adsabs/AstroCLIMB huggingface dataset:
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Example of the curve of flux growth of the PACS 70 μm map of NGC 4945. Y-axis is flux within the circle of a certain radius. The error bar shows background rms plus 7% absolute flux calibration error.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: Plot showing the ratio of each element normalized to O and divided by its photospheric value, X/O:X/Ophot, organized by FIP value for the two CME plasma populations in Figure 4.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: Plot showing the absolute abundance of each element, X/H, organized by mass for the high C/Fe CME plasma population shown in the black diamonds of Figure 4 from this work as compared to the abundances computed for a depleted streamer core and leg, and typical coronal abundances from SOHO/UVCS in Raymond et al. (1997b), and the solar wind depleted periods from Weberg et al. (2012).
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: (Left plot) Count distribution of all 2 hr CME periods across the solar cycle in blue, periods associated with the black diamonds in Figure 4 in black, and the red curve is the sunspot number. The right plot shows the ratio of the black to blue distributions from the left plot and the sunspot number in red and the error bars are the Poisson counting statistics uncertainties.
Paper: Manifestation of Gravitational Settling in Coronal Mass Ejections Measured in the Heliosphere
Authors: Yeimy J. Rivera, John C. Raymond, Enrico Landi, Susan T. Lepri, Katharine K. Reeves, Michael L. Stevens, B. L. Alterman
Figure caption: Normalized distribution of the 〈QFe〉 values of the black and red diamond CME periods shown in Figure 4.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Evolution of the eVDF in the proton frame at six different times on 2020 October 2. Each  eVDF plot corresponds to an increasing magnetic field rotation angle: (A) 0.13° [11h:34m:47s], (B) 14.52° [16h:09m:58s], (C) 28.81°[12h:59m:22s], (D) 90.80°[23h:32m:56s], (E) 110.54°[23h:18m:08s], and (F) 146.31°[23h:12m:26s]. The portions of the electron distribution with velocity components parallel to the B field (smaller pitch angles) are shown in blue. Those with antiparallel components (larger pitch angles) are in red, as shown by the color bar. The solid black lines and dashed lines in the panels are cuts through the fits in the perpendicular and parallel/antiparallel directions, derived as described below. During this period, the electron strahl flows in the antiparallel direction.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Scatterplot of the number density (n) for the strahl, halo, suprathermal FA (antistrahl direction), and suprathermal AFA (strahl direction) populations, with their respective averages, in relation to magnetic field rotation angle for 2020 October 2. Each dot on the plot represents an individual measurement point.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Close-up view of the antistrahl side of the eVDFs from Figure 1 for 2020 October 2. Like Figure 1, each eVDF plot corresponds to an increasing magnetic field rotation angle: (A) 0.13°, (B) 14.52°, (C) 28.81°, (D) 90.80°, (E) 110.54°, and (F) 146.31°. The portions of the electron distribution with velocity components parallel to the B field (small pitch angles) are shown in blue.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Scatterplot of the heat flux(q) for the FA suprathermal (blue), AFA suprathermal (red), and suprathermal total (FA + AFA) (orange) populations, with their respective averages. FA suprathermal heat flux goes from a deficit to excess, while AFA heat flux decreases slightly at large magnetic field rotation angles. Total heat flux shows an anticorrelation with magnetic field rotation angle, primarily due to the FA contribution.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Various core electron parameters plotted as a function of time for 2018 November 2. From top to bottom: Magnetic field rotation angle/B angle (degrees) and nominal Parker spiral angle (degrees), core number density (per cubic centimeter), core parallel component temperature (electronvolts), core anisotropy, and core electron plasma beta.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Strahl distribution width and height from a Gaussian fit to the pitch angle distribution measured at 314 eV, as a function of magnetic field rotation angle, for 2019 April 1. The height of the Gaussian is the amplitude of the curve. The strahl height is dimensionless as the amplitude of the strahl is normalized to the magnitude of the distribution at 90° angle. The strahl width represents the standard deviation of the Gaussian and is in units of degrees.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Scatterplots of the FA suprathermal number density and heat flux for selected dates. The color of each data point represents the heat flux, with positive (FA) heat flux shown in red and negative (AFA) in blue. Both the FA number density and heat flux become positive at larger magnetic field rotation angles. Nominal Parker spiral angle and the average solar wind speed are also listed for each day.
Paper: Switchbacks in the Young Solar Wind: Electron Evolution Observed inside Switchbacks between 0.125 au and 0.25 au
Authors: Raaman Nair, Jasper S. Halekas, Phyllis L. Whittlesey, Davin E. Larson, Roberto Livi, Matthieu Berthomier, Justin C. Kasper, Anthony W. Case, Michael L. Stevens, Stuart D. Bale, Robert J. MacDowall, Marc P. Pulupa
Figure caption: Core electron plasma beta correlation to the rotation of the magnetic field for 2018 November 5. Results show a direct correlation between the beta parameter and magnetic field rotation angle.
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Transit light curves of a moon-hosting exoplanetary system: (a) with r  p  = 0.1, r  m  = 0.01, t 0b  = 5 days, t 0m  = 10 days, P  b  = 300 days, P  m  = 20 days, r pm = 200, M  p /M  m  = 1411, i  b  = 90 o , i  m  = 90 o , α mb = 20 o , u 1 = 0.4, and u 2 = 0.25; (b) replacing t 0m  = 8 days and α mb = 30 o .
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Transit light curves of a moon-hosting exoplanetary system: (a) with r  p  = 0.075, r  m  = 0.02, t 0b  = 5 days, t 0m  = 10 days, P  b  = 60 days, P  m  = 15 days, r pm = 25, M  p /M  m  = 81, i  b  = 90 o , i  m  = 90 o , α mb = 0 o , u 1 = 0.4, and u 2 = 0.25; (b) same but with t 0m  = 5 days. The dashed red lines show the transit light curves of the planet in the absence of a moon. The TTV due to the presence of a moon can be observed in (a).
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Transit light curves of a moon-hosting exoplanetary system: (a) with r  p  = 0.1, r  m  = 0.01, t 0b  = 5 days, t 0m  = 10 days, P  b  = 300 days, P  m  = 20 days, r pm = 200, M  p /M  m  = 1411, i  b  = 90 o , i  m  = 90 o , α mb = 0 o , u 1 = 0.4, and u 2 = 0.25; (b) replacing t 0m  = 8 days.
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Orbital orientation of the star–planet–moon system from the observer’s point of view, showing z sp, z pm, and z sm, the separations between the centers of the star and the planet, the planet, and the moon, and the star and the moon, respectively; z  sb , z  pb , and z  mb , the separation of the planet–moon barycenter from the centers of the star, the planet, and the moon, respectively; α mb, the angle between the major axes of the projected orbits of the planet–moon barycenter around the star and the moon around the planet–moon barycenter; a  b  and a  m , the orbital semimajor axes of the planet–moon barycenter around the star and the moon around the planet–moon barycenter, respectively.
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: (I) Alignment with star–planet and planet–moon intersections showing l 1s  and l 2s , the separation of the star from the points of intersection of the planet and the moon; (II) alignment with star–planet and star–moon intersections showing l 1p  and l 2p , the separation of the planet from the points of intersection of the star and the moon; (III) alignment with star–planet and star–moon intersections showing l 1m  and l 2m , the separation of the moon from the points of intersection of the star and the planet.
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Alignment with intersection of all the three bodies (i.e., the star, the planet, and the moon) showing A △, the area of the triangle, and A sa, A pa, and A ma1, the areas of the arcs within the common area of intersection of the three bodies.
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: An instance of all possible cases of alignment for the star (blue), the planet (red), and the moon (green).
Paper: Transit Light Curves for Exomoons: Analytical Formalism
Authors: Suman Saha, Sujan Sengupta
Figure caption: Alignment of the three bodies with star–planet and planet–moon intersections.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: The total kinetic energy in the accelerated CRs integrated over the SNR volume as a function of age for models A1 to A3. The line formats are the same as in Figure 3. The top panel shows the time evolution of the total energy in all CRs inside the SNR in units of the SN explosion energy E SN. Likewise, the middle panel shows the evolution of the reacceleration component. The bottom panel shows the energy ratio between the reacceleration component and the total.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Spectral index evolution at 1 GHz and 10–100 GeV. We denote α as in S  ν  ∝ ν −α , where S  ν  is the flux density at frequency ν, and Γ is defined by ﹩{dN}/{dE}\propto {E}^{-{\rm{\Gamma }}}﹩. Indices from observations are overlaid as data points for reference, with the red and blue points for Type Ia and CC remnants, respectively.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Time snapshots of CR proton spectra at three different dynamical ages integrated over the whole SNR volume for models A1 and A2. The total spectra (red solid) are decomposed into components from the freshly accelerated CRs (green dashed–dotted) and the reaccelerated CRs (blue dashed–dotted) to visualize their relative contributions to the accelerated CRs.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Local phase-space distribution of CR protons at the shock plotted at three time epochs. Same as Figure 9, the total spectrum (red solid) is decomposed into components from the freshly accelerated CRs (green dashed–dotted) and the reaccelerated CRs (blue dashed–dotted). The spectral break from the ion−neutral damping effect is applied to the total spectrum only for clarity. The background Galactic CRs are also plotted for reference (gray dotted line).
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Light curves in the 10–40 keV energy range separated into the (a) nonthermal bremsstrahlung and (b) IC components. The line formats are the same as in Figure 1. The horizontal solid, dashed, and dotted lines indicate the 3.5σ sensitivity of FORCE at 1 kpc with exposure times of 104, 105, and 106 s, respectively. (c) Same as panels (a) and (b), but for the synchrotron component from model A2 in the black solid line.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Same as Figure 10, but for the models in Group B. The line formats are the same as in Figure 6.
Paper: Long-term Evolution of Nonthermal Emission from Type Ia and Core-collapse Supernova Remnants in a Diversified Circumstellar Medium
Authors: Ryosuke Kobashi, Haruo Yasuda, Shiu-Hang Lee
Figure caption: Same as Figure 7, but zoomed into the energy range of 1–80 keV. In the top panel, the total SED of Model A2 is overlaid as a black solid line. The red shaded area indicates the 10–40 keV range, in which future observations by FORCE are optimal.
Paper: Galaxy Alignments with Surrounding Structure in the Sloan Digital Sky Survey
Authors: Dhvanil D. Desai, Barbara S. Ryden
Figure caption: Color–magnitude diagram (u − r vs. M  r ) for the target galaxies. The four subsamples (luminous blue, luminous red, faint blue, and faint red) are labeled. Solid green line is the color divider of James & Ryden (2022).
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: (a) Exposure-corrected, background-subtracted, Gaussian-smoothed image of Abell 4059 in the 0.5–7.0 keV energy band. The sectors used to extract the ICM spectra (green) and the masked regions (blue) are overlaid. (b) Exposure-corrected, background-subtracted, Gaussian-smoothed image of JO194 in the 0.5–7.0 keV energy band with on top the regions used for the spectral extraction based on the contours of the Hα emission and the stellar disk. The three blue sources are background galaxies, according to their MUSE optical spectra. Therefore, we exclude them from the analysis.
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: Multiwavelength view of JO194 in a 1.″5 × 1.′7 region centered on the galaxy. (a) MUSE white-light image (4650–9300 Å) with, on top, the contours of the stellar disk (yellow) and Hα emission (light blue), (b) residual X-ray image of JO194 in the 0.5–7.0 keV band (see Section 2.2) with, on top, the contours of the stellar disk (yellow) Hα (red) and positive residuals (white). (c) Exposure-corrected, background-subtracted image in the 2.0–7.0 keV band, smoothed with a 3σ pixel Gaussian. For reference, we show the stellar disk (blue) and the lowest contour of the Hα emission (white).
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: Exposure-corrected, background-subtracted image of Abell 4059 in the energy band 0.5–7.0 keV smoothed with a 3σ Gaussian.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: (Left) Cold dust temperature (T c) as a function of IR luminosity surface density (﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩). (Right) Warm dust temperature (T w) as a function of ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩. The AGN- and SF-dominated galaxies are shown in blue and red points, respectively.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Correlations between ﹩{L}_{\mathrm{HCN}}^{{\prime} }﹩ and luminosities of different IR bands. Top left: total IR luminosity. Top right: far-IR luminosity. Bottom left: near-/mid-IR luminosity. Bottom right: warm component IR luminosity. The adopted wavelength ranges and dust components are labeled at the top of each panel.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: The masses and rotation periods for stars in our wide binary sample. The four triangles denote M dwarfs with a white-dwarf companion from Table 3, the nine diamonds denote M dwarfs with an FGK primary from Table 4, and the 25 pairs of circles denote M–M binaries from Table 2. For suspected unresolved binaries, the circle denotes the upper limit of the mass of the rotating component, with a dashed arrow indicating this point may be moved leftwards. When the masses of two components are known but it is unclear which is responsible for the observed rotation, the second option is denoted with an open circle, joined to the first with a dashed line. M–M pairs are colored based on their rotation rate: systems where both components are rapidly rotating (P rot < 2  days) are shown in shades of blue; systems where one component is rapidly rotating and the other has begun spindown are red; systems where both stars are slowly rotating are green. For the WD-M and FGK-M pairs, symbols are colored based on age: young (<1 Gyr) systems are black, intermediate (1–3 Gyr) are gray, and those known to be old (>5 Gyr) are white. Small, semitransparent black crosses denote the single field M-dwarf sample from Newton et al. (2017), with updated masses using Gaia parallaxes. Rectangles show the binned Praesepe data from the right panel of Figure 5, with the dotted line showing the 90th percentile of Praesepe stars. The offset between the slowly rotating sequence for early M dwarfs in Praesepe and the Newton et al. (2017) field sample is possibly surprising. If these stars stall at Praesepe-like periods for ages up to 2.7 Gyr (Curtis et al. 2020), one might expect to observe a substantial number of field stars at these periods.
Paper: Constraints on the Spindown of Fully Convective M Dwarfs Using Wide Field Binaries
Authors: Emily K. Pass, David Charbonneau, Jonathan M. Irwin, Jennifer G. Winters
Figure caption: Masses and rotation periods for presumed single M dwarfs in the 600 Myr Praesepe cluster, one of the oldest clusters with measured photometric rotation periods for a large number of M dwarfs. Rotation periods are taken from Douglas et al. (2019). In the left panel, masses are also taken from that work, while in the right panel, masses are estimated using the Benedict et al. (2016) K-band relation. Based on Praesepe eclipsing binaries, we argue that the masses in the right figure are correct (Figure 4). We use various shades of red such that individual points can be more easily distinguished; the same star is the same shade in both panels. Black rectangles denote median properties of bins containing equal numbers of stars, with error bars noting the interquartile range of masses and rotation periods in that bin. A dotted black line marks the 90th percentile of rotation periods in each bin; for stars with masses >0.35 M ⊙, the most slowly rotating stars appear to converge onto a slowly rotating sequence. The open circles in the right panel show the small number of early M dwarfs in studies of older clusters from the literature, with masses again calculated using the Benedict et al. (2016) K-band relation: yellow denotes the 1.0 Gyr cluster NGC 6811 (Curtis et al. 2019); green denotes the 1.4 Gyr cluster NGC 752 (Agüeros et al. 2018); and blue denotes the 2.7 Gyr cluster Ruprecht 147 (Curtis et al. 2020). Those authors interpret the small differences between the rotation periods in Praesepe and in these older clusters as evidence of stalling in K dwarfs and early M dwarfs. We note that the 1.0 Gyr points fall below the slowly rotating Praesepe sequence; this may suggest that properties other than age (e.g., metallicity) influence the slowly rotating sequence for a cluster.