Saturn’s faint outermost ring, discovered in 2009 (ref. 1), is probably formed by particles ejected from the distant moon Phoebe2,3. The ring was detected1 between distances of 128 and 207 Saturn radii (RS = 60,330 kilometres) from the planet, with a full vertical extent of 40RS, making it well over ten times larger than Saturn’s hitherto largest known ring, the E ring. The total radial extent of the Phoebe ring could not, however, be determined at that time, nor could particle sizes be significantly constrained. Here we report infrared imaging of the entire ring, which extends from 100RS out to a surprisingly distant 270RS. We model the orbital dynamics of ring particles launched from Phoebe, and construct theoretical power-law profiles of the particle size distribution. We find that very steep profiles fit the data best, and that elevated grain temperatures, arising because of the radiative inefficiency of the smallest grains, probably contribute to the steepness. By converting our constraint on particle sizes into a form that is independent of the uncertain size distribution, we determine that particles with radii greater than ten centimetres, whose orbits do not decay appreciably inward over 4.5 billion years, contribute at most about ten per cent to the cross-sectional area of the ring’s dusty component.
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This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research was supported by grants from NASA Outer Planets and Origins (D.P.H.).
The authors declare no competing financial interests.
Extended data figures and tables
We organize these nine independent images so that each row contains three images centred at approximately the same ecliptic latitude (vertical direction). For each row, spacecraft orbital precession shifts Saturn in the ecliptic longitude direction so that the planet moves from left to right. The vertical ring extent is about 50 pixels and the horizontal extent exceeds 200 pixels, so even the single exposures can be binned to yield modest signal to noise ratio on the ring.
The image is rotated so that ecliptic north is up and east is to the left. In this Atlas Image, the bright emission from Saturn is outside the WISE field of view, but one of its diffraction spikes is visible at top right; processing artefacts to the bottom left and right should be ignored. The ring flux (horizontal stripe) is uncontaminated by Saturn’s scattered light, although the orbital motion of Saturn smears the embedded image of Phoebe into a bright oval. The faint point sources are distant stars and galaxies.
Each selected Level 1B image was free from significant artefacts from Saturn’s scattered light. The frames have been shifted, offset to a common background level and stacked with trimmed average pixel filtering in Saturn’s frame of reference (so that Phoebe, the point source on the east/left side of the ring, appears unsmeared). Ecliptic north is up and east is to the left. Green lines highlight the regions used for flux extraction.
a, Direct image of the star. b, The same image rotated by 90° and subtracted from itself mitigating scattered light. The large blob-shaped artefacts up, down, left and right from the central star are due to the reflection of starlight from the telescope’s internal structure. Significant artefacts from azimuthally asymmetric scattered flux near the star, by contrast, are not evident in the subtracted image b. Residuals after subtraction arise largely from frame offset mismatch and are typically of order 0.2 DN in the image in b (compared with 3 DN for the ring flux at 160RS).
a, A WISE Band 3 (12 μm) optimally frame-matched mosaic oriented in ecliptic coordinates with north up and east to the left. b, Band 4 (22 μm) optimally frame-matched mosaic. The ring is evident in the middle of the Band 4 image, extending left and right horizontally from the central white over-exposed image of Saturn. The backgrounds are largely uniform, especially in Band 4, with the exception of a north–south gradient characteristic of zodiacal dust emission. Ring flux is not obviously evident in the 12 μm Band 3 exposure.
This figure plots the average background level in DN (vertical axis) row-by-row (horizontal axis) in the Band 4 image shown in Extended Data Fig. 5. The analysis region slightly overlaps the ring flux, which appears as the small bump around line 3300 and establishes the ring plane. The sense of the rotation used in the 90° subtraction carries flux from line numbers 3500–4000 into the ring midplane. Because the DN values are so similar, the bias introduced by the rotation is no greater than 0.1 DN while the inner ring flux is of order 6 DN.
Mosaics of images in WISE Bands 2, 3 and 4 (4.6, 12 and 22 μm) comprise the composite image in ecliptic coordinates. North is up and east is to the left. Scattered light from Saturn forms the bright white circle at the centre of the image and the ring is the faint horizontal bar that cuts across Saturn.
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Hamilton, D., Skrutskie, M., Verbiscer, A. et al. Small particles dominate Saturn’s Phoebe ring to surprisingly large distances. Nature 522, 185–187 (2015). https://doi.org/10.1038/nature14476
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