adsabs/AstroCLIMB huggingface dataset:
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: Logarithm of the production rates for the observed molecular species and A(0°)fρ for the dust as a function of time from perihelion (1997 April 1). Observations obtained from Lowell Observatory are shown as circles, while those from Perth Observatory are given as triangles; neither OH nor NH were observed from Perth. Inbound data are plotted with open symbols and outbound as filled. Color-coding is based on aperture size, using the logarithm of the projected radius in kilometers within bins shown at the top of the figure. The large scatter among data taken beyond about 6 au is generally due to the small fraction of the signal that remains following continuum subtraction, often resulting in negative gas values. Negative results are shown as downward arrows near the bottom of each panel and are also listed as “undefined” in Table 3.
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: The distribution of photometry observations and associated solar phase angles. In addition to the extreme extent of time and the very wide range of heliocentric distances of these narrowband observations, the observing geometries oscillated over a large range of phase angles, for which adjustments were made to dust production rates (see late Section 2.3).
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: Logarithm of production rate ratios plotted as a function of time from perihelion inside of 4.0 au. Symbols and colors are identical to Figure 2. The trends at larger distances (for instance, NH to OH and CN to OH) or lack thereof (C2 to OH and C3 to CN) are thought to be mostly due to inadequacies with the Haser model and the standard scalelengths when extrapolated to large distances. However, most noteworthy is the large trend seen in C2 to CN inbound but absent outbound; since model deficiencies cannot be the cause of this asymmetry, this must be indicative of a real seasonal effect due to differences in abundance ratios between source regions.
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: Logarithm of water production rates plotted as a function of log heliocentric distance as determined by a variety of different types of measurements. Preperihelion data are shown as open symbols, and postperihelion are filled. Our data, derived from the OH measurements reported in this paper, are presented as circles, while other data sets are given in the key, including the method of observation (see Section 3.5 for details regarding each data set). The dashed curve represents the prediction of a simple sublimation model scaled to these data at intermediate distances, using an active area of 2200 km2 (see text for details). While the overall behavior of water production is well matched by the sublimation model, there is a clear asymmetry between inbound and outbound data beyond about 2.3 au that largely reverses inside of 2 au. An excess above this baseline of activity is also evident in the few months surrounding perihelion; these deviations from the simple curve are largely explained by the seasonal effects associated with our preliminary modeling of the major source regions (see Section 3.6).
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: Logarithm of the production rates for the observed molecular species and A(0°)fρ for the dust as a function of the logarithm of the heliocentric distance. Symbols and colors are identical to Figure 2. However, unlike in Figure 2, where all data are presented, observations at large heliocentric distances that are not considered useful due to large scatter are no longer shown (see text for details). Linear fits in log–log space were computed and shown as solid lines based on data between 1.2 and 4.0 au, with preperihelion given in red and postperihelion in blue. These fits are extrapolated to the full range of observations using dotted lines. Due to the gap in observations outbound, the postperihelion fits actually begin at 2.16 au, partially explaining the difference between the pre- and postperihelion slopes, most evident for the dust.
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: The subsolar (solid curve) and sub-Earth (dashed curve) latitudes for H-B as a function of time, based on our preliminary derived pole orientation from our jet modeling (see Section 3.6 for details). Note that the subsolar latitude only moves significantly northward in the latter half of 1996. Also note the strong asymmetry about perihelion in both curves.
Paper: The Extreme Activity in Comet Hale–Bopp (C/1995 O1): Investigations of Extensive Narrowband Photoelectric Photometry
Authors: David G. Schleicher, Peter V. Birch, Tony L. Farnham, Allison N. Bair
Figure caption: Detail from Figure 2 for the perihelion time frame for early 1997. Again, the logarithm of the production rates for the observed molecular species and A(0°)fρ for the dust as a function of time from perihelion. Aperture trends (see color key) are quite evident, as well as significant rotational variability for gas species, but are nearly nonexistent for the dust.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Echo power spectra of asteroid Atira obtained at Arecibo Observatory on 2017 January 20. The OC signal (solid line) is considered to be a single reflection by a surface that is smooth in the wavelength scale; the SC signal (dashed line) is considered to be caused by multiple scattering or asymmetric single scattering by wavelength-scale or large particles. The ratio of these signals, SC/OC = μ  c , is 0.213 ± 0.011. The echo from the secondary is superimposed upon the primary's echo, seen as the large spike near 0 Hz. Δf is the Doppler frequency resolution.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: A mosaic of delay-Doppler images with 150 m × 0.95 Hz resolution (2 μs baud length) of Atira obtained at Arecibo Observatory on 2017 January 20; time of observation progresses to the right and down. Time delay, or range, increases downward with the vertical axis, and the Doppler shift, or frequency, increases to the right. The small, radar-bright object circled in red is the secondary. Note the secondary’s decrease in range indicative of its orbit.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Delay-Doppler image collages for the two overall best-fitting models. Contrast of delay-Doppler images has been increased for clarity. The left column is ecliptic longitude, ecliptic latitude (150°, −10°) and a volume-equivalent diameter of ∼7 km; the right column is ecliptic longitude, ecliptic latitude (187°, −53°) and a volume-equivalent diameter of ∼5 km. For each collage, the leftmost panel is the observed delay-Doppler image, the middle panel is the model delay-Doppler image, and the rightmost panel is the multifaceted model, where the purple shaft is the spin axis and the red and green shafts are the principal axes. The black pixels covering the primary’s signal in the delay-Doppler observation and model panels are a pixel mask covering the secondary. The observations were made on 2017 January 23 at 150 m × 0.95 Hz resolution. Note that the original radar data had different frequency and delay resolutions, but all images have been stretched (along both axes) and cropped so that they are displayed as square frames with a side length corresponding to 9 km. This means that the original delay-Doppler pixels can appear rectangular here.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: To test previously published rotation periods, we performed a period search covering 2500–2780 deg day−1 (3.107–3.456 hr) in 1 deg day−1 increments using only 2017 radar and lightcurve data. The vertical axis represents the weighted sum of χ 2 values, and the horizontal axis represents spin rate. Spin rate is found as 8640/P rot [hr]. At this stage, we used the best orientations found so far: the collection of models at the top have a northern hemisphere orientation (ecl. lon. 300°, ecl. lat. 33°), and the collection at the bottom has a southern hemisphere orientation (ecl. lon. 170°, ecl. lat. −40°); objective function values have not been altered. Note two prominent minima at 2541.8 deg day−1 (3.399 hr) and 2722.5 deg day−1 (3.174 hr) shown by blue and red vertical lines, respectively. For reference, the spin rate found by P. Pravec (2003) is 2547.9 deg day−1 (3.391 hr), and the spin rate found by E. Rondón et al. (2022) is 2740.2 deg day−1 (3.153 hr).
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Results of a coarse, 10° increment pole search across the entire celestial sphere with finer, 3° increment grid searches conducted near local minima (seen as the several large groupings) using ellipsoidal models. Each data point represents a model with a specific ecliptic latitude and ecliptic longitude, and the color of the data point represents the value of the objective function (see Section 3 for details), where a darker color means a better fit. The green triangle is the orientation of the best-fitting, ∼5 km model, and the purple triangle is the orientation of the alternate, ∼7 km model. Note that the group of models near longitude 0°, latitude −10° are darker in color; however, these models were ruled out based on being too small in size, ∼4 km equivalent diameter, to match delay-Doppler observations. The red crosses are the line of sight to Atira during radar observations and are annotated with their corresponding observed date.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Atira lightcurve from 2017 March 27 and 29. (a) The data showing all lightcurve components, folded with the apparent orbital period. (b) The secondary/orbital lightcurve component, derived after subtraction of the primary lightcurve component, showing the brightness attenuations caused by mutual events between the binary system components at orbital phases from 0.22 to 0.30. (c) The primary lightcurve component, folded with the synodic rotation period. The blue curve is the fourth-order Fourier series fitted to the primary lightcurve data.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Delay-Doppler images of the primary (signal at top of images) and secondary (signal at bottom of images) processed at different frequency resolutions. The left panel is processed at 0.95 Hz frequency resolution, and the right panel is processed at 0.125 Hz frequency resolution. Note the increase in the number of pixels containing signal for the secondary when the frequency resolution is increased.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Results of the simulated orbit using SHAPE, specifically at times of mutual events. Each row contains one simulated observation window with dates (from top to bottom): 2017 February 25, 2017 February 27, 2017 March 27, and 2017 March 29. Images (per row) are separated in time by roughly 20 minutes. The red and green arrows represent the principal axes of each body, and the purple arrow represents the spin axis of each body. The orientation of the primary (and the asteroid system) is ecliptic longitude, ecliptic latitude (187°, −53°). These figures indicate that the orbital solution of the secondary and the pole orientation of the system show the timing of eclipse events that correctly correspond with the timing of mutual events observed in the lightcurve data.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Observed lightcurves (red) and model lightcurves (black) for the two overall best-fitting models. The left column is ecliptic longitude, ecliptic latitude (150°, −10°) and a volume-equivalent diameter of ∼7 km; the right column is ecliptic longitude, ecliptic latitude (187°, −53°) and a volume-equivalent diameter of ∼5 km. For each panel, the shape model on the right is the simulated plane-of-sky image as observed during the middle of the observation. Note that lightcurves from different dates have different amplitudes, so these different frames are plotted with different ranges along their y-axes.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Resulting CW (opposite-sense) models for the two overall best-fitting models. (a) and (b) are ecliptic longitude, ecliptic latitude (150°, −10°); (c) and (d) are ecliptic longitude, ecliptic latitude (187°, −53°). The red line is the observation, and the blue line is the model. The 3D model in the top right of each frame shows the plane-of-sky view at the time of observation.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Predictability study of background magnetic field perturbations observed during Enceladus’s flybys and crossings of Enceladus’s orbit by the Cassini spacecraft. Circles show observed magnetic field perturbations calculated as deviation from Saturn’s average time-constant internal field taken at Enceladus’s average distance from Saturn r = r av and colatitude Θ = 90°. Crosses show predicted background field perturbations due to Enceladus’s eccentric orbit at the location of the crossings/flybys and the PPO fields.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Delay-Doppler image collages of model 2. Contrast of delay-Doppler images has been increased for clarity. Time of observation progresses to the right and down, where the first 14 images are from 2017 January 20 and the last 18 images are from 2017 January 23. The first two images are 4 μs, the next three images are 0.5 μs, and the last 27 images are 2 μs baud length; see Table 1 for resolutions. The leftmost panel is the observed delay-Doppler image, the middle panel is the model delay-Doppler image, and the rightmost panel is the multifaceted model, where the purple shaft is the spin axis and the red and green shafts are the principal axes. The black pixels covering the primary’s signal in the delay-Doppler observation and model panels are a pixel mask covering the secondary. Note that the original radar data had different frequency and delay resolutions, but all images have been stretched (along both axes) and cropped so that they are displayed as square frames with a side length corresponding to 9 km. This means that the original delay-Doppler pixels can appear rectangular here.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Delay-Doppler image collages of model 1. Contrast of delay-Doppler images has been increased for clarity. Time of observation progresses to the right and down, where the first 14 images are from 2017 January 20 and the last 18 images are from 2017 January 23. The first two images are 4 μs, the next three images are 0.5 μs, and the last 27 images are 2 μs baud length; see Table 1 for resolutions. The leftmost panel is the observed delay-Doppler image, the middle panel is the model delay-Doppler image, and the rightmost panel is the multifaceted model, where the purple shaft is the spin axis and the red and green shafts are the principal axes. The black pixels covering the primary’s signal in the delay-Doppler observation and model panels are a pixel mask covering the secondary. Note that the original radar data had different frequency and delay resolutions, but all images have been stretched (along both axes) and cropped so that they are displayed as square frames with a side length corresponding to 9 km. This means that the original delay-Doppler pixels can appear rectangular here.
Paper: Analysis of Enceladus’s Time-variable Space Environment to Magnetically Sound its Interior
Authors: Joachim Saur, Stefan Duling, Alexander Grayver, Jamey R. Szalay
Figure caption: Sketch of induction processes at Enceladus. On the left-hand side, three mechanisms generating time-periodic, inducing fields around Enceladus are shown. On the right-hand side, Enceladus’s three main layers, i.e., its icy crust, conducting ocean, and conducting core, are displayed. Within the conductive layers electric currents and induced magnetic fields are generated. The north polar region is particularly well suited for induction studies through spacecraft flybys (Plumes: Image Credit NASA).
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Delay-Doppler image collages of model 1. Contrast of delay-Doppler images has been increased for clarity. Time of observation progresses to the right and down, where the first 14 images are from 2017 January 20 and the last 18 images are from 2017 January 23. The first two images are 4 μs, the next three images are 0.5 μs, and the last 27 images are 2 μs baud length; see Table 1 for resolutions. The leftmost panel is the observed delay-Doppler image, the middle panel is the model delay-Doppler image, and the rightmost panel is the multifaceted model of the primary and the ellipsoidal model of the secondary, where the purple shaft is the spin axis and the red and green shafts are the principal axes. Note that the original radar data had different frequency and delay resolutions, but all images have been stretched (along both axes) and cropped so that they are displayed as square frames with a side length corresponding to 20 km. This means that the original delay-Doppler pixels can appear rectangular here.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Final shape model for Atira with a volume-equivalent diameter of 4.92 ± 0.95 km viewed along the principal axes. Yellow regions indicate facets that were seen at incidence angles greater than 60° (or not seen at all) in all delay-Doppler images and therefore have shape details that are not well constrained. The model shows the asteroid to be relatively round and shows concavities, seen in the +Y and −Y directions viewing from +Z, that most likely produce the characteristic “flat” edge in delay-Doppler images such as the bottom row of panels of Figure 2.
Paper: Physical and Mutual Orbit Characteristics of Near-Earth Binary Asteroid (163693) Atira
Authors: Aaron P. Deleon, Sean E. Marshall, Tracy M. Becker, Petr Pravec, Ellen S. Howell, Michael C. Nolan, Anne K. Virkki, Edgard G. Rivera-Valentín, Patrick A. Taylor, Bryce T. Bolin, Beth Aponte-Hernández, Israel Cabrera, Peter Kušnirák, Kamil Hornoch, Hana Kučáková
Figure caption: Observed lightcurves (red) and model lightcurves (black) of model 1. The observatory is indicated in parentheses in the individual lightcurve titles. For each panel, the shape model on the right is the simulated plane-of-sky image of the binary system as observed during the middle of the observation. Note that lightcurves from different dates have different amplitudes, so these different frames are plotted with different ranges along their y-axes.