adsabs/AstroCLIMB huggingface dataset:
Paper: Obliquity Constraints for the Extremely Eccentric Sub-Saturn Kepler-1656 b
Authors: Ryan A. Rubenzahl, Andrew W. Howard, Samuel Halverson, Cristobal Petrovich, Isabel Angelo, Guđmundur Stefánsson, Fei Dai, Aaron Householder, Benjamin Fulton, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Daniel Huber, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Eccentricity–semimajor axis diagram for transiting exoplanets. Giant planets, defined as >100 M ⊕ or >8 R ⊕ if there is no mass measurement, are plotted as faded points. Following Dong et al. (2021), the y-axis is scaled uniformly in e 2, and the high-eccentricity migration track is shaded in light gray. The dashed gray line traces a = 0.05/(1 − e 2), corresponding to the minimum semimajor axis to excite f-mode oscillations and produce rapid orbital decay (Wu 2018). Planets above this line would therefore be extremely rare. The black dashed upper boundary (0.034/(1 − e 2)) represents the line of constant angular momentum where a 1 M J, 1.3 R J exoplanet would become tidally disrupted at its closest approach to a solar mass star (Dong et al. 2021); no giant planets can persist above this boundary. The lower boundary (0.1/(1 − e 2) corresponds to a final semimajor axis of 0.1 au, beyond which circularization timescales become much longer than typical system ages. The boundaries are not exact as they depend on the strength and efficiency of tides in the system. Exoplanets with e > 0.6 are labeled; Kepler-1656 b is the only sub-Saturn firmly in the HEM track. Data are from the NASA Exoplanet Archive, accessed on 2024 April 1 (NASA Exoplanet Archive 2019).
Paper: Obliquity Constraints for the Extremely Eccentric Sub-Saturn Kepler-1656 b
Authors: Ryan A. Rubenzahl, Andrew W. Howard, Samuel Halverson, Cristobal Petrovich, Isabel Angelo, Guđmundur Stefánsson, Fei Dai, Aaron Householder, Benjamin Fulton, Steven R. Gibson, Arpita Roy, Abby P. Shaum, Howard Isaacson, Max Brodheim, William Deich, Grant M. Hill, Bradford Holden, Daniel Huber, Russ R. Laher, Kyle Lanclos, Joel N. Payne, Erik A. Petigura, Christian Schwab, Josh Walawender, Sharon X. Wang, Lauren M. Weiss, Joshua N. Winn, Jason T. Wright
Figure caption: Left: the KPF RV time series, in black, during the transit of Kepler-1656 b. The blue curve shows the median RV from the posterior distribution of the full model, with the shaded band denoting the 16th–84th percentiles. The red curve shows the same for the aligned model where λ is fixed to 0°. The bottom panel shows the residuals to the median full model. Right: the posterior distribution for λ and ﹩v\sin {i}_{\star }﹩ for the full model. Misaligned λ requires ﹩v\sin {i}_{\star }\gt 3﹩ km s−1.
Paper: TOI-1685 b Is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target
Authors: Jennifer A. Burt, Matthew J. Hooton, Eric E. Mamajek, Oscar Barragán, Sarah C. Millholland, Tyler R. Fairnington, Chloe Fisher, Samuel P. Halverson, Chelsea X. Huang, Madison Brady, Andreas Seifahrt, Eric Gaidos, Rafael Luque, David Kasper, Jacob L. Bean
Figure caption: Ternary plot depicting different fractional combinations of water, rock, and iron for solid planet compositions. The solid and dashed black lines mark the possible position of TOI-1685 b and the 68% credible intervals. The red dot depicts the model planet at an estimated internal pressure of P 0 = 600 GPa, which results in relative mass fractions of 94.2% MgSiO3, 3.3% Fe, and 2.5% H2O.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Top: energy dissipation rate and accretion luminosity evolution (from ﹩\dot{M}﹩; see right axis) compared to the Eddington luminosity and a t −5/3 slope. Bottom: estimated photon diffusion timescale along different lines of sight (see legend). Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Eddington Envelopes: The Fate of Stars on Parabolic Orbits Tidally Disrupted by Supermassive Black Holes
Authors: Daniel J. Price, David Liptai, Ilya Mandel, Joanna Shepherd, Giuseppe Lodato, Yuri Levin
Figure caption: Optical luminosity (top), blackbody radius (middle), and temperature (bottom) evolution from our simulation using β = 1 (left) and β = 5 (right), measured along different lines of sight (see legend). Markers represent the fits to various observed TDEs taken from van Velzen et al. (2021) plus ASASSN-18jd (Neustadt et al. 2020). Transparency at t ≲ 30 days indicates when the photosphere is unresolved. Data and scripts used to create the figure are available on Zenodo: doi:10.5281/zenodo.11438154.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Left panel: continuum emission imaged with ALMA at 341 GHz toward MWC 349A (black contours). The continuum emission modeled at 341 GHz with the MORELI code is shown in red contours. Contour levels are [−3, 10, 20, 30, 50, 100, 200, 300, 500, 700, 900] times the 1σ rms noise level of the observations, 0.14 mJy beam−1. The synthesized beam of size 0.″025 × 0.″012 is represented with the ellipse at the bottom left corner. Top right panel: observed (black) and modeled (red) integrated spectral profile of the H26α line emission toward MWC 349A. Bottom right panel: zoom-in into the lower intensity levels of the H26α spectral profile. The arrow indicates additional line emission, which is discussed in Section 3.3.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Sketch—not to scale—of the geometry of the model for the ionized region of MWC 349A. All angles are described in Section A.1, and the values are listed in Table 1. The outer cone of semiopening θ  a  encloses the disk of thickness θ  d  and the ionized wind (gray shaded cone) and the jet (red and blue shaded cone). The rotation axis is inclined an angle θ  i  with respect to the plane of the sky. The northern jet is tilted at an angle θ jet,north with respect to the rotation axis, while the southern jet is tilted at an angle θ jet,south. Blue and red colors represent blueshifed and redshifted radial velocities of the jet, respectively, as seen by the observer. Note that the jet in the model has the same size as the wind, and its shape is exaggerated in the sketch for clarity.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Integrated-intensity (moment-zero) maps of the H26α emission in bins of 13.09 km s−1 for the blueshifted portion of the spectrum. Grayscale and black contours represent the observed H26α emission; blue contours represent the emission modeled with MORELI. Contour levels are [−3, 5, 7, 10, 20, 30, 50, 100, 200, 300, 500, 700] times the 1σ rms noise level of each map shown in the bottom right corner of each panel. Central velocities of each panel are indicated in their upper right corner. The synthesized beam is shown with an ellipse at the bottom left corner. The central radial velocity of the source is 8.72 km s−1.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Same as Figure 2 but for the redshifted portion of the spectrum of H26α. The modeled images are shown with red contours. Note that the top left panel is centered at the systemic velocity of the source, 8.72 km s−1.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Left: continuum emission from the line-free channels of the line spectral window in thin contours. Levels are [10, 20, 30, 50, 100, 200, 300, 500, 700, 900] times the 1σ rms of the map, 0.18 mJy beam−1. In thick contours, the integrated-intensity (moment-zero) map of the line emission is between 353.74 and 353.90 GHz, with the contribution from H26α removed. Contour levels are [−3, 3, 5, 7, 10, 20] times the 1σ rms of the map, 6.5 mJy beam−1 km s−1. Top right: integrated spectral profile of MWC 349A showing faint emission in three peaks, (1), (2), and (3). The peaks are partially blended with the blueshifted wing of H26α. Red dashed vertical lines represent the frequencies of He26α and C26α at the radial velocity of MWC 349A, 8.72 km s−1. The line-of-sight velocity in the top axis is obtained with respect to the rest frequency of the H26α line. Bottom right: in gray scale, channel maps at the frequencies of peaks (1), (2), and (3). Contours are the thick contours from the left panel.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Integrated-intensity (moment-zero) maps of the H26α emission from −50.19 to −37.09 km s−1 (top panels) and from 67.62 to 80.72 km s−1 (bottom panels). Grayscale, contour colors, and levels and text insets are the same as in Figures 2 and 3. Each column shows the model result for different inclinations of the disk θ  i  with respect to the plane of the sky, where positive values of θ  i  correspond to the northern cone expanding away from the observer.
Paper: Imaging the Jet of MWC 349A with Resolved Radio Recombination Line Emission from ALMA
Authors: Antonio Martínez-Henares, Qizhou Zhang, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Nuria Huélamo, Sirina Prasad, James Moran, Alejandro Báez-Rubio
Figure caption: Opening angle of the integrated-intensity maps from Figures 2 and 3 for modeled and observed maps, separated by velocity range and by northern and southern lobe emission. The error bars in the velocity axis represent the width of the integrated-intensity maps, 13.09 km s−1.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Left: confidence contours (2σ) of PD and PA obtained in epoch IX1 are shown with different colors for different energy bands. Middle: variations of PD and PA with energy for epoch IX1 (MJDstart 60145.63) and IX2 (MJDstart 60165.99). Histograms denote MDP99%, and confidence levels (%) for PD variations with energy are mentioned in the legend. Right: correlation of PD (model-independent) with luminosity and flux ratio (F BB/F PL) from spectropolarimetric modeling of IXPE data. PD variations are significant at 74% and 73% in the respective energy bands.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Normalized stokes parameters (Q/I and U/I) obtained with PCUBE analyses for (a) different epochs (2–8 keV), (b) energy bands (epoch IX1), and (c) phase bins (epoch IX1 in 2–8 keV). The radii of colored circles represent 1σ uncertainty values corresponding to 2 degrees of freedom. See the main text for details.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Panel (a): pulse profile of Swift J0243.6+6124 obtained from NuSTAR in different energy bands are depicted with different colors. Panel (b): variation of PD and pulse profile with the pulse phase (2–8 keV) for epoch IX1. Histograms denote MDP99%. Panel(c): variation of PA with pulse phase for epoch IX1. Note that the variations of PD and PA over different phase bins are marginal. See the main text for details.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Left: corner plot shows the covariance between best-fitted A index and A norm parameters of the polpow model in the 2–8 keV energy band, obtained using the MCMC method. The contours represent the 1σ, 2σ, and 3σ confidence ranges, respectively. Right: best-fitted I, Q, and U Stokes spectra of IXPE combining all DUs in the 2–8 keV energy range (top panel) and corresponding residual variation (bottom panel). See the main text for details.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Panel (a): 1 day binned MAXI/GSC (orange) and Swift/BAT (red) light curves of Swift J0243.6+6124 since its discovery (2017 October) in the 2–20 keV and 15–50 keV energy bands. Panels (b) and (c): zoomed view of the 2023 outburst observed with Swift/BAT (magenta) and MAXI/GSC (green). Epochs of NICER and NuSTAR observations are marked with vertical lines. The gray patch indicates the duration of IXPE observations, and blue circles denote the corresponding IXPE count rates of 1000 s bin combining all three DUs (2–8 keV).
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Phase-resolved polarimetric analysis of Swift J0243.6+6124 during epoch IX1 in the 3–8 keV energy range over 24 phase bins. In panels (a)–(e), variations of normalized intensity, normalized Stokes parameters (Q/I and U/I), PD, and PA with pulse phase are shown. In panel (d), the histograms denote the MDP99% level. In panel (e), the gray shaded area represents 90% confidence intervals. See the main text for details.
Paper: First Detection of X-Ray Polarization in Galactic Ultraluminous X-Ray Pulsar Swift J0243.6+6124 with IXPE
Authors: Seshadri Majumder, Rwitika Chatterjee, Kiran M. Jayasurya, Santabrata Das, Anuj Nandi
Figure caption: Best-fitted broadband energy spectra of Swift J0243.6+6124 in the 0.6–70 keV energy band from quasi-simultaneous NICER and NuSTAR observations (NI0 and NU0) and NICER spectra (0.6–11 keV) during epoch NI1, NI2, and NI3, respectively. See the main text for details.
Paper: PO and PN in the Envelope of VY Canis Majoris: Elucidating the Chemistry and Origin of Phosphorus
Authors: R. Ravi, A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Combined moment 8 ALMA and SMT images of J = 5.5 → 4.5 e transition of PO (left, a), J = 5 → 4 transition of PN (left, b), J = 5.5 → 4.5 e transition of NS (right, c), J = 5 → 4 transition of SiO (right, d). Synthesized beam sizes are shown at the lower left, crosses indicate the stellar position. Flux scale (Jy beam−1) is indicated in the figure. The axes are in arcseconds relative to the (0, 0) position corresponding to α = 07h22m58.ˢ33, δ = −25°46′03.″2 (J2000.0 ICRS). PN is clearly more extended than PO, with a close correspondence to NS and partly to SiO.
Paper: PO and PN in the Envelope of VY Canis Majoris: Elucidating the Chemistry and Origin of Phosphorus
Authors: R. Ravi, A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Emission contours of PN superimposed over (a) the image of NS from Figure 1 (in black) and (b) the HST F656N (6563.7 Å) image (in red) from Humphreys et al. (2021). The axes are defined as in Figure 1. The SW Fan, Cloudlets I–IV, and certain HST dust features are indicated. PN emission coincides with NS and some of the dust clumps, including South Knots B, E1 and E2, and SW Knots A and G (see Table 1). Spectra of PN ( black) and NS (red) for the SW Fan and the cloudlets are shown in (c), plotted on the same velocity scale.
Paper: PO and PN in the Envelope of VY Canis Majoris: Elucidating the Chemistry and Origin of Phosphorus
Authors: R. Ravi, A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Spectra arising from the spherical flow of the J = 5 → 4 transition of PN (upper) and the J = 5.5 → 4.5 e (in red), f (in black) transition of PO (lower). The presence of phosphorus hyperfine structure broadens the PO line profile relative to that of PN.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: Mass–radius posterior distributions using the N3LO χEFT band up to 1.5n 0 for the three new NICER scenarios (green shaded regions), in comparison to the “Baseline” scenario (red contours), using the PP model (left panels) and the CS model (right panels). The results using the N3LO χEFT band up to 1.1n 0 are qualitatively very similar.
Paper: Erratum: “The NANOGrav 15 yr Data Set: Search for Signals from New Physics” (2023, ApJL 951 L11)
Authors: Adeela Afzal, Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Paul T. Baker, Bence Bécsy, Jose Juan Blanco-Pillado, Laura Blecha, Kimberly K. Boddy, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Curt J. Cutler, Megan E. DeCesar, Dallas DeGan, Paul B. Demorest, Heling Deng, Timothy Dolch, Brendan Drachler, Richard von Eckardstein, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Lydia Guertin, Kayhan Gültekin, Jeffrey S. Hazboun, Sophie Hourihane, Kristina Islo, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, Andrew R. Kaiser, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Nima Laal, Michael T. Lam, William G. Lamb, T. Joseph W. Lazio, Vincent S. H. Lee, Natalia Lewandowska, Rafael R. Lino dos Santos, Tyson B. Littenberg, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Jonathan Nay, Priyamvada Natarajan, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Polina Petrov, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Tobias Schröder, Levi Schult, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Peter Stratmann, Jerry P. Sun, Abhimanyu Susobhanan, Joseph K. Swiggum, Jacob Taylor, Stephen R. Taylor, Tanner Trickle, Jacob E. Turner, Caner Unal, Michele Vallisneri, Sonali Verma, Sarah J. Vigeland, Haley M. Wahl, Qiaohong Wang, Caitlin A. Witt, David Wright, Olivia Young, Kathryn M. Zurek
Figure caption: Updated contour plots for the PT-BUBBLE and PT-SOUND models, superseding Figure 8 in Afzal et al. (2023).
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: The same as Figure 10, but also including results for the χEFT bands at N2LO.
Paper: Constraining the Dense Matter Equation of State with New NICER Mass–Radius Measurements and New Chiral Effective Field Theory Inputs
Authors: Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L. Watts, Kai Hebeler, Jonas Keller, Chanda Prescod-Weinstein, Devarshi Choudhury, Geert Raaijmakers, Tuomo Salmi, Patrick Timmerman, Serena Vinciguerra, Sebastien Guillot, James M. Lattimer
Figure caption: The same as Figure 8, but for N2LO.
Paper: Extensive Intrusive Magmatism in the Lunar Farside Apollo and South Pole–Aitken Basins, Chang’e-6 Landing Site
Authors: Yuqi Qian, James Head, Joseph Michalski, Shengxia Gong, Wei Yang, Zilong Wang, Long Xiao, Xianhua Li, Guochun Zhao
Figure caption: Thorium abundance of the Apollo-Oppenheimer region. The thick white line represents the boundary of Mg-rich materials. The base map is Lunar Prospector thorium abundance data (Prettyman et al. 2006).
Paper: Study of a Red Clump Giant, KIC 11087027, with High Rotation and Strong Infrared Excess—Evidence of Tidal Interaction for High Lithium Abundance
Authors: Raghubar Singh, Anohita Mallick, Bacham E. Reddy, Jeewan C. Pandey, Gang Zhao
Figure caption: Kepler light-curve analysis of KIC11087027: (a) Black is a raw, and red is a median smoothed light curve. (b) Comparison of the power spectral density of KIC11087027 (black) with a similar mass star KIC12645107 (red) with no activity. (c) Seventh-quarter Kepler LC of KIC11087027, and three flares are marked. (d) The detrended light curve in the flare region and fitted flare model. Measured flare parameters are given in the figure. (e) The Lomb–Scargle periodogram of the entire 18-quarter light curve. The vertical red dashed line is measured period. (f) The rotation period measured in different quarters (Q2–Q16) gives different values.
Paper: On the Association of GW190425 with Its Potential Electromagnetic Counterpart FRB 20190425A
Authors: Ignacio Magaña Hernandez, Virginia d'Emilio, Soichiro Morisaki, Mohit Bhardwaj, Antonella Palmese
Figure caption: Posterior probability of the luminosity distance from GWTC-3 samples marginalized along the FRB line-of-sight (LOS; black line). The top panel shows low-spin results; the bottom panel shows high-spin results. The marginal posterior distribution is computed using localization FITS files (dotted line), a Clustered KDE (dashed line), and a GP density estimator (solid line). The shaded band shows the GP’s 2σ uncertainty. The LOS PE samples obtained in this work are also shown here for comparison (as histograms).
Paper: Study of a Red Clump Giant, KIC 11087027, with High Rotation and Strong Infrared Excess—Evidence of Tidal Interaction for High Lithium Abundance
Authors: Raghubar Singh, Anohita Mallick, Bacham E. Reddy, Jeewan C. Pandey, Gang Zhao
Figure caption: (a) H α  emission in KIC11087027. Three spectra are taken at different times and resolutions: LAMOST LRS (R = 1800), MRS, and HESP (R = 7500, 60,000). At higher resolution, the two H α  emission peaks become visible. (b) SED fitting to observed fluxes.