adsabs/AstroCLIMB huggingface dataset:
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Channel maps of the 12CO (2-1) line. Each channel has a width of 4 km s−1. The central velocity of each channel is labeled in each panel. Only the C3 configuration data are used, and the synthesized beam is shown in the lower-left corner of each panel. The dashed lines in the channel of V lsr = 52 km s−1 show the directions of the identified four outflow components. The four crosses mark the four sources that we identify as the driving sources of these outflow components. From north to south (N–S), the four sources and their associated cores are source 1 (core A), source 2 (core B), source 14 (core C), and source 17 (core E).
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Histograms of temperature for the northern and southern CGM for both the warm and hot components. Marked in cyan are the North Polar Spur for the northern CGM and the Eridanus Enhancement for the southern CGM. Marked in black are the fields used in the stacked spectra. Near the bottom of each histogram is the median value for the data, with an uncertainty that is equivalent to the average uncertainty (90% confidence interval). This uncertainty serves to compare the typical uncertainty in the individual measurements to the distribution of measured values.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: Integrated map of the 12CO (2-1) line shown in grayscale, overlaid with integrated maps of the blueshifted and redshifted SiO emission shown in blue and red contours, respectively. The integrated velocity ranges of the lines are shown in the upper-right corner of the figure. The dashed lines show the directions of the identified four outflow components (same as those in the channel of V lsr = 52 km s−1 in Figure 19). The four crosses mark the four driving sources. From N–S, the four sources and their associated cores are source 1 (core A), source 2 (core B), source 14 (core C), and source 17 (core E).
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Histograms of EM (cm−6 pc) for the northern and southern CGM for both the warm and hot components. The colors follow Figure 3. Near the bottom of each histogram, the median value for the data is shown, with an uncertainty that is equivalent to the average uncertainty (90% confidence interval). This uncertainty serves to compare the typical uncertainty in the individual measurements to the distribution of measured values.
Paper: Massive Protostars in a Protocluster—A Multi-scale ALMA View of G35.20-0.74N
Authors: Yichen Zhang, Kei E. I. Tanaka, Jonathan C. Tan, Yao-Lun Yang, Eva Greco, Maria T. Beltrán, Nami Sakai, James M. De Buizer, Viviana Rosero, Rubén Fedriani, Guido Garay
Figure caption: (a) PV diagram of the SO2 line along a direction with maximum velocity gradient across source 1 (P.A. = 0°, the positive offset is toward the south). The combined data of C3, C6, and C9 configurations are used. The black contours show the model of an infalling-rotating envelope (see the text). (b) Same as panels (a) and (b), but for the CH3OH (42,2 − 31,2; E) line. The contours show the same model for the SO2 emission.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: HaloSat fields included in this analysis shown in Galactic coordinates. The Galactic center is in the middle of the figure. Each field is marked with its HaloSat catalog number. The green contour is the full response field of view, and the red contour is where the response drops to zero. The gaps in the upper left and lower right are the fields near the ecliptic poles, which were removed by the Sun angle selections.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: The blue line is the ROSAT R2/R1 ratio for a given APEC temperature. The orange lines mark the R2/R1 ratio for the LHB of 0.86, which corresponds to a temperature of kT = 0.084 keV.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Top: radial metallicity gradient as a function of Galactocentric radial distance of the Atari disk sample. Bottom: vertical metallicity gradient of the Atari disk as a function of [Fe/H]. Error bars denote the standard deviation in each bin and show the statistical uncertainty only.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Top: rotational velocity as a function of [Fe/H] resulting in a gradient of ∂V  ϕ /∂[Fe/H] = 13.22 ± 1.57 km s−1 dex−1. Bottom left: rotational velocity as a function of the Galactocentric radial distance R with a gradient of ∂V  ϕ /∂R = − 2.6 ± 0.4 km s−1 kpc−1. Bottom right: rotational velocity as a function of scale height Z with a gradient of ∂V  ϕ /∂∣z∣ = −8.96 ± 0.75 km s−1 kpc−1. Error bars denote the standard deviations throughout.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Top panel: distribution of our calculated parallax zero-points for our final sample of 36,010 stars with available RV measurements. Bottom panel: calculated parallax distances with the zero-point correction (black circles), those without the zero-point correction (gray circles), and the Bailer-Jones et al. (2021) values (blue circles) as a function of the mean value distances calculated using a space density prior. The blue solid line represents the one-to-one relation.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Distribution of the angular momenta of our final SMSS Atari disk sample for different Galactic radii (R) cuts. The distributions have the same x-axis range to allow visual comparisons of the shift of the peak of the L  z  distributions between different R bins. The selection procedure for this sample is explained in Sections 4.1 and 4.2.
Paper: The Atari Disk, a Metal-poor Stellar Population in the Disk System of the Milky Way
Authors: Mohammad K. Mardini, Anna Frebel, Anirudh Chiti, Yohai Meiron, Kaley V. Brauer, Xiaowei Ou
Figure caption: Toomre diagram for our halo, thick disk, and thin-disk stars, shown with yellow, red, and gray points, respectively. Blue dashed curves denote ﹩{v}_{\mathrm{tot}}=\sqrt{{U}_{\mathrm{LSR}}+{V}_{\mathrm{LSR}}+{W}_{\mathrm{LSR}}}=70﹩ and 180  km s−1.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The PDFs of the flare energies (left panel) and durations (right panel) of simulated flares. Types of flares (A, B, C, M, and X) are identified based on the GOES classification system. A power-law function is fitted to both distributions. The power indices are 1.45 ± 0.02 and 1.71 ± 0.02, with p-values of 0.98 and 0.90 for the left and right panels, respectively.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The HXR emissions of a solar flare registered by the Yohkoh satellite. The flaring event occurred at 17:09 on 1998 March 1 and was recorded by the HXT instrument in different energy bands (L: 13.9–22.7 keV, M1: 22.7–32.7 keV, M2: 32.7–52.7 keV, and H: 52.7–92.8 keV). The vertical axis represents the average count rate over the 64 spatially modulated subcollimators (SC).
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The normalized PSDs of the HXR emissions of a solar flare (Figure 3) registered in four different energy bands (L, M1, M2, and H) by the Yohkoh satellite. The frequency (period) components are extracted by applying the Lomb–Scargle periodogram. The horizontal lines represent the FAP significance levels of 50%, 10%, 1%, and 0.01% shown in red, yellow, purple, and green, respectively. The top panels correspond to the smoothed time series (Equation (11)) while the bottom panels are obtained for normalized time series (Equation (10)).
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: Histograms of the extracted periods for the simulated QPPs for (a) D ≤ 50 s and (b) D > 50 s. Panel (c) exhibits the combined number of periods of both regimes. The global maxima of the lognormal distributions are located at 33.66 ± 0.71 s and 29.29 ± 0.67 s for panels (b) and (c), respectively. The goodness-of-fit is assessed applying both the R-squared statistics and the KS-test.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The simulated QPPs of Figure 2 vs. the ARIMA(4, 1, 5) model (top left panel), the obtained residual (bottom left panel), and the ACF of the residuals (right panel).
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The log-frequency presentation of the PSDs for some of the simulated events.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: Scatter plots of the extracted periods for the simulated QPPs vs. the host flare durations (top panel) and energies (bottom panel). The black rectangles illustrate some examples of the QPPs for which multiple periods are detected.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The AICs of 900 ARIMA models applied on the simulated QPPs of Figure 2 with p, q = 1, …, 30, and d = 1.
Paper: Do Cellular Automaton Avalanche Models Simulate the Quasi-periodic Pulsations of Solar Flares?
Authors: Nastaran Farhang, Farhad Shahbazi, Hossein Safari
Figure caption: The ACF (left panel) and PACF (right panel) of the time series of the simulated QPPs presented in Figure 2.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: A section of an ELiXer report for detection ID 2100325857, the line from an LAE in our sample. The report contains information about the detected line and imaging at the detection position. The 2D spectra from the four fibers contributing the highest S/N to the detection are in the upper left corner; the stacked signal is shown on the top row, outlined in black. The pixel flats and smoothed 2D spectra are displayed in the right two columns. Plots to the right show the sky subtraction and the emission-line model fit (black line). The middle row contains 10″ imaging cutouts, with the fiber positions shown in gray in the first image and the locations of cataloged sources marked with colorful boxes in all subsequent images. White boxes indicate sources too far to be considered, and white circles show the aperture for brightness measurement in F606W. The AB magnitude of the nearest likely source is reported. The upper right corner shows the photo-z probability distributions calculated by the CANDELS team (B. Andrews et al., in preparation) for sources of matching color in the imaging, and the [O II] and Lyα redshifts are shown as vertical dashed green and red lines. Finally, the bottom row shows the full 1D spectrum. Flux densities have units of erg s−1 cm−2 2 Å−1.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: An example of the visualizations used to select imaging counterparts for Lyα detections. The figure shows a 10″ image cutout with the detection positioned marked with a magenta star and sources marked with crosses of various colors, 1D spectra extracted at each source position, the original detection 1D spectrum, and SED fits (with redshift fixed assuming Lyα emission) of all sources with significant measured fluxes. The table in the upper right corner contains the χ 2 value of each SED fit, the separation between each source and the emission-line detection position (labeled θ), and the significance (labeled S/N) and the line flux in erg s−1 cm−2 of the emission line extracted at the source position. The colors are consistent across all plots and tables, so each source corresponds to a unique color. The SED plots also contain normalized filter response curves as gray lines. In this case, while the red and orange sources have similarly small distances from the detection position and similar line fluxes, the SED fit χ 2 strongly favors the orange source to be an LAE at z = 2.90.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: A section of an ELiXer report, in the same format as Figure 1, for detection ID 2100037191, corresponding to the [O II] λ λ3726, 3729 feature in a galaxy at z ≈ 0.24. The black trace in the 2D fiber spectrum (blue rectangle) indicates a clear detection of continuum emission, which is also evident in the 1D spectrum in at the bottom of the figure. The imaging shows a large, bright source (m AB = 22.0) centered on the detection position, and the source has a cataloged spectroscopic redshift consistent with [O II] indicated as an open blue circle in the photometric redshift plot in the upper right corner.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The distributions, expressed as the fraction of objects in a given bin, of (a) separation, (b) position-extracted emission-line S/N (relative to that of the detection), and (c) SED χ 2 assuming z Lyα , for objects identified as the detection imaging counterparts and those that happened to be spatially coincident. Histograms are normalized to the population size. The top panel indicates that finding a counterpart with an imaging separation larger than 1″ from the detection position is exceedingly rare.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The fractional error between I-band (F775W) fluxes of sources measured in our derived stacked-detection catalog matched to sources in the original catalog from Finkelstein et al. (2022) as a function of flux in the latter catalog. The median offset is indicated with the dashed pink line, and its value is given with text, showing good agreement between these two catalogs.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The distribution of P(Lyα) for detections visually classified as low-redshift galaxies (light blue) and high-confidence (scores of 4 and 5) LAEs (light red). Adopting a minimum threshold for P(Lyα) can remove a large fraction of low-redshift interlopers without eliminating very many LAEs.
Paper: Stellar Populations of Lyα-emitting Galaxies in the HETDEX Survey. I. An Analysis of LAEs in the GOODS-N Field
Authors: Adam P. McCarron, Steven L. Finkelstein, Oscar A. Chavez Ortiz, Dustin Davis, Erin Mentuch Cooper, Intae Jung, Delaney R. White, Gene C. K. Leung, Karl Gebhardt, Viviana Acquaviva, William P. Bowman, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Wolfram Kollatschny, Martin Landriau, Chenxu Liu, Daniel N. Mock, Ariel G. Sánchez
Figure caption: The distribution of visual classifications of candidate detections. Making cuts based on P(Lyα) to remove low-z sources can dramatically reduce the visual inspection workload.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Disk surface temperature versus radius with a sublimation region for two models of a M * = 0.3 M ⊙ star, on the left with ﹩\dot{M}=1\,\times \,{10}^{-7}{M}_{\odot }\,{\mathrm{yr}}^{-1},{R}_{* }=1.6{R}_{\odot },{R}_{\mathrm{in}}=2.7{R}_{\odot },{T}_{0}\,=\,6000﹩ K and on the right with ﹩\dot{M}=1\,\times \,{10}^{-5}{M}_{\odot }/\mathrm{yr},{R}_{* }={R}_{\mathrm{in}}=1.6\ {R}_{\odot },{T}_{0}\,=\,3400﹩ K. The disk with the lower accretion rate (left) is cut into three rings: the inner gaseous region, with luminosity mainly from the viscous heating; the intermediate sublimation region, which radiates like a 1400 K blackbody; and the outer dusty region, with luminosity mainly from the superheated surface dust layer. The disk with the higher accretion rate (right) is cut into three rings: the inner gaseous region, keeping its temperature via viscous heating; the hotter dusty region, keeping its temperature via viscous heating; and the cooler dusty region, receiving energy from stellar radiation.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Schematic view of magnetospheric accretion. The accretion flow, displayed as a slice in the yz-plane, starts from the disk surface (not shown, in the xy-plane) at a range of radii (R M, curly brackets), follows the trajectories specified in Equation (11), and reaches the star at a range of polar angles (θ M, with ﹩{\theta }_{{\rm{M}},\min }﹩ and ﹩{\theta }_{{\rm{M}},\max }﹩ annotated). The accretion shock area A shock is colored in cyan on the stellar surface. In Equation (13), the flux is integrated from area elements (blue) with the normal vector (θ, ϕ). The normal vector forms an angle γ with the normalized vector pointing to the observer, which has spherical coordinates (i, 0).
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Schematic view of the star–disk system, adapted from Figure 1 in Hartmann et al. (2016), with magnetospheric accretion and the four emission components (shown as squiggle arrows) in our models. The disk temperature decreases with radius, forming an inner gas disk where the temperature is hotter than the dust sublimation temperature T sub = 1400 K and a dust disk further outside. The gas disk is assumed to be geometrically thin. If the accretion rate ﹩\dot{M}﹩ increases, the disk inner boundary will move inward until the disk material directly reaches the star (see the definition of R in in Section 2.1).
Paper: Testing Model-determined Temperatures in the Hyades: A Bayesian Approach
Authors: Elizabeth J. Jeffery, Benjamin J. Taylor, Michael D. Joner
Figure caption: Comparison of photometric temperatures measured by TJJ and individual stellar temperatures determined by BASE-9 for each model set, normalized by photometric temperature. Also included (bottom right) is a comparison of the photometric temperatures to spectroscopic temperatures from Cummings et al. (2017) and Paulson et al. (2003), as available. The stars from the Cummings et al. (2017) sample are plotted as blue squares, while those in the Paulson et al. (2003) study are plotted as red circles.
Paper: Testing Model-determined Temperatures in the Hyades: A Bayesian Approach
Authors: Elizabeth J. Jeffery, Benjamin J. Taylor, Michael D. Joner
Figure caption: Comparison of photometric temperatures measured by TJJ and individual stellar temperatures determined by BASE-9 for each model set, normalized by TJJ’s photometric temperature.