adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Balmer emission-line ratios of Hγ/Hβ and Hδ/Hβ for the ERO objects (04590 in red, 05144 in emerald green, 06355 in orange, and 10612 in green) are shown in the main panel. The colored filled circles represent the new emission-line flux measurements and errors with our improved reduction, while the other symbols show the measurements based on the early data release, as shown in the legend (Arellano-Córdova et al. 2022; Curti et al. 2023a; Rhoads et al. 2023). For the measurements of Arellano-Córdova et al. (2022), we adopt the average values based on the two spectra (o007 and o008) for 06355 and 10612, but refer only to the o008 value for 04590. For those with line ratios outside the ranges of the plot, we place them close to the edge of the plot with an arrow to indicate the direction toward the actually reported line ratio. The lines show the expected Balmer decrements as a function of E(B−V) for the three different attenuation curves (Cardelli et al. 1989 with dashed; Calzetti et al. 2000 with dotted; and SMC from Gordon et al. 2003 with dotted–dashed) and the two different electron temperatures (T  e  = 10,000 K in gray and 25,000 K in magenta), although the different attenuation curves and T  e  values have a small impact on this diagram. The deviation of the Hδ/Hβ ratio from the theoretically expected value based on the Hγ/Hβ ratio (ΔHδ/Hβ = ((Hδ/Hβ)obs − (Hδ/Hβ)expected) normalized by (Hδ/Hβ)expected) is highlighted in the upper panel, and that of the Hγ/Hβ ratio based on the Hδ/Hβ ratio in the left panel, for each symbol as in the main panel. The corresponding E(B−V) values are printed in these subpanels, where the Calzetti et al. (2000) attenuation curve and T  e =17,500 K are adopted for reference. Our measurements all follow the sequence of the expected Balmer decrements within the uncertainties, while quite a few of the measurements from the earlier studies show the ratios that are not physically and/or consistently explainable.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: O32 vs. R23 diagram comparing the JWST sample at z = 4–9, analyzed in this work, with lower-redshift samples at z = 2–3. The JWST objects are shown as red filled symbols, with circles representing ERO data, pentagons representing GLASS data, and diamonds representing CEERS data. Objects with metallicity measurements obtained using the direct T  e  method are indicated with red open circles. The gray open symbols represent the averages of lower-redshift samples of continuum-selected galaxies (Nakajima & Ouchi 2014; Troncoso et al. 2014; Sanders et al. 2016; Onodera et al. 2016; Strom et al. 2017) and Lyα emitting galaxies (LAEs; Nakajima & Ouchi 2014; Erb et al. 2016; Nakajima et al. 2020), as indicated in the legend. Arrows indicate 3σ lower limits. Gray shading illustrates the equivalent distribution for nearby SDSS galaxies.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Observed NIRSpec spectra for the five z = 5–8.5 ERO objects. For each object: (top) 2D spectra for the six individual exposures (three nods each in o007 and o008); (bottom) 1D composite spectrum. We generate the 1D composite spectrum by first median stacking the individual 2D spectra and then extracting the 1D spectrum with a small aperture (see text). This procedure allows us to minimize the possible impacts of hot pixels and to rescue some individual 2D frames where the spectrum is partly out of the slit (e.g., two nod2 frames of 10612).
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: The [N II] BPT diagram. Red symbols represent the JWST objects, as shown in Figure 4, whose Hα+[N II] lines are covered in the NIRSpec spectra. Arrows indicate 3σ limits. Two popular demarcation curves between AGNs and star-forming galaxies, from Kewley et al. (2001; dot long dashed; “Kew01”) and Kauffmann et al. (2003; short dash long dashed; “Kau03”), are also shown. None of the objects fall above the demarcation curves significantly beyond the measurement uncertainties.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Redshift distribution of the high-redshift galaxy samples used in this work. The red histogram presents the JWST sample constructed in this study using our analyzed ERO, GLASS, and CEERS spectra. The blue histogram shows the samples compiled from the literature (see Section 3.2.3). The sum of these samples, represented by the gray histogram, is used to investigate the MZ relationship at z = 4–10 in this work.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to the right panel of Figure 13, but employing the SFR–MZ relation of Curti et al. (2020). As similarly found in Figure 13, our analysis (red) and the JADES+CEERS study by Curti et al. (2023b; emerald green) suggest a consistent evolution of the SFR–MZ relation from z = 4–10 on average. If we adopt the formalism of Curti et al. (2020), which is defined at z = 0, our JWST objects begin to deviate from the SFR–MZ relation at z ∼ 6. This finding contrasts with the use of the z = 0 SFR–MZ relation of Andrews & Martini (2013), which suggests deviations starting at z ∼ 8 (Figure 13(b)). It is worth noting, however, that a simple extrapolation of the relation toward lower masses and higher SFRs is assumed for the majority of the JWST objects (see Figure 14(b)).
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Metallicity difference from the SFR–MZ relation of Andrews & Martini (2013) as a function of stellar mass in three different redshift bins: (a) z = 4–6, (b) z = 6–8, and (c) z = 8–10. The symbols are consistent with those in Figure 11. No clear dependence of ﹩{\rm{\Delta }}\mathrm{log}﹩ (O/H) on stellar mass is evident beyond the statistical errors.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to Figure 10, but excluding the individual JWST objects whose stellar masses are empirically derived, so all the plotted data points have stellar masses that are derived based on SED fitting to NIRCam photometry. The average of the JWST objects plotted on this figure are represented by purple inverted stars. As a comparison, the average relations based on the full sample are shown with the red stars and the gray long-dashed line, as presented in Figure 10, which are positioned almost behind the purple inverted stars. This confirms that our results remain unchanged when adopting the subsample with certain estimations of M ⋆.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to the right panel of Figure 13, but excluding the individual JWST objects with μ 0.66 < 7.5. The average relations of the subsample are denoted with the blue inverted stars. As a comparison, the average relations based on the full sample are shown with the red stars, as presented in Figure 13, which are positioned almost behind the blue inverted stars. This confirms that our results on the redshift evolution of the SFR–MZ relation remains unchanged when considering only objects with μ 0.66 > 7.5.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to Figure 10, but excluding the individual JWST objects, and instead focusing on comparisons with low-redshift MZ relations based on empirically estimated metallicities using strong line indicators, as indicated in the legend. Each MZ relation is depicted in the mass range explored in the original paper.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to Figure 15, but excluding the individual JWST objects without JWST/NIRCam photometry. The average relations of the JWST objects in each panel are represented by purple inverted stars. In the z = 8–10 panel, only a single average point is displayed due to the limited sample size.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to Figure 13, but excluding the individual JWST objects without JWST/NIRCam photometry. The average relations of the JWST objects in each panel are represented by purple inverted stars.
Paper: JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators
Authors: Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yuichi Harikane, Yechi Zhang, Yoshiaki Ono, Hiroya Umeda, Masamune Oguri
Figure caption: Similar to Figure 11, but excluding the individual JWST objects without JWST/NIRCam photometry. The average relations of the JWST objects in each panel are represented by purple inverted stars.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Left: locations of DGPS sources (gray circles) in the HR1 − HR2 plane. The dashed lines represent typical spectra for HMXBs, magnetars, and stars as outlined in Appendix C. The arrows mark the general location of these sources with respect to the lines. Right: the mean hardness ratios of LMXBs, IP CVs, HMXBs, and magnetars from 2SXPS are shown for comparison.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: The location of DGPS sources in Galactic coordinates. The sources are colored based on the logarithm of their X-ray flux. The blue crosses show the locations of known magnetars. The black star (bottom panel) marks a dominant source of stray light, leading to an obvious lack of sources at that region of the survey.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Histograms of the number of sources detected per Galactic longitude on both sides of the plane and in Galactic latitude (combining both sides of the plane). We note that the dip in sources at l ≈14 deg and 340 deg is due to stray light contaminating those fields.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Left: histogram of source location in Galactic latitude for constant (gray) and variable (red) sources (see Section 4.3). Right: distribution of sources in the hardness ratio plane. Red squares are sources on the GP with ∣b∣ < 0.1 deg, and gray circles are off-plane sources with ∣b∣ > 0.1 deg.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Distribution of DGPS sources (gray circles) in terms of hardness ratio and X-ray flux. For reference, we display LMXBs, IP CVs, HMXBs, and magnetars from the 2SXPS catalog.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: The location of DGPS sources in Galactic coordinates. The sources are colored based on their hardness ratio (either HR1 or HR2). The black star (bottom panels) marks a dominant source of stray light, leading to an obvious lack of sources in that region of the survey.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Mosaic of the GP at negative Galactic longitudes in the SB (0.3–1 keV), MB (1–2 keV), and HB (2–10 keV). The background variation across the plane is due to higher exposure in regions with overlapping tiles and is not due to an intrinsic structure in the emission.
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Histogram of source classification breakdown for 45 GCSs and eight CCGCSs based on results from Yang et al. (2022).
Paper: The Swift Deep Galactic Plane Survey (DGPS) Phase I Catalog
Authors: B. O'Connor, C. Kouveliotou, P. A. Evans, N. Gorgone, A. J. van Kooten, S. Gagnon, H. Yang, M. G. Baring, E. Bellm, P. Beniamini, J. Brink, D. A. H. Buckley, S. B. Cenko, O. D. Egbo, E. Göğüş, J. Granot, C. Hailey, J. Hare, F. Harrison, D. Hartmann, A. J. van der Horst, D. Huppenkothen, L. Kaper, O. Kargaltsev, J. A. Kennea, K. Mukai, P. O. Slane, D. Stern, E. Troja, Z. Wadiasingh, R. A. M. J. Wijers, P. Woudt, G. Younes
Figure caption: Mosaic of the GP at positive Galactic longitudes in the SB (0.3–1 keV), MB (1–2 keV), and HB (2–10 keV).
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: Illustrative example of an electron energy distribution function (EDF) showing the photoelectrons and the ambient electrons in the solar wind near 1 au. The red solid line shows the median of the energy flux, ﹩{f}_{e}\left(E\right)﹩ (eV+1 cm−2 s−1 sr−1 eV−1), at each energy over all 88 solid angle bins vs. energy, E (eV), on a log–log scale. The vertical lines indicate values or ranges of values for the estimated ϕ sc of this EDF (see labels). The magenta lines (Method 1, see text for definition) show the region bounding the region of positive curvature (note left-hand bound covered by green dashed line). The orange lines show the region bounding the transition from negative to positive slope (Method 2). The green lines show the region bounding the minimum-to-maximum curvature transition (Method 3). Finally, the blue line shows the point of minimum in ﹩{f}_{e}\left(E\right)﹩ (Method 4).
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: Characteristic EDFs representing the four shapes observed herein, shown as the red solid lines. All ﹩{f}_{e}\left(E\right)﹩ were normalized to the peak magnitude prior to calculation for this figure. Type A is the ideal case, illustrated in Figure 2. Type B is the next best shape but often shows a shoulder or saddle point rather than a local minimum, increasing the uncertainty of the ϕ sc estimates. Type C1 has ϕ sc < ﹩{E}_{\min }﹩ and the lowest-energy bin has ﹩\tfrac{{df}}{{dE}}﹩ ∼0. Type C2 also has ϕ sc < ﹩{E}_{\min }﹩ but the lowest-energy bin has ﹩\tfrac{{df}}{{dE}}﹩ > 0. Both Types C1 and C2 are not considered useful shapes as we can only constrain the upper bound on ϕ sc. The green line in each panel represents the median of all EDFs for each type. The blue (magenta) line in each panel represents the corresponding 5th (95th) percentile of all EDFs of each type.
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: Example electron energy distribution function (EDF) from the Wind 3DP instrument. The multicolored thin lines show the phase space density (# cm−3 km−3 s+3) of each of the 88 solid angle bins vs. energy, E (eV). The photoelectrons are seen to the left of the vertical magenta line marking the spacecraft floating potential, ϕ sc. The thick green and black lines show simplified model EDFs for the photoelectrons (following the method in Wilson et al. 2022) with parameter ranges shown in the legend of the plot.
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: Two-dimensional histograms of the ϕ sc estimates for Methods 1–4 (shown in order). The thick black line in each panel shows the ﹩{E}_{\min }﹩ value vs. time. The horizontal (time) axis is parsed into 4 week bins while the vertical axis is parsed into 16 uniformly sized bins between 0 and 30 eV (i.e., roughly 2 eV each). The color scale shows total counts in each two-dimensional histogram bin. The bottom two panels show solar irradiances (in W m−2) measured with two different detectors from the TIMED SEE experiment. These are shown as proxies for solar cycle variation and ionizing photon intensities vs. time. The two vertical magenta lines indicate the rough boundaries between solar cycles.
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: The power spectral density (PSD) (eV+2 days−1) of the fast Fourier transform of all ϕ sc estimates for all four EDF types, using Method 4 (note this is the median of the three PADs), versus frequency (days−1) shown in purple. The red line is the smoothed PSD, using a running boxcar average with an eight-point bin width. Overplotted are four vertical lines corresponding to the frequency of the synodic Carrington rotation period (∼27.2753 days) and its first three harmonics.
Paper: Spacecraft Floating Potential Measurements for the Wind Spacecraft
Authors: Lynn B. Wilson III, Chadi S. Salem, John W. Bonnell
Figure caption: Histograms of the CC values for each type are shown as percentages of the total number of counts for each type.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Sketch map of the MDN where Gaussian mixture models are combined with the neural network. Three hidden layers are involved in the neutral network and each layer has 512 neurons. Twenty Gaussian mixture components are adopted for each output variable and each component is characterized by the mean μ, variance σ 2, and mixing coefficient α. The inputs into the MDN are some planet bulk parameters such as mass, radius, bulk molar ratio Fe/(Mg + Si), and static Love number k 2. The outputs from the MDN contain the radial fractions of each layer and interior properties at the core–mantle boundary (CMB), such as water radial fraction (WRF), mantle radial fraction (MRF), core radial fraction (CRF), CMF, as well as the CMB pressure and temperature. The training data set are generated from three-layer interior models (top right): an iron-rich core, lower and upper silicate mantles, and a water–ice outer shell.
Paper: Machine-learning Inferences of the Interior Structure of Rocky Exoplanets from Bulk Observational Constraints
Authors: Yong Zhao, Dongdong Ni, Zibo Liu
Figure caption: Histogram of bulk molar Fe/Mg ratios used for the training data set. The bulk Fe/Mg of the Sun (Asplund et al. 2009), Mars (Wanke & Dreibus 1994), Earth (McDonough 2003), and Mercury (Nittler et al. 2018) are denoted by red, green, blue, and navy arrows, respectively. The average Fe/Mg for 5220 FGK stars (Unterborn & Panero 2019) is also shown by orange arrows with uncertainties. The top panel shows the distribution of CMFs vs. the bulk molar Fe/Mg ratio.