adsabs/AstroCLIMB huggingface dataset:
Paper: SpinTrace: A Python Library to Study the Physical Properties of Small Bodies Using Survey-based Photometry
Authors: F. L. Rommel, E. Fernández-Valenzuela, A. C. Souza-Feliciano, B. E. Morgado, B. Proudfoot
Figure caption: Chiron’s reduced magnitudes as a function of time as obtained from the ZTF database. The color scale indicates the astrometric offset between the predicted-by-JPL coordinates and the selected PSF ones.
Paper: Simultaneous Detection of the Size and Velocity of the Largest Ejecta Particles with Velocities Exceeding 1 km s−1
Authors: Akiko M. Nakamura, Keita Nomura, Sunao Hasegawa
Figure caption: Results for one shot (#4982). (a) The crater on the basalt target. (b)–(d) Images taken by Cam 1, and (e)–(i) by Cam 2. All images are partially cropped, brightness-adjusted versions of the original images. In panels (e)–(g), the two vertical white lines represent the edges of the glass plates, and the black grid on the glass plates has approximately 10 mm spacing. The light blue lines in panel (e) delineate the metal frame supporting the glass plates (see Figure 1(d)). (b) Cam 1 image obtained just after the projectile impacted the basalt target. (c) The subsequent Cam 1 image, taken 2 μs later. (d) The ejecta cone captured by Cam 1 taken 66 μs after panel (b). (e) Cam 2 image obtained just before the projectile struck the basalt target. (f) Image taken one frame after panel (e), i.e., 33.3 μs later. (g) Image taken two frames after panel (f), i.e., 66.7 μs later. (h) Enlarged and enhanced view of the square outlined by the red dashed lines in panel (g). The bright spots (numbered 1 and 2) are shown in Figures 4(a)–(c). (i) Enlarged and enhanced view of the rectangle outlined by the orange dashed lines in panel (g). The bright spots (numbered 3) are shown in Figure 4(d). (j) Time sequence of the Cam 2 operation and the event. The projectile impact occurred at ﹩{T}_{1}﹩, and the fastest ejecta impacted the secondary target at ﹩{T}_{2}.﹩
Paper: Simultaneous Detection of the Size and Velocity of the Largest Ejecta Particles with Velocities Exceeding 1 km s−1
Authors: Akiko M. Nakamura, Keita Nomura, Sunao Hasegawa
Figure caption: Image of the glass plates (shot #4982). (a) A low-resolution optical microscope image of craters in the central plate. The bright spots numbered 1 and 2 are those in Figure 3(h). The grid with approximately 10 mm spacing that appears black in Figures 3(e)–(g) appears white in Figure 4(a). The white letter “2” on the plate indicates that this is the central plate in the three-plate set. (b) Enlarged view of doublet craters 1 in panel (a). Each side of the image is 0.7 mm in length. (c) Enlarged view of crater 2 in panel (a). Each side of the image is 1 mm in length. (d) Optical microscope image (2.8 mm wide) showing craters on the right glass plate, corresponding to area 3 in Figure 3(i). The insets show magnified views, each 0.35 mm on a side. (e) SEM image (secondary electron image) of radially patterned aluminum deposits on the left glass plate. Scale is 0.5 mm in length. (f) An optical microscope image corresponding to the bottom-right region of the SEM image in panel (e).
Paper: Simultaneous Detection of the Size and Velocity of the Largest Ejecta Particles with Velocities Exceeding 1 km s−1
Authors: Akiko M. Nakamura, Keita Nomura, Sunao Hasegawa
Figure caption: Experimental setup. (a) Schematic view from the direction vertical to the projectile trajectory. Strobe 1 was mounted on an obliquely downward-facing window above the chamber and illuminated the target at a 45° angle from above. (b) Schematic view of the ejecta trajectory and the secondary target. (c) Outside view of the chamber from the side of the cameras (Cam 1 and Cam 2). The mirror (omitted from Figure 1(a)) was mounted at a 45° angle above the upper window of the chamber and was used by Cam 3 to capture images of the primary target from above. (d) Inside view of the chamber from the direction opposite to that shown in panel (c).
Paper: Simultaneous Detection of the Size and Velocity of the Largest Ejecta Particles with Velocities Exceeding 1 km s−1
Authors: Akiko M. Nakamura, Keita Nomura, Sunao Hasegawa
Figure caption: Optical microscope images of craters formed during calibration shots at impact velocities of (a) 3.38 km s−1 and (b) 7.07 km s−1. Blue and orange arrows indicate the outermost and innermost boundaries between the uneven outer region and the outermost fissure region, corresponding to the maximum and minimum diameters, respectively (see main text for details). Scale bars: 2 mm. (c) Normalized crater diameters (circles) at each impact velocity. The two ends of the error bar correspond to the maximum and minimum values. The dashed line shows the empirical relationship of Equation (2).
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Variety of datasets collected for the three initially chosen craters. Maturity indices are being investigated across these datasets, with promising results. (Top) Byrgius A (19.7 km; 24.6°S, 63.5°W), a young highlands crater. (Middle) Dufay B (19.8 km; 8.3°N, 171°E), an intermediate-aged highlands crater. (Bottom) Golitsyn J (19.5 km; 27.9°S, 102.9°W), an old highlands crater. The columns show the appearance of the crater across wavelengths, from UV (WAC UV; left) to radar (Mini-RF radar; right).
Paper: Evaluating Lunar Crater Ejecta Maturation across Wavelengths
Authors: Angela M. Stickle, Anna C. Martin, Robyn M. Meier, Tyler M. Powell
Figure caption: Different wavelengths interact with different size fractions. The UV data are sensitive to the smallest size fraction, within the top few microns of the surface. Longer wavelengths are progressively sensitive to larger rock fractions. The horizontal bars show the approximate grain sizes each separate dataset is sensitive to. Schematics of representative-sized objects show the relative sizes.
Paper: High-temperature He+ Irradiation of Low-iron-bearing Olivine: Laboratory Simulations of Space Weathering on Mercury
Authors: Surya Snata Rout, Ulrich Kentsch, Ralf Dohmen, Franziska Traeger, Swarna Prava Das, Hans-Werner Becker, Stefan Facsko, Martin Ritter
Figure caption: (a) STEM-HAADF image of a region of the lamella prepared from U-olivine. Line profiles extracted from TEM-EDS spectrum image (SI) obtained from the region in panel (a) show the variation in (b) element distribution and (c) element ratios from the interior of the irradiated grain to the surface as marked by the arrow in panel (a). (d) STEM-HAADF image of a region of the lamella prepared from H-olivine. (e) The line profile extracted from TEM-EDS SI of the region in panel (d) shows the variation in element distribution from the interior of the irradiated grain to the surface as marked by the arrow in panel (d). The dashed line in panels (b) and (e) marks the position of the interface between the crystalline part of the grain and the ion-damaged region. (f) TEM-EDS SI for element Fe (FeKα) from the region in panel (d) showing the distribution of Fe-rich nanoparticles (marked with arrows) on the top surface of the lamella.
Paper: High-temperature He+ Irradiation of Low-iron-bearing Olivine: Laboratory Simulations of Space Weathering on Mercury
Authors: Surya Snata Rout, Ulrich Kentsch, Ralf Dohmen, Franziska Traeger, Swarna Prava Das, Hans-Werner Becker, Stefan Facsko, Martin Ritter
Figure caption: (a) BF-TEM image of the lamella prepared from U-olivine crystal. The layer with numerous vesicles on top of the crystalline olivine (Olv) is marked with dashed lines. Various dislocations in the olivine crystal are indicated with arrows. C = combination of sputter deposited carbon and carbon deposited from a precursor gas using a gas-injection system (GIS) attached to the focused ion beam instrument. (b) STEM-HAADF image of the lamella from H-olivine (irradiated at 450 °C). The ion-damaged region is marked with dashed lines and is characterized by the presence of numerous bright nanoparticles. (c) HRTEM image of a region from panel (a), showing the interface (dashed line) between crystalline olivine and the overlying ion-damaged region. Crystal lattice fringes are seen in the crystalline olivine, and the inset is the fast Fourier transform (FFT) of the crystalline and the overlying partially amorphous region. (d) HRTEM image of a region from panel (b) illustrating the polycrystalline ion-damaged layer and the underlying crystalline olivine. The interface between crystalline olivine and the ion-damaged layer is marked with a dashed line. The inset shows the FFT of the crystalline olivine and the ion-damaged region. The circled regions within the polycrystalline layer point to islands of olivine crystallites.
Paper: High-temperature He+ Irradiation of Low-iron-bearing Olivine: Laboratory Simulations of Space Weathering on Mercury
Authors: Surya Snata Rout, Ulrich Kentsch, Ralf Dohmen, Franziska Traeger, Swarna Prava Das, Hans-Werner Becker, Stefan Facsko, Martin Ritter
Figure caption: (a) STEM-HAADF image of the film deposited using the PLD technique on a MEMS-based chip for an in situ TEM annealing experiment. The film was deposited at 450 °C, and the bright regions are <1 nm sized Fe-rich inclusions present in a dark amorphous matrix. (b) BF-TEM image of the film shown in panel (a) after being heated for a few milliseconds up to 1200 °C. The spherical inclusions with dark contrast are Fe-metal particles.
Paper: Surface Response of Mercury’s Sulfides under Solar Wind Ion Irradiation
Authors: Noah Jäggi, Catherine A. Dukes
Figure caption: XPS data (Experiment) compared to surface evolution of the corresponding SDTrimSP simulation for oldhamite (Old) and niningerite (Nng). The S diffusion case in the 2 keV ﹩{{\rm{H}}}_{2}^{+}﹩ on the Old (CaS) plot uses the same damage-dependent S diffusion rates determined for the RIS in FeS (J. M. Christoph et al. 2022). Measurement errors are two SDs of the composition obtained by using either the 2p or 2s peaks of Ca, Mg, and S for analysis or the experiment error, whichever is larger. For C, the F error of ±0.2 at% was used (F ≤ 0.5 at%; not shown). The final fluence step S is compared to the bulk S content (with a two SD error) by applying the bulk sulfur:metal ratio measured by EDS to the respective measured Mg/Ca content.
Paper: Surface Response of Mercury’s Sulfides under Solar Wind Ion Irradiation
Authors: Noah Jäggi, Catherine A. Dukes
Figure caption: XPS spectra of CaS binding states compared between the fresh sample, the first He-irradiated fluence step (1.6 × 1016 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2), and the final fluence step (2.2 × 1019 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2). In the Ca 2p, the plasmon loss feature (>353 eV; J. F. Moulder 1992; M. Engelhard & D. Baer 1999) is not fitted, and neither are the Ca 2p sulfate and sulfite features due to their low abundance, as is apparent in the S 2p feature.
Paper: Surface Response of Mercury’s Sulfides under Solar Wind Ion Irradiation
Authors: Noah Jäggi, Catherine A. Dukes
Figure caption: XPS spectra of CaS binding states compared between the fresh sample, the first He-irradiated fluence step (1016 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2), and the final fluence step (2 × 1019 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2). In the Ca 2p, the plasmon loss feature (>353 eV; J. F. Moulder 1992; M. Engelhard & D. Baer 1999) is not fitted, and neither are the Ca 2p sulfate and sulfite features due to their low abundance, as is apparent in the S 2p feature.
Paper: Surface Response of Mercury’s Sulfides under Solar Wind Ion Irradiation
Authors: Noah Jäggi, Catherine A. Dukes
Figure caption: XPS spectra of MgS binding states compared between the fresh sample, the first proton-irradiated fluence step (1016 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2), and the final fluence step (3 × 1019 ﹩{{\rm{H}}}_{2}^{+}﹩ cm−2). In the Mg 1s, the sulfate and sulfite features are not fitted due to their low abundance, as is apparent in the S 2p feature.
Paper: Surface Response of Mercury’s Sulfides under Solar Wind Ion Irradiation
Authors: Noah Jäggi, Catherine A. Dukes
Figure caption: MgS powder (a) before and (b) after hand milling.
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Rasters of the threshold turbulence parameter α  ν,th as a function of planetesimal radius R and macroporosity ϕ  M  for OC and BA pebbles, two different fragmentation threshold velocities v  f,ice, and t  f  ≃ 0.5 Myr after CAIs. Red vertical lines in Figure 2(a) correspond to inferred radii of NC IMPBs based on metallographic cooling rates of their respective iron meteorites groups (e.g., IVA) from L. Qin et al. (2008; see Section 4.3.1 for discussion).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Plots of pressure at the centermost point in the planetesimal P  m,c  as a function of characteristic pebble radius a  p  for different (a) macroporosities ϕ  M  and (b) grain radii a  g . Here, we assume R ≃ 100 km, t  f  ≃ 0 Myr, P  D  ≃ 10−4 bar, and OC as pebble analogs. For a given choice of ϕ  M  and a  g , there are two threshold a  p  at which P  m,c  exceeds the water triple point pressure of ≃6 mbar, corresponding to two regimes in the model. The relevant threshold in the context of planetesimal formation is the smaller of the two (see Section 3.1 for discussion).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Plots of the threshold pebble radius a  p,th for melting water–ice as a function of planetesimal radius R assuming (a) OC and (b) BA as pebble analogs. As is clear, a  p,th decreases with increasing formation time t  f , macroporosity ϕ  M , and microporosity ϕ  m , but increases with R. Points corresponding to R ≃ 50 km and t  f  ≃ 0.5 Myr are designated with a blue marker (see Section 3.2 for discussion).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Rasters of ﹩{\mathrm{log}}_{10}({\alpha }_{\nu }/{\alpha }_{\nu ,\mathrm{th}})﹩ across ﹩\tilde{\alpha }-\psi ﹩ parameter space assuming (a) OC and (b) BA pebbles, and fiducial values for planetesimal structural parameters in Table 1. Here, v  f,ice ≃ 5 m s–1. As is clear, no melting of water–ice is expected to occur for quiescent disks, with α  ν  ≲ 10−3 (see Section 4.3.2 for discussion).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Flowchart displaying the procedure for computing the threshold turbulence parameter α  ν,th, involving an iterative process seeking to minimize the deviation between the threshold Stokes number Stth (from a  p,th) and the characteristic Stokes number of disk pebbles limited by fragmentation, independent of the planetesimal model (see Section 4.2 for details).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Illustration of an SS disk with α  ν  (a) <α  ν,th, (b) =α  ν,th, and (c) >α  ν,th. Melting of water–ice in the interior of the planetesimal formed by the agglomeration of icy pebbles beyond the ice line is achievable in (b) and (c). As α  ν  increases (for a given ψ), pebble sizes across the disks decrease, and the ice line sits farther from the Sun (see Section 4.3.2 for discussion).
Paper: Early Solar System Turbulence Constrained by High Oxidation States in the Oldest Noncarbonaceous Planetesimals
Authors: Teng Ee Yap, Konstantin Batygin, François L. H. Tissot
Figure caption: Illustrations of the icy NC planetesimal in consideration at the (a) disk, (b) planetesimal, and (c) pebble scales. In (a), the planetesimal accreted beyond the ice line now sits interior to it, such that its surface is permeable to water vapor loss. In (b), the packing of rocky and water–ice pebbles composing the planetesimal results in macropores, the pressure within which increases with depth. In (c), the packing of silicate and water–ice grains composing each rocky pebble results in micropores, the pressure within which increases with proximity to the pebble center (see Section 2 and Table 1).
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Contour plots (using 15 logarithmically spaced contour levels ranging from the peak value of each image—6.64 MJy sr−1 for F200W and 2.06 MJy sr−1 for F277W—to the background level of ∼0.01 MJy sr−1 in each image) of the inner coma of 358P/PANSTARRS constructed from (a) F200W and (b) F277W NIRCam median composite images shown in Figures 2(a) and (b), respectively. A 0.″5 angular scale bar (760 km at the distance of the comet) is shown in each panel, where the orientations of the images and contour plots are the same.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Comparison of measured H2O emission with a modeled spectrum, where the measured H2O 0−0 band emission at 2.69 μm for 358P is shown in black with error bars, and the modeled emission for a 0.″4 beam for a Haser-like distribution of water outgassing with a total production rate of ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}=(5.0\pm 0.2)\times {10}^{25}﹩ molecules s−1 split between two components with characteristic temperatures of 15 and 30 K is shown in red. A small 0.003 μm wavelength correction has been added to the JWST data, as is standard practice for PSG retrievals (G. Villanueva, private communication). A representative sample of the walkers from the MCMC sampler is shown in blue, and residuals and 3σ errors are shown in magenta. Note that the excess residuals at 2.64 and 2.72 μm are just within the 3σ error.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Median composite images of 358P/PANSTARRS, aligned on the photocenter of the comet in each individual image, constructed from NIRCam data obtained using the (a) F200W and (b) F277W broadband filters, comprising 1031 s of total exposure time each. Labeled arrows indicate the directions of celestial north (N) and east (E) and the projected anti-Sun (−⊙) and negative heliocentric velocity (−v) vectors as seen from JWST. A 5″ angular scale bar (7600 km at the distance of the comet) is also shown in each panel. Color scaling in both panels is linear, where regions in the inner coma (in the center of each image) that are shown as solid white consist of pixels with fluxes that are ∼20% of the peak central flux or larger.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Plot of Af ρ as a function of photometry aperture radius (solid blue line) in terms of arcseconds projected on the sky (bottom x-axis labels) and kilometers at the distance of the comet (top x-axis labels) as measured for a composite image of 358P constructed from data obtained on UT 2024 February 2 by Gemini North, with a ρ −0.3 power law (dashed black line) shown for reference.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: One-dimensional background-subtracted NIRSpec spectra for each dither extracted using 0.″4 radius apertures, along with the median-combined spectrum.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Relative reflectance spectrum with 1σ error in gray of 358P (black line) derived from the median-combined spectrum shown in Figure 1 and the STScI CALSPEC solar reference spectrum. Also shown are a linear reflectance (2.25 ± 0.03%/100 nm) and blackbody curve fit (blue dashed line) to the observed reflectance, where the blackbody spectrum has a temperature of T BB = 200 K and is normalized at 4 μm.
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Sample fits from the MCMC models for the CO (top left), CH3OH (top right), and CO2 (bottom) emission band regions for NIRSpec observations of 358P. Black points are observations, and blue-to-gray lines indicate a subsample of the MCMC model fits to the data, showing the spread of those fits. Also shown are model spectra for each gas with production rates equal to our 99.7th percentile upper limit and 10 times that upper limit (thin solid and dashed red lines, respectively).
Paper: The Volatile Composition and Activity Evolution of Main-belt Comet 358P/PANSTARRS
Authors: Henry H. Hsieh, John W. Noonan, Michael S. P. Kelley, Dennis Bodewits, Jana Pittichová, Audrey Thirouin, Marco Micheli, Matthew M. Knight, Michele T. Bannister, Colin O. Chandler, Carrie E. Holt, Matthew J. Hopkins, Yaeji Kim, Nicholas A. Moskovitz, William J. Oldroyd, Jack Patterson, Scott S. Sheppard, Nicole Tan, Chadwick A. Trujillo, Quanzhi Ye, 泉志 叶
Figure caption: Normalized radial surface brightness profile of the non-nucleus-subtracted coma of 358P (blue line) measured from a composite image constructed from data obtained on UT 2024 February 2 by Gemini North, with diagonal lines indicating power law slopes of −1 (black line) and −1.5 (gray line) shown for reference. Vertical dotted lines mark (from left to right) the FWHM seeing (θ  s ) from Table 3, ρ = 5000 km, and ρ = 4″.