adsabs/AstroCLIMB huggingface dataset:
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Right-handed (s = 1) eastward (d = −1) for γ = 60°, 75°.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Right-handed (s = 1) eastward (d = −1) for γ = 0°, 15°.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Right-handed (s = 1) eastward (d = −1) for γ = 90°.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Upper panel: distribution of quiescent galaxies and the total number of galaxies across various redshift bins, as determined by the ML method. Lower panel: evolution of the fraction of quiescent galaxies as a function of redshift for galaxies with stellar masses MQG ≥ 109.5M⊙, comparing the NUVrJ (J. Weaver et al. 2023), SED-fitting, and ML methods on the COSMOS2020 data sample.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Confusion matrices compare the predicted classifications from different methods against the ground truth and each other. The matrices display (left) ML predictions vs. the actual labels, (middle) SED-fitting predictions vs. the actual labels, and (right) a direct comparison of the predictions from the ML and SED-fitting methods. The actual labels are derived from the mock catalog described in Section 3.4.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Distribution of training and testing sets in the mock sample, visualized using UMAP. Red and black points represent star-forming and quiescent galaxies, respectively. The dimensions of the 2D plots (D1 and D2) are arbitrary labels and do not carry any physical significance.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Precision–recall curve for quiescent galaxy classification (AUC = 0.97). The red circle marks our operating threshold (0.5), achieving 90% precision and 88% recall. The dashed line shows random-classifier performance.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Heat map comparison of the mock (with and without injected noise) and COSMOS2020 galaxy colors (u − F814W and F814W − Y). The injected mock galaxies show similar color distributions and cover the COSMOS2020 galaxies manifold, indicating good representation of real colors.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Relative importance of the top 10 colors (of 28 total color features) in the trained model for classifying quiescent and star-forming galaxies in the COSMOS2020 sample.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: A 2D UMAP projection provides a clear visualization of the distinct populations of quiescent and star-forming galaxies using ML within the COSMOS2020 sample data. The dimensions of D1 and D2 are arbitrary labels and do not carry any physical significance.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Precision (purity), recall (completeness), and F1 score of ML and SED-fitting classifiers on the testing set for quiescent galaxies as a function of redshift bins.
Paper: Global Distribution of the Key Species on the Surface of Europa
Authors: Jiazheng Li, Yinsi Shou, Cheng Li, Xianzhe Jia
Figure caption: Global distribution of the four major nonwater species in the surface ice of Europa for the baseline model. (a) H2SO4. (b) SO2. (c) H2O2. (d) O2.
Paper: Global Distribution of the Key Species on the Surface of Europa
Authors: Jiazheng Li, Yinsi Shou, Cheng Li, Xianzhe Jia
Figure caption: Global distribution of the four major nonwater species in Europa’s surface ice with reaction rate coefficients scaled down by a factor of 10. (a) H2SO4. (b) SO2. (c) H2O2. (d) O2.
Paper: Cold Gas in a Post-starburst Pair in the z ∼ 1.4 HeavyMetal Survey: Major Mergers as a Pathway to Retain Gas in Quenched Galaxies
Authors: Katherine A. Suess, Aliza G. Beverage, Mariska Kriek, Justin S. Spilker, Rachel Bezanson, Vincenzo R. D'Onofrio, Jenny E. Greene, Jamie Lin, Yuanze Luo, Desika Narayanan, Imad Pasha, Sedona H. Price, David J. Setton, Margaret E. Verrico, Yunchong Zhang
Figure caption: Left: sSFR as a function of gas fraction for a sample of star-forming galaxies at z ∼ 0.5–1.5 (PHIBSS & PHIBSS-2; L. J. Tacconi et al. 2013; J. Freundlich et al. 2019; gray contours) and quiescent galaxies at z > 1 (colored points). sSFRs for our sample are from our Prospector fits, while sSFRs for literature samples are taken from the relevant paper. Gas detections are outlined in black. Dashed lines indicate constant depletion times (﹩{t}_{\mathrm{dep}}\equiv {M}_{{{\rm{H}}}_{2}}/\mathrm{SFR}﹩). Our observations are at or below the expectations for star-forming galaxies, with depletion times longer than 1 Gyr. Right: molecular gas mass as a function of time since quenching both for our sample of PSBs at z ∼ 1.4 and the SQuIGG﹩\overrightarrow{L}﹩E sample of PSBs at z ∼ 0.7 (R. Bezanson et al. 2022). While the SQuIGG﹩\overrightarrow{L}﹩E galaxies show a clear trend that gas-rich galaxies quenched more recently, no clear trend is present in our observations at higher redshift.
Paper: Cold Gas in a Post-starburst Pair in the z ∼ 1.4 HeavyMetal Survey: Major Mergers as a Pathway to Retain Gas in Quenched Galaxies
Authors: Katherine A. Suess, Aliza G. Beverage, Mariska Kriek, Justin S. Spilker, Rachel Bezanson, Vincenzo R. D'Onofrio, Jenny E. Greene, Jamie Lin, Yuanze Luo, Desika Narayanan, Imad Pasha, Sedona H. Price, David J. Setton, Margaret E. Verrico, Yunchong Zhang
Figure caption: Nondetections of our primary HeavyMetal targets. Left: ALMA CO(2–1) spectra extracted at the position and redshift of our target. Center left: CO(2–1) line map; white “x” at the center shows the position of our target. Center: HST-F160W images with CO contours overlaid (3σ, 4σ, 5σ). No sources are detected in the cubes for HM2-23351 or HM2-57702. In the HM-213947 cube we serendipitously detect UVISTA-214044 at z ∼ 1.4; in the HM1-217249 cube we serendipitously detect 217299 at z ∼ 1.38. Center right: multiband photometry and Prospector fits to each galaxy. Right: best-fit star formation history for each galaxy.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: The parameter space of detection limits for various methods, adapted from D. J. Hutter et al. (2021). The approximate conversion between the mass ratio, and ΔV were computed assuming a B0V primary from M. J. Pecaut & E. E. Mamajek (2013). The separation and period relation is computed for a B2V/B5V binary, with no eccentricity. For spectroscopy detection limits, we adopt H. Sana et al. (2009) where the binary detection probability drops beyond a year for their simulations of massive stars. The dashed and dotted lines represent the speckle detection limits (20 mas–1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2) at distances of 100, and 1000 pc (approx. distances of stars in this study). The complementarity of different methods in discovering binaries is showcased here. Also shown are detected binaries in our sample from speckle imaging presented in this work (black circles), literature spectroscopy (red circles), archival seeing-limited imaging observations (cyan circles), and interferometric (green) observations. Note that the limits shown here are illustrative, and depend on the exact instrumental configuration for each case.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: The upper and lower limits of separation range from the primary captured by the speckle observations, as a function of distance. Distances are taken from Gaia EDR3 data of C. A. L. Bailer-Jones et al. (2021).
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Projection of observed targets on all-sky DSS image. Speckle identified binaries are marked.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Histogram of spectral types for all observed targets.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Averaged detection limits for companions around Be stars computed using the contrast curves, and converted to mass ratios assuming A. Dotter (2016) stellar models for the EO 716 (top) and EO 832 filters (bottom). Gray-shaded regions describe the variation among the detection limits.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Color–magnitude diagrams (left panel) and reconstructed images and contrast curves (right panel) of multiples detected in two speckle filters. A. Dotter (2016) isochrones computed in the appropriate filters are plotted for 1, 10, 100 Myr using dashed, dotted, and solid lines. The dashed dotted line is for 1 Gyr. Stars with magnitude in only one filter are assumed to have the same Δm in the other for plotting purposes, and are marked by a caret with a color error of 0.2 mag.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Candidate binaries meeting either of the Gaia binary indicators. RUWE candidates are shown by black squares, with the cut-off of 1.4 marked, and ipd_frac_multi_peak candidates are shown as blue circles where the cut-off (>2) is shown by a solid line. Detected archival, or speckle companions are shown by filled green and red markers respectively. For visual purposes, the maximum ipd_frac_multi_peak value was set to 10, and the RUWE value to 6.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Reconstructed image of 66 Oph in the speckle EO832 filter. The contrast curves for that filter, and the bluer EO562 filter are shown. The companion is visible close to the binary, around 50 mas away, at a position angle of 211° (a 180° ambiguity exists in the position angle of the companion).
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Zoomed-in reconstructed images for very close companions. The companion location is shown by the red arrow for 66 Oph (top left), HD 139431 (top right) in the EO832 filter, and in both EO 562 and EO 832 for HD 56039 in the bottom panel.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption:  ﹩\upsilon /{\upsilon }_{{\rm{\max }}}﹩ of all the selected CBe stars with spectral types between B0-B5 having Gaia DR2 parallaxes >1 mas found in the BeSS database, and also the observed sample. The dotted histogram represents the ﹩{d}^{2}/{d}_{{\rm{\max }}}^{2}﹩ values for the observed sample.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: Histogram of separations of known companions. No candidates are included. Black bars represent companions identified in speckle imaging, whereas cyan and red bars are literature imaging and spectroscopic companions respectively. The cyan bar at separation less than 1 au is the interferometric binary identified in QV Tel. The information presented is given in tabular form in Tables 1, 3, and 4.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Left: inferred magnetic field orientations around HH 211 from the Band 3 polarized continuum with a robust parameter of 0.5. The line segments represent plane-of-sky magnetic field directions, with green for PI > 2σPI and red for 1.5σPI < PI < 2σPI. The blue and red contours indicate CO (2–1) integrated intensities in velocity ranges from 0 to 8 and from 10 to 18 km s−1, respectively. The blue and red contour levels are 0.03, 0.035, 0.05, 0.1, and 0.2 K km s−1. The black lines are the Band 3 dust continuum with a robust parameter of 0.5, showing 5, 10, 20, 50, 100, 200, and 500 times the rms noise level. Right: inferred magnetic field orientations around HH 211 from the Band 6 polarized continuum with a robust parameter of 2.0. Green segments represent plane-of-sky magnetic field directions with green for PI > 2σPI and red for 1.5σPI < PI < 2σPI. The black lines are the Band 6 dust continuum with a robust parameter of 2.0, showing 5, 10, 20, 50, 100, 200, and 500 times the rms noise level. The gray U-shaped curves indicate the pinched magnetic field patterns around the protostar. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: The density-enhanced model. Top: temperature and dust mass density in the x–z plane (y = 0). Middle: synthetic images in Band 3 (97.5 GHz) and Band 6 (233 GHz), and the spectral index from the two synthetic images. Contour levels are 5, 10, 20, 50, 100, 200, and 500 times the rms noise level in the observations. Bottom: the line-of-sight averaged temperature and the column density calculated from the two synthetic images. The black dotted line indicates the optical depth of 0.1 at 233 GHz. Note that the estimated values are uncertain in the central region.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: The temperature-enhanced model. Individual panels are the same as Figure 17.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Polarization fraction around the HH 211 envelope in Band 3 with a robust parameter of 0.5 (left) and in Band 6 with a robust parameter of 2.0 (right). The black lines represent Stokes I intensity levels with 5 (left)/3 (right), 10, 20, 50, 100, 200, and 500 times the rms noise level in each observation. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Polarized intensity around the HH 211 envelope in Band 3 with a robust parameter of 0.5 (left) and in Band 6 with a robust parameter of 2.0 (right). The black lines represent Stokes I intensity levels with 5 (left)/3 (right), 10, 20, 50, 100, 200, and 500 times the rms noise level in each observation. The synthesized beam size and spatial scale bar are shown in the bottom left and bottom right of both panels, respectively.
Paper: The Hourglass-shaped Magnetic Fields and Dust Filaments in the HH 211 Protostellar Envelope
Authors: Youngwoo Choi, Woojin Kwon, Leslie W. Looney, Ian W. Stephens, Zhi-Yun Li, Floris F. S. van der Tak, John J. Tobin
Figure caption: Dust continuum around HH 211 in Band 6 (233 GHz) with a robust parameter of 2.0. The synthesized beam and spatial scale bar are shown in the bottom-left and bottom-right corners, respectively.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Planet radius as a function of planet mass. We plot the exoplanets in our subsamples as black-bordered shapes and solar system terrestrial planets as filled black circles. Four exoplanets in our sample have lower densities than predicted by M. Plotnykov & D. Valencia (2020) for 100% rock compositions: Kepler-36 b, Kepler-105 c, 55 Cnc e, and WASP-47 e. We indicate the exoplanets Kepler-36 b and Kepler-105 c as black-bordered light-blue squares. Kepler-36 b was likely formerly in a mean motion resonance with Kepler-36 c, while Kepler-105 c is in a mean motion resonance with Kepler-105 b. They are the only two terrestrial exoplanets in our sample that are or were likely formerly mean motion resonant. We indicate 55 Cnc e and WASP-47 e as black-bordered light-green squares. Both 55 Cnc e and WASP-47 e are USP exoplanets with multiple giant exoplanet companions orbiting the two most metal-rich stars in our sample. We indicate the only super-Mercury in our sample, Kepler-107 c, as a black-bordered gray diamond.
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: Similar to Figure 4, except the intensities are normalized to their peak, and the peak intensities’ locations are shown as vertical lines. The height of the vertical lines is only meant to help differentiate results that have the same peak location. The resolution of the models and data is 3°. Results suggest an average slab percentage of 50% ± 28% (standard deviation) and ±5% (standard error).
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Comparisons of updated planetary masses and radii from our approach using Doppler and transit observables and accurate, precise, homogeneous, and physically self-consistent stellar masses and radii based on photospheric stellar parameters from our analyses, APOGEE DR17, and J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). We indicate the mean deviation about the line y = x line in each panel, and those values support the mutual consistency of the updated planetary masses and radii implied by Doppler/TTV and transit observables and these three independent photospheric stellar parameter analyses.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Comparisons of inferred stellar masses and radii based on our approach using as inputs photospheric stellar parameters from our analyses, APOGEE DR17, and J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). We indicate the mean deviation about the line y = x line in each panel, and those values support the mutual consistency of the stellar masses and radii implied by these three independent photospheric stellar parameter analyses.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Comparisons of inferred photospheric stellar parameters between between our analyses, APOGEE DR17, and J. M. Brewer et al. (2016) and J. M. Brewer & D. A. Fischer (2018). We indicate the mean deviation about the line y = x in each panel, and those values support the mutual consistency of the photospheric stellar parameters produced by these three independent analyses.
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: Simulated ribbon maps for the slab-50% case, where the neutral SW source is averaged over (left) 2004 through 2008, (middle) 2005 through 2007, and (right) 2006 through 2008.
Paper: Terrestrial Exoplanet Internal Structure Constraints Enabled by Comprehensive Host Star Characterization Reveal That Terrestrial Planets in Mean Motion Resonances Are Water Rich
Authors: Alejandra Ross, Henrique Reggiani, Kevin C. Schlaufman, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Normalized spectrum for each star in our archival sample, grouped by instrument and sorted by [Fe/H].