adsabs/AstroCLIMB huggingface dataset:
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Ratios of spin-integrated count rates (Ratei/Rate3), where i = 1, 2, 4 as a function of the ratio of the center energy of the E-Step over the mean ISN energy in the S/C frame (﹩{E}_{i}/{E}_{\mathrm{ISN}}﹩) for postacceleration voltages of 16 kV (2009–2012, blue) and 7 kV (≥2013, red). The yellow bars indicate optional finer E-Steps with IMAP-Lo.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Westward drift of the pointing of the IBEX spin axis ϵE and of the IBEX-Lo FoV (elongation angle) ηE over the course of an orbit or orbit arc relative to the Sun. Two positions (not to scale) of IBEX are shown for illustration, at the point of Sun-pointing and at a point where the spin axis has moved to a positive ecliptic spin-axis angle ϵE. Both angles ϵE and ηE are projected and calculated within the ecliptic plane.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Spin-integrated count rates as a function of spin-axis pointing for orbit 396, arcs a (left) and b (right). Orbit 396b is an example of an orbit in which the spin-axis angle rotated through Sun-pointing, which is the nominal case for IBEX in most orbits or orbit arcs. Orbit 396a is a case where the spacecraft spin axis was intentionally directed to larger spin-axis angles ϵE. The lines show fits to the observed spin-integrated count rates, and the derived rates at ϵE = 0° and ϵE = 5° are shown.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Spin-integrated count rates of the He ISN flow, obtained in E-Steps 1–4 at the location of exact Sun-pointing of the IBEX spin axis, corrected for aberration. The count rates have been transformed from flux to phase-space density and adjusted for ionization loss and the presence of secondary He. Also shown are the chi-squared fits to a Gaussian with the resulting peak longitudes.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Peak longitudes λPeak with fit error bars as a function of E-Step energy. The dashed–dotted horizontal line shows the inverse-variance-weighted average value for the first three energy steps (λPeak = 130.°29 ± 0.°15), and the dashed vertical line shows the ISN He bulk flow energy in the spacecraft frame.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Spin-integrated count rates of the He ISN flow, obtained in E-Steps 1–4 at the location of the ϵE = 2° off-pointing of the IBEX spin axis, corrected for aberration. The count rates have been transformed from flux to phase-space density and adjusted for ionization loss and the presence of secondary He. Also shown are the chi-squared fits to a Gaussian with the resulting peak longitudes.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Spin-integrated count rates of the He ISN flow, obtained in E-Steps 1–4 at the location of the ϵE = 5° off-pointing of the IBEX spin axis, corrected for aberration. The count rates have been transformed from flux to phase-space density and adjusted for ionization loss and the presence of secondary He. Also shown are the chi-squared fits to a Gaussian with the resulting peak longitudes.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Ecliptic longitude of the ISN flow peak λPeak as a function of elongation ηE in the heliocentric reference frame, based on observations (see Figures 8–10) and on analytic modeling for the ISN parameter tubes (Appendix B).
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Following λPeak with different elongations ηE from the Sun provides different ISN parameter tubes using the relations in Appendix B. Shown here are the range of elongations and associated parameter tubes accessible with IBEX. Insets show the left and right regions of parameter tube crossings. The range of possible inflow longitudes extends over ﹩75\buildrel{\circ}\over{.} {28}_{-2.21}^{+2.27}﹩ for the weakly crossed parameter tubes observed by IBEX.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Count rates of the He ISN flow in the spacecraft reference frame as a function of the spin angle (angle from north-ecliptic pole, NEP), obtained in E-Steps 1–3 for ecliptic spin-axis angles: ϵE = 0.99 ± 0.22 (top left) from orbit arcs 234b and 274b; ϵE = 2.52 ± 0.30 (top right) from orbit arcs 195b, 235a, and 235b; ϵ = 2.19 ± 2.13 (bottom right) from orbit 355b; and ϵE = 6.18 ± 1.06 (bottom left) from orbit arcs 356b and 397a. Also shown are the chi-squared fits to a Gaussian with the resulting peak latitudes.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Ecliptic latitude of the ISN flow peak ﹩{\psi }_{\mathrm{Peak}}^{{\prime} }﹩ in the spacecraft frame as a function of elongation ηE, based on observations (see Figure 13) and on analytic modeling for the ISN parameter tubes (Appendix B) and including secondary populations (Appendix C). We show both model results including primary and secondary populations (solid curve) and including only the primary population. The model curves represent averages over the regions analyzed. The shaded region shows the range of variation associated primarily with spacecraft motion and additional uncertainties in the parameter tube. For E-Step 3 (blue points), the model predictions generally agree with observations within the 1σ uncertainty intervals and over at least a portion of the region associated with spacecraft motion (blue shaded region).
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: On the IMAP, the IMAP-Lo instrument will follow λPeak with a wide range of different elongations ηE (shown here from 60° to 135°) to provide ISN parameter tubes that cross over a narrow range of local interstellar longitudes. The yellow cross-hatch shows an uncertainty range of ∼±0.°08 in ecliptic longitude and ∼±0.09 km s−1 in local interstellar inflow speed.
Paper: Interstellar Neutral He Parameters from Crossing Parameter Tubes with the Interstellar Mapping and Acceleration Probe Informed by 10 yr of Interstellar Boundary Explorer Observations
Authors: N. A. Schwadron, E. Möbius, D. J. McComas, J. Bower, E. Bower, M. Bzowski, S. A. Fuselier, D. Heirtzler, M. A. Kubiak, M. A. Lee, F. Rahmanifard, J. M. Sokół, P. Swaczyna, and R. Winslow
Figure caption: Two ISN flow bulk trajectories with different values for ﹩{\lambda }_{\mathrm{ISN}\infty }﹩ and ﹩{V}_{\mathrm{ISN}\infty }﹩ (solid and dashed line) are shown along with indications for the ISN velocity distribution at infinity and at 1 au. The ISN flow trajectory plane (gray) intersects Earth’s orbit, where IBEX observes the ISN bulk flow at its perihelion or exactly 90° from the Sun (at ecliptic longitude λPeak). The trajectory plane is tilted relative to Earth’s orbit by the angle ψPeak, i.e., the latitudinal angle at which the ISN flow arrives at IBEX in the rest frame. The ISN flow longitude ﹩{\lambda }_{\mathrm{ISN}\infty }﹩ and latitude ﹩{\beta }_{\mathrm{ISN}\infty }﹩ are also shown.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Maps of the normalized residuals for the maximum degree of spherical harmonics from 1 to 6 (from top left to bottom right). The derived ribbon mask for each degree is outlined by the white line. The maps are approximately centered at the upwind direction: top and bottom edges of each map correspond to the North and South ecliptic poles, while the left and right edges are at ecliptic longitude λ = 72°.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Normalized power spectrum of the spherical harmonic decomposition of the time-combined maps without separating the ribbon flux.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: GDF and ribbon flux separation results for the time-combined map for central energy 1.1 keV. Panels from left to right show: the total signal (the original IBEX data), the GDF reconstructed using the spherical harmonic decomposition, the ribbon flux, the statistical significance of the ribbon flux, the residual flux (see text), and the statistical significance of the residual flux. Rows from top to bottom correspond to the maximum degree of spherical harmonics from 1 (top) to 6 (bottom). The white lines outline pixels in the ribbon mask, and the yellow lines outline pixels excluded due to the poor statistical significance of the data.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Same as for Figure 3 but for central energy 2.7 keV.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Histograms of normalized residuals of the IBEX flux with the reconstructed GDF subtracted outside the ribbon mask for all the energy steps and years. The blue histograms show the normalization by the data uncertainty only, and the red histograms show the normalization by the full uncertainty matrix. Panels from top left to bottom right show results for ﹩{{\ell }}_{\max }﹩ from 1 to 6. The green line shows the normal distribution centered at 0 with standard deviation equal to 1.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Separation of the ribbon flux using the spherical harmonic decomposition with ﹩{{\ell }}_{\max }=3﹩ of the GDF for central energy 0.7 keV. The top row shows the results for the time-combined map, and the rest shows results for yearly maps from 2009 to 2019. The columns are the same as in Figure 3.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Same as for Figure 6 but for central energy 1.1 keV.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Same as for Figure 6 but for central energy 1.7 keV.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Same as for Figure 6 but for central energy 2.7 keV.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Same as for Figure 6 but for central energy 4.3 keV.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Time evolution of the ribbon flux and GDF inside the ribbon regions. The top inset shows areas R1-R6, for which the GDF and ribbon flux are plotted as a function of time in columns from left to right. The far right column shows the combined results from all areas. The blue, orange, and green lines show the total, GDF, and ribbon flux, respectively. The dotted–dashed and dotted orange lines show the GDF component obtained for ﹩{{\ell }}_{\max }=2﹩ and 4, respectively.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Stationary LOS-integrated pressure of the proton plasma forming the ENA observed by IBEX, obtained from the time-combined GDF reconstructed maps. The following directions are marked with 3σ ellipses: the maximum pressure (this study, dark blue), the ISN He flow (Swaczyna et al. 2018; purple), the ISN H flow (Lallement et al. 2005; gray), the Warm Breeze (Kubiak et al. 2016; cyan), the local interstellar magnetic field (Zirnstein et al. 2016b; orange), and the IBEX ribbon center (Dayeh et al. 2019; yellow). In addition, the approximate position of the ribbon is marked with gray dashed lines, and the B–V plane is marked with the white line. White arrows indicate positive and negative inclinations to the B–V plane, and the angular distance of the maximum pressure from the nose is marked with a green arrow.
Paper: IBEX Ribbon Separation Using Spherical Harmonic Decomposition of the Globally Distributed Flux
Authors: P. Swaczyna, T. J. Eddy, E. J. Zirnstein, M. A. Dayeh, D. J. McComas, H. O. Funsten, and N. A. Schwadron
Figure caption: Position of the maximum pressure (black symbols) and maximum flux (with color-coded energy steps) relative to the upwind direction (left panel) and the B–V plane (right panel). The time series shows how the position changes with time, and the subpanels on the right part of each panel show the time-combined results. Missing data points correspond to times when the maximum in the proximity of the upwind direction was not present or was not statistically significant (see Figures 6–10).
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Top panel: RBP−RP/RBP−G, as a function of (BP − RP), for different reddening values. The circles are empirically determined values; the lines are the fitting results. Middle and bottom panels: fitting residuals, as a function of (BP − RP) and E(B − V), respectively. In these panels a dashed line is provided at the 0.00 residual level for reference.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Color–magnitude diagram for the training sample. Colors indicate number densities, as shown in the color bar at right. Dwarfs and giants are separated by the red line: MG = − (BP − RP)2 + 6.5 × (BP − RP) − 1.8.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: The phot_bp_rp_excess_factor as a function of (BP − RP). Colors in the top panel indicate [Fe/H] values, as shown in the color bar at right. The middle and bottom panels show before (blue circles) and after (red circles) comparisons as the result of the 3σ clipping for giants and dwarfs, respectively.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Left panels: distributions of the giant (top) and dwarf (bottom) training samples in the [Fe/H] vs. (BP − RP) plane. The colors indicate the number densities, as shown in the color bar at right. Right panels: G magnitude distributions of the giant (top) and dwarf (bottom) training samples. Note that the stars of 14 < G < 16 in the bottom right panel are metal-poor dwarfs ([Fe/H] < −0.8).
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Same as Figure 4, but for the test samples.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Top panels: fitting residuals, as a function of (BP − RP) color (left) and [Fe/H] (right), for the giant training sample. The colors indicate the number densities, as shown in the color bar at right. In these panels a dashed line is provided at the 0.00 residual level for reference. Bottom left: histogram distributions of the fitting residuals, with the Gaussian fitting profile overplotted in black. Bottom right: variations of stellar loci for different metallicities, relative to the one at [Fe/H] = 0.0.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Same as Figure 6, but for the dwarf training sample.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Results for the giant training sample. Top left: histogram of the metallicity differences between those estimated from Gaia photometry and LAMOST spectroscopy. Gaussian fitting is overplotted in red; the mean and sigma values are marked. Top right: Gaia metallicities vs. LAMOST metallicities. The red line is the one-to-one line. Bottom panels: metallicity differences, as a function of (BP − RP) color (left) and [Fe/H]LAMOST (right). The black lines indicate the medians; red lines indicate the standard deviations.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Same as Figure 8, but for the dwarf training sample. Note that in the top left panel, the excess on the left side is due to the presence of dwarf−dwarf binary stars.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Results for the giant test sample. Top left: histogram distribution of the metallicity differences that are respectively deduced from Gaia photometry and LAMOST spectroscopy. Gaussian fitting is overplotted in red; the mean and sigma values are marked. Top right: LAMOST metallicities vs. Gaia metallicities. The red line is the one-to-one line. Middle panels: metallicity differences, as a function of (BP − RP) (left) and [Fe/H] (right). Bottom panels: metallicity differences, as a function of reddening (left) and G magnitude (right).
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Same plot as Figure 10, but for the dwarf test sample.
Paper: Stellar Loci. V. Photometric Metallicities of 27 Million FGK Stars Based on Gaia Early Data Release 3
Authors: Shuai Xu, Haibo Yuan, Zexi Niu, Lin Yang, Timothy C. Beers, and Yang Huang
Figure caption: Analysis of the outliers. Top left: G magnitude distributions of the normal (blue line) and outliers (red line) for the giants. Top right: the phot_bp_rp_excess_factor, as a function of (BP − RP), for the giants. Bottom: same as the top panel, but for the dwarfs. To avoid crowding, only 1% of randomly selected stars are plotted.