adsabs/AstroCLIMB huggingface dataset:
Paper: Putative Methanogenic Biosphere in Enceladus's Deep Ocean: Biomass, Productivity, and Implications for Detection
Authors: Antonin Affholder, François Guyot, Boris Sauterey, Régis Ferrière, Stéphane Mazevet
Figure caption: (a) Standing cell and (b) biomass population estimates. Dark curves are probability density estimates approximated from simulations using the equations in Section 2.2 and parameter values from Table 1. The black solid line uses the prior distributions in Table 2, and the dotted line uses the posterior distribution obtained by sampling simulations that best match escape rates of H2 and CH4 inferred from the Cassini data. The solid line represents the prior estimate, ignoring information from plume abundances of CH4 and H2, while this information is used to refine the estimate for the dotted curve (posterior). The blue region in panel (a) represents the estimates of methanogenic cell abundance in Ray et al. (2021). In panel (b), the biomass of a single average baleen whale is given as an illustration and is taken from Pershing et al. (2010).
Paper: Putative Methanogenic Biosphere in Enceladus's Deep Ocean: Biomass, Productivity, and Implications for Detection
Authors: Antonin Affholder, François Guyot, Boris Sauterey, Régis Ferrière, Stéphane Mazevet
Figure caption: Cell densities in the ocean plume. The solid and dotted black curves are, respectively, the prior and posterior probability density estimates of dead cells’ concentration in water escaping the ML and composing the initial ocean plume. Our baseline assumption is that this sets the concentration throughout the ocean plume, as we assume all the dilution to occur in the ML. The orange dashed line corresponds to the estimate of plausible cell density in the plume from Porco et al. (2017). The blue dashed line represents the calculation in Steel et al. (2017) (≈1011 cells kg−1). The red dashed line highlights the limit of detection (LOD) assumed to design the Orbilander concept (MacKenzie et al. 2021) for reference.
Paper: Putative Methanogenic Biosphere in Enceladus's Deep Ocean: Biomass, Productivity, and Implications for Detection
Authors: Antonin Affholder, François Guyot, Boris Sauterey, Régis Ferrière, Stéphane Mazevet
Figure caption: (a) Total hydrothermal vent productivity; (b) HF specific productivity. Dark curves are probability density estimates approximated from simulations using Equation (22) and parameter values from Table 1. The black solid curve uses the prior distributions in Table 2, and the dotted curve uses the posterior distribution obtained by sampling simulations that best match escape rates of H2 and CH4 observed by the Cassini mission. The vertical dotted line indicates an estimate of the biomass production in the HF and seawater mix around Earth’s hydrothermal vents obtained from computations in McCollom (2000).
Paper: Moonraker: Enceladus Multiple Flyby Mission
Authors: O. Mousis, A. Bouquet, Y. Langevin, N. André, H. Boithias, G. Durry, F. Faye, P. Hartogh, J. Helbert, L. Iess, S. Kempf, A. Masters, F. Postberg, J.-B. Renard, P. Vernazza, A. Vorburger, P. Wurz, D. H. Atkinson, S. Barabash, M. Berthomier, J. Brucato, M. Cable, J. Carter, S. Cazaux, A. Coustenis, G. Danger, V. Dehant, T. Fornaro, P. Garnier, T. Gautier, O. Groussin, L. Z. Hadid, J.-C. Ize, I. Kolmasova, J.-P. Lebreton, S. Le Maistre, E. Lellouch, J. I. Lunine, K. E. Mandt, Z. Martins, D. Mimoun, Q. Nenon, G. M. Muñoz Caro, P. Rannou, H. Rauer, P. Schmitt-Kopplin, A. Schneeberger, M. Simons, K. Stephan, T. Van Hoolst, J. Vaverka, M. Wieser, L. Wörner
Figure caption: Forty-five flybys of Enceladus distributed over two segments (one segment for the nominal mission + one segment for an extended mission). Mission scheme: a first segment (dark blue; A: departure from Titan outbound, B: return to Titan inbound) provides 23 grazing flybys of Enceladus (magenta) over the south polar regions. For an extended mission, a 2:3 inbound–outbound orbit (black) could initiate a second segment (light blue) with 22 flybys shifted 30° clockwise. C: departure from Titan. D: return to Titan for disposal or transition to a new segment initiating a new extended mission.
Paper: Moonraker: Enceladus Multiple Flyby Mission
Authors: O. Mousis, A. Bouquet, Y. Langevin, N. André, H. Boithias, G. Durry, F. Faye, P. Hartogh, J. Helbert, L. Iess, S. Kempf, A. Masters, F. Postberg, J.-B. Renard, P. Vernazza, A. Vorburger, P. Wurz, D. H. Atkinson, S. Barabash, M. Berthomier, J. Brucato, M. Cable, J. Carter, S. Cazaux, A. Coustenis, G. Danger, V. Dehant, T. Fornaro, P. Garnier, T. Gautier, O. Groussin, L. Z. Hadid, J.-C. Ize, I. Kolmasova, J.-P. Lebreton, S. Le Maistre, E. Lellouch, J. I. Lunine, K. E. Mandt, Z. Martins, D. Mimoun, Q. Nenon, G. M. Muñoz Caro, P. Rannou, H. Rauer, P. Schmitt-Kopplin, A. Schneeberger, M. Simons, K. Stephan, T. Van Hoolst, J. Vaverka, M. Wieser, L. Wörner
Figure caption: Main characteristics of Enceladus and its plume as currently understood. Reproduced from Cable et al. (2021), under CC BY license (https://creativecommons.org/licenses/by/4.0/). Background image: PIA20013 (NASA/JPL-Caltech).
Paper: Moonraker: Enceladus Multiple Flyby Mission
Authors: O. Mousis, A. Bouquet, Y. Langevin, N. André, H. Boithias, G. Durry, F. Faye, P. Hartogh, J. Helbert, L. Iess, S. Kempf, A. Masters, F. Postberg, J.-B. Renard, P. Vernazza, A. Vorburger, P. Wurz, D. H. Atkinson, S. Barabash, M. Berthomier, J. Brucato, M. Cable, J. Carter, S. Cazaux, A. Coustenis, G. Danger, V. Dehant, T. Fornaro, P. Garnier, T. Gautier, O. Groussin, L. Z. Hadid, J.-C. Ize, I. Kolmasova, J.-P. Lebreton, S. Le Maistre, E. Lellouch, J. I. Lunine, K. E. Mandt, Z. Martins, D. Mimoun, Q. Nenon, G. M. Muñoz Caro, P. Rannou, H. Rauer, P. Schmitt-Kopplin, A. Schneeberger, M. Simons, K. Stephan, T. Van Hoolst, J. Vaverka, M. Wieser, L. Wörner
Figure caption: Artist view of the Moonraker mission concept. Note that the geometry adopted for the image does not reflect reality. Enceladus orbits in the ring plane. The plume sources are at most 20° of the south pole (Porco et al. 2014) and do not extend as far as 45° as suggested by the rendition.
Paper: Moonraker: Enceladus Multiple Flyby Mission
Authors: O. Mousis, A. Bouquet, Y. Langevin, N. André, H. Boithias, G. Durry, F. Faye, P. Hartogh, J. Helbert, L. Iess, S. Kempf, A. Masters, F. Postberg, J.-B. Renard, P. Vernazza, A. Vorburger, P. Wurz, D. H. Atkinson, S. Barabash, M. Berthomier, J. Brucato, M. Cable, J. Carter, S. Cazaux, A. Coustenis, G. Danger, V. Dehant, T. Fornaro, P. Garnier, T. Gautier, O. Groussin, L. Z. Hadid, J.-C. Ize, I. Kolmasova, J.-P. Lebreton, S. Le Maistre, E. Lellouch, J. I. Lunine, K. E. Mandt, Z. Martins, D. Mimoun, Q. Nenon, G. M. Muñoz Caro, P. Rannou, H. Rauer, P. Schmitt-Kopplin, A. Schneeberger, M. Simons, K. Stephan, T. Van Hoolst, J. Vaverka, M. Wieser, L. Wörner
Figure caption: Moonraker science traceability matrix.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2019 March 9 to 2019 March 11. See the caption of Figure 1 for a description of the content of the panels. The data points from the individual nights and the Fourier series (Equation (1)) fitted to them (outside mutual events) are color-coded in this plot (as well as in Figures 7–10); this is to facilitate seeing the quality of the fit to the data outside events in panel (a), where the data from different nights phased with the orbit period heavily overlap. The red curve is the best-fit secondary light curve; see Section 4. Note that the zero-point time (epoch) for this plot was arbitrarily shifted by −0.25 in orbital phase—the observed secondary events are plotted around orbital phase 0.50 and not 0.75, as in all of the other plots—to show the secondary light-curve variation (outside of mutual events) on one continuous plot; it would break at orbital phase 1.0 if we plotted the events around phase 0.75.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2020 December 12 to 2020 December 23. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2021 January 17 to 2021 January 18. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2021 January 8 to 2021 January 10. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2019 January 31 to 2019 February 2. See the caption of Figure 1 for a description of the content of the panels. Note that in this and subsequent figures showing the high-quality data from 2019 and 2020–2021 with errors around 0.01 mag, we do not plot error bars for the individual data points, as they are comparable to the sizes of the data point symbols.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2017 March 31 to 2017 April 2. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2017 February 23 to 2017 March 1. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2017 April 18 to 2017 May 4. See the caption of Figure 1 for a description of the content of the panels.
Paper: Photometric Observations of the Binary Near-Earth Asteroid (65803) Didymos in 2015–2021 Prior to DART Impact
Authors: P. Pravec, C. A. Thomas, A. S. Rivkin, P. Scheirich, N. Moskovitz, M. M. Knight, C. Snodgrass, J. de León, J. Licandro, M. Popescu, A. Thirouin, D. Föhring, C. O. Chandler, W. J. Oldroyd, C. A. Trujillo, E. S. Howell, S. F. Green, J. Thomas-Osip, S. S. Sheppard, T. L. Farnham, E. Mazzotta Epifani, E. Dotto, S. Ieva, M. Dall'Ora, R. Kokotanekova, B. Carry, D. Souami
Figure caption: Didymos light curve from 2021 January 12 to 2021 January 14. See the caption of Figure 1 for a description of the content of the panels.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Plot of NIR spectra of JD1 (solid black line) and selected RELAB meteorites, minerals, and E-type asteroids. Top left panel: reflectance of aubrites Mayo Belwa (RELAB sample code s1tb46), Khor Temiki (RELAB sample code c1tb48), Bishopville (RELAB sample code c1tb47), Peña Blanca silicate and sulfide regions (RELAB sample codes c1tb45 and c1tb55, respectively), and minerals troilite and Paragould troilite (RELAB sample codes cdmb06 and latb50, respectively). Bottom left panel: NIR blue reflectance of JD1 and aubrite ALH 78113 (RELAB code bkr1ar001). Right panel: JD1 visible and NIR spectra and E-type asteroids (434) Hungaria, (44) Nysa, and (64) Angelina obtained from Binzel et al. (2001), Clark et al. (2004), and Bus & Binzel (2002), respectively, plus an offset in the reflectance for clarity. The NIR reflectance of JD1 was smoothed using a median filter from the Scipy Python package and offset to match the visible reflectance. All of the spectra in the left and right panels were normalized at 1 and 0.55 μm, respectively.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Top panel: Sloan ﹩{g}^{{\prime} }﹩ - ﹩{r}^{{\prime} }﹩ color variation as a function of time since the beginning of the LDT observation. The horizontal dashed blue line and blue shaded area indicate the average ﹩{g}^{{\prime} }﹩ - ﹩{r}^{{\prime} }﹩ color and standard deviation, respectively. Bottom panel: NIR continuum–spectral slope variation as a function of time since the beginning of the observation. Slope variation can be noticed after ∼1.9 hr.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Plot of RELAB meteorite reflectances showing the effect of grain sizes in the NIR slope. Left: reflectance of the aubrite ALH 78113 at different grain sizes (low-iron sample). The RELAB sample codes are bkr1ar001, bkr1ar001a, bkr1ar001b, and bkr1ar001c for ALH 78113 reflectances with grain sizes in the range of “chip” and 125–500, 45–125, and <45 μm, respectively. Right: reflectance spectra of the Mundrabilla meteorite at different grain sizes (iron-rich sample). The RELAB sample codes are cbmb06, ccmb06, cemb06, cfmb06, and c1mb06 for Mundrabilla’s reflectances with grain sizes in the range of 25–45, 45–63, 125–250, 250–500, and <250 μm, respectively. Both meteorites’ spectra become bluer as grain sizes increase.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: The NIR spectral slope as a function of the ﹩{g}^{{\prime} }-{r}^{{\prime} }﹩ Sloan colors (top panel) and geometric albedo (bottom panel) of JD1 (filled circles), E-types (pentagons), M-types (diamonds), ALH 78113 (squares), Peña Blanca aubrites (thick plus signs), Khor Temiki aubrites (thin plus signs), and minerals (triangles). The red line represents a linear relationship between NIR spectral slope (s                      ﹩{}^{{\prime} }﹩) and Sloan ﹩{g}^{{\prime} }-{r}^{{\prime} }﹩ color given by ﹩{{\rm{s}}}^{{\prime} }﹩ = (﹩{g}^{{\prime} }-{r}^{{\prime} }﹩) * (0.969 ± 0.291) −0.453.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: (a) CPRs from Benner et al. (2008) and Aponte-Hernandez et al. (2020) as a function of the Bus–DeMeo taxonomy (DeMeo et al. 2009). (b) CPRs of JD1 as a function of observing days. (c) CPRs of JD1 (black dot), selected E-types (red filled diamonds), and spacecraft-visited NEAs (black filled diamonds). (d) Comparative radar albedos for the asteroids in panel (c). The black and green circles correspond to the OC and total radar albedo of JD1, respectively.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Visible and NIR spectra of JD1 obtained at LCO and LDT. The top and bottom blue solid lines correspond to the featureless nonsmoothed spectra of JD1 obtained at LDT. The red, cyan, green, and blue shaded areas are the ±1σ spectra of X-, Xe-, L-, and B-type asteroids, respectively, from Bus–DeMeo taxonomy. Bus–DeMeo and JD1 visible and NIR spectra have been normalized at 0.55 μm. The gray shaded areas indicate residual telluric features from the data reduction. Both NIR spectra from LDT (blue spectra) have been normalized to unity at 1 μm plus an offset in reflectance for clarity.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Compilation of Arecibo delay-Doppler images of JD1 from 2019 November 3 showing roughly one-sixth of its full rotation. In each frame, the resolution is 7.5 m pixel−1 (vertical) × 0.0745 Hz pixel−1 (horizontal). Each radar image is the weighted sum of 15 consecutive transmit/receive cycles. Time increases from left to right and is indicated at the bottom of each panel.
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Pixel shift of JD1 as a function of time (starting at 01:39:32 UTC). Black and red circles are the delta central aperture position of each spectrum at the A and B slit positions, respectively. The gray shaded area indicates the timing of the largest slit drift (spectral variability occurs after ∼1.9 hr).
Paper: Physical Characterization of 2015 JD1: A Possibly Inhomogeneous Near-Earth Asteroid
Authors: Andy López-Oquendo, David E. Trilling, Annika Gustafsson, Anne Virkki, Edgard G. Rivera-Valentín, Mikael Granvik, Colin Orion Chandler, Joseph Chatelain, Patrick Taylor, Luisa Fernanda-Zambrano
Figure caption: Distribution of echo power as a function of normalized echo depth, made by collapsing the horizontal dimension of the range-Doppler image. The strong signal in at least 20 rows at 7.5 m pixel−1 suggests ∼150 m along the long axis.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Example plot displaying the imaging conditions of available test imagery and the expected TAG imaging conditions for feature R0015. Green circles in the top and bottom panels represent available test images. In the top panel, the purple crosses represent expected image emission and incidence angles on the TAG trajectory where feature R0015 would be used. This shows that the available imagery for testing completely bounded the expected use cases for this feature. On the bottom panel, the blue dotted lines represent the expected TAG GSDs. Images 1−23 exceed the expected TAG GSDs by a factor of 2. As such, these images are not useful for feature evaluation. Images 23−38 have acceptable GSDs for this specific feature, meaning that these images could be valuable for feature evaluation.
Paper: Autonomous Navigation Performance Using Natural Feature Tracking during the OSIRIS-REx Touch-and-Go Sample Collection Event
Authors: C. D. Norman, C. J. Miller, R. D. Olds, C. E. Mario, E. E. Palmer, O. S. Barnouin, M. G. Daly, J. R. Weirich, J. A. Seabrook, C. A. Bennett, B. Rizk, B. J. Bos, D. S. Lauretta
Figure caption: Example plot of correlation score vs. correlation error for feature M0003. The x-axis is the correlation score, or the closeness of match, between each image and this feature. A score of 1 is perfectly correlated, and a score of 0 is uncorrelated. The y-axis shows how closely a feature's detected position matches the correct position in the imagery. Green circles represent primary correlation peaks (highest-scoring matched locations). Blue crosses represent secondary correlation peaks (all other matched locations). The red dotted lines represent the desired thresholds for correlation score and detected position error (x-axis values should be higher and y-axis values should be lower). Well-performing features have a large spread between their primary peak and secondary peak correlation scores, which ensures that a false match is unlikely.