adsabs/AstroCLIMB huggingface dataset:
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: As Figure 17, in the case of a 9.20 M ⊙ model during the phase in which a convective core induced by the 25(Mg, Na) URCA pair is formed. The vertical gray dashed line marks the 25(Mg, Na) URCA shell.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 21 but zoomed in on the inner 0.03 M ⊙.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected central quantities as a function of the central density of the 9.2 M ⊙ model during the activation of the 25(Mg, Na) pair: temperature (red line, left y-axis), adimensional entropy per baryon (green line, right y-axis), and nuclear (purple), gravitational (blue), and neutrino (magenta) energies (right y-axis).
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: 1–300 GeV photon indices and fluxes of blazars with bright flares. Only data points with TS > 9 are plotted. The blue dashed horizontal lines indicate the average photon indices of those data. The insets show the photon index resulting from an analysis where photons were sorted in five bins using 5 day fluxes plotted vs. the 5 day flux (red points).
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: The correlation between 1 and 300 GeV photon indices and the luminosity of 74 blazars. The solid lines represent the fitting results of the linear regressions.
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: The redshift distribution of each type of blazar in the sample. The histogram is illustrated in five bins, which are 0 ∼ 0.2, 0.2 ∼ 0.4, 0.4 ∼ 0.6, 0.6 ∼ 0.8, and 0.8 ∼ 1.0. The blue bar stands for BCU, the orange bar stands for FSRQ, the green bar stands for HBL, the red bar stands for IBL, and the violet bar stands for LBL.
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: Flare profiles for six TeV blazars with a single sharp peak in their 5 day binned light curves; an analytic function (dashed red curve) was used to fit the profile.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Convective (green shaded areas) and chemical (color codes reported in the color bar) internal history of selected models from the main-sequence phase up to an advanced stage of the TP-SAGB phase (top and middle left panels) or the onset of the iron core collapse prior to the CCSN explosion (middle right and bottom panels). The dashed line in the top and middle left panels marks the onset of the TP phase. The x-axis reports the logarithm of the time until the end of the evolution (t fin − t) in units of years.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolutionary path in the H-R diagram of selected models. The blue line refers to the AGB star, i.e., the one that develops a degenerate CO core, does not ignite C burning, and enters the TP phase. The red lines refer to SAGB stars, i.e., those that ignite C burning and then do not ignite Ne burning; these stars develop a degenerate ONeMg core and enter the TP phase. The black lines refer to those stars that ignite Ne burning and eventually explode as CCSNe. The horizontal green dashed line marks the final luminosity of the lowest mass that explodes as CCSNe, i.e., the expected minimum luminosity of CCSNe (Smartt 2015).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Central 12C mass fraction at core He depletion (black line and dots) and at first thermal pulse (red line and dots). The blue line refers to the mass of the central zone where the 12C mass fraction is larger than 0.01. The figure shows that the models with initial mass between 7.5 and 8.8 M ⊙ form a hybrid degenerate CO core.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: He core mass at various evolutionary stages (see legend).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: CO core mass at various evolutionary stages (see legend).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: CO core mass (left panels) as a function of time, total mass (middle panels) as a function of time, and total mass as a function of CO core mass (right panels) for the 8, 8.50, 8.80, and 9.00 M ⊙ models (top to bottom). The time has been reset at the beginning of the thermal pulses. The solid red line in the left and middle panels refers to the linear regression of the black line over the last few thermal pulses, superimposed on the black line itself. The values reported in the plots (MCOdot and M dot) refer to the rate of growth of the CO core and the rate of mass loss obtained with the linear regression. The dashed lines in the right panels refer to the extrapolation at late times of the various quantities shown in the figure, obtained with the linear regression mentioned before. The vertical blue dashed line marks the CO core mass corresponding to the central density threshold for the activation of the EC on 24Mg derived as discussed in the text (Zha et al. 2019).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Final CO and ONeMg core masses obtained with the “extrapolated evolution” based on a linear regression (see text). Also shown is the CO core mass corresponding to the threshold central density for the activation of the EC on 24Mg.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Convective (green shaded areas) and chemical (color codes reported in the color bar) internal history during off-center Ne burning for the 9.25 M ⊙ (left panel) and 9.50 M ⊙ (right panel) models. The x-axis reports the logarithm of the time until the end of the evolution (t fin − t) in units of years.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the central temperature as a function of the central density for three models of initial mass 9.20 M ⊙ prior to the onset of the TIR (see text), computed with the following assumptions: URCA processes and convective mixing taken into account (reference model; red line), URCA processes taken into account and convective mixing artificially suppressed (blue line), and URCA processes neglected (green line).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the central density as a function of time for three models of the initial mass 9.20 M ⊙ prior the onset of the TIR (see text), computed with the following assumptions: URCA processes and convective mixing taken into account (reference model; red line), URCA processes taken into account and convective mixing artificially suppressed (blue line), and URCA processes neglected (green line).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Convective (green shaded areas) and chemical (color codes reported in the color bar) internal history during the phase when the URCA processes are active. The x-axis reports the logarithm of the time until the end of the evolution (t fin − t) in units of years.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: CO (dashed line) and ONeMg (solid line) core mass as a function of the initial mass at various evolutionary stages: core He depletion (red line and dots), first thermal pulse (blue line and dots), and Ne ignition (magenta line and dots).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 23 but for the 9.15 M ⊙ model and during the TIR (see text) induced by the 25(Mg, Na) URCA pair.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 27 but for the 9.10 M ⊙ model.
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: Distribution of the fractional variability F var for the light curves of FSRQs, HBLs, IBLs, and LBLs.
Paper: GeV Variability Properties of TeV Blazars Detected by Fermi-LAT
Authors: Gege Wang, Hubing Xiao, Junhui Fan, Xin Zhang
Figure caption: Distribution of rise and decay time for the six sharp peak flare profiles fitted to the data.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the surface 12C (red line) and 14N (blue line) mass fraction and the mass coordinate of the bottom of the convective envelope (green line) as a function of time during the AGB phase (for the 7.0 M ⊙ model; upper left panel) and the SAGB phase (for the 8.0, 8.5, and 9.2 M ⊙ models; upper right, lower left, and lower right panels, respectively). The time has been reset at the core He exhaustion.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Ignition mass coordinate of C (black line and dots) and Ne burning (red line and dots) as a function of the initial mass (see legend).
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the H (blue line) and He (red line) luminosities as a function of time during the AGB phase (for the 7.0 M ⊙ model; upper left panel) and the SAGB phase (for the 8.0, 8.5, and 9.2 M ⊙ models; upper right, lower left, and lower right panels, respectively). The time has been reset at the core He exhaustion.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the convective envelope (green shaded area) and the He convective shell (red line) as a function of time during the last four thermal pulses for the AGB 7.0 M ⊙ model (upper left panel) and the 8.0, 8.5, and 9.2 M ⊙ SAGB models, (upper right, lower left, and lower right panels, respectively). The time has been reset at the core He exhaustion.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the temperature at the base of the convective envelope as a function of time during the AGB phase (for the 7.0 M ⊙ model; upper left panel) and the SAGB phase (for the 8.0, 8.5, and 9.2 M ⊙ models; upper right, lower left, and lower right panels, respectively). The time has been reset at the core He exhaustion.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected interior properties of a 8.5 M ⊙ model during the off-center C burning (see the legend). The chemical composition and degeneracy parameter are reported on the left y-axis, while the temperature is reported on the right y-axis. The degeneracy parameter is divided by 10 in order to improve the readability.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the He (blue line) and C (red line) core masses as a function of time during the AGB phase (for the 7.0 M ⊙ model; upper left panel) and the SAGB phase (for the 8.0, 8.5, and 9.2 M ⊙ models; upper right, lower left, and lower right panels, respectively). The time has been reset at the core He exhaustion.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Evolution of the central temperature and density of all of the computed models.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.22 M ⊙ (left panel) and 12.0 M ⊙ models when the ONe burning front has reached the center.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.22 M ⊙ star when the Si–S burning front has reached the center.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.22 M ⊙ star during the off-center Si–S burning.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 11.0 M ⊙ model during the shell O-burning phase.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.50 M ⊙ model during the off-center neon burning.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.22 M ⊙ star at off-center Si–S ignition.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Selected chemical and physical properties (see the legend) of the 9.22 M ⊙ star at the presupernova stage.
Paper: Evolution and Final Fate of Solar Metallicity Stars in the Mass Range 7–15 M ⊙. I. The Transition from Asymptotic Giant Branch to Super-AGB Stars, Electron Capture, and Core-collapse Supernova Progenitors
Authors: Marco Limongi, Lorenzo Roberti, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Schematic view of some of the evolutionary properties and expected final fate.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Eccentricity distributions of single and multiple giants beyond 0.3 au. The top purple distribution is for multiple giants, and the green bottom distribution is for single giants. The histograms show the distributions of individual maximum posterior values. The vertical bars show 68% confidence intervals. The curves show the median and many draws from beta distribution posteriors, produced using hierarchical inference.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Left: eccentricity with respect to semimajor axis for single giant planets and multiple giant planets. Vertical bars show 15.9%–84.1% confidence intervals. Circle radius is proportional to ﹩M\sin i﹩. Right: same as the left, but color coded by host-star metallicity. The curve shows the estimate of the tidal disruption limit assuming that periastron at 0.03 au leads to disruption (Dawson & Johnson 2018).
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Beta distribution posteriors for the single and multiple giant eccentricity distributions. The two populations are ∼3σ distinct.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Planet eccentricity vs. host-star metallicity for single and multiple giant systems.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Top: average search completeness contours for giant hosts below their median metallicity. Bottom: average search completeness contours for giant hosts above their median metallicity. The two contours are nearly equivalent, implying that sensitivity bias to metal-rich stars is not the cause of the single–multiple host distinction seen in Figure 5.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Cumulative metallicity distributions for hosts of single giant planets and hosts of multiple giant planets. The solid and dashed steps show the distributions of the median metallicity measurements, while the transparent steps show the metallicities drawn many times from Gaussian distributions, with the means and standard deviations taken from measurement means and uncertainties. Anderson–Darling tests show that the two groups are distinct.
Paper: The California Legacy Survey. IV. Lonely, Poor, and Eccentric: A Comparison between Solitary and Neighborly Gas Giants
Authors: Lee J. Rosenthal, Andrew W. Howard, Heather A. Knutson, Benjamin J. Fulton
Figure caption: Cumulative metallicity distributions for hosts of circular (e < 0.5) giant planets, hosts of eccentric (e ≥ 0.5) giant planets, and multigiant hosts. See Figure 5 for a description. The eccentric single hosts are inconclusively drawn from the same underlying metallicity distribution as the less eccentric singles or the multiples.