (denoted as R) and the corresponding two-sided p-value (obtained from a t-test) are presented in upper right corner.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The significant correlation between the γ and stellar radius for stars with R ≳ 15R ⊙. The markers have the same meaning as in Figure 7.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: The scaling relation between characteristic frequencies (ν char) as a function of ﹩g\cdot {T}_{\mathrm{eff}}^{-1/2}﹩ (top panel), and the scaling relation between the amplitude and ﹩{({g}^{2}M)}^{-1/4}﹩ (bottom panel) are illustrated. The markers in each panel have the same meaning as in Figure 6.
Paper: A Study of Stochastic Low-frequency Variability for Galactic O-type Stars
Authors: Dong-Xiang Shen, Chun-Hua Zhu, Guo-Liang Lü, Xi-zhen Lu, Xiao-long He
Figure caption: Evolution of the radial locations of the iron convective regions as function of time for stars with different masses. The inset illustrates a magnified view of the radial locations of the iron convective regions for stars transitioning from the zero-age main sequence to the mid-main sequence.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Top: representative stellar spectra (F  λ (λ)) normalized to have the same peak flux, from three stars (A0, G5, M5 types; A. J. Pickles 1998), compared with the transmission curves for six HST/WFC3 filters spanning the UV (F275W, F336W), optical (F475W, F184W), and NIR (F110W, F160W), to illustrate how distinguishing between intrinsic stellar properties (i.e., variation in temperature between A0 and M5 stars) and the effects of dust reddening requires broad wavelength coverage. Bottom: dust extinction curves of varying R  V  and curve shape.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Example three-color images of fields in the SMC (top) and LMC (bottom) with (left) and without (right) extended emission. Images were created using aplpy by normalizing the observed flux range from the F814W (red), F475W (green), and F336W (blue) filters from WFC3. Three-color (or two-color where F336W is not available) images for all fields are available as part of our data release.
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Cumulative distribution functions of ancillary tracers of the ISM at the position of Scylla fields in the SMC (orange) and LMC (blue). (a) Dust surface density (Σdust; C. J. R. Clark et al. 2023); (b) H I column density (N(HI); S. Kim et al. 1999; N. M. Pingel et al. 2022); (c) Hα emission (I Hα ; J. E. Gaustad et al. 2001); (d) dust temperature (T dust; C. J. R. Clark et al. 2023); (e) 24 μm intensity (I 24μm; K. D. Gordon et al. 2011).
Paper: Scylla. I. A Pure-parallel, Multiwavelength Imaging Survey of the ULLYSES Fields in the LMC and SMC
Authors: Claire E. Murray, Christina W. Lindberg, Petia Yanchulova Merica-Jones, Benjamin F. Williams, Roger E. Cohen, Karl D. Gordon, Kristen B. W. McQuinn, Yumi Choi, Clare Burhenne, Karin M. Sandstrom, Caroline Bot, L. Clifton Johnson, Steven R. Goldman, Christopher J. R. Clark, Julia C. Roman-Duval, Karoline M. Gilbert, J. E. G. Peek, Alec S. Hirschauer, Martha L. Boyer, Andrew E. Dolphin
Figure caption: Maps of the peak brightness temperature of 21 cm emission in the LMC (S. Kim et al. 1999) and the SMC (N. M. Pingel et al. 2022), overlaid with observed Scylla fields. In each panel, regions where fields overlap are identified by dashed red bounding boxes and expanded at right. There are 96 fields as part of the release described in this paper, 48 in the SMC and 48 in the LMC. The number of filters used to observe each field is illustrated by the number of concentric circles overlaid at each position. Each field is tagged by its “short” name number (see Table 8). In the expanded panels, the size of each footprint is plotted in white outline.