adsabs/AstroCLIMB huggingface dataset:
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: The final planetary configurations obtained from the numerical simulations.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: The timescales of tidal damping and the secular evolution. The light gray region represents the orbital period range p ∈ [0.365, 1] day, while the dark gray region corresponds to p ∈ [1, 2] day.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: A schematic figure illustrates the main formation process of the WASP-47 system. Panel (a) shows the orbital migration process, where the innermost planet halts near the inner edge of the gas disk. Panel (b) depicts the eccentricity excitation due to MMRs trapping and giant planet perturbation. Panel (c) displays the eccentricity damping caused by the tidal effects and the semimajor axis of the innermost planet decreases gradually, ultimately forming a USP planet. The right panel presents the orbital configurations of the planetary systems at different formation stages.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: The distribution of orbital period ratios between adjacent planets in the system from group 1. Panel (a) shows the period ratio between W1 and W2 as it changes with the orbital period of W1. Panel (b) displays the period ratio between W2 and W3 as it changes with the orbital period of W2. Panels (c) and (d) present the number distribution of the period ratios. A zoomed-in view of the period ratio distribution between 2.0 and 4.0 is provided in panel (c). Black and gray dots represent systems in which a USP planet and an SPSE planet are formed, respectively.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: The orbital evolution of a typical run that forms a planetary configuration closely resembling the observed WASP-47 system. Panels (a) and (b) show the evolution of the orbital periods and eccentricities. The red, green, and blue lines and dots represent the evolution of W1, W2 and W3, respectively. Panel (c) illustrates the evolution of the period ratios between adjacent planets. Panels (d1) and (d2) show the evolution of the resonant angles between neighboring planets, where θ21 = 2λ2 − λ1 − ϖ1 and θ32 = 2λ3 − λ2 − ϖ2.
Paper: Formation of Ultra-short-period Planets in Hot Jupiter Systems: Application to WASP-47
Authors: Su Wang, Mengrui Pan, Yao Dong, Gang Zhao, Jianghui Ji
Figure caption: Confirmed planetary systems that have one giant planet accompanied by nearby low-mass planetary companions.
Paper: The Large-scale Structure Supplies the Formation of Gas-star Misaligned Galaxies
Authors: Min Bao, Yanmei Chen, Qiusheng Gu, Huiyuan Wang, Yong Shi, Peng Wang
Figure caption: The distributions of ﹩| \cos \theta | ﹩, where θ is the angle between gas (or stellar) spins and ﹩{{\boldsymbol{e}}}_{{\bf{3}}}﹩ of the LSS. (a) The PDFs of ﹩| \cos \theta | ﹩ for MaNGA galaxies. (b) The PDFs of ﹩| \cos \theta | ﹩ for aligned controls. (c) The PDFs of ﹩| \cos \theta | ﹩ for misaligned galaxies. In panels (a), (b), and (c), the green circles show the PDFs of ﹩| \cos \theta | ﹩ between gas spins and ﹩{{\boldsymbol{e}}}_{{\bf{3}}}﹩, and the orange circles show the PDFs of ﹩| \cos \theta | ﹩ between stellar spins and ﹩{{\boldsymbol{e}}}_{{\bf{3}}}﹩. The green and orange bars on the top mark the corresponding median values. The gray-, blue-, and pink-shaded areas show the ±1σ, ±2σ, and ​​​​​​±3σ scatters for the corresponding mock samples.
Paper: The Large-scale Structure Supplies the Formation of Gas-star Misaligned Galaxies
Authors: Min Bao, Yanmei Chen, Qiusheng Gu, Huiyuan Wang, Yong Shi, Peng Wang
Figure caption: The distances of galaxies to their nearest filament spines in the filament environments. (a) An illustration of the reconstructed filaments with decl. ∼[25∘, 30∘]. The gray points show the distributions of SDSS galaxies. The black profiles represent the projected filament spines. (b) The black solid profile shows the Dfilament–M⋆ correlation for MaNGA galaxies. Each black circle shows the median distance in a certain stellar mass bin. The gray-shaded area shows the 40%–60% scattering region. The red square and triangle show the median Dfilament for low-mass and high-mass misaligned galaxies, while the blue square and triangle show the median Dfilament for low-mass and high-mass aligned controls, respectively.
Paper: The Large-scale Structure Supplies the Formation of Gas-star Misaligned Galaxies
Authors: Min Bao, Yanmei Chen, Qiusheng Gu, Huiyuan Wang, Yong Shi, Peng Wang
Figure caption: The large-scale environments of misaligned galaxies and their aligned controls. (a) The red histogram displays the distributions of Dfilament for misaligned galaxies. The blue histogram displays the distributions of Dfilament for aligned controls. The red and blue bars on the top show the corresponding median distances. (b) The red histograms display the distributions of environments for misaligned galaxies. The blue histograms display the distributions of environments for aligned controls.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: A visual representation of the OP calculation done for the individual years of X-ray observations (given in the upper left of each panel) and the H2CO observations divided into the same velocity ranges shown in Figure 2 (given in the upper right of each panel). The blue-filled shapes are the X-ray contours at a level of 3 × 10−9 counts s−1 cm−2 pixel−1 shown as the outer contours in previous figures, and they trace even the diffuse X-ray emission from the cloud. The pink-filled shapes are the 3σ H2CO contours. The purple regions show where the two sets of contours overlap. The OPs with X-ray being the primary data set are shown in blue in the lower left of each panel, and the percentages with H2CO being the primary data set are shown in pink in the lower right of each panel.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: A comparison between each year of X-ray data and NH3 integrated images made using an equal number of consecutive velocity slices contained within the full velocity range of the Sticks cloud. Each panel shown has the average velocity indicated at the bottom of the image. The contours for each X-ray year were matched with an integrated NH3 image sequentially. We see relatively good agreement between the X-ray and molecular gas features, especially in the bottom three panels. The contour colors and widths are the same as shown in Figure 2. This analysis is the same as that shown in Figure 2 using NH3 instead of H2CO.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: This is the same type of comparison as shown in Figure A1; however, the blue-filled shapes are the X-ray contours at a level of 7 × 10−9 counts s−1 cm−2 pixel−1 also shown in previous figures as the interior contours, and they trace the densest parts of the cloud. The OPs with X-ray being the primary data set are shown in blue in the lower left of each panel, and the percentages with H2CO being the primary data set are shown in pink in the lower right of each panel. These percentages for the dense cores of the cloud are, on average, 27% higher than the percentages shown in Figure A1, which makes sense as H2CO is a dense gas tracer.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: A comparison between each year of X-ray data and SiO integrated images made using an equal number of consecutive velocity slices contained within the full velocity range of the Sticks cloud. Each panel shown has the average velocity indicated at the bottom of the image. The contours for each X-ray year were matched with an integrated SiO image sequentially. We see relatively good agreement between the X-ray and molecular gas features, especially in the bottom three panels. The contour colors and widths are the same as shown in Figure 2. This analysis is the same as that shown in Figures 2 and A3 but using SiO.
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Top: r-band apparent magnitude (from Las Cumbres Observatory) and R-band polarization with respect to days since the explosion. The light dashed gray line is the maximum ISP in the R band as discussed in Section 3. The triangle data points are from MOPTOP observations, and the square symbols are continuum polarization calculated from our SPOL data in the 6000–7000 Å range. Circle and star points represent data from A. Singh et al. (2024) and S. S. Vasylyev et al. (2023), respectively. Polarization detections during the initial rising phase and fall from the plateau suggest asphericity in the CSM and He core, respectively. Bottom: PA with respect to phase for R-band data. In both panels, the dashed blue lines represent epochs that are presented in the Figure 3 sketch.
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Evolution of R-band Stokes q and u with phase for SN 2023ixf after ISP correction (Section 3.1). The points include data from MOPTOP and SPOL, and data from S. S. Vasylyev et al. (2024) and A. Singh et al. (2024). For the SPOL data we calculated the continuum polarization in the 6000–7000 Å range (Section 2.2).
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: Contour plots of the solar wind speed (vsw) as a function of normalized cross helicity (∣σc∣) and helium abundance (AHe). Panel (a) uses the mean vsw. Panels (b) and (c) use the 10% and 90% quantile of vsw, respectively. The color scale in panels (b) and (c) is larger than the range in panel (a). Contours for mean vsw = 355, 399, 407, 439, 450, and 484 km s−1 are drawn on all three panels. The color of the contours depend on the panels and are chosen for contrast. The first two are vslow and the upper bound on it. The middle two are the slowest and fastest vs. The latter two are the speed at which Gaussians fit to the slow and fast wind peaks during solar minima intersect and the lower bound on this intersection value. The area between the vslow, vs, and vi contour pairs are labeled with the corresponding vX text. All contours are smoothed with a 1σ filter for visual clarity.
Paper: Cross Helicity and the Helium Abundance as an In Situ Metric of Solar Wind Acceleration
Authors: B. L. Alterman, Raffaella D'Amicis
Figure caption: A suggestive cartoon derived from Figure 10(a). Contours indicating suggested regions of the (∣σc∣, AHe) plane. Black contours are drawn at vsw = 425 and 460 km s−1. The bottom region indicates solar wind likely from closed field source regions. The right side of the plane is solar wind likely from Open field source regions. The middle of the plane is solar wind that, when measured at 1 au, is from a mixture of sources. A forthcoming publication demonstrates that high speed solar wind in the top left corner of the plane is from transients. The gray region indicates the full range of saturation speeds vs. The arrow in the middle region suggests that the Mixed source region is more likely to contain solar wind from an Open field region roughly along the direction of the arrow. The region for vs is grayed out to indicate that the exact vsw at which this transition happens likely depends on the solar wind sample under consideration.
Paper: Andromeda XXXV: The Faintest Dwarf Satellite of the Andromeda Galaxy
Authors: Jose Marco Arias, Eric F. Bell, Katya Gozman, In Sung Jang, Saxon Stockton, Oleg Y. Gnedin, Richard D'Souza, Antonela Monachesi, Jeremy Bailin, David Nidever, Roelof S. de Jong
Figure caption: Left: surface density map of candidate red giant branch stars with iron abundances between −2.5 ≲ [Fe/H] ≲ −2 at the distance of M31. This density map was created using point sources selected from the PAndAS “Combined stellar catalog” (A. W. McConnachie et al. 2018). The extent of the PAndAS footprint is represented by the thick black solid line. The coordinates on the tangent plane projection are (ξ, η) centered on M31. The image has been smoothed using a top-hat filter with adaptive widths that depend on the local density in ﹩1\mathop{.}\limits^{{\rm{^{\prime} }}}2\times 1\mathop{.}\limits^{{\rm{^{\prime} }}}2﹩ grid cells. Contaminants have been removed from this map by subtracting a supplementary map constructed from objects with colors and magnitudes indicative of foreground and background contamination sources. The dwarf galaxies within the PAndAS footprint are highlighted by red circles, with And XXXV distinguished by a thicker outline and bold red font. The dashed circles correspond to projected radii of 150 kpc from M31, and 50 kpc from Triangulum (M33). All major stellar substructures in the halo of M31 are visible. For reference, the names of these stellar substructures are provided in Figure 12 of A. W. McConnachie et al. (2018). Upper right: PAndAS CFHT/MegaCam g-band discovery mosaic of And XXXV. Lower right: HST/WFC3 F606W follow-up image of And XXXV. Red circles mark sources within And XXXV’s best-fit ellipse that meet our photometric quality metrics for point sources. Both images are 80″ × 80″.
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: The accretion rate from the SN fallback simulations presented in Figure 1 (solid lines) and the long-term accretion based on a power-law decay extrapolation (dashed lines): ﹩\dot{M}\propto {t}^{-\beta }﹩, with β ≈ 1. The gray vertical line shows the time of merger expected from the newly assembled BH binary, while the horizontal blue and green lines show the lower limit for hypercritical neutrino-cooled accretion (R. A. Chevalier 1993) and the photon Eddington accretion limit, respectively. The right-hand y-axis shows the accretion luminosity ﹩L=\epsilon \dot{M}{c}^{2}﹩ with ϵ = 0.1. The gray shaded region represents the peak luminosity range of the kilonova associated with GW170817 and short γ-ray bursts (C. D. Kilpatrick et al. 2017; S. Ascenzi et al. 2019).
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: Diagram illustrating the evolution of a relic accretion disk in a merging BH binary. Disk formation is assumed to result from the formation of the second BH in the binary in a fallback SN. The simulation results presented in Figure 2 are used to inform the conditions of the gas in and around the binary (panel (a)). At this stage, tmerger(a = a0) = 3.16 Myr. Here we focus on the evolution of the more massive disk, which is found to be around the companion. The evolution of the disk is expected to be altered when the binary has reached a separation at which tidal forces on the disk will impact angular momentum transport (panel (b)). This takes place as the binary shrinks via gravitational-wave emission and a = aτ ≈ 2.24 R⊙. At this separation, the accretion disk, whose initial circularization radius Rdisk ≈ 0.56 R⊙, will be effectively truncated owing to the tidal force from the M2 BH. At this point, tmerger(a = aτ) = 0.75 Myr. By the time the merger takes place, we expect the orbiting BHs to merge in a gas-free environment (panel (c)). However, if a relic disk is able to endure, the binary will evolve until acrit ≪ aτ. At this final stage, the viscous accretion time around the BH is expected to be similar to the gravitational-wave inspiral time, tmerger(a = acrit) ≈ 15.5 hr, potentially resulting in an electromagnetic flaring signature (Section 2.1).
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: Spiral shocks in binary BHs. Top panel: gas density snapshots in the orbital plane at t = 200 for Am3 (left) and Am5 (right). The inset panel in Am3 shows the gas surface density of Am3_nc at the same time, where we set the companion BH’s gravity GM2 = 0.0. Bottom panel: gas surface density snapshots of Am3 (left) and Am5 (right) plotted in the ﹩\mathrm{log}R-\phi ﹩ coordinate system to illustrate the pitch angle of the spiral shocks. We sample the Mach number, ﹩{ \mathcal M }﹩, and rotation speed, Ω(r), locally at the points marked by the red crosses. The white line segments are pitch angles fitted with linear wave theory as in Equation (A4). The white dashed lines in the top panels show the spiral patterns fit using the average Mach number and rotation speed from the red crosses in the bottom panels.
Paper: XRISM Reveals Low Nonthermal Pressure in the Core of the Hot, Relaxed Galaxy Cluster A2029
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Tommaso Bartalesi, Stefano Ettori, Roman Kosarzycki, Lorenzo Lovisari, Tom Rose, Arnab Sarkar, Ming Sun, Prathamesh Tamhane
Figure caption: (Left) Chandra image of A2029 overlaid with the 1.4 GHz Very Large Array radio contours and the Resolve field of view. (Top right) Resolve counts image from the two observations combined. Locations of individual photons are randomized within each pixel in the pipeline processing. (Bottom right) Residuals after subtracting a 2D model from the Chandra image, clearly showing the sloshing spiral that extends throughout most of the Resolve field. The Chandra data used were taken in 2004.
Paper: Disk Draining in LIGO Progenitor Black Hole Binaries and Its Significance to Electromagnetic Counterparts
Authors: Xiaoshan Huang, Sierra Dodd, Sophie Lund Schrøder, Shane W. Davis, Enrico Ramirez-Ruiz
Figure caption: The perturbed angular momentum at a given radial distance in the non-corotating frame for a disk with (Am3; left panel) and without (Am3_nc; right panel) a companion BH. Components of the perturbed angular momentum terms are listed in the right panel and are derived in Appendix B. The results are time averaged over the disk-draining phase. The black solid curves correspond to the rate of perturbed angular momentum change (Equation (B2)). The orange solid curves are associated with the angular momentum transport of the accreting mass flux (Equation (B3)). The blue solid curve represents the Reynolds and viscous stress terms (Equation (B3)), and the red dashed curve corresponds to the torque from the companion (Equation (B6)). The dotted black curves represent the difference between the total stress and the torque, which we defined as dissipation that induces angular momentum transport and accretion. In the case of low αk = 10−5, where the hydrodynamics are nearly inviscid, the companion’s presence leads to the nonzero torque term, and shock dissipation gives rise to mass accretion.