Help Shape the Future of Space Exploration

Join The Planetary Society Now  arrow.png

Join our eNewsletter for updates & action alerts

    Please leave this field empty
Blogs

Headshot of Emily Lakdawalla

DPS 2012: The most detailed images of Uranus' atmosphere ever

Posted by Emily Lakdawalla

22-10-2012 16:14 CDT

Topics: atmospheres, weather and climate, explaining science, optical telescopes, Uranus, explaining image processing

Experience has shown that the most useful way to get through a backlog of notes from a productive conference is to write up the most interesting results in bits and pieces. So here's a nugget from the Thursday afternoon poster session at last week's Division for Planetary Sciences meeting in Reno, Nevada.

Let's begin with this pair of images, which attracted me from several meters away. They were printed on a poster presented by Patrick Fry, Larry Sromovsky, Kathy Rages, Heidi Hammel, and Imke de Pater. It was hard to believe what I was seeing, and as I turned to look for one of the authors, I found another planetary astronomer, Leigh Fletcher, staring at the same pictures in open-mouthed amazement.

High signal-to-noise images of Uranus from Keck II

NASA / ESA / L. A. Sromovsky / P. M. Fry / H. B. Hammel / I. de Pater / K. A. Rages

High signal-to-noise images of Uranus from Keck II
Two specially processed sets of images of Uranus taken from the Keck telescope on July 25 and 26, 2012, reveal astounding level of detail in Uranus' clouds.

You are seeing fine-scale structure in the atmosphere of Uranus, in images containing vastly more detail than anything achieved by Voyager or Hubble. Voyager was handicapped at Uranus and Neptune (not to mention Titan) by its blindness to infrared wavelengths; the opacity of methane at shorter wavelengths frustrated its ability to see even the highest-level cloud structure.

Sitting comfortably on Earth, the adaptive-optics-equipped Keck II telescope employed its NIRC2 camera to take these images. There is astonishing structure visible here. Near the equator, there's a beautifully rhythmic wave structure in one cloud belt. Near the north pole (at right), there's a mottled texture of high clouds and atmospheric holes that looks shockingly similar to an infrared view of Saturn's pole (which I wrote a lengthy post about in May 2010):

Saturn's north polar hexagon

NASA / JPL / U. Arizona

Saturn's north polar hexagon
This image of Saturn's north pole was taken by Cassini's VIMS spectrometer at a mid-infrared wavelength of 5 microns. It was winter at Saturn's north pole; all illumination is thermal radiation (heat) welling up from Saturn's depths. Some of the heat radiation is blocked by clouds floating in Saturn's atmosphere at about 75 kilometers below the cloud tops that can be seen in visible wavelengths. The pressure at that level is about three times Earth's atmospheric pressure. The patterns in the image are created by alternating cloudy and clear areas. The image has been contrast-reversed so that the glouds show up as bright spots, while open areas appear dark.

It was only after a conversation with Larry Sromovsky (involving Leigh as well) that I came to understand how much processing lies behind these "images." Several techniques were required to bring out what are, in fact, very subtle (but clearly coherent) details.

The left image is actually composed of 117 exposures, the right 118. It has become quite common in astronomy to take large numbers of images at a fairly rapid rate and then stack them (or a subset of the sharpest ones) in order to bring out details. "Stacking" essentially means that you carefully align the images and then average them. This method accomplishes two things: it helps reduce the effects of random noise, and it sharpens the images.

Sromovsky explained that they did stack the images, but not before doing some preliminary work. Uranus rotates pretty quickly. The images shown here are about 350 pixels across, so Uranus' circumference is roughly 1000; divide that by the 17-hour rotation rate and you get roughly 60 pixels per hour, or one per minute. The smallest features I see here are a few pixels across; they'd be hopelessly smeared after a few minutes of imaging unless the rotation were accounted for.

That's pretty easy to fix, in a bit of work that's quite common in image processing. You "reproject" the images to flat maps. A view of Uranus from Earth is essentially an orthographic map projection. Convert each image from an orthographic to some cylindrical map projection. Then shift images left or right to account for Uranus' rotation. (I should be able to figure out whether it's left or right as time increases but Uranus, with its upside-down or retrograde-ness, gets me tied up in directional knots and I'd be guaranteed to pick the wrong one.)

But wait, it's more complicated than that. Uranus' visible "surface" is not a solid body; it's a hydrodynamically circulating atmosphere. Like all self-respecting giant planets, its winds move at different rates at different latitudes. So there's a second-order correction that the astronomers had to do, warping the image by shifting lines of pixels at different latitudes left or right, depending upon the observed zonal wind speeds. What are the wind speeds on Uranus? In fact, it's the same group of astronomers who figured out the answer to that question, publishing the (currently) definitive paper on Uranus' wind speeds as observed from cloud motions. Here's the graph:

Uranus' zonal wind speeds

Larry Sromovsky et al., 2009

Uranus' zonal wind speeds
Chart from a 2009 publication about Uranus' wind speeds based upon observations through 2007.

The difference in wind speeds between the northern midlatidues and the equator is 300 meters per second, or about 1000 kilometers per hour. Uranus' circumference is about 300,000 km, so one degree is roughly 1000 km; so for every hour, there's about one degree -- about three pixels' worth -- of shear, moving midlatitude features to the east with respect to equatorial features. This is not as big a correction as the rotational one, but it was clearly significant enough for them to apply it.

Only then did they stack all the images. And even then, one further step was applied. Most of the variation in pixel values in their stacked composite was from broad-scale atmospheric banding. They high-pass filtered the composite to remove the broad features, leaving only the smaller, more local features.

The detail is lovely. But what does it all mean? The answer to that question is: they don't know yet. There are some guesses and hypotheses, but as with everything else in space science, achievement of new detail in observations generates more questions than it does answers. Which is one of the things that makes space science so fun!

 
See other posts from October 2012

 

Or read more blog entries about: atmospheres, weather and climate, explaining science, optical telescopes, Uranus, explaining image processing

Comments:

ranjones: 10/24/2012 09:44 CDT

Love your last sentence! :-D

dougforworldsexplr: 10/27/2012 11:37 CDT

One thing occurred to me after reading your article Emily that I hadn't ever thought of before. For Earth observation we attach great importance to satellites in geostationary orbit. You were mentioning in the article about the rotation or Uranus and the problems for imaging, as also for other planets. Has Nasa or other space agencies conducting any orbiting missions around any other celestial bodies that match their rotation period and were over the same point. This would negate the problems of accounting for rotation but would of course mean only part of the planet could be observed. Also it would need to be determined what part of the planet or celestial body is most interesting. Perhaps 3 or 4 satellites around the celestial body in different directions could be used to watch the whole planet. How much is this being considered?

Emily: 11/13/2012 06:05 CST

@doug: I don't think it's being considered at all. We can't afford to send one spacecraft to Uranus, much less three or four.

Leave a Comment:

You must be logged in to submit a comment. Log in now.
Facebook Twitter Email RSS AddThis

Blog Search

JOIN THE
PLANETARY SOCIETY

Our Curiosity Knows No Bounds!

Become a member of The Planetary Society and together we will create the future of space exploration.

Join Us

Featured Images

Rosetta view of Comet 67P/Churyumov-Gerasimenko on September 14, 2014

What Lies Beneath
MAVEN enters orbit
Finding jets in the September 19, 2014 NavCam image of comet 67P
More Images

Featured Video

View Larger »

Fly to an Asteroid!

Travel to Bennu on the OSIRIS-REx spacecraft!

Send your name

Join the New Millennium Committee

Let’s invent the future together!

Become a Member

Connect With Us

Facebook! Twitter! Google+ and more…
Continue the conversation with our online community!