adsabs/AstroCLIMB huggingface dataset:
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Comparison between C2N (left) and OTFMAP (right) observations of Circinus at 89 μm. First row: Herschel observations at 70 μm (color scale) of Circinus within an FOV of 350 × 350 arcsec2 with overlaid C2N (left) and OTFMAP (right) configurations. For C2N, on-source (white) and off-source (yellow) positions with the FOV of HAWC+ at 89 μm are shown. For OTFMAP, the Lissajous curve (white solid line) of the scan is shown. Second row: HAWC+ total flux observations for C2N and OTFMAP within the same FOV as above. Contours start at 32σ  I  and increase in steps of 2 n  σ, where n = 5, 5.5, 6,... and σ  I  = 0.3 mJy arcsec−2. The beam size is shown as a red circle in the bottom left. Third row: same as above within an FOV of 120 × 120 arcsec2. Polarization measurements (white lines) are shown for P/σ  P  ≥ 3, PI/σ PI ≥ 3, P < 30%, and I/σ  I  ≥ 50. A 5% polarization measurement is shown at the bottom right. Fourth row: HAWC+ polarized flux observations (color scale) within the same FOV and polarization as above. Contours start at 3σ PI and increase in steps of 1σ PI, where σ PI = 0.45 mJy arcsec−2.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: OTFMAP polarimetric observations of a planet (Neptune) and polarization skydip (poldip) at 53 μm. Top panels: polarization observations of a planet. Stokes I (left) in ﹩{\mathrm{log}}_{10}﹩ scale, normalized Stokes q = Q/I (middle), and u = U/I (right) are shown. The FOV is 40 × 40 pixels (48 × 48 arcsec2, with pixel scale of 1.″21). Bottom panels: polarization observations of a skydip. Normalized Stokes q = Q/I (middle) and U/I (right) are shown. The FOV is 32 × 40 pixels (82 × 102 arcsec2, with a pixel scale of 2.″55). Definitions and details of the estimation of the IP are described in Sections 2.5 and 3.3.
Paper: Extragalactic Magnetism with SOFIA (SALSA Legacy Program). III. First Data Release and On-the-fly Polarization Mapping Characterization 
Authors: Enrique Lopez-Rodriguez, Melanie Clarke, Sachin Shenoy, William Vacca, Simon Coude, Ryan Arneson, Peter Ashton, Sarah Eftekharzadeh, Rainer Beck, John E. Beckman, Alejandro S. Borlaff, Susan E. Clark, Daniel A. Dale, Sergio Martin-Alvarez, Evangelia Ntormousi, William T. Reach, Julia Roman-Duval, Konstantinos Tassis, Doyal A. Harper, Pamela M. Marcum
Figure caption: Sensitivity comparison between C2N (red) and OTFMAP (blue) observations of Circinus at 89 μm. Histograms of the total intensity (top left), polarized intensity (top right), standard deviations of the total flux (middle left), and polarized flux (middle right) are shown. The median and 1σ uncertainty of the distribution of the standard deviations are shown in the middle panels. The polarization fraction (bottom left) and polarization angle (bottom right) for C2N and OTFMAP observations are shown. A 1:1 line (black dashed line) is shown.
Paper: A Magnetogram-matching Method for Energizing Magnetic Flux Ropes Toward Eruption
Authors: V. S. Titov, C. Downs, T. Török, J. A. Linker
Figure caption: The initial pre-eruptive equilibrium: maps of α (panel (a)) and ﹩{\mathrm{log}}_{10}\,Q﹩ (panel (b)) in the central cross section of the configuration whose magnetic field lines and current layers are shown in panels (c) and (f) (side view) and panels (d) and (g) (top view), respectively. Field lines of the MFR and SMA are colored in green and yellow, respectively. Isosurfaces ﹩j/{j}_{\max }=0.438﹩ (magenta) and ﹩\alpha /{\alpha }_{\min }=0.079﹩ (semitransparent cyan) show the corresponding layers of direct and return currents. Panel (e) depicts representative field lines corresponding to observed morphological features (see Titov et al. 2021). The photospheric B  r  distribution is shown by gray shading from white (B  r  > 0) to black (B  r  < 0); the overlaid high-Q lines colored in magenta (if B  r  > 0) and cyan (if B  r  < 0) outline the footprints of the MFR and SMA. The two quasi-separators (QS1 and QS2) described in this section are indicated in panel (b).
Paper: Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins
Authors: Matthew M. Dallas, M. S. Oey, Norberto Castro
Figure caption: Panel (a): CDFs of distances to the nearest O-type star for the populations shown. The top and bottom axes show the separation in parsecs and degrees, respectively. The maximum and minimum CDFs from which the median is constructed are shown by the shaded regions for Early O stars and Be stars (see text). Panel (b): only allowing confirmed O stars as candidate nearest O stars. Panel (c): only allowing field O stars, including uncertain OB stars, as candidate nearest O stars.
Paper: Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins
Authors: Matthew M. Dallas, M. S. Oey, Norberto Castro
Figure caption: Cumulative distribution functions of distances to the nearest O-type star for the shown populations similar to Figure 2, but with OB and OBe populations binned by stellar mass as shown. Representative maximum and minimum CDFs from which the medians are constructed are shown by the shaded regions for OB stars with m > 30 M ⊙ and OBe stars with m < 20M ⊙.
Paper: Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins
Authors: Matthew M. Dallas, M. S. Oey, Norberto Castro
Figure caption: Mass distributions when including the stellar lower-mass limits (left) versus upper-mass limits (right) for stars with uncertain classifications spanning a range of spectral types. The bimodality for the upper-mass estimates results from the fixed adopted spectral-type ranges (see text), which translate into a limited range of upper-mass limits, most of which overestimate the true masses. These mass estimates show that our sample of OBe stars is not significantly biased toward lower masses.
Paper: Classical OBe Stars as Post-supernova Runaways: Confirming Binary Origins
Authors: Matthew M. Dallas, M. S. Oey, Norberto Castro
Figure caption: OB (blue) and OBe (red) stars from OKP plotted on an Hα image of the SMC (Smith et al. 2005). The 29 stars of uncertain emission-line status in Table 2 are included here as OBe stars.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: The left panel shows the synthetic light curves of the different radio frequencies (shown in different colors and line styles) for two different cases. In one case, we take the planetary magnetic field as 3 G (dashed curve H in the figure), and in another case, we take the value as 0.33 G (solid curve in the figure). The thick black dashed line indicates the midpoint of the transit. The right panel is the same as the left panel, but zoomed in, focusing only on the transit phase between 0.4 and 0.6. The planet is placed at a distance of 10R * from the star.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Top: a zoom-in on the planetary magnetosphere for the close-orbit case for a nonmagnetized (left), weakly magnetized (middle), and strongly magnetized (right) planet. Bottom: a zoom-in on the planetary magnetosphere for the far-orbit case for a nonmagnetized (left), weakly magnetized (middle), and strongly magnetized (right) planet. The display is similar to Figure 2. This figure indicates that the size of the planetary magnetosphere is larger for the higher planetary magnetic field.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Evolution of the star–planet interactions at different planetary phases. The thin black line corresponds to different planetary phases like 0.25, 0.375, 0.458, 0.5, 0.625, and 0.75. The thick black line corresponds to the midtransit line (phase 0.5) along which the telescope is placed. The eye symbol in the figure represents the observing telescope. The planet is placed at a distance of 10R * from the star.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Same as Figure 3, but for the case when the planet is placed at 20R * from the central star. The thick black dashed line corresponds to the midtransit line (phase 0.5). The dashed line corresponds to the higher magnetic field (3 G), while the solid line corresponds to the lower magnetic field (0.33 G).
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: A sample of synthetic radio images produced by the model. Results are shown for 10 MHz (top) and 1 GHz (bottom) for the corresponding viewing phase angle of 0.25 (left), 0.5 (middle), and 0.75 (right). These images are for the case where the planet is located at 10R * and has a planetary field of 3 G, and the planet’s signature is clearly seen in all images. The planet is visible in the radio images for all other cases as well.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Same as Figure 2, but for the case where the planet is nonmagnetized. The thin black line corresponds to different planetary phases like 0.25, 0.375, 0.5, 0.625, 0.75, and 0.875. The thick black line corresponds to the midtransit line (phase 0.5) along which the telescope (eye symbol in the figure) is placed.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Same as Figure 2, but for the case where the planet is located at 20R *. The thin black line corresponds to different planetary phases like 0.25, 0.375, 0.5, 0.625, 0.79, and 0.83. The thick black line corresponds to the midtransit line (phase 0.5) along which the telescope (eye symbol) is placed.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Same as Figure 3, but for the case when the planet is nonmagnetized. The thick black dashed line corresponds to the midtransit line (phase 0.5).
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Total system W  r (Ca II K) (left) and W  r (Na I 5891) (right) versus the dust reddening measured along the QSO sight line, E(B − V)(g−i). Upper limits, indicated with open squares, are shown in cases in which ﹩{W}_{r}\lt 3{\sigma }_{{W}_{r}}﹩, and represent 3σ limits. Sight lines shown in light blue and orange have no intervening systems that are unassociated with the known foreground galaxy. Sight lines indicated in red exhibit one or more unassociated intervening systems in their SDSS spectra. The solid blue curves show the best-fit relations between the W  r  of these ions due to the Milky Way’s ISM/halo and dust reddening measured by Murga et al. (2015). The dashed blue curves represent the ±1σ uncertainties in these fits. The purple curves show the best-fit relation (and the  ±1σ uncertainty in the relation) between W  r (Na I 5891) and dust reddening in the Milky Way measured by Poznanski et al. (2012). The small purple circles/triangles show W  r (Na I 5891) values/3σ upper limits measured from high-resolution QSO spectra by Poznanski et al. (2012), plotted versus the reddening toward that coordinate in the Planck Collaboration et al. (2016) dust map. Data points outlined in dark blue are offset by >3σ from the closest point on the best-fit Murga et al. (2015; left) and Poznanski et al. (2012; right) relations.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Top row: total system column density of Ca II (left) and Na I (right) versus projected distance from the associated GOTOQs. Symbols correspond to those used in Figure 6. The filled regions indicate the range in column densities predicted for a Milky Way–like ISM observed from an external viewpoint using the simple model described in Section 6.1, and assuming three different disk inclinations (i = 0°, 50°, and 75°, shown in red, purple, and turquoise, respectively). The horizontal dotted lines show the value of the central perpendicular column density of the Milky Way disk model, adjusted by a factor ﹩1/\cos i﹩. Bottom row: fitted component velocity offsets relative to z Hα  for Ca II (left) and Na I (right) absorbers. Systems fit with single velocity components are shown with solid light blue and orange squares. The primary and secondary components of systems fit with two components are shown with filled and open squares outlined in a complementary color. Error bars show the span of velocities included in the Δv 90 measurement for the Ca II K and Na I 5891 lines. Colored boxes indicate the maximum projected line-of-sight velocity width predicted using simple tilted-ring models with extraplanar layers placed at z = ±0.82 kpc (for Ca II) and ±0.43 kpc (for Na II). The maximum rotation velocity (V ∞) of each model is set by the stellar mass Tully-Fisher Relation, and the R V parameter is varied to model both steeply rising (purple boxes) and gradually increasing (turquoise boxes) rotation curves.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: The total system Na I equivalent width (W  r,tot(Na I) = W  r (Na I 5891) + W  r (Na I 5897)) versus ﹩\mathrm{log}\,{M}_{* }/{M}_{\odot }﹩ measured in our ESI spectroscopy. Upper limits, indicated with open squares, are shown in cases in which ﹩{W}_{r,\mathrm{tot}}\lt 3{\sigma }_{{W}_{r,\mathrm{tot}}}﹩, and represent 3σ limits. Measurements of GOTOQJ0851+0791 have been excluded, as the Na I 5897 profile in that sight line is contaminated by blending. The turquoise and magenta filled regions show the distribution of W  r  values measured by Chen et al. (2010b) in coadded SDSS galaxy spectra for the blueshifted and systemic components of the Na I absorption profile, respectively. The open regions show the locus of values covered by the Chen et al. (2010b) measurements if they are corrected upward by a factor of two to account for the potential contribution of material located on the far side of the stellar continua.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Total system W  r (Ca II K) (left) and W  r (Na I 5891) (right) versus ﹩\mathrm{log}\,{M}_{* }/{M}_{\odot }﹩ (top row) and SFRlocal (bottom row) measured for the foreground host system. Large colored points indicate constraints from our ESI spectroscopy. Upper limits, indicated with open squares, are shown in cases in which ﹩{W}_{r}\lt 3{\sigma }_{{W}_{r}}﹩ and represent 3σ limits. Gray points show measurements reported in Straka et al. (2015) for the parent GOTOQ sample. The filled boxes indicate the ±34th percentile Wilson score confidence intervals, with respect to the right axes, for the covering fraction of absorbers having W  r  > 0.2 Å in our ESI sample.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: ESI GOTOQ spectra showing the locations of the Ca II H & K and Na I λ λ5891, 5897 transitions in the rest frame of the foreground galaxy. The velocity is defined relative to the GOTOQ redshift estimated from a Gaussian fit to its Hα emission as described in Section 4.1 (z Hα ). The gray horizontal line indicates the continuum level, and the gray shaded region shows the velocity window selected for computation of W  r , N a od, and Δv 90. Absorption from unassociated blends is shown with a dotted histogram. The blue and red bars show the pixels that contain >5% of the total apparent optical depth of the line (determined by stepping inward from the profile edges), and the length of these bars corresponds to Δv 90. Best-fit profile models are shown with cyan (for Ca II) and orange (for Na I) curves for systems with significantly detected absorption (see Section 4.2 for details).
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Left: the fraction of the total SFR of each foreground galaxy probed by the corresponding SDSS fiber, as implied by our exponential disk modeling. The rose-colored horizontal dashes indicate the fraction of H II region emission observed if the galaxy is viewed face-on, while the vertical turquoise lines show the range in this observed fraction in the case that the galaxy is oriented close to edge-on with i = 75° (accounting for uncertainty in the positional angle of the fiber placement). Right: the SFRlocal measured in each fiber observation (magenta squares) vs. R ⊥. The ranges indicated in orange show the span of SFRtot values implied by the fractions shown at left.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Fitted component velocity offsets relative to z Hα  for Ca II (light blue) and Na I (orange) absorbers. Systems fit with single velocity components are shown with solid light blue and orange squares. The primary and secondary components of systems fit with two components are shown with filled and open squares outlined in a complementary color. Error bars show the span of velocities included in the Δv 90 measurement for the Ca II K and Na I 5891 lines. Symbols have been offset horizontally by ±0.1 for clarity.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: XMM-Newton/RGS (stacked) 0.35–1.8 keV and Chandra High Energy Transmission Gratings (HETG; 1−9 keV) light curves from the 2020 August campaign on Her X-1, with a resolution of 100 s. The campaign consisted of three full-orbit XMM-Newton observations as well as two shorter Chandra observations. Aside from the high state and a brief low flux period, we observed one full and two partial eclipses of Her X-1 by the secondary and four absorption dipping periods. The 0.3–10 keV European Photon Imaging Camera (EPIC) pn light curve has a very similar shape to the RGS light curve, but the absorption dips are less pronounced due to the higher energy coverage of pn. Chandra count rate during observation 23356 was scaled by the RGS/HETG count ratio during observation 23360 with simultaneous coverage of both instruments. The light curve of Chandra observation 23360 is not shown, as the same time interval is covered by XMM-Newton. The elapsed time of 0 corresponds to MJD 59071.69035.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: EPIC pn spectrum of the high state from observation 0865440501 (80 ks clean exposure), focusing on the Fe K region. The data are shown in the top plot in black (error bars are so small they are difficult to see in the spectrum). The blue curve shows the best-fitting model containing one broad Gaussian, while the red curve corresponds to the model containing two broad Gaussian lines. The red dashed lines in the top subplot are the individual spectral components in the more complex, two-Gaussian model. The Gaussian components are shifted by a constant amount for better visual clarity. The bottom subplot shows the residuals to the blue model in black, as well as how the model with two Gaussians fits the data (in red).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Left panel: periods of excited ℓ = 1 g modes as a function of the effective temperature, with the palette of colors (right scale) indicating the logarithm of the e-folding time (τ e in years), for the PG 1159 sequence with M ⋆ = 0.565M ⊙. Right panel: same as left panel, but for ℓ = 2 modes. In both panels, the pulsation periods with the identification of ℓ according to our asteroseismic model (see Table 7) are shown as horizontal segments, where their widths represent the possible T eff interval, according to the best asteroseismic model (Table 8).
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: A schematic of the Her X-1 system, showing the different regions producing emission lines of various velocity widths. The x-axis of the schematic is in logarithmic scale. For simplicity, the scheme omits the accretion disk wind (detected through its absorption lines), likely originating from the inner parts of the accretion disk atmosphere.