Comet studied at Three Wavelengths

Principal investigator Diane Wooden of NASA’s Ames Research Center, who had proposed that Comet ISON be studied at three infrared wavelengths – 11.1, 19.7, and 31.5 microns, was aboard the Oct. 24 SOFIA flight. Two of those wavelengths, 19.7 and 31.5 microns, cannot be seen from Earth-based telescopes because water vapor in Earth’s atmosphere blocks infrared energy from reaching the ground. The 31.5-micron wavelength was detected simultaneously with the 11.1 and 19.7-micron images.

The 11.1-micron wavelength allows the SOFIA observations to be tied to ground-based measurements with the Subaru Telescope on Mauna Kea, Hawaii, and the Great Canary Telescope on the island of La Palma, in Spain’s Canary Islands. Currently, there are no space-borne telescopes operating at wavelengths longer than 4.5 microns, making SOFIA the only telescope able to see these limited wavelengths.

Wooden, who made more than 75 flights on SOFIA’s predecessor, the Kuiper Airborne Observatory, is working with a diverse team that will combine its numerous observations to better understand the composition of Comet ISON. Her observations aboard SOFIA were to measure the thermal emission from small and large dust grains in the coma of Comet ISON by measuring the mid-infrared wavelengths with the Faint Object InfraRed CAmera for the SOFIA Telescope (FORCAST) instrument. FORCAST collects infrared photons at wavelengths between five- and 40-microns.

“The long wavelength photometry, only possible from SOFIA, will allow us to measure the thermal emission from larger grains, which cannot be seen in scattered light at visible wavelengths,” said Wooden. “Compared with smaller submicron grains, larger grains have cooler temperatures and emit at longer wavelengths.

“Only the FORCAST instrument on SOFIA can obtain the longer wavelength photometry measurements that sample the thermal emission of the larger grains,” she explained. “By modeling the FORCAST photometry, we can constrain the grain size distribution and the dust mass. The mass and loss rate of the dust are one of the fundamental characterizations of a comet.”

Making the Observations

“When we got onto the comet leg of the flight, we clearly saw the extended coma in the fine guiding camera but not in the wide-angle camera,” Wooden said. “We acquired images at 11.1 microns and immediately saw the comet was faint. We then shifted to the 19.7-micron filter, where the comet was expected to be brighter.

“Soon we could see the comet was about as weak at 19.7 microns as it was 11.1 microns, consistent with the expectations of a typical grain-size distribution, Wooden continued. “If the 19.7-micron images had a stronger signal, that would have meant there were more, larger grains.

Wooden said these measurements are important because they serve as constraints or upper limits on the flux of thermal emissions from larger dust grains in the coma.

“Studying the dust’s thermal emission from SOFIA enables us to derive the grain size, its distribution, and the mass of the amount of dust coming from the comet,” she said. “This is a critical complement to studying the gases that are released, and thereby contributes significantly to understanding the origins of comets.

“We learned that the comet is dust-poor not only for small grains, as already known by the weak scattered light at visible wavelengths, but also for larger grains detectable at these mid-IR wavelengths from SOFIA,” Wooden concluded.

Nicholas A. Veronico, SOFIA Public Affairs
NASA Ames Research Center

SOURCE: NASA