adsabs/AstroCLIMB huggingface dataset:
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: CMD showing the distribution of WD–MS binary candidates identified through χ2 fitting of XP spectra (red circles). The background gray scale shows the density distribution of all stars, with the scale bar indicating the logarithmic number of stars per bin. The x-axis shows the dereddened Gaia color (B – R)0, while the y-axis shows the absolute G magnitude (MG0) after extinction correction. The 10 cyan stars are examples of the χ2-selected WD–MS binaries; the yellow lines show the best-fit spectral decomposition of a WD and an MS by XP spectra. The binary candidates primarily occupy the region between the MS (right) and WD sequence (left), as expected for composite systems. The blue dotted line denotes the requirements of the WD component of a binary model fit, which should lie to the left of this line as in the WD regime.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: CMDs illustrating the classification performance metrics of the GPC method for identifying WD–MS binaries within the validation data set, which is based on synthetic spectra. Left: purity (precision) map showing the fraction of true WD–MS binaries among all objects classified as WD–MS in each CMD pixel. Right: completeness (recall) map showing the fraction of correctly identified WD–MS binaries among all true WD–MS binaries in each CMD pixel. The color scale ranges from 0 (purple) to 1 (yellow), where yellower regions indicate better performance. The blue and red contours represent the density distribution of individual WD and MS stars, respectively, in CMD space. Both metrics demonstrate robust performance (yellow regions) in the characteristic WD–MS locus, with some expected degradation (darker colors) in regions where WD–MS binaries overlap with the single-star MS populations.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Left: CMD comparing WD–MS binary samples from different surveys. Red circles show our GPC-identified WD–MS binaries from Gaia XP, the blue contour represents LAMOST DR5 WD–MS binaries (J. J. Ren et al. 2018), and the yellow contour shows SDSS DR12 WD–MS systems (A. Rebassa-Mansergas et al. 2013, 2016). The background shows the density of all stars in our sample. Right: the 2D KDE distribution of the LAMOST and SDSS WD–MS binaries is shown in coordinates of the renormalized χ2 difference and the binary probability (PWD−MS​).
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: CMD showing the classification of stars into single and binary systems by the GPC. The four panels show different probability ranges for binary classification: 0.0 < PWD−MS < 0.2, 0.2 < PWD−MS < 0.5, 0.5 < PWD−MS < 0.8, 0.8 < PWD−MS < 1.0. The orange line represents the PARSEC isochrone with [M/H] = 0.0. The distribution reveals that stars falling between the MS and WD regions are more likely to be classified as binaries, consistent with expectations for WD−MS binary systems.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Gaia XP spectra and best-fitting models for 8 of 10 WD–MS binaries selected using the χ2 fitting method are shown as examples in Figure 3. In each panel, the black line represents the observed flux, with the gray shading indicating flux error. The cyan solid line represents the best-fit single model, while the orange dashed line shows the best-fit binary model. The pink dotted line corresponds to the MS component of the binary model, and the blue dotted line represents the WD component of the binary fit.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: CMD illustrating the mock data of single MS stars, single WDs, and the synthetic WD–MS binary systems. The gray 2D histogram background represents the WD sequence and the MS stars. The red stars indicate synthetic WD–MS binaries. The yellow lines connect the WD and MS components of individual binary systems for synthetic WD–MS binaries.
Paper: Identification of 30,000 White Dwarf–Main-sequence Binary Candidates from Gaia DR3 BP/RP (XP) Low-resolution Spectra
Authors: Jiadong Li, Yuan-Sen Ting, Hans-Walter Rix, Gregory M. Green, David W. Hogg, Juan-Juan Ren, Johanna Müller-Horn, Rhys Seeburger
Figure caption: Comparison of the stellar mass between χ2-selected WD–MS binaries (red) and single WDs (blue) from the Gaia sample (M. Kilic et al. 2025).
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: E-Step 2 H− count rate maps in the ram direction for ISN seasons 2009–2020. Start time, end time, orbit range, and ISN season orbit range for each year are provided in Table 1. The x-axis tick labels represent orbits for the years 2009–2011 (at the top) and 2012–2020 orbit arcs (at the bottom). The spin angle orientation is identical to that in Figure 2.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: E-Step 3 H− count rate maps in the ram direction for ISN seasons 2009–2020. Start time, end time, orbit range, and ISN season orbit range for each year are provided in Table 1. The x-axis tick labels represent orbits for the years 2009–2011 (at the top) and 2012–2020 orbit arcs (at the bottom). The spin angle orientation is identical to that in Figure 2.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Counts (panel (a)), exposure times (panel (b)), and count rates (panel (c)) maps in the ram direction for the year 2009, E-Step 2. These maps contain orbits from 2008 December through 2009 December (see Table 1). Each column represents one orbit, which is pixelated by 6° spin bins. Spin bin 0 represents the spin bin centered on the north ecliptic pole, and 29 represents the spin bin that ends 3° before the south ecliptic pole. Gray indicates that no data are available for the entire orbit; such pixels are represented by −1.0 values in the data files. White pixels represent either actual zero values or pixels with no data that belong to orbits where there are some data available. A list of such orbits is provided in Table 6. Exposure times are identical across all E-steps; thus, we do not specify the E-step in panel (b). Data files associated with counts, exposure times, and count rates maps for seasons 2009–2020 are provided in the data release (https://ibex.princeton.edu/ApplicationDataRelease1). In this paper, we only show count rate maps.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Differential H− count rates obtained by subtracting E-Step 3 (Figure 4) from E-Step 2 (Figure 3). The axis ticks and labels are identical to those in Figures 3 and 4. Count rates in E-Step 3, primarily generated by He atoms, are typically higher than those in E-Step 2. As a result, negative count rates are observed at the peak of the primary He signal for each year. In contrast, pixels associated with secondary He and H atoms exhibit positive values.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Redistribution of the count rates to correct for the 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 shift in the spin bins. Blue circles and x signs show the observed count rates at the spin bin center + 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 and their fitted values, while red circles and x signs represent the corrected count rates and their fitted values at the spin bin center. Panel (a) shows a Gaussian, and panel (b) shows a linear fit.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: E-Step 2 and E-Step 3 H− count rate maps in the ram direction for ISN seasons 2009 and 2014. The faint tail observed for the year 2009 (solar minimum) in panel (a) is associated with ISN H, whereas this tail is insignificant in panel (b) (E-Step 3). During solar maximum (2014), this tail falls to background levels also in E-Step 2 (panel (c)).
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Top panel: the peak of H− count rates observed in E-Step 2 and E-Step 3. The vertical dashed line separates the operation times with different PAC voltages. Bottom panel: the sunspot number variations with solar activity.
Paper: Tuning the Legacy Survey of Space and Time Observing Strategy for Solar System Science: Incremental Templates in Year 1
Authors: James E. Robinson, Megan E. Schwamb, R. Lynne Jones, Mario Jurić, Peter Yoachim, Bryce T. Bolin, Colin O. Chandler, Steven R. Chesley, Grigori Fedorets, Wesley C. Fraser, Sarah Greenstreet, Henry H. Hsieh, Lauren J. McGinley, Stephanie R. Merritt, Cyrielle Opitom, John K. Parejko
Figure caption: Left: A sky map showing the total number of visits, in all filters, at the end of Year 1 for the one_snap_v4.0_10yrs observing strategy (Mollweide projection). This sky map was generated using a HEALPix (Hierarchical Equal Area isoLatitude Pixelization; K. M. Górski et al. 2005) resolution of nside = 256. The plots are centered on R.A. α = 0° and decl. δ = 0∘, with R.A. increasing to the left. R.A. and decl. lines are marked every 30∘. The main sky regions of the survey are labeled as follows: Low-dust Wide–Fast–Deep (WFD), North Ecliptic Spur (NES), Galactic plane (GP) WFD, dusty (Galactic) plane, south celestial pole (SCP), Deep Drilling Fields (DDFs), and the Virgo cluster. Right: the color map denotes the on-sky extent of the different survey regions.
Paper: Tuning the Legacy Survey of Space and Time Observing Strategy for Solar System Science: Incremental Templates in Year 1
Authors: James E. Robinson, Megan E. Schwamb, R. Lynne Jones, Mario Jurić, Peter Yoachim, Bryce T. Bolin, Colin O. Chandler, Steven R. Chesley, Grigori Fedorets, Wesley C. Fraser, Sarah Greenstreet, Henry H. Hsieh, Lauren J. McGinley, Stephanie R. Merritt, Cyrielle Opitom, John K. Parejko
Figure caption: Sky maps of the total number of visits per filter accumulated during Year 1 of the one_snap_v4.0 cadence simulation. Visits associated with DDFs and the low-solar elongation twilight survey have been removed. In each panel, we display the number of visits in each filter (ugrizy) to highlight the variations in footprint area and coverage (note the different ranges of each color bar). The sky maps were generated using a HEALPix resolution of nside = 256.
Paper: Tuning the Legacy Survey of Space and Time Observing Strategy for Solar System Science: Incremental Templates in Year 1
Authors: James E. Robinson, Megan E. Schwamb, R. Lynne Jones, Mario Jurić, Peter Yoachim, Bryce T. Bolin, Colin O. Chandler, Steven R. Chesley, Grigori Fedorets, Wesley C. Fraser, Sarah Greenstreet, Henry H. Hsieh, Lauren J. McGinley, Stephanie R. Merritt, Cyrielle Opitom, John K. Parejko
Figure caption: A representative patch randomly selected from the Rubin Data Preview (DP) 0.2/DESC DC2 (LSST DESC) simulated data products Year 1 annual templates. The extent of a single patch is ﹩13\mathop{.}\limits^{{\rm{^{\prime} }}}\,7\,\times \,13\mathop{.}\limits^{{\rm{^{\prime} }}}\,7﹩. The color bar reflects how many visits went into that patch pixel. The nonuniform coverage is a result of overlapping detector footprints from multiple visits taken with spatial and rotational dithers.
Paper: Tuning the Legacy Survey of Space and Time Observing Strategy for Solar System Science: Incremental Templates in Year 1
Authors: James E. Robinson, Megan E. Schwamb, R. Lynne Jones, Mario Jurić, Peter Yoachim, Bryce T. Bolin, Colin O. Chandler, Steven R. Chesley, Grigori Fedorets, Wesley C. Fraser, Sarah Greenstreet, Henry H. Hsieh, Lauren J. McGinley, Stephanie R. Merritt, Cyrielle Opitom, John K. Parejko
Figure caption: A cartoon schematic of tracts and patches in the LSST on-sky data management tessellation. The sky is divided into overlapping tracts each 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 × 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6. Each tract is comprised of 49 overlapping patches. Patches are roughly the size of an individual LSSTCam CCD detector with dimensions of ﹩13\mathop{.}\limits^{{\rm{^{\prime} }}}\,7\,\times 13\mathop{.}\limits^{{\rm{^{\prime} }}}\,7﹩.
Paper: Generalized Fluid Models of the Braginskii Type. II. The Boltzmann Operator
Authors: P. Hunana
Figure caption: Left panel: Function ﹩1-\cos \theta ﹩ representing the rigid core model (391), with the chosen value v = 10,000. For larger v-values the function just becomes more oscillatory, but the average is obviously 1. Right panel: Function ﹩(1-\cos \theta ){v}_{0}﹩ representing integral (392), plotted for the same v = 10,000. As v increases, the area under the curve converges to 1/2.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: SEDs for Type 1 AGN with WISE/2MASS (M. F. Skrutskie et al. 2003; E. L. Wright et al. 2019), GALEX (doi: 10.17909/25nx-tp05), and SDSS photometry. Nineteen Type 1 AGN have photometry from WISE/2MASS, GALEX, and SDSS. SDSS photometry is from DR14 Skyserver database. The flux, Fν (erg s−1 cm−2 Hz−1) for W1–W4, J, H, and Ks, has been normalized by the corresponding Fi and plotted as a function of the shifted rest frequency. The black line is −0.97log(νrest) + 13.74, a typical standard slope of a quasar spectrum averaged over a wide wavelength baseline. We then deredden this black line power law using E. F. Schlafly & D. P. Finkbeiner (2011)’s extinction coefficients (black dashed line) and the J. A. Cardelli et al. (1989) model (gray dashed line) for RV = 3.1.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: SED of Kepler AGNs against different templates. The black lines were taken from Figure 11 in J. Stern & A. Laor (2012a). These lines are the mean SEDs with different LbHα bins, with the R06 line being the net AGN SED. The gray line is the composite SED of Spitzer AGNs, while the dashed gray line is the AGN with the stellar contribution template from J. Lyu & G. H. Rieke (2018). The gray dots are the template for normal quasars that J. Lyu & G. H. Rieke (2018) have taken from L. Xu et al. (2015). In the mid-IR (log νrest ≤ 14), the plot is independent of luminosity, while there is a characteristic blue bump in the UV for very luminous quasars.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: BPT diagram of log([O III]/Hβ) vs. log([N II]/Hα). This graph displays 16 galaxies with narrow components in Hβ, [O III]-5007, Hα, and [N II]-6584. The triangle indicates a narrow Type 1 AGN, in which we tried to fit the narrow components. Four out of these 16 objects (25%) are composite galaxies (between the Ka03 and Ke01 lines) with major narrow-line emissions from H II regions. The rest of the galaxies above the Ke01 line (75%) are in the AGN region. Another 11 objects, marked by the crosses, are either at high redshifts where we lost Hα+[N II] past the red end of the spectra or we could not get a good fit of Hα+[N II].
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: The luminosity distribution of narrow Hα to broad Hα vs. LbHα. The black solid line is the best fit of the data. The gray dashed line is the best-fit power law of the T1 sample from Figure 3 in J. Stern & A. Laor (2012b). The relationship between LnHα and LbHα in our data is consistent with that of J. Stern & A. Laor (2012b), and the NLR/BLR ratio is increasing with decreasing luminosity.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: Venn diagram of the different AGN selection methods. Our Kepler AGN sample is selected through several methods, as mentioned in Sections 2 and 5. This Venn diagram shows the distribution of the candidates for the EM12 and D. Stern et al. (2012) methods: EM12 W2R, EM12 W2, and the WISE color cut. The sample is further divided into Type 1/2 AGN and other non-AGN, such as stars and normal galaxies.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: Deblending of Hβ in a Seyfert 1.5 galaxy. This candidate is a Seyfert 1.5, with comparable narrow and broad components of Hβ. The dotted curves are the fits. The FWHMs for Hβ are 4800 (broad) and 470 (narrow) km s−1. [O III]-5007 has a FWHM of 570 km s−1.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: The luminosity ratio of [N II] to broad Hα vs. LbHα. The black solid line best fits the data, while the gray dashed line is from Figure 1 in J. Stern & A. Laor (2013). The same tendency for the narrow components to dominate at low luminosity appears here as in the previous two plots.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: An example where Hα + [N II] could not be deblended. Due to B-band absorption at ∼6870 Å, we could not confidently deblend Hα from [N II]. We therefore estimated the width of Hα by eye. However, the half-maximum falls at about 3.3 × 10−16 erg s−1 cm−2 Å−1, which is an ambiguous level due to [N II]-6548 absorption.
Paper: Infrared-selected Active Galactic Nuclei in the Kepler Fields
Authors: Tran Tsan, Matthew Malkan, Rick Edelson, Krista Smith, Daniel Stern, Matthew Graham
Figure caption: A spectrum of a narrow-line Type 1 AGN galaxy. Hβ has an FWHM of 1300 km s−1 (Δv < 2000 km s−1) and a much broader base than that of [O III]-5007. Hence, we classified such cases as “narrow-line” Type I AGN. [O III]-5007’s FWHM is 670 km s−1.
Paper: A Deep Learning Method for Automatic Coronal Mass Ejection Feature Identification
Authors: P. Yang, H. S. Fu, J. B. Cao, F. Shen
Figure caption: Comparison of our method with four classical methods for detection and tracking across consecutive time frames.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Predicted E-Step 2 H− count rate maps for solar minimum (top row: 2010, middle row: 2019, bottom row: 2020) based on the aFINM in comparison with observed maps. Panels on the left show the predicted ISN He signal (primary and secondary) based on parameters from Table 3. In the middle panels, we have added the ISN H primary and secondary population. Observed H− count rates are shown in the right panels. While the ISN H tail is present in the data, it is significantly weaker than the predicted tail shown in the middle panels.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Predicted E-Step 2 H− count rate maps for the 2014 season (during solar maximum) along with the observed map in the same format as in Figure 8. The predicted ISN H tail from the combined model (middle panel) is not observed in the data (right panel) as the ISN H count rates fall to background levels during the solar maximum more rapidly than our model predicts.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Differential maps showing the difference between predicted count rates and observed data from Figure 10, presented in the same format as in Figure 9.
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Top panel: residual count rates after subtraction of the E-Step 2 H− count rates for the 2014 season (normalized to the peak of 2019) from the 2019 season count rates. Bottom panel: the sum of residuals over spin bins 0–29 for each orbit. The x-axis represents the orbit index, which is the orbit number from the beginning of the year (second column in Table 1).
Paper: 12 yr Full Solar Cycle Maps from IBEX-Lo Interstellar Neutral Atom Observations (2009–2020)
Authors: F. Rahmanifard, H. Islam, N. A. Schwadron, E. Möbius, K. Fairchild, D. Heirtzler, P. Swaczyna, J. M. Sokół, A. Galli, D. J. McComas, S. A. Fuselier, P. Wurz, M. Bzowski
Figure caption: Differential maps presenting the difference between predicted count rates and observed data from Figure 8. Panels on the left show data subtracted by predicted He, and panels on the right show data subtracted by predicted He and H results.