adsabs/AstroCLIMB huggingface dataset:
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: Two pulses from CHIME J0630+25 detected by CHIME/Pulsar. The top panel for each burst contains frequency-averaged and dedispersed time series. The red line is the smoothed profile. The plots are not necessarily centered on the extracted TOA; rather, the center is chosen to best show the burst morphology. The second panel shows the dynamic spectrum of each burst, and the bottom panel shows the dedispersion heat map for each burst. The dedispersion heat map shows the power for many different DM trials. All astrophysical pulses of CHIME J0630+25 center on DM ≈ 22pc cm−3.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: No EFACs were included in any of the timing residual plots. (a) Timing residuals using the glitch model. (b) Timing residuals using the nonglitch model. (c) Timing residuals obtained by fitting only to the bursts before the glitch epoch. (d) Zoomed in timing residuals of panel (b) showing a clear downward sloping structure.
Paper: The Sun Reversed Its Decades-long Weakening Trend in 2008
Authors: Jamie M. Jasinski, Marco Velli
Figure caption: Solar wind measurements of various parameters measured at 1 au since 2008. The measurements are averaged over a complete solar rotation and show mean (red), median (black), 5%–95% ranges (light gray), and 25%–75% ranges (dark gray), and blue shows a fitted trend from the start of 2008 onward (see the text for details). The blue numbers show the values at the start (left) and end (right) of the fitted trend. From top to bottom are (a) proton speed, (b) proton density, (c) proton temperature, (d) proton dynamic pressure, (e) magnetic field magnitude, and (f) sunspot number. In panel (f), the dashed lines show the averaging completed to produce Table 2 for the ascending phases of solar cycle 24 (2008.92–2013) and solar cycle 25 (2019.92–2024).
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: Timing residuals for PSR J0012+5431. On the left, we show timing residuals fit with only using CHIME/FRB metadata; on the right, we show a combination of CHIME/Pulsar intensity data and CHIME/FRB metadata.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: Additional dynamic spectra analogous to Figure 1.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: Continued.
Paper: CHIME/Fast Radio Burst/Pulsar Discovery of a Nearby Long-period Radio Transient with a Timing Glitch
Authors: Fengqiu Adam Dong, Tracy E Clarke, Alice Curtin, Ajay Kumar, Ryan Mckinven, Kaitlyn Shin, Ingrid Stairs, Charanjot Brar, Kevin Burdge, Shami Chatterjee, Amanda M. Cook, Emmanuel Fonseca, B. M. Gaensler, Jason W. Hessels, Victoria M. Kaspi, Mattias Lazda, Robert Main, Kiyoshi W. Masui, James W. McKee, Bradley W. Meyers, Aaron B. Pearlman, Scott M. Ransom, Paul Scholz, Kendrick M. Smith, Chia Min Tan
Figure caption: We show only the minimum when we perform a grid search over frequency and frequency derivative parameters. The χ2 increases rapidly as we deviate away from the optimum parameters; therefore, we choose to zoom in on the minimum.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: SPHERE/IRDIS multiband image of the WISPIT 2 system. The H-band Qϕ image was added as the blue channel and the median combination of the H-band and Ks-band Qϕ images was added as the green channel. The red channel is a combination of the Ks-band Qϕ image and the Ks-band cADI image in which we masked all but the gap containing the thermal emission from WISPIT 2b .
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: 2D contours (for 68% CL and 95% CL) for H0 and S8 from ΛCDMP18, ΛCDMξTEBW, ΛCDMξTTBW, ﹩{{\rm{\Lambda }}}{{\rm{CDM}}}{\xi }_{{\mathtt{TTBW}}+{\mathtt{SN}}}﹩, and ΛCDMξTTBW + τ2. The dark and light gray regions represent the 68% and 95% CL, respectively, for the SH0ES H0 measurement and the KiDS-1000 S8 constraint under the ΛCDMξ model (see Section 3).
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: 2D contours (68% and 95% CL) for H0 and Mν (ξ3) from ΛCDMξTTBW, ΛCDM﹩{\xi }_{{\mathtt{TTBW}}+{\mathtt{SN}}}﹩, ΛCDM﹩{\xi }_{{\mathtt{TTBW}}+{\tau }_{2}}﹩ (left panels), and ΛCDMξTTBW (right panels), with scatter points colored according to values of ξ3 (Mν) in the upper (lower) panels. The colored lines are from Equations (6) and (7), with the stars representing the corresponding reference points.
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: ns − r contours (for 68% CL and 95% CL) and several selected inflation models’ predictions, shown as red, green, and dark gray lines, with uncertainties in the number of e-folds of 50 < N < 60 (more details can be found in Section 5.2). ﹩{M}_{{{\rm{\max }}}}﹩ is the upper bound of the model parameter M in E. J. Copeland et al. (1994).
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: Ratios of DV/rd (upper panel) and DM/DH (lower panel) to the corresponding predictions from ΛCDMP18, denoted as “fid.” Data with error bars are from the DESI BAO results (DESI Collaboration et al. 2025a, 2025b). The blue, purple, and brown lines are calculated by the cosmological parameters from ΛCDMξTTBW, ΛCDM﹩{\xi }_{{\mathtt{TTBW}}+{\mathtt{SN}}}﹩, and ΛCDM﹩{\xi }_{{\mathtt{TTBW}}+{\tau }_{2}}﹩, respectively.
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: 1D marginalized posterior PDFs and 2D contours (68% and 95% CL) of cosmological parameters for different models from different data sets as shown in the legend.
Paper: Refitting Cosmological Data with Neutrino Mass and Degeneracy
Authors: Shek Yeung, Wangzheng Zhang, Ming-chung Chu
Figure caption: Left panels are the same as the right panels of Figure 2, but with the light beige lines constrained by BAO data. The right panels show the corresponding normalized likelihood ﹩{ \mathcal L }﹩, with the shaded areas representing 95% CL.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Zoom-in on the innermost disk ring (ring 3). We show polarized light Qϕ images in the gray color scheme in the left and middle panels and the total intensity cADI Ks-band image in the blue color scheme in the right panel. The middle panel shows the Qϕ image after image deconvolution was applied. The left and middle panels are displayed on a log scale due to the large dynamic range of the inner disk region, while the right panel is on a linear scale. The gray hashed circle in the image center marks the area covered by the coronagraphic mask. We indicate with dotted lines (left and middle panels) and with a solid encircling ellipse (right panel) the signature of the inner disk bottom side.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Full sample of all disk observations in near-infrared scattered light for which multiple rings were detected. We show the location and width of the widest gap in each system as given in the literature. When no specific gap widths were given, we used the difference between the peaks of adjoining rings as a measure for the gap width instead. Positional uncertainties are typically low and on the order of ∼1 au. We distinguish between T Tauri and Herbig stars. The systems with a similar or larger gap width as WISPIT 2 are labeled. The systems with a detected planet (WISPIT 2 ) or planet candidates (HD 169142, HD 163296, HD 97048) are indicated with a black circle around the marker.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Panel (a): definition of the PA, measured counterclockwise from north to east. In this convention, the PA is measured from north to the major axis and contains the forward scattering side, corresponding to a PA of 357°in this diagram. Panel (b): image of the disk de-projected using the height and inclination measurements extracted from individual rings following this convention, with angular size on sky translated to astronomical unit.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Stellar evolution isochrones for various masses (solid lines) and ages (dashed lines). The models are, from left to right, BHAC15, PARSEC 1.2, and SPOTS (f = 0.17). WISPIT 2 is indicated with a blue marker.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Distance vs. reddening E(B − V) for stars within 1°, with distances based on Gaia DR3 parallaxes and reddening from E. Paunzen et al. (2024).
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Results from fitting the age of the cluster using the EW(Li) and Teff values listed in Table 6 with EAGLES (top panels) and EAGLES v2.0 (bottom panels).
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Relationship between the gap width and the mass ratio q. Here, the K. D. Kanagawa et al. (2016) model is represented by the dots, and the S. Zhang et al. (2018) is represented by the crosses. A triangle marker has been inserted to show the star–planet mass ratio based on magnitude and age estimates.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: Ks-band Stokes Q and U and derived Qϕ and Uϕ images of the WISPIT 2 disk. We note that polarized light observations are typically not sensitive to planet thermal emission, which is predominantly unpolarized. Consequently, the planet WISPIT 2b is not visible in these images.
Paper: WIde Separation Planets In Time (WISPIT): A Gap-clearing Planet in a Multi-ringed Disk around the Young Solar-type Star WISPIT 2
Authors: Richelle F. van Capelleveen, Christian Ginski, Matthew A. Kenworthy, Jake Byrne, Chloe Lawlor, Dan McLachlan, Eric E. Mamajek, Tomas Stolker, Myriam Benisty, Alexander J. Bohn, Laird M. Close, Carsten Dominik, Sebastiaan Haffert, Rico Landman, Jie Ma, Ignas Snellen, Ryo Tazaki, Nienke van der Marel, Lukas Welzel, Yapeng Zhang
Figure caption: H-band Stokes Q and U and derived Qϕ and Uϕ images of the WISPIT 2 disk. We note that polarized light observations are typically not sensitive to planet thermal emission, which is predominantly unpolarized. Consequently, the planet WISPIT 2b is not visible in these images.
Paper: A Constraint on the Density of Jupiter’s Moon Thebe from Primordial Dynamics
Authors: Ian R. Brunton, Konstantin Batygin
Figure caption: Three simulations of the scenario described in the text and more thoroughly described in I. R. Brunton & K. Batygin (2025). Io, Thebe, and Amalthea form in a zone of satellite building blocks near r0 ∼ 0.1 RH, where Io subsequently captures the smaller moons on interior mean-motion resonant orbits once it type-I migrates inward. Each plot shows the joviancentric distance evolution of the three moons. Shaded envelopes around Amalthea and Thebe trace the difference in their perijove and apojove, thus characterizing their eccentricity in resonance. The light-blue band marks the magnetospheric cavity beginning at the disk’s truncation radius, Rt = 5 RJ. In each run, Thebe’s density is given an equivalent value to Amalthea’s known density, ρT = ρA = 0.86 g cm–3, and the disk aspect ratio is varied from h/r = 0.06, 0.10, and 0.14.
Paper: A Constraint on the Density of Jupiter’s Moon Thebe from Primordial Dynamics
Authors: Ian R. Brunton, Konstantin Batygin
Figure caption: A grid of outcomes for 10,000 simulations as described in the text. Color corresponds to the success rate of Io’s delivery of both Amalthea and Thebe to the inner disk edge, while replicating their proper modern ordering (﹩{a}_{{\rm{A}}}\lt {a}_{{\rm{T}}}﹩). Dotted density lines indicate Amalthea- and Callisto-like densities, corresponding to the exemplary runs shown in Figures 1 and 2.
Paper: A Constraint on the Density of Jupiter’s Moon Thebe from Primordial Dynamics
Authors: Ian R. Brunton, Konstantin Batygin
Figure caption: A similar grid of outcomes for 10,000 simulations as that of Figure 3, now instead with minor flaring in the disk, as β = 1/4, and varying the reference aspect ratio between h0 =  0.08 and 0.15. Since ﹩h/r={h}_{0}{(r/{r}_{0})}^{\beta }﹩, this adjustment decreases the overall success rate throughout parameter space, with a slight but notable exception between h0 ≈ 0.09–0.12 and ρT ≲ 1.0 g cm–3, in which the success rate increases.
Paper: A Constraint on the Density of Jupiter’s Moon Thebe from Primordial Dynamics
Authors: Ian R. Brunton, Konstantin Batygin
Figure caption: Three simulations with the same setup as Figure 1, except Thebe is now given a Callisto-like density, ρT = ρC = 1.83 g cm–3.
Paper: Spectral Characteristics of Interstellar Object 3I/ATLAS from SOAR Observations 
Authors: Thomas H. Puzia, Rohan Rahatgaonkar, Juan Pablo Carvajal, Prasanta K. Nayak, Baltasar Luco
Figure caption: Optical reflectance spectrum of comet 3I obtained at 4.4 au compared with literature data for interstellar objects and asteroids. Main panel: our 3I spectra obtained using two solar normalization methods are shown: G2V solar analog HD 168595 (blue) and SOLSPEC solar spectrum (red; M. Meftah et al. 2018). Shaded regions show literature reflectance spectra: VLT-MUSE observations of 3I (C. Opitom et al. 2025, dark gray), SNIFS observations of 3I (D. Z. Seligman et al. 2025, light gray), reflectance of 1I (A. Fitzsimmons et al. 2018, cadet/grayish blue), 2I (J. de León et al. 2020, light green), D-type asteroids (F. E. DeMeo et al. 2009, pink), and 2012DR30 (T. Seccull et al. 2021, coral). Colored vertical bands highlight typical molecular emission regions: CN (3860–3880 Å, yellow), C3 (4050 Å, purple), and C2 (4750 Å and 5150 Å, red and green), along with forbidden oxygen transitions [O I] (6300 Å and 6364 Å, blue). Zoom-in panels: the left panel compares the 20 Å smoothed and normalized (at 5500 Å and arbitrarily offset) 3I flux spectrum in the 1- and 2-FWHM extraction apertures with the continuum subtracted Hale–Bopp comet emission (right ordinate; from H. Rauer et al. 2003, obtained at rh = 3.8 au), across the 3500–6500 Å region. The top right panel shows the 3I reflectance spectral dip region at 6000–7000 Å with linear continuum fits extrapolated from the feature-free region at 4000–5600 Å to assess absorption features relative to the underlying continuum. Dark and lighter lines are spectra for 1- and 2-FWHM extraction apertures, respectively. The bottom right panel shows a detailed view of the CN(0–0) vibration band feature region (3780–3940 Å) with 50 Å smoothing applied to reveal the subtle spectral structure. Solid and dashed lines represent the 1- and 2-FWHM extraction apertures, respectively.
Paper: Spectral Characteristics of Interstellar Object 3I/ATLAS from SOAR Observations 
Authors: Thomas H. Puzia, Rohan Rahatgaonkar, Juan Pablo Carvajal, Prasanta K. Nayak, Baltasar Luco
Figure caption: Modeled thermal evolution of 3I during its perihelion passage. Solid curves show the time-temperature profiles at multiple depths (0–40 cm; see the legend) obtained with the 1D conduction model described in Section 4.1. All subsurface layers were initialized at TISM = 10 K at t = −105 days and preconducted to the instantaneous radiative-equilibrium surface temperature prior to the plotted window. The solid vertical line marks the epoch of perihelion (Tp = 2025 October 29, see the top axis). Dashed horizontal lines indicate vacuum sublimation thresholds for selected volatiles (CO, NH3, CO2, and H2O). A twin right-hand axis gives the corresponding temperature in °C. The bottom x-axis shows the temporal perihelion offset in days, while the upper x-axes provide the corresponding heliocentric distance and date. The gray shading encodes 3I’s solar elongation, and the vertical dotted lines indicate encounters with major solar system planets, with their minimum passage distances shown in the labels. The vertical dotted–dashed line marks the date our SOAR observations were taken.
Paper: The Potential Danger to Satellites due to Ejecta from a 2032 Lunar Impact by Asteroid 2024 YR4
Authors: Paul Wiegert, Peter Brown, Jack Lopes, Martin Connors
Figure caption: Time of flight from ejecta launch from the Moon until reaching the Earth for clones A through D. The inset panel shows a zoomed-in view to show that first arrivals occur roughly 3 days after the impact for clone B and 5 days for clone A. The first material from clones C and D does not arrive until over 80 days after impact.
Paper: Carbon-rich Sub-Neptune Interiors Are Compatible with JWST Observations
Authors: Zifan Lin, Sara Seager
Figure caption: Simulated transmission spectra of sub-Neptune GJ 1214 b compared with HST and JWST observations.
Paper: Ubiquitous Occurrences of Multiscale Layers of Magnetic Reconnection across a Solar Wind Stream Interaction Region at 1 au
Authors: S. Eriksson, A. Chasapis, A. Mallet, M. Swisdak
Figure caption: Wind satellite observations on 2019 January 1–9 (left) and 2019 January 4 06:00 UT to 2019 January 5 18:00 UT (right): (a) pitch-angle distribution of 165 eV electron differential energy flux, (b) ratio of parallel to antiparallel electron energy flux, (c) magnetic field strength (B), (d) BxGSE component of BGSE, (e) azimuthal φB angle of ecliptic plane BGSE (φB = 0° for BxGSE > 0 and ByGSE = 0; φB = 90° for BxGSE = 0 and ByGSE > 0), (f) solar wind speed (V), (g) VyGSE component of VGSE, (h) proton number density (Np), and (i) proton average temperature (Tp). Two red horizontal dotted lines in (e) mark φB = 45° and φB = 225°. Three magenta-colored, vertical dotted lines mark a forward shock at 2019 January 4 10:11:20 UT, an SI at 2019 January 4 21:48:00 UT, and a reverse shock at 2019 January 5 09:58:00 UT. A horizontal magenta bar along the top marks the SIR. Two blue vertical dotted lines at 2019 January 4 16:56:40 UT and 2019 January 5 02:20:30 UT mark a magnetic SB (horizontal blue bar, top right).