adsabs/AstroCLIMB huggingface dataset:
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: (Left panel, blue) Cumulative size distribution of the 24 exocomets identified in the RZ Psc system with radii in units of kilometers, calculated from Equations (B1), (B2), and (B3) in Appendix B. We report a power-law index γR<break = −0.12 ± 0.02 for the power-law fit before the turnover point at ∼2.5 km and a power-law index γR>break = 3.45 ± 0.17 for the power-law fit after the turnover point, which was calculated from Equation (3). (Green) Cumulative size distribution of the 24 exocomets identified in the RZ Psc system with radii in units of kilometers, calculated from Equation (B4) in Appendix B. We report a power-law index γR<break = −0.39 ± 0.03 for the power-law fit before the turnover point at around ∼2.26 km and a power-law index γR>break = 2.48 ± 0.05 for the power-law fit after the turnover point. (Yellow) We compare to the size distribution of β Pictoris from A. Lecavelier des Etangs et al. (2022). (Gray dashed–dotted) We also compare it to solar system populations from A. Lecavelier des Etangs et al. (2022). (Gray dotted) We plot a vertical line representing the estimated radius of the most recent interstellar object, 3I/ATLAS, of 5.6 ± 0.7 km from C. O. Chandler et al. (2025). Right panel: a comet frequency distribution in AD space to highlight our detection ability for smaller ADs. We report a power-law fit γAD>break = 2.32 ± 0.12 and γAD<break ​​​​​​ = 0.11 ± 0.04, where the ADs in the region of incomplete recovery were not fit. We expect that far fewer than 100% of the exocomets will be detectable in the region of incomplete recovery. This calculation was performed with a cadence of 200 s, matching the cadence of sectors 57 and 84.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: Top: simulated EVE observation of an exocomet transit of a K7V at 100 pc expected during a 20 day stare at ∼20 Myr Theia 43 or 45 associations. We scale the optical light-curve template used for the RZ Psc events into the NUV and NIR bands using a 50%–50% weighted average of empirical extinction curves of ∼200 nm water ice (W. Krätschmer & N. Sorg 1985) and olivine dust (D. R. Huffman 1975). Bottom: distribution of optical ADs vs. spectral type for 590 simulated detections. The SNR of the NUV detections (left) enables color differences due to composition (middle) and grain size (right) to be distinguished given the color predictions for the narrow-tail multiband comet models of S. Kálmán et al. (2024). Each panel highlights the region in which EVE should detect exocomets given a 20% M star disk fraction, but not for a 2.1% fraction.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: Left: dependence of the pipeline scaling of the measured RZ Psc cumulative occurrence rate by stellar mass. Right: additional noise from stellar activity observed in 2 minute cadence TESS light curves of candidate EVE sources relative to that expected from the TESS precision curve. The magnitude at which the decrease in TESS precision overtakes the relatively constant stellar activity signal is predicted for the EVE bands and used to construct stellar activity precision-vs.-magnitude relations.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: The Lomb–Scargle periodogram, computed from the combined TESS data across all three sectors (black), with the initial exocomet models subtracted, shows that the maximum period of 3.73 ± 0.2 days is consistent across all sectors and is indicated here by the dashed yellow line, with the 1σ uncertainty shaded. Some of the later peaks are harmonics of the 3.73 day period. The Lomb–Scargle periodogram for the individual sectors is overplotted: sector 17 (red), sector 57 (blue), and sector 84 (green).
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: Examples of exocomet models across all three sectors. In the left panel, sector 17 is shown with the highest-AD (AD ≃ 0.20, R = 5.27 ± 0.069 km) exocomet modeled, the middle panel shows an exocomet (AD ≃ 0.14, R = 5.086 ± 0.13 km) in sector 57, and the right panel shows a smaller exocomet (AD ≃ 0.019, R = 1.16 ± 0.14 km) modeled in sector 84.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: The top three panels show all three TESS sectors from start to finish, with the stellar variability and outliers subtracted. Each exocomet is denoted by a dashed line (orange). The bottom three panels are zoomed-in examples in sectors 57 and 84.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: GP models for all sectors of RZ Psc. The center value is shown by the solid orange line, with the 1σ uncertainty shown by the orange shaded region. This uncertainty was propagated into the exocomet model parameters, from which radii and transit times were calculated in Section 3.3.
Paper: TESS Discovers a Second System of Transiting Exocomets in the Extreme Debris Disk of RZ Psc
Authors: Adalyn Gibson, Meredith A. MacGregor, Ward S. Howard, Ann Marie Cody, Mark Swain, Jennifer A. Burt, Laura Venuti, Evgenya Shkolnik, Neal J. Turner, Alan Didion, Jaime Nastal, David Makowski
Figure caption: Noncumulative histogram of the number of exocomets as a function of AD; the bin width is 0.02. We report a power-law index α = 0.42 ± 0.18, which was calculated from Equation (2).
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: The weighted number overdensity map of PCL0217—“Bigfoot.” The upper left panel shows the distribution of the weighted number overdensity of galaxies with 3.73 < zphot < 4.23 in PRIMER-UDS. The red open circles show the position of the eight confirmed subgroups observed by the JWST/PRIMER survey (J. S. Dunlop et al. 2021); the pink circle shows a previously reported overdensity of quiescent galaxies (QGs; M. Tanaka et al. 2024) covered by the JWST/BEACON survey (T. Morishita et al. 2025). The upper right panel shows the three-dimensional distribution of the 11 subgroups. An animated version of this figure is available at https://box.nju.edu.cn/f/d6e29ce33a704cd29439/?dl=1. The lower figures show the enlarged overdensity map of the eight confirmed subgroups covered by the PRIMER survey. The purple and red crosses show the location of massive (M* > 109.5M⊙) SFGs and QGs. The overdensities shown in the upper and lower panels are measured in circular areas with radius ﹩1^{\prime} ﹩ and 15″, respectively.
Paper: The Bigfoot: A Footprint of a Coma Cluster Progenitor at z = 3.98
Authors: Hanwen Sun, Tao Wang, Emanuele Daddi, Qiaoyang Hao, Ke Xu, David Elbaz, Luwenjia Zhou, Houjun Mo, Huiyuan Wang, Longyue Chen, Yangyao Chen, Shuowen Jin, Yipeng Lyu, Nikolaj Sillassen, Kai Wang, Tiancheng Yang
Figure caption: Example of spectroscopically confirmed members of Bigfoot. The upper panel presents the redshift distribution of 55 spectroscopically confirmed galaxies. As examples, the lower panels show the JWST spectroscopy of four confirmed member galaxies in 0217A, their best-fit SED from Bagpipes, and the 4″ × 4″ RGB cutouts from the JWST/NIRCam images.
Paper: Quasi-thermal Noise in the Heliosphere, Including the Electron, Proton, and Shot Noise
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: The numerical results of the QTN spectral profiles related to heliocentric distances and model parameters. The frequency is normalized by the total plasma frequency fpt. Panel (a) presents the typical power density of the electron QTN, proton QTN, and shot noise at 215 Rs (1 au). The results of the total noise spectrum for several radial distances in the inner heliosphere are shown in panel (b). The results in the outer heliosphere within and beyond the termination shock are shown in panel (c) with the solid and dashed lines, respectively. Examples of the proton QTN at 1 au with variations of the model parameters are shown in the middle row, including the density ratio αep (panel (d)) and the temperature ratio τep (panel (e)) of the electrons to protons, and the solar wind velocity vD (panel (f)). The black line is the electron QTN spectrum at 1 au, as a reference. Panels (g), (h), and (i) show the results of the QTN spectra at 20 au with the superposition of drifting Maxwellian and kappa electrons. The effects of the drift velocities as well as the angle β between the antenna and drift velocity vD are given in panels (g) and (h), respectively. Panel (i) shows the shifted electron QTN when the core and halo electrons take different combinations of drift velocities.
Paper: Quasi-thermal Noise in the Heliosphere, Including the Electron, Proton, and Shot Noise
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Radial distribution of plasma parameters and power density of noise components at f/fpt = 0.95, from 0.01 to 120 au. Variations of the plasma density, temperature, and solar wind velocity are shown in panels (a), (b), and (c), respectively. The left side of the vertical gray dashed line at 1 au shows the empirical results from the Helios plasma data fitting, while the right side shows the in situ proton measurements from PLS on board Voyager 2. The radial evolutions of the power spectral density, sliced at f/fpt = 0.95 with antenna lengths of 3.5, 10, and 10 m, are shown in panels (d), (e), and (f), respectively. The blue, red, and yellow lines indicate the contributions of the electron QTN (eQTN), the proton QTN (pQTN), and the shot noise, respectively. The black line represents the variation with heliocentric distance of the Debye length, and the gray dashed line in the horizontal direction denotes the antenna length.
Paper: Quasi-thermal Noise in the Heliosphere, Including the Electron, Proton, and Shot Noise
Authors: Yi-Lun Li, 逸伦 李, Ling Chen, 玲 陈, De-Jin Wu, 德金 吴
Figure caption: Electron QTN spectrum computed with different parameters for the superposition of Maxwellian and kappa electron velocity distributions with drift velocity vDc = vTc and vDh = 2vTc. The parameters include: (a) the density ratio of the halo to core αhc; (b) the temperature ratio τhc; and (c) the kappa index κ. The default αhc = 0.1, τhc = 10, κ = 3, and the antenna length L = 10 m is set.
Paper: How Fast Could Supermassive Black Holes Grow at the Epoch of Reionization?
Authors: Ziyong Wu, Renyue Cen, Romain Teyssier
Figure caption: Following A. J. Taylor et al. (2025), we present the redshifts and BH masses from our simulations, along with the population of spectroscopically confirmed quasars at z > 6. We also include a simple growth model for 102 M⊙ (blue shading) and 104 M⊙ (red shading) BH seeds accreting at the Eddington limit. A vertical black dotted line marks the transition from the super-Eddington accretion phase to the self-regulation phase. By z ∼ 10, the SMBH in the steadier, Eddington-limited scenario surpasses its initially super-Eddington jump-start counterpart in mass, indicating that the Eddington-limited mode provides the fastest sustainable pathway for SMBH growth. To account for the ≳109 M⊙ quasars observed at z = 7–10, seed BHs with initial masses of 104–105 M⊙ are required.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: Spatial scales of supergranules near the poles. In each panel we plot the spatial autocorrelation function of the mean line-of-sight velocity (blue colored curves) from the corresponding meridian band in Figure 1, as labeled. This autocorrelation function is plotted as a function of spatial lag in degrees (lower abscissa) and megameters (upper abscissa). The yellow shaded curves are the 1σ standard deviation in the autocorrelation signal. The dotted horizontal lines mark the zero of the autocorrelation function. See Appendix A.1 for more details.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: Latitudinal migration of the magnetic network at high latitudes. (a) A 15 hr temporally averaged EUI/FSI304 Å intensity map in the zenithal equidistant projection is shown. The south pole is identified by the white dot, with dashed concentric circles denoting latitudes with 5° spacing. The yellow dotted wedge subtends an angle of 120° at the pole. EUV bright points within this wedge are tracked for their motion on the Sun. (b) Latitudinal tracks of EUV bright points with lifetimes of at least 10 hr (90 in total) are plotted with gray symbols. The various colored solid lines are linear fits to the observed tracks. The colors themselves indicate the latitudinal velocity of the moving bright points (we assign negative values for the bright points moving toward the south pole). (c) Longitudinally and temporally averaged velocity signal, derived from a Fourier local correlation tracking technique, as a function of solar latitude is plotted as gray symbols. The red horizontal line marks the 0 m s−1 level. In this representation too, negative velocities correspond to motions toward the south pole. See Appendices B and B.1 for more details.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: The latitudinal migration of supergranular structures. Latitudinal signal of the longitudinally averaged line-of-sight components of the velocity (a) and magnetic field (b) are displayed as functions of time. In panel (a) we highlight a feature that is drifting toward the pole with a velocity of −105 m s−1. The negative sign indicates that the flow is away from the north pole, i.e., toward the south pole. See Appendix A.1 for more details.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: Chromospheric bright points. Plotted in the same format as Figure 5(a) but showing the FSI304 map obtained at 2025 March 21 UT 21:09. The green contours within the yellow wedge region outline the bright points at that instance. Only those bright points that lived for at least 10 hr are highlighted.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: Same as Figure 1(a) but without the lines of longitude overplotted to better visualize the ripple-like velocity structures.
Paper: Supergranulation and Poleward Migration of the Magnetic Field at High Latitudes of the Sun
Authors: L. P. Chitta, D. Calchetti, J. Hirzberger, G. Valori, E. R. Priest, S. K. Solanki, D. Berghmans, C. Verbeeck, E. Kraaikamp, K. Albert, T. Appourchaux, F. J. Bailén, L. R. Bellot Rubio, J. Blanco Rodríguez, A. Feller, A. Gandorfer, L. Gizon, A. Lagg, A. Moreno Vacas, D. Orozco Suárez, J. Schou, U. Schühle, J. Sinjan, H. Strecker, R. Volkmer, J. Woch, X. Li, T. Oba, A. Ulyanov
Figure caption: Same as Figure 5(a) but showing the FSI304 map obtained by averaging the whole 8 day data set.
Paper: Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM
Authors: Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro
Figure caption: The 5.0–10.5 keV Resolve spectrum and residuals in the fit with the model including the three-zone UFO components, shown in the rest frame. Panels (a) and (b) include a broad Gaussian and XSTAR emission model, respectively, while panel (c) shows the fit without any broad emission-line model. Red, purple, blue, green, and cyan show the total source spectrum, power-law continuum absorbed by UFOs, broad Gaussian emission line, narrow Fe–Kα emission line, and NXB spectrum, respectively. Vertical solid and dotted lines indicate the approximate positions of the Fe XXV/XXVI Kα and Kβ absorption features, respectively, in Zones 1 (red), 2 (green), and 3 (blue).
Paper: Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM
Authors: Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro
Figure caption: Top: the 0.5–10 keV source (black) and background (gray) light curves derived by Xtend. Middle: the 1.5–4 keV (red) and 4–10 keV (blue) light curves. Bottom: the hardness ratio obtained by dividing the 4–10 keV count rate by the 1.5–4 keV count rate. The observation start time is 2024 August 9 17:34:01 (UT).
Paper: Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM
Authors: Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro
Figure caption: Left: the Xtend spectrum normalized with the effective area (black) shown with the spectra obtained by Chandra/ACIS (red and green), XMM-Newton/EPIC PN (orange, light green, and yellow-green), Suzaku/XIS (light blue), and NuSTAR (blue, cyan, magenta, and yellow) that were used in S. Yamada et al. (2021). Right: the deconvolved Xtend spectrum in a νFν form fitted with the model of AbsGal ∗ [Absint ∗ [(three XSTARUFO) ∗ PL + Gauss + Fe–Kα] + PLscat + HostGal]. Both are shown in the observer frame.
Paper: Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM
Authors: Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro
Figure caption: Resolve spectra in the rest frame, divided into the first 140 ks (black) and the later 144 ks (red). The black and red lines show the best-fit models for the first and later intervals, respectively, obtained from a simultaneous fit using the model AbsGal ∗ Absint ∗ [(three XSTARUFO) ∗  PL + Gauss + Fe–Kα], in which the UFO parameters were untied and allowed to vary freely. Vertical solid lines indicate the approximate positions of the Fe XXV/XXVI Kα absorption lines in Zone 3 at the first interval (black) and the later interval (red).
Paper: Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM
Authors: Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro
Figure caption: Schematic picture of the UFO components with multiple velocities and velocity dispersions in IRAS 05189−2524.
Paper: Orbital Characterization of a Newly Discovered Small Satellite around Quaoar
Authors: Benjamin Proudfoot, Richard Nolthenius, Bryan J. Holler, Ana Carolina de Souza-Feliciano, Flavia L. Rommel, Cameron Collyer, Will M. Grundy, Estela Fernández-Valenzuela
Figure caption: The evolution of the new satellite’s on-sky probability density after discovery, with high densities shown by brighter color. The 2D histogram is log-scaled and normalized at each individual epoch to better show the evolution of the distribution. After detection, Keplerian shear rapidly broadens the probability distribution until the distribution is roughly uniform in phase after 1–2 months.
Paper: Orbital Characterization of a Newly Discovered Small Satellite around Quaoar
Authors: Benjamin Proudfoot, Richard Nolthenius, Bryan J. Holler, Ana Carolina de Souza-Feliciano, Flavia L. Rommel, Cameron Collyer, Will M. Grundy, Estela Fernández-Valenzuela
Figure caption: The inclination of the local Laplace plane as a function of the inner satellite’s semimajor axis and Weywot’s mass. Dotted lines show Weywot’s expected mass from different densities based on Weywot’s diameter of ∼165 km (E. Fernández-Valenzuela et al. 2025, in preparation).