adsabs/AstroCLIMB huggingface dataset:
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The velocity profiles of [O I] λ6300 lines of 10 CTTSs in our sample. In each panel, the gray vertical dashed line indicates the center of the line, and the blue dashed line marks the wind velocity of the blueshifted wind or peak of the line. In a special case of HK Tau, we also show a green dashed line to represent the blueshifted wind velocity, which is likely originating from a companion of the binary system, HK Tau A, and the blueshifted peak velocity marked with a blue dashed line belongs to the other companion of the system, HK Tau B.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The time-series mass accretion rates of DL Tau and Haro 6-13 are shown in the top and bottom panels, respectively. The left axis shows the mass accretion rates derived from the TESS, ASAS-SN, and ZTF observations, while the right axis displays the corresponding accretion luminosities.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The distribution of mass accretion rates derived from all available emissions in the spectra of our CTTSs. The names of the stars marked with an asterisk in the upper right indicate that they are binary or multistar systems.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: Left panel: a burst event of DL Tau at BT–2,457,000 = 2504 was captured by TESS, ASAS-SN g, and ZTF g. Right panel: a burst event of Haro 6-13 at BT–2,457,000 = 2516 was observed by TESS, ZTF g, and ZTF r. In each panel, the black curve represents the burst event observed by TESS, and the green filled circles are g-band observations from the ZTF survey. The green open diamond represents the data from the ASAS-SN survey. In the case of Haro 6-13, the red filled circle represents the observation from the ZTF r band.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The flare frequency distribution and the best-fit power-law function with a slope of −0.68 ± 0.20 of our CTTS sample based on 13 detected flares in this study.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The velocity profiles of [S II] lines observed in the spectra of AA Tau and HL Tau. In each panel, the gray vertical dashed line indicates the center of the line, and the blue dashed line marks the wind velocity of the blueshifted wind or peak of the line.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The velocity profiles of [Ca II] lines of HL Tau. The gray vertical dashed line indicates the center of the line, and the blue dashed line marks the wind velocity of the blueshifted peak of the line.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The profiles of 13 flare events detected in the Section 43 and 44 TESS light curves of BP Tau (three flares), DN Tau (six flares), and FN Tau (four flares).
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The relationship between the flux asymmetry metric M and the disk inclination of our CTTSs is shown in the top panel, and the relationship between the periodicity metric Q and the disk inclination is shown in the bottom panel. Our samples are represented by rhombus symbols, with different colors indicating different variability classes. We also include the results obtained by Robinson et al. (2022) for M vs. inclination and by Cody et al. (2022) for Q vs. inclination as the comparisons, shown as yellow circles. The stars surrounded by black open circles in this diagram are binary or multistar systems. Note that the large uncertainty of HK Tau's inclination is because it is an unresolved binary system in LAMOST observations, which is composed of two companions, HK Tau A with i = 56.°9 and HK Tau B with i = 84°. The blue dashed lines in both panels indicate the thresholds of bursting (M < − 0.25), dipping (M > 0.25), periodic (Q < 0.15), and aperiodic (Q > 0.85).
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The comparison between CTTSs’ [O I] λ6300 projected wind velocities (vertical axis) and inclinations in terms of cosine angle (horizontal axis). The purple circles represent the data from Appenzeller & Bertout (2013), and the red circles are the data in this study.
Paper: Mass Accretion, Spectral, and Photometric Properties of T Tauri Stars in Taurus Based on TESS and LAMOST
Authors: Chia-Lung Lin, Wing-Huen Ip, Yao Hsiao, Tzu-Heng Chang, Yi-han Song, A-Li Luo
Figure caption: The relationship between the inclination and mass accretion rates derived from the Hα emission luminosities. The Pearson's correlation coefficient is about 0.34, indicating that the correlation is not significant.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Orbital alignment. Orbits of six KBOs of the Sedna family projected onto the ecliptic plane. The blue line is drawn parallel to the projection of ﹩{\hat{{\boldsymbol{n}}}}_{G}﹩ onto the ecliptic plane. The orbits and ﹩{\hat{{\boldsymbol{n}}}}_{G}﹩ lie essentially in the ecliptic plane, so the projection does not induce significant distortion. The major axes of the orbits are seen to align with the direction to the center of the galaxy, with the aphelion oriented toward the Galactic center. This result is intuitively plausible since the aphelion is the heavy end of the orbit in secular perturbation theory. The KBO orbital parameters used to generate this plot are taken from the Minor Planet Database of the International Astronomical Union.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Orbital dynamics in the quadrupole approximation. (a) Contours of fixed ﹩{{ \mathcal S }}_{Q}^{\mathrm{eff}}﹩ are wavy lines that extend across the ﹩({e}_{K}^{2},{\omega }_{K})﹩ plane for 3/5 ≤ h 2 ≤ 1. (b) For 0 ≤ h 2 < 3/5, the phase space is dominated by two fixed points. The contours of fixed ﹩{S}_{Q}^{\mathrm{eff}}﹩ are loops around the fixed points but remain wavy lines on the other side of the separatrix shown in red. The orbital elements thus precess along the wavy lines or oscillate about the fixed-point values around the loops. The phase-space flow is along the contours clockwise around the loops and from left to right (increasing ω  K ) along the wavy lines. The timescale of the dynamics is 107 yr for a KBO orbit with a semimajor axis of 1000 au.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption:  Phantom mass distribution. The phantom mass is rotationally symmetric about the z-axis and is localized at distances comparable to the MOND radius R  M . The Sun is at the origin, and the galactic center is on the positive z-axis. Distance along the axes is marked in units of R  M  = 7000 au, and the density ρ ph is in units of ﹩{M}_{\odot }/(4\pi {R}_{M}^{3})﹩. We take γ  N  = 0.9 a 0 consistent with the acceleration of the Sun toward the center of the galaxy (McGaugh 2018). An interesting feature is that the phantom mass distribution changes sign near the point where the Newtonian field of the galaxy and the Sun add up to zero.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Phase-space clustering. Plot of ﹩({e}_{K}^{2},{\omega }_{K})﹩ for the six KBOs of the Sedna family (blue points) and the location of the corresponding fixed point of the MOND orbital dynamics in the quadrupole approximation (red points). The two points for each KBO have been connected by a dashed line to guide the eye. The KBO orbital parameters used to generate this plot are taken from the Minor Planet Database of the International Astronomical Union.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: Plot of the phantom density harmonics ρ ph,ℓ  as a function of distance from the Sun for ℓ = 0 (blue), ℓ = 1 (green), and ℓ = 2 (orange). The density is in units of ﹩{M}_{\odot }/{R}_{M}^{3}﹩ and distance is in units of R  M . In generating these plots, we took γ  g  = 1.5a 0 as discussed in the main text. As expected the mass densities are peaked at a distance of the order of the MOND radius. The origin of the kinks at a common distance from the Sun is discussed in the Appendix text.
Paper: Modified Newtonian Dynamics as an Alternative to the Planet Nine Hypothesis
Authors: Katherine Brown, Harsh Mathur
Figure caption: The orbit of Planet Nine is taken to lie in the z–x plane with the Sun at the origin. The perihelion is assumed to lie on the positive z-axis. The multipole moments for this reference configuration are denoted J (0) and ﹩{{ \mathcal J }}^{(0)}﹩. The eccentric anomaly ξ is taken to be zero at perihelion and to increase clockwise in the figure. Also shown in the figure is the angle θ for an arbitrary point on the orbit. θ is the spherical polar colatitude of that point, and it also represents the true anomaly around the orbit.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: The normalized mass-weighted sine morte stellar metallicity distribution, evaluated at the position of the Sun and integrated over the range of the Milky Way disk we are modeling. Vertical lines show the range in [Fe/H] for which we model variations in the water mass fraction ﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ of ISOs
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: The best-fit values of the density modeling parameters for each monoabundance population with 20 or more observed stars, and ρ sm/n giants, the ratio between the sine morte stellar mass density and the red giant number density, explained in Section 2.3.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: Primary prediction for the distribution of ISO water mass fractions, evaluated at the position of the Sun and integrated over the Milky Way disk, for β = 1.
Paper: The Galactic Interstellar Object Population: A Framework for Prediction and Inference
Authors: Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, J. Ted Mackereth, John C. Forbes
Figure caption: Comparison of the [Fe/H] distribution of red giants and the [Fe/H] distribution of the sine morte stellar population around the Sun, both normalized. Though similar, there are subtle differences largely caused by the fact that the distribution of ages changes as a function of [Fe/H], as shown in Figure 1.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: RV time series and periodograms from analysis using RVSearch. (a) We plot the RV time series using the available data from CARMENES, HARPS (TERRA pipeline), HIRES (pre- and post-2004), and MAROON-X (red and blue arms). The blue line represents the detected signal from the known rotation period (2.71 days; Guinan & Engle 2018). (b) The time series residuals after the stellar rotation activity signal is removed. (c) The folded time series for the rotation period signal. (d) The periodogram before removing the rotation period signal. The highest peak corresponds to the rotation period signal (2.71 days), and the second peak corresponds to half the rotation period (1.4 days). (e) We find that the quantification of the strength of the detection for the 2.7 day signal as a function of the number of observations monotonically increases as expected. (f) The periodogram of the residuals after removing the 2.71 day signal from the stellar rotation period. We do not find evidence of any additional candidates above our false-alarm probability threshold (0.1%). The local peak at 4370 days corresponds to a ΔBIC = 7.0 (0.001 false-alarm probability corresponds to ΔBIC = 45.7).
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Simulated contrast curve for JWST broadband imaging at 21 μm. The solid black line shows the contrast in the raw image, the dashed black line is the residual after KLIP (assuming it is possible to achieve performance comparable to Rajan et al. 2015), and the dotted black line shows the photon noise limit from stellar flux. The dashed–dotted black line shows the 5σ noise limit due to background emission. The shaded blue region above the KLIP contrast line and background emission line indicates the parameter space where it should be possible to detect exoplanets. The apparent magnitude of cloudy 100 Myr and 1 Gyr, 0.12 M Jup exoplanets is shown by the red lines. This shows that a cloudy 100 Myr, 0.12 M Jup exoplanet should be detectable at separations of >1.5 au, and a cloudy 1 Gyr, 0.12 M Jup exoplanet is detectable at separations of >4 au. For this simulation, we assumed [F2100W] = 5.3 mag based on the star's WISE band 4 (λ = 22.2 μm) magnitude.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Simulated JWST NIRCam coronagraphic imaging 5σ contrast curves with the F444W filter. (Left) We show contrast curves simulated using PanCAKE for three NIRCam exposure times in ADI and RDI mode. We predict that if a cloudless exoplanet existed with a mass greater than 1 M Jup outside of ∼1.5 au, it would be detectable with 20 minutes of integration time. (Right) The NIRCam F444W 5σ ADI contrast curves were converted to mass space using the Linder et al. (2019) models with an adopted age of 500 Myr. We find that exoplanets larger than 1 Saturn mass will be detectable outside of 2 au if Wolf 359 is in the younger part of its age range. A Neptune-mass planet will be detectable beyond 6 au if Wolf 359 is younger than 500 Myr and a >10 hr exposure is used.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Simulated atmospheric models for Wolf 359 and a cloudless 1 M Jup companion. The modeled companion spectra shown correspond to ages of 100 Myr (orange), 500 Myr (green), and 1.5 Gyr (red). The simulated spectrum of the Wolf 359 host star is shown in blue. The estimates of the flux between 3.881 and 4.982 μm were used to determine the expected brightness and S/N for each companion type to simulate a NIRCam observation with F444W+MASK335R using PanCAKE.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Emission from a cloudy (solid lines) and clear (dashed lines) sub-Saturn (0.12 M Jup) at 100 Myr (blue) and 1 Gyr (red). The black line shows the emission from the star, Wolf 359, assuming an M5V spectral type. The black bars show the 3 hr, 5σ detection limits of NIRCam F444W and MIRI broadband imaging. At 21 μm, the contrast ratio between the star and a 100 Myr, 0.12 M Jup exoplanet is only 1120×. For the older exoplanet, the contrast ratio is 15,800×.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: RV survey completeness. We used the injection-recovery function within RVSearch to determine the completeness of our Wolf 359 RV survey as a function of the minimum planet mass and semimajor axis. Our analysis methods yield a 32% chance of recovering a signal that matched the Wolf 359 b candidate as described by Tuomi et al. (2019; green star).
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: Left: the distribution of 8 hr rms CDPP values for the Praesepe targets in blue, and for the full K2 data set in orange. The 1200 ppm cut-off is shown as the dashed line—it primarily removes faint, late-type M dwarfs. Right: the distribution of 8 hr/2 hr CDPP slope values for the targets below the 1200 ppm cut-off, with Praesepe shown in blue and the full K2 data set in orange. For white noise, the CDPP slope is expected to be 0.5—both distributions peak just above 0.5 and lie primarily between 0.5 and 1.0, indicating nonpathological light curves. The Hyades targets we investigated follow comparable noise patterns.
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: Left: the spatial distribution of the Praesepe cluster members on the sky observed by K2; targets observed in campaigns 5 and 18 are shown in blue, and targets observed in campaign 16 are shown in green. Right: the temperature, radii, and metallicity of the Praesepe cluster members with 8 hr rms CDPP < 1200 ppm. The stellar parameters are from the uniform catalog of K2 stellar parameters published in Hardegree-Ullman et al. (2020), and were derived using a random forest regression on photometry, trained on a large set of targets with LAMOST spectra; where the machine learning parameters were unavailable, they were supplemented with parameters from isochrone fitting.
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: The occurrence rates of hot sub-Neptunes with time, from the young TESS FGK stars (15–450 Myr) from Fernandes et al. (2023), to the intermediate-age (600–800 Myr) K2 Praesepe GKM sample studied here, to the field K2 GKM stars (3–9 Gyr). The age uncertainties capture the width of the age distributions in each case. The shaded regions indicate the putative timescales for the photoevaporation (<100 Myr) and core-powered mass loss processes (0.5–2 Gyr). The persistently high rate of hot sub-Neptunes at ∼700 Myr is more consistent with predictions of core-powered mass loss sculpting this population than with photoevaporation.
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: Praesepe planet candidates are shown as red stars, and Hyades planet candidates are shown as yellow plus symbols. The full K2 planet candidate catalog of Zink et al. (2020a) is shown in blue, and all confirmed planets at the NASA Exoplanet Archive (2023a) are shown in gray. The red box shows the hot sub-Neptune parameter space (1–10 days, 1.7–4 R ⊕) analyzed in Section 3.
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: The normalized distributions of the Praesepe GKM sample in orange and the field K2 GKM sample in blue, for stellar effective temperature (left) and stellar metallicity (right). The vertical dashed lines in the right panel are the median values of the distributions. The known supersolar metallicity of the Praesepe cluster is clear, although the distribution of our photometrically derived values is wider than what is seen spectroscopically (Boesgaard et al. 2013; D’Orazi et al. 2020). The systematic differences in the stellar samples necessitate an appropriate parametric model that can account for any known correlations.