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Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Empirical distribution functions for the S93 Voyager 2 stellar and solar occultation profiles, following Figure 7. The colors in this figure correspond to the colors used in Figure 6. As in Figure 7, notice that the distribution functions for the occultation blocks are all clearly different from the tightly grouped baseline distributions, especially at the tails.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Example of the difference between using the Elliot et al. (2003) minimum binning approach and our ratchet binning approach. In panel (a), we show an isothermal profile, and in panel (b), we show a more realistic profile for Uranus (both in black). Each profile was simulated into the light curves and then processed back into the profiles. The light curves that were processed using minimum binning as in Elliot et al. (2003) are shown in blue, and those processed using ratchet binning are shown in red. Light curves with 3% random noise are shown with solid lines, and those with 20% random noise are shown with dashed lines. The minimum binning procedure creates large, systematic errors that are not created using ratchet binning, leading us to use ratchet binning in this work.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption:  Q–Q plot for a section of baseline residual. Here the distribution lies entirely within the 90% confidence intervals, meaning that we cannot reject the null hypothesis that the baselines of the residuals (away from the occultation) are normally distributed. That is, the baseline distribution fails to clear a low bar (90%) for non-normality, leading to the conclusion that the baseline is normally distributed.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Flowchart showing the steps of forward modeling. For the definition of each symbol, see the text. Notice that the temperature profile, impact parameter (y), and reference values are the only independent inputs to the process.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: 39P’s orbit from the years of 1900–2060, divided into three periods, is shown here to highlight the drastically varying orbital path it has and will be taking. The period from 1900 to 1937 is green, the period from 1937 to 1963 is in red, and the period from 1963 to 2060 is blue. The orbit of 39P changed significantly from 1943 to 1963, moving from a JFC designation, and a tisserand parameter (T  J ) that is between 2 and 3, perihelia (q) < 5.2 au, and aphelia (Q) < 7 au (Sarid et al. 2019) with q = 3.4 au to a centaur, with an orbit entirely contained in the giant planet region, with q = 5.5 au, due to a close encounter with Jupiter in 1963. The rapid change in 39P’s orbit was accompanied by a significant change in solar heating, especially to the outer layers of the nucleus. This figure was generated using the REBOUND Python package (Rein & Liu 2012). The progression of time is in the counterclockwise direction.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: The CO2 column density (left), continuum intensity (center), and their 1D relative spatial profiles (right). The spatial profile of the CO2 gas is broader than the dust profile, and it shows a possible small asymmetry in the sunward direction (dashed line in the second panel) when compared to the continuum (nucleus and dust) profile, which instead appears centered and symmetric. Both profiles are normalized to unity for comparison and visualization purposes. The 1σ uncertainties in the continuum profile are not as visible in the plot because of the higher signal-to-noise ratio relative to the gas profile.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: The continuum of centaur 39P compared to the icy coma of comet 103P/Hartley 2 and the global average surface of comet 67P/Churyumov–Gerasimenko. Left: this graph investigates the 3 μm bands, detrended and stretched as described in the text. We see that beyond 3.1 μm 39P and 67P have the same spectral behavior. Right: this graph shows the relative reflectance spectra of all three objects (39P, 67P, and 103P), normalized to 1.0 at 2.2 μm.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: Radial profiles of 39P from the LDT ﹩{r}^{{\prime} }﹩ images. The area around the centaur is divided into two halves based on the PS of the comet’s motion (1.″2 = 5 pixele per exposure along PA = 250°), and the data points colored accordingly. An ellipse highlights pixels within the PA = 70°–250° half that are affected by the background source. The mean radial profile for the unaffected half (PA = 250°–70°) is shown as a line.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: Cumulative completeness of the diameter, C(D >), at the end of 2022 as a result of the KOM computed for 10 random realizations of the NEA reference model with the minimum size set to 40 m. The average cumulative completeness is shown as the solid line, showing that the KOM estimates an average completeness of 88% for NEAs larger than 1 km and 38% for NEAs larger than 140 m. The discrepancy between our completeness estimate at 1 km and the estimates of 90+% completeness from Mainzer et al. (2011a) and Granvik et al. (2018) are due to the fact that the KOM does not include specialty surveys (such as the low solar elongation surveys, NEOWISE, etc.). NEOWISE has, for example, contributed at least 55 NEA discoveries with diameters larger than 1 km, which would account for ∼6% of completeness for this size range.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: Cumulative and differential completeness of the absolute magnitude, C(H  V  < ), at the end of 2022 as a result of the KOM for 10 instances of the reference model with the minimum size set to 40 m. The differential completeness is shown as the light gray solid lines, while cumulative completeness is shown as the dark gray solid lines. The cumulative and differential completenesses as a function of absolute magnitude as derived by Harris & Chodas (2021) are shown as the solid and dashed red lines, respectively. The missing completeness in the KOM at H  V  < 20 mag is due to the KOM not modeling the low solar elongation surveys and NEOWISE.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The fraction of objects observed by the KOM as a function of absolute magnitude H  V  in bins of ±0.25 mag around the absolute magnitude. The Amor subpopulation is favored by almost 10% for H  V  < 23 mag over the Apollo subpopulation. For objects with H  V  > 23 mag, there is little difference in the biases of these two subpopulations. The Atens have significantly higher chances of being detected by the KOM for H  V  > 22 mag.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The distribution of perihelion distance for the objects cataloged by KOM up until the end of 2022 (red histogram), the NEOS 5 yr nominal mission (blue histogram), and the two combined (black solid histogram). The distribution of objects identified as cataloged by KOM that are not observed by NEOS is shown as a yellow histogram. This shows that the majority, ∼59%, of known objects missed by the NEOS are Amors, where the current surveys are fairly efficient due to the favorable geometry.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The comparison of the KOM using the NEA reference model with the known NEA population from the MPC for objects with H  V  ≤ 23 mag (the proxy of objects larger than ∼140 m). The orbital elements of perihelion distance, eccentricity, and inclination are shown from left to right. The KOM applied to 10 random realizations of the NEA reference model is shown in gray, while the MPC distribution is shown in blue.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The comparison of the KOM using the reference model with the known NEA population from the MPC for objects with H  V  ≤ 17.75 mag (the proxy for objects larger than ∼1 km). The orbital elements of perihelion distance, eccentricity, and inclination are shown from left to right. The KOM applied to 10 random realizations of the NEA reference model is shown in gray, while the MPC distribution is shown in blue.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The cumulative completeness of the effective diameter for NEAs in the reference model for the KOM (red solid line), the NEOS mission (blue solid line), and the combined result of the KOM and the NEOS mission (black solid line). Also shown is the fraction of objects seen by KOM that NEOS is not likely to detect in its 5 yr nominal mission (yellow solid line).
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The eccentricity distribution of the objects cataloged by KOM up until the end of 2022 (red histogram), NEOS 5 yr nominal mission (blue histogram), and the two combined (black solid histogram). The distribution of objects identified as cataloged by KOM that are not observed by NEOS are shown as a yellow histogram. As expected, NEOS is very efficient at detecting and tracking low-eccentricity objects, similar to the current surveys.
Paper: The NEO Surveyor Near-Earth Asteroid Known Object Model
Authors: Tommy Grav, Amy K. Mainzer, Joseph R. Masiero, Dar W. Dahlen, Tim Spahr, William F. Bottke, Frank J. Masci
Figure caption: The visible albedo distribution of the objects that are larger than 140 m from an instance of the reference model identified by the KOM (red histogram) as currently cataloged. The objects identified as cataloged by NEOS are given as a blue histogram, with the combined set of objects cataloged by both KOM and NEOS shown as a black histogram. The NEAs larger than 140 m that are identified as cataloged by the KOM and not seen by the NEOS in a nominal 5 yr survey are shown as the yellow histogram.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Left-hand panel: DEM from Beddingfield et al. (2022) placed over the mosaic of Inverness Corona (Figure 3). The black lines indicate the location of topographic profiles and the black box indicates the location of the zoomed-in portion in the upper right. Upper right-hand panel: black lines indicate the location of the eight topographic profiles, labeled A-H. Middle right-hand panel: an example of a topographic profile (profile C in upper right). Note the vertical exaggeration (meters on the y-axis and kilometers on the x-axis). Lower right-hand panel: an example of the FFT analysis of a topographic profile (profile C in upper right).
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Correlation of map units (COMU) for the Inverness Corona region on Miranda: cp = cratered plains material, c = crater material, ce = crater ejecta material, s = scarp material, oc = outer corona material, ic = inner corona material, r = rounded ridge material, ch = chasma material, bc = bright corona material. The jagged line in the time arrow on the left-hand side indicates that there was likely a few billion years of geologic history between the formation of cp/c/ce and the rest of the geologic units identified.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Fast Fourier Transform of each of the eight topographic profiles from Figure A1. Wavelengths are considered significant when occurring with a power >100. Broad peaks at the longer wavelengths (as in E, F, and G) are discarded as not real due to their broadness and the similarity to the length of the topographic profile input.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Topographic profiles at each of the eight lines indicated in Figure 6. Note the difference in scale on the y-axis and the x-axis.
Paper: Unraveling the Geologic History of Miranda’s Inverness Corona
Authors: Erin J. Leonard, Chloe B. Beddingfield, Catherine M. Elder, Tom A. Nordheim
Figure caption: Geologic map of Inverness Corona and the surrounding region with map key below. Note, “SP” denotes the location of the south pole of Miranda.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Comparison of the temperature–pressure profiles produced by three archival remote-sensing measurements: Voyager 2 radio occultations, Voyager 2 UV stellar and solar occultations, and the U0 Earth-based stellar occultation. The radio occultations are shown in black in the lower atmosphere. The H87 retrieved temperatures from the Voyager UV occultations are shown by green and red points connected by thermal gradients. The S93 models fit to the H87 data are shown with red, green, and navy dotted lines. The U0 occultation is shown in blue with shaded 1σ uncertainty. Note the large discrepancy between the Earth-based and Voyager 2 temperatures, especially at the 10−3 mbar pressure level.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Orientation of Uranus as seen from Earth during the U0 occultation. The line is the projected path of the occultation star (“occultation chord”) on the disk of Uranus, moving from the green circle (right) to red square (left). The open circle indicates the location of the subsolar point. As shown, the obliquity of the planet makes the occultation path almost entirely equatorial.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Temperature profiles resulting from reprocessing the U0 light curve, with ingress on the left and egress on the right. The reprocessed results for the three channels are shown with solid lines in red, blue, and green with 1σ shaded error regions. The originally published profiles (Elliot & Dunham 1979) are shown by large black dots with 1σ shaded error regions. Temperatures are shown as a function of pressure, and the altitudes corresponding to channel 2 of the reprocessed results from this work are shown for reference. Notice that all three reprocessed channels agree with each other (except for the bottom of the ingress profile) and the original profile on ingress but disagree with the original profile on egress. In addition, the upper ends of all reprocessed profiles show a more rapidly warming lower thermosphere than the original profiles do. The reprocessed profiles have a vertical resolution of sub-1 km, increasing slightly to a few kilometers at the bottom of the profiles.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Same as Figure 1 but with the reprocessed U0 results from this work, including shaded 1σ uncertainty regions. Notice that the tension between the U0 and Voyager 2 profiles is less prevalent at the 10−2 mbar pressure level but still exists at the 10−3 mbar pressure level. While the reprocessed profiles may have decreased the tension, stellar occultation processing alone cannot account for it.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Results of reprocessing the U0 occultation with different boundary conditions. The originally published profiles (Elliot & Dunham 1979) and reprocessed channel 2 data with a thermal gradient model are shown as in Figure 13. The reprocessed channel 2 data with an isothermal model are shown by a dashed blue line. The boundary condition strongly impacts only the top end of the profile.
Paper: The Upper Atmosphere of Uranus from Stellar Occultations. I. Methods and Validation
Authors: William R. Saunders, Michael J. Person, Paul Withers, Richard G. French, Chanita Tubthong
Figure caption: Observer altitude in kilometers vs. normalized flux for the channel 2 light curve (ingress and egress), with full resolution in small black points, binned data in black lines, and the thermal gradient model fit in blue. We show only channel 2 here because it is the highest S/N of the three channels.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: These images of 39P are extracted from each of the four NIRSpec data cubes at the median over the wavelength axis of wavelengths from the data cubes, ∼2.95 μm. The data were all taken on 2022 July 27 and the UT starting exposure time is provided in the upper right of each image panel. A 0.″5 diameter aperture (denoted with a red circle and corresponding to a projected diameter of 1994.5 km at the centaur’s distance from JWST) was used to extract the 39P spectrum. A background galaxy was imaged in frames 2–4, but does not contaminate 39P’s coma in the aperture used. The images are oriented with north up and east to the left. The projected Sun–comet vector (PsAng) and projected negative orbital velocity vector (PsAMV) are shown, obtained using JPL’s Horizons. These vectors are used as indicators of the potential tail direction.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: H2O (left) and CO (right) spectra of 39P with the continuum subtracted. Neither volatile was clearly detected. Here we get upper limits of 10.0 × 1023 molecules s−1 and 12.1 × 1023 molecules s−1, respectively. In both spectra, the wavelengths from Table 2 where we would expect to see the molecular peak are located between the dashed purple lines; these purple lines mark the beginning and end of the region that was integrated to get the upper limits of the production rates. The noise surrounding the purple dashed lines is comparable to the molecular signatures themselves. The uncertainties of the relative flux densities associated with each spectral channel are shown by the region highlighted in light blue.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: CO2/H2O over different heliocentric distances. 39P could possibly follow the fractional production rate of CO2 to water. 39P is included, as a green diamond, to compare against comets, and centaur 29P (green circle). The CO2/H2O of 39P displayed in the graph is a lower limit.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: CO/CO2 over different heliocentric distances. 39P is included as a green diamond for comparison to comets, and centaur 29P (green circle). The CO/CO2 of 39P displayed in the graph is an upper limit.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: JWST NIRSpec spectrum of 39P is shown, where the bump at 4.26 μm is the detection of CO2. CO and H2O signatures are not detected. CO and H2O would be seen at 4.67 and 2.66 μm, if their emissions were stronger.
Paper: First Detection of CO2 Emission in a Centaur: JWST NIRSpec Observations of 39P/Oterma
Authors: O. Harrington Pinto, M. S. P. Kelley, G. L. Villanueva, M. Womack, S. Faggi, A. McKay, M. A. DiSanti, C. Schambeau, Y. Fernandez, J. Bauer, L. Feaga, K. Wierzchos
Figure caption: JWST NIRSpec spectrum of CO2 emission in 39P after the dust continuum has been subtracted. This is the first detection of CO2 emission in a centaur. A double Gaussian fit is superimposed on the double peaks of the CO2 (ν 3 band) which we used to measure the integrated flux density. We derive a production rate of ﹩{Q}_{{\mathrm{CO}}_{2}}﹩ = 5.96 ± 0.80 × 1023 molecules s−1. The uncertainties of the relative flux densities associated with each spectral channel are shown by the region highlighted in light blue.