adsabs/AstroCLIMB huggingface dataset:
Paper: Size Distribution of Small Grains in the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina
Figure caption: (a) Percent change in the impact amplitude due to the finite cadence of 8 hr impact rate intervals and due to the possible eccentricity of the grains. For each effect, six curves are shown corresponding to β = 0−0.5. (b) Power-law envelopes to the family of normalized mass-dependent impact charge curves for heliocentric distances of 0.11 and 0.24 au.
Paper: Size Distribution of Small Grains in the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina
Figure caption: Size distribution of collisional fragments. Left: differential mass distributions, with α = 1.1  to 1.4 highlighted in black and the largest fragment size marked with the vertical dashed lines. Right: visual representation of fragments, with the single largest fragment in the center and the size of the largest size fragment denoted below each. The fragments that are 1/2 and 1/4 of the largest fragment size are shown in different shades, with the number of circles proportional to their size distribution. Red indicates where the majority of fragment mass resides, where the largest grains carry the mass for α < 1 and the smallest grains carry the mass for α > 1.
Paper: Size Distribution of Small Grains in the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina
Figure caption: Distribution of fragmentation products depending on the cumulative mass index. Fragments with α > 1 have most of the mass distributed into small grains, while for α < 1 the majority of mass is distributed into the few largest fragments.
Paper: Size Distribution of Small Grains in the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina
Figure caption: Maximum fragment cutoff size as a function of minimum fragment size and cumulative mass index α. The shaded region shows the average cumulative mass indices found to be consistent with the near-Sun environment.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Dufay region with a water + hydroxyl anomaly, located near 7.°7N, 170.°3E. (a) NIR apparent reflectance. (b) 2.8 μm OH map. (c) 3 μm water absorption map. (d) Color composite of 2 μm pyroxene absorption (red), OH (green), and water (blue). Note that the water signature has sharp boundaries at both the anomaly and Dufay Y, whereas the OH at the anomaly is more diffuse. The derived OH spectral feature type map (Figure 6) shows a yellow core surrounded by red/orange. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: A small farside crater near 32.°6N, 143.°6E, northwest of Moscoviense, and representative spectra. Top, left to right: M3 reflectance, 3 μm water band depth, and 2.8 μm OH band depth. Bottom: spectra from the locations in the top left panel show (A) low water, (B) water with 2.8 μm OH band, and (C) another location with water with less OH. The dashed lines (offset) show the spectra before thermal emission. Thermal emission has little effect on the observed band depths. Note that the 2.8 μm absorption produces a different spatial pattern than the water absorption. This geologically fresh crater shows evidence for excavation of water- and hydroxyl-rich materials from depth. Scale is 0.33 km pixel−1.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Compton crater and the Compton–Belkovich volcanic complex (upper left, near 61.°1N, 99.°6E). (a) NIR apparent reflectance. (b) 2.8 μm OH map. (c) 3 μm water absorption map. (d) Color composite of NIR reflectance (red), OH (green), and water (blue). The small circle in panel (a) marks the spot where water and OH-rich streamers appear to converge. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Region near 40°N, 130°E on the lunar farside. (Top) NIR apparent reflectance. (Bottom) 2.8 μm OH map. Small fresh craters have penetrated through a surface layer of OH-rich regolith. The OH becomes more diffuse with time. The slow erasing of the craters in the OH spectral signatures creates diffuse arcs following the crater rims. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         Bullialdus region map with the six OH band positions from Figure 6. The colors match the spectra from Figure 4(b). This is an enlargement from Figure 6 and shown at the full 0.33 km pixel−1 resolution of the mosaicked data. On the top is a blend of NIR apparent reflectance and the hydroxyl map. On the bottom is the hydroxyl map unmodified. The yellow zone corresponds to the central peak. The orange/red around the yellow zone appears to be weathering of the hydroxyl materials. Note the similar hydroxyl type (yellow/orange) to the east–southeast of Bullialdus. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Water-rich region near 45°N, 52°E. (a) NIR apparent reflectance. (b) 2.8 μm OH map. (c) 3 μm water absorption map. (d) Color composite of NIR reflectance (red), OH (green), and water (blue). The region shows units with sharp boundaries of water but a general background of 2.8 μm OH. Note the fresh water-rich crater at upper left, which is 2.8 μm OH-poor. This and other small craters have penetrated through a surface layer of OH-rich regolith. Note the variations in OH intensity from older craters and how the crater rims become more diffuse with age. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         Hydroxyl map with the six OH band positions from Figure 6 for the crater Genimus, near 34.°5N, 56.°7E, north of Mare Crisium. This region contains relatively abundant water (Figure 5(a)). The colors match the spectra from Figure 4(b). This is an enlargement from Figure 6 and shown at the full 0.33 km pixel−1 resolution of the mosaicked data. On the left is a blend of NIR apparent reflectance and the hydroxyl map. On the right is the hydroxyl map unmodified. The yellow zone corresponds to the crater rim. The orange/red around the yellow zone appears to be general background hydroxyl. Scale is 0.33 km pixel−1. North is up.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption: Absorption bands detected in the 2–2.5 μm region. This colored map is a Tetracorder standard product. While mineral names are given for the reference spectra used by Tetracorder, the spectral resolution of the M3 global mode is insufficient to make specific identifications. These are very weak absorptions, typically less than 1% band depth. The main detection is near 2.2 μm, and that position and shape are common in montmorillonite group absorptions (smectites) due to an Al–OH plus OH stretch–bend combination band, though, again, at the spectral resolution of the M3 global mode, specific mineral identifications are uncertain. The 2.2 μm absorption signature increases toward the poles. North is up in this simple cylindrical map.
Paper: The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
Authors: Roger N. Clark, Neil C. Pearson, Thomas B. McCord, Deborah L. Domingue, Keith Eric Livo, Joseph W. Boardman, Daniel P. Moriarty, Amanda R. Hendrix, Georgiana Kramer, Maria E. Banks
Figure caption:                         Copernicus region map with the six OH band positions from Figure 6 and colors matching the spectra from Figure 4(b). See water in this crater in Figure 5(b). Left: OH on a reflectance background for better context. Right: OH map only. The yellow zone corresponds to the melt sheet from the cratering event dominated by hydroxyl at 2.81 μm. The orange/red around the yellow zone appears to be weathering of the hydroxyl materials. Scale is 0.33 km pixel−1. North is up.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Infrared spectra obtained from the RELAB database for carbonates that could be present on the surface of Ceres. Most carbonates include an absorption band between 3.3 and 3.6 μm, complicating the identification of the 3.4 μm band characteristic of aliphatic organics when both are present. Vertical gray bars represent regions of the detector affected by the filter junctions (M. C. De Sanctis et al. 2011).
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: The left panel displays an FC2 image showcasing the Ernutet crater, where organics have been detected. The red and gray squares correspond to organic-rich and nonorganic-rich areas, respectively. On the right panel, the VIR spectra of these areas are presented, utilizing the same color scheme and with an offset for clarity. Within the organic-rich area, the red spectrum exhibits a distinctive absorption band near 3.4 μm. Ranging from 3.3 to 3.6 μm, the wavelengths display an asymmetrical shape with numerous subfeatures, highlighted here by prominent black dashed vertical bars around 3.38–3.39 μm and 3.40–3.42 μm, indicative of aliphatic hydrocarbons (M. C. De Sanctis et al. 2017).
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Top panel: FC2 spectral endmember O (organic-rich), B (global Ceres background), and S (shade), respectively. Bottom panel: RGB map where the abundance of the endmember O is represented in red, the endmember B in green, and the S in blue. The pixel scale of this mosaic is ∼136 m pixel−1, and the images were acquired with a phase value of ∼50. Ernutet is the central crater (pointed out by the yellow arrow) of the scene in which the organics are visible.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: (a) Areas rich in aliphatic organics (red) obtained after applying SMA (Figure 2), overlaid on an FC2 mosaic with XMO images. The Ernutet crater is pointed out by the yellow arrow. The color-coded stars indicate areas of higher concentration of the organics-rich endmember in the outer region in the southwest of Ernutet. The yellow line marks the rim of the ancient crater on which Ernutet is superposed. (b) Same as panel (a), but using a clear filter image with a different viewing geometry, thereby allowing for a better appreciation of the spatial distribution relative to the older crater. The higher concentrations of the organic-rich endmember within the degraded crater could be related to the unearthing of deeper-seated material by the ancient impact. Additionally, subsequent smaller impacts may have further exposed the underlying material, as Ernutet’s ejecta concealed the older crater entirely.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Regions that are candidates to harbor organics according to the SMA algorithm and FC2 data. The images are oriented with north and east pointing up and to the left, respectively. Except for candidates 4 (panel (c)) and 8 (panel (g)), all are found either inside or on the wall of craters. However, the analyses carried out with the VIR spectrometer are not conclusive, and thus the presence of organics cannot be confirmed in these 10 locations. The colors are as in Figure 3.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: (a) Mosaic built from FC2 clear filter images of the region (centered at Yalode quadrangle) where organics candidates are suggested. The region outlined in red delimits the area of the FC2 color filters used in this work. (b) RGB map of Yalode quadrangle where the O endmember has been identified (∼136 m pixel−1). The abundance of the O endmember is represented in red, the B endmember in green, and the S in blue. Bright spots BS1, BS2, and BS3 show the highest abundance of potential organics, but there are also potential organics scattered in the layer over the adjacent north area.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Global RGB map for qualitative analysis of the role played by the carbonates identified between the Urvara and Yalode basins compared to the rest of Ceres’s carbonates. We observe that this region bears a closer resemblance to the Ernutet crater and Urvara (where organics are present) than to the other carbonate-rich regions. In this figure, R corresponds to the band depth at 3.95 μm, G to the band depth at 2.7 μm, and B to the center of the 3.95 μm band.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Ceres surface global map in which we indicate the candidate organic regions. Yellow stars indicate the Ernutet crater (1) and the Urvara basin (11), where organics have previously been identified (M. C. De Sanctis et al. 2011, A. Nathues et al. 2022). In red is the region where we have identified a new organic region, located in the Yalode quadrangle. Green stars mark locations where SMA suggested that organics may exist, but this cannot be confirmed because they lack 3.4 μm absorptions. Credits for background map: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Abundance map of the endmember O (representative of aliphatic organics) in the Ernutet crater with a pixel scale of 36 m pixel−1 (XMO6 phase images).
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Bright spots BS1, BS2, and BS3 using FC2 clear filter images, with a pixel scale of ∼36 m pixel−1. The bright spots extend several meters. The inset on the right is a zoom-in of the area of interest, where the contrast has been modified for better visualization.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: FC2 spectra of the bright spots identified in Yalode, along with the average spectrum of Ceres (gray) and the Ernutet organics spectrum (red). All spectra are normalized at 653 nm.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: VIR spectra for bright spots BS1 (left), BS2 (middle), and BS3 (right). In all cases an absorption band centered at 3.4 and 3.95 μm is present.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Center vs. depth of the 3.95 μm band (modified from F. G. Carrozzo et al. 2018). The bright spots BS1 and BS2 form a distinct group along with the carbonates from the Ernutet crater and the Urvara basin. The gray point represents the average Ceres surface. BS3 is not in this data set.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: (a) Comparison of the spectra of the three bright spots identified between the Urvara and Yalode basins with the organic matter identified in the Ernutet crater. Spectra are normalized at 2.6 μm and presented with an offset for clarity. (b) Same as panel (a), but zoomed into the 3.2–3.6 μm range, and including the antigorite and dolomite for comparison. The dashed vertical lines indicate the most prominent absorptions. The bright spots’ spectra are compatible with a mixture of the organic matter discovered in Ernutet plus dolomite.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: (a) Shadeless spectra from 10 locations across the scene (Yalode–Urvara region; see Figure A4 for details on the locations) with different endmember abundances. (b) Hyperspectral endmembers obtained after applying Equation (2). The red line corresponds to the carbonates/organics compound, and the blue line represents the Ceres background. The blue dashed line indicates the location of the 3.4 μm absorption feature.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: 3.4 μm absorption band map computed through the extrapolated data set. Pixel scale ∼136 m pixel−1.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Geologic units from the Yalode and Urvara quadrangles (modified from D. A. Crown et al. 2018). In black lines, we delimit the region covered by the FC2 color filters used in this work. The black arrow points toward the identified SB1, BS2, and BS3 organics candidates, all of which are located in the Urvara/Yalode smooth material. The green arrow on the left indicates the area in which the presence of organics has been proposed by A. Nathues et al. (2022), inside the Urvara basin.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: (a) Same as Figure 16, but zoomed in on BS2, showing the distribution of the 3.4 μm absorption band of the possible organics. This material has a horseshoe-shaped distribution. (b) Same area as seen by the FC2 clear filter for contextualization. No ancient crater or geological feature is aligned with this distribution.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Top panel: the extrapolated data set combining FC2 (pixel scale of ∼136 m pixel−1) with VIR in the Yalode region. Bottom panel: mosaic using VIR IR data of the same region as in the top panel (with the area of the extrapolated data set outlined in red), exemplifying how the submaps present neither a homogeneous pixel scale nor viewing geometry. In both panels, we present the I/F at 2 μm because there are no distinct spectral features in this range.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Fractional abundance maps obtained after applying the SMA in the FC2 mosaic over the Ernutet area.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Fractional abundance maps obtained after applying the SMA in the FC2 mosaic over the XMO images from the Ernutet region.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Color composite of three fractional abundance maps of the Yalode–Urvara region. Locations for representative spectra (presented in Figure A5) are shown.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Measurement of VIR spectra for each one of the locations indicated in Figure A4. Each panel includes the number of pixels occupied by both FC2 and VIR, the fractional abundance of each endmember, and the geocentric coordinates. The vertical blue line is located at 3.4 μm.
Paper: New Candidates for Organic-rich Regions on Ceres
Authors: J. L. Rizos, J. M. Sunshine, R. T. Daly, A. Nathues, C. De Sanctis, A. Raponi, J. H. Pasckert, T. L. Farnham, J. Kloos, J. L. Ortiz
Figure caption: Fractional abundance maps obtained after applying the SMA in the FC2 mosaic over the Yalode and Urvara basins.
Paper: Size Distribution of Small Grains in the Inner Zodiacal Cloud
Authors: J. R. Szalay, P. Pokorný, D. M. Malaspina
Figure caption: Impact rates for PSP’s first 17 orbits. (a) Top-down view in ecliptic J2000 coordinates, where rates within each orbital group are averaged. The innermost location of the Helios dust measurements (E. Grün et al. 1980) outside 0.3 au is also indicated. (b, c) Time series of each orbit as a function of days from perihelion, where the color bar in panel (b) is shared with that of panel (a).