adsabs/AstroCLIMB huggingface dataset:
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature and pressure data for brine with varied stirring speed. All temperature data are TC3 (the deepest TC), and pressure data are the mass-independent sensor.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature, pressure, and mass data for three trials of pure water. The left column is the first 20 s, while the right column is the data for the full experiment. TC1 is the deepest TC, and TC3 is the closest to the top of the cup.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature and pressure data for trials with incomplete degassing of pure water.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature, pressure, and mass data for three trials of eutectic brine with the glass beads.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Data from the “fast stirring” brine showing possible supercooling and sudden freezing at about 90 s.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature, pressure, and mass data for three trials of brine.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Temperature, pressure, and mass data for three trials of water 1:3 with glass beads. (Mass data are unavailable for trial 1).(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: EOI measured on Didymos at 5 m pixel−1. The thresholds in EOI values have been chosen to enhance the location of smooth, intermediate, and rough terrains on the asteroid.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: EOI measured on Dimorphos at 35 cm pixel−1. The thresholds in EOI values have been chosen to clearly separate boulders from pebbles.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: RFS method applied to the reconstructed tridimensional models of comet 67P/Churyumov–Gerasimenko and asteroid (25143) Itokawa. Models taken from public archives; processing and rendering done with shapeViewer (J. B. Vincent 2018). We use the same reference images as in Figure 1. The smooth/rough terrains visually identified in the images of 67P and Itokawa can also be found in the RFS measurements, albeit within the limitations of the shape model resolution. The spatial distribution of RFS on Bennu appears less localized than on the other bodies, with no obvious units. Note that this figure only shows a qualitative example of the method. A thorough comparison of RFS measurements across asteroids, as well as comparison with previous methods, is given in C. Herrmann & J.-B. Vincent (2024).
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: Example of a morphological unit identified on Didymos, overlaid on the original image and the map of EOI. The dotted area shows the contiguous smooth equatorial region. Dotted lines and arrows indicate putative mass wasting. A complete description of the geological units is available in O. S. Barnouin et al. (2023).
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: Comparison between the RFT and the illumination angles (incidence and emission) on Didymos and Dimorphos at the time of image acquisition. There is no apparent correlation between these quantities, which suggests that the measurement is robust against a wide range of illuminations. Top row: resolution is 5 m pixel−1; bottom row: resolution is 0.35 m pixel−1.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: EOI measured on (a) Didymos and (b) Dimorphos at multiple scales. Image resolution is 5 m pixel−1; the measurement scale is given in pixels and also represented visually by a white square in the upper left corner of each panel.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: EOI vs. incidence and emission angles for both asteroids; mean and standard deviations are calculated in bins of 10°. The EOI does not correlate with incidence and emission, except for extreme angles (i, e < 20° and i, e > 80°) where photometric effects and long shadows start to become significant.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: Comparison between RFT and RFS. Colors indicate qualitatively the distribution of smooth and rough terrains. Both methods lead to a similar description of the surfaces of Didymos and Dimorphos. Top row: resolution is 5 m pixel−1; bottom row: resolution is 0.35 m pixel−1. The shape models are oriented and shaded using the same geometric conditions as at the time of image acquisition.
Paper: Macroscale Roughness Reveals the Complex History of Asteroids Didymos and Dimorphos
Authors: Jean-Baptiste Vincent, Erik Asphaug, Olivier Barnouin, Joel Beccarelli, Paula G. Benavidez, Adriano Campo-Bagatin, Nancy L. Chabot, Carolyn M. Ernst, Pedro H. Hasselmann, Masatoshi Hirabayashi, Simone Ieva, Özgür Karatekin, Tomáš Kašpárek, Tomáš Kohout, Zhong-Yi Lin, Alice Lucchetti, Patrick Michel, Naomi Murdoch, Maurizio Pajola, Laura M. Parro, Sabina D. Raducan, Jessica Sunshine, Gonzalo Tancredi, Josep M. Trigo-Rodriguez, Angelo Zinzi
Figure caption: DRACO images of Didymos and Dimorphos acquired respectively 2 m 43 s (panel (a)) and 11 s (panel (b)) before impact. The yellow arrow indicates the direction of the north pole of both asteroids (Didymos’s positive spin axis).
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Tadpole craters show a statistically significant preference for smaller craters. (a) Histogram of the proportion of all craters that are tadpole craters in the latitude band 24°–52° south as a function of diameter, normalized for degradation state. (b) Histogram of the proportion of all craters that are tadpole craters with a single exit breach by diameter. (c) Histogram of the proportion of all craters that are tadpole craters with multiple breaches by diameter. For all panels, black bars show ﹩\sqrt{n}﹩ error bars, where n is the total number of tadpole craters in each bin (n  a  = 233 is the total number of tadpole craters with D  c  ≥ 4 km for the full tadpole crater population, n  s  = 145 for single-exit-breach tadpole craters, n  m  = 77 for multiple-breach tadpole craters). Dashed red lines show a linear best fit. Dotted red lines bounding red shaded areas indicate 99.8% confidence intervals for linear best fit found using 5000 bootstrapped samples of size n  R  = 13,538 (the total number of craters in latitude band 24°–52° south with D  c  ≥ 4 km in the Robbins database; Robbins & Hynek 2012a) with replacement.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Schematic illustration of our four overspilling hypotheses for tadpole craters. (a) H1: crater filled to rim with liquid water where breaches form when water level exceeds topographic lows on rim. (b) H2: ice-filled crater where breaches form when localized melt pond(s) overspill the crater rim. (c) H3: crater at the margins of a retreating regional ice sheet where breaches form when meltwater in the crater exceeds topographic lows on the rim, and new topographic lows are exposed as the ice sheet retreats. (d) H4: crater buried beneath regional ice sheet where breaches form as subglacial channels. All breaches may form in a single overspilling event, or sequentially as rim topography is modified or exposed by changing ice extent and topography or erosion.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Tadpole craters do not show a clear elevation trend but preferentially occur on relative highs across all length scales. (a) Histogram of degradation-state-normalized (see Section 2.2) percentage of total crater population that are tadpole craters with MOLA elevation. (b–f) Histogram of degradation-state-normalized tadpole crater percentage with residual MOLA topography. We generate smoothed MOLA topography with smoothing radii (r  s ) of 50, 100, 200, 500, and 1000 km. We then subtract the smoothed topography from the original MOLA mosaic to find the residual MOLA topography. Black bars show ﹩\sqrt{n}﹩ error bars, where n is the total number of tadpole craters in each bin (n  a  = 233 is the total number of tadpole craters with D  c  ≥ 4 km for the full tadpole crater population). Dashed red lines show a linear best fit to inverse ﹩\sqrt{n}﹩ weighted bin totals. Dotted red lines bounding red shaded areas indicate 95% confidence intervals for linear best fit found using 5000 bootstrapped samples of size n  R  = 13,538 (the total number of craters in latitude band 24°–52° south with D  c  ≥ 4 km in the Robbins database (Robbins & Hynek 2012a) with replacement). Elevation data correspond to crater floor elevation as in the Robbins database (Robbins & Hynek 2012a).
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: HiRISE imagery of crater floor fill, interpreted as crater-filling ice. Blue arrows indicate wrinkling at the boundary between the steep topography and texturally altered bedrock-like (Conway et al. 2018) appearance of the preserved crater rim and the flatter crater fill. Black arrows indicate decameter-scale polygonally dissected crater fill resembling polygons observed in latitude-dependent mantle occurring alongside CCF and brain terrain (Levy et al. 2009), and in transitions between different brain terrain textures in ice and LDM-filled craters (Mangold 2003). White ellipses indicate candidate ring mold craters (Kress & Head 2008). Yellow arrows indicate areas of closed-cell brain terrain (Levy et al. 2009), interpreted as indicators of crater-filling ice or ice-rich debris beneath LDM. Red arrows indicate arcuate, parallel ridges of light-toned, knobby material, interpreted as arcuate ridges (Conway et al. 2018), likely associated with ice fill. (a) Hellas (left: ESP_012014_1335): decameter-scale bright mounds surrounded by mid-toned, relatively smooth material throughout the image resemble buttes of partially dissected brain terrain (Mangold 2003) and knobby textures observed on LDAs (Pierce & Crown 2003); (b) Arabia Terra 2 (left: ESP_053736_2180); (c) Noachis (left: ESP_074112_1455); (d) Arabia Terra 1 (left: ESP_052510_2150): ring mold crater indicating impact into ice-rich substrate in center left of image (Kress & Head 2008).
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: (a) HiRISE imagery of unincised portions of multiple-breach crater rims showing mottled rim textures resembling texturally altered bedrock (Conway et al. 2018) along the most topographically elevated portions of the rim in (a, g) Arabia Terra 1 (left: ESP_053736_2180), (c, i) Arabia Terra 2 (left: ESP_053736_2180), (e) Hellas (left: ESP_012014_1335), and (k) Noachis (left: ESP_074112_1455) (Table 1). (b) Topographic profiles of crater rims (see Figure 7 for profile transects) in (b, h) Arabia Terra 1, (d, j) Arabia Terra 2, (f) Hellas, and (l) Noachis, showing topographically rounded rims (e.g., panels (h), (d), and (l)) and sharper rim sections (e.g., panels (b) and (j)) more closely resembling the steep, narrow shape of fresh crater rims (e.g., Robbins & Hynek 2012b). In all profiles, the crater interior is to the left.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: (a) HiRISE imagery of crater rim breaches infilled with discontinuous material resembling crater-filling ice-rich deposits (white arrows; Section 3.2.1) in (i) Hellas (left: ESP_012014_1335) and (ii,iii) Arabia Terra 2 (left: ESP_053736_2180). Red dashed circles highlight small craters filled with material morphologically consistent with ice-rich deposits. (b) Downstream topographic profiles of ice-rich deposit-free exit breaches (traces of profiles shown in Figure 7) for (i, ii) Arabia Terra 1 and (iii) Arabia Terra 2.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: DEMs of multiple-breach tadpole craters showing measurement areas for other figures. (a) Arabia Terra 1 (left: ESP_052510_2150), (b) Arabia Terra 2 (left: ESP_053736_2180), (c) Hellas (left: ESP_012014_1335), (d) Noachis (left: ESP_074112_1455) (Table 1). White solid lines indicate breach long profiles (Figure 10), with breach labels corresponding to those in Figure 1; black solid lines indicate rim topographic profiles (Figure 9); and black dashed boxes indicate regions shown in other figures.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Map of reliable tadpole craters in the latitude band 24°–52° south overlaid on MOLA topography. Yellow circles indicate craters with a single exit breach, teal circles craters with two exit breaches, and blue circles craters with ≥3 exit breaches.
Paper: Multiple Overspill Flood Channels from Young Craters Require Surface Melting and Hundreds of Meters of Midlatitude Ice Late in Mars’s History
Authors: Alexandra O. Warren, Sharon A. Wilson, Alan Howard, Axel Noblet, Edwin S. Kite
Figure caption: Percentage of craters in each degradation state classification (Robbins & Hynek 2012a) that are tadpole craters, separated into tadpole craters with a single exit breach (blue) and those with multiple breaches (red). A degradation state of 4 corresponds to a pristine, fresh crater, and a degradation state of 1 corresponds to the most degraded craters, which are highly infilled/modified by fluvial and aeolian processes with no preserved topographic rims or ejecta. The total tadpole crater fraction is the sum of the two bars, i.e., 2.4% for degradation state 2. Error bars show fractional error corresponding to ﹩\sqrt{n}﹩, where n is number of single-breach (blue) or multiple-breach (red) tadpole craters in each degradation state category.
Paper: Constraints on the Long-term Existence of Dilute Cores in Giant Planets
Authors: A. Tulekeyev, P. Garaud, B. Idini, J. J. Fortney
Figure caption: Left: time series of nondimensional mean vertical density profiles (with ﹩\bar{\rho }﹩ on the horizontal axis and the z-coordinate on the vertical axis) for Pr = τ  =  0.1 and ﹩{R}_{0}^{-1}\,=\,4.0﹩. Each line represents a mean density profile at a specific time, and each density profile is horizontally offset (shifted) from earlier time steps for ease of visualization. Lines are plotted in increments of 2500 time units, in 10 different colors. Each blue line corresponds to Δt = 25,000 time unit increments. Right: inverse density ratios (vertical axis) vs. time (horizontal axis): R −1(0, t) (green) and R −1( ± 75, t) (orange). The red horizontal dashed line shows ﹩{R}_{L}^{-1}\simeq 1.5﹩, which is the layering threshold for Pr = τ  =  0.1.
Paper: Constraints on the Long-term Existence of Dilute Cores in Giant Planets
Authors: A. Tulekeyev, P. Garaud, B. Idini, J. J. Fortney
Figure caption: Same as Figure 1, but for Pr = τ  =  0.1 and ﹩{R}_{0}^{-1}\,=\,2.5﹩. Left: time series of vertical density profiles. Each blue line corresponds to Δt = 12,500 time unit increments. Right: inverse density ratios vs. time: R −1(0, t)(green) and R −1( ± 75, t) (orange). The red horizontal dashed line shows ﹩{R}_{L}^{-1}\simeq 1.5﹩, which is the layering threshold for Pr = τ  =  0.1, and the black dashed line corresponds to t = 60,000 when convection is triggered.
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Map showing the search areas on the sky during the time span of this project. The sky is shown with an overlay of the equatorial sky-plane coordinates. Superimposed are ellipses for the area that includes 67% of the encounterable CCKBO population at opposition for the indicated year. The different colors correspond to the three distinct search epochs discussed in this paper (color-coded by common effort). No searches were conducted in years with white ellipses. Also shown are curves for the ecliptic and the Galactic plane.