≡ Menu

WISE 0855: Probing a Brown Dwarf’s Atmosphere

A brown dwarf as a ‘quieter’ version of Jupiter? That’s more or less the picture offered in a new paper on WISE 0855 from Andrew Skemer (UC-Santa Cruz) and colleagues. Here we’re working in the Solar System’s close neighborhood — WISE 0855 is a scant 7.2 light years from Earth — and we’re observing an object that is the coldest known outside of the Solar System. That makes the observational task difficult, but it has yielded rich results in the discovery of clouds of water or water ice.

We learn that WISE 0855 is about five times the mass of Jupiter, with a temperature in the range of 250 K (-23 Celsius). This is the nearest known object of planetary mass, but it is too faint to characterize with conventional spectroscopy — separating light into its component wavelengths — in the optical or near infrared. But it turns out the object can be studied through thermal emissions from deep in its atmosphere in the range of 5 µm (a range frequently used to study Jupiter’s own deep thermal emissions). Skemer calls spectroscopy of such a faint object in this 5 µm ‘window’ “challenging but not impossible.”

And while we have no current space observatories that can perform 5 µm spectroscopy, we can use ground-based instruments working through the 4.5-5.2 µm atmospheric window of our own planet, although the target is a dim object indeed and observations are limited by the brightness of the Earth’s sky. WISE 0855 becomes the faintest object yet detected with ground-based 5 µm spectroscopy, fully five times fainter than the previous such detection.

The observations were performed with the Gemini-North telescope and the Gemini Near Infrared Spectrograph at Mauna Kea, where the infrared background is the lowest for any telescope of its class. Skemer and team observed WISE 0855 over a thirteen night period for a total of about 14 hours. The resulting spectrum reveals the presence of atmospheric water vapor and clouds. The results depict an object with an appearance similar to Jupiter, a place that fits the team’s calculations involving an atmosphere dominated by water vapor.

wise-image-400

Image: Artist’s rendering of WISE 0855 as it might appear if viewed up close in infrared light. Credit: Joy Pollard, Gemini Observatory/AURA.

The cloud models used here make no assumptions about the composition of cloud being observed, but the paper notes that the temperature of WISE 0855 is such that a composition of water or water ice is likely. Even so, the authors add that the fit of their cloudy model to the observations is not exact, suggesting that there is further complexity here, perhaps involving the vertical and horizontal structure of the clouds, which would affect the brown dwarf’s appearance.

How to move forward from these results? The paper suggests the following:

To understand the nature of clouds and vertical mixing in cold gas giants, we need 5 µm spectra of objects across a continuum of temperatures. After Jupiter (130 K) and WISE 0855 (250 K), the next coldest object with a 5 µm spectrum is Gl 570D (700 K) (Sorahana & Yamamura 2012). In the near term, ground-based telescopes have the sensitivity to obtain spectra of a handful of objects in this temperature range. Future facilities, like the James Webb Space Telescope (JWST), will have the sensitivity to characterize cold gas giants with higher precision, and at wavelengths not possible from Earth (Morley et al. 2014).

As mentioned above, it will be interesting to see what we can learn about Gl 570D, which is a cool brown dwarf about 1500 AU from the triple star system Gl 570, itself composed of a K-class dwarf separated by 190 AU from two red dwarfs that orbit the primary. The brown dwarf here has an estimated mass about 50 times greater than Jupiter and a temperature of about 700 K. The system is approximately 19 light years from Earth.

And we should bear in mind that next-generation Earth-based telescopes (the so-called Extremely Large Telescopes, or ELTs) will have the ability to study large samples of exoplanets in the 5 µm atmospheric window, allowing us to compare not just them but brown dwarfs of various sizes and temperatures with the gas giants here in the Solar System.

Given WISE 0855’s similarities to Jupiter especially regarding the water absorption features in its spectrum, it’s interesting to note the differences. The researchers found that the spectrum of WISE 0855 does not show a strong phosphine (PH3) signal:

If WISE 0855 had Jupiter’s abundance of PH3, it would easily be visible in our spectrum. The fact that WISE 0855 has less PH3 than Jupiter most likely implies that WISE 0855 has less turbulent mixing than Jupiter, although atmospheric metallicity and gravity may also play a role.

So we have a less turbulent atmosphere than Jupiter’s on a cloudy world that probably looks much like the giant planet. We’re probing dynamical and chemical features of an ultra-cool brown dwarf, characteristics we have long studied in our own gas giants. Lacking the mass to spark fusion following the gravitational collapse of the original proto-stellar cloud, WISE 0855 is an ‘almost star’ that may eventually teach us much about the formation of such objects as we expand our range of observations to perform similar studies of gas giant exoplanets.

The paper is Skemer et al., “The First Spectrum of the Coldest Brown Dwarf,” accepted at Astrophysical Journal Letters (preprint). A UC-Santa Cruz news release is available.

tzf_img_post

Comments on this entry are closed.

  • Stan Erickson July 11, 2016, 12:38

    This confuses me. Wiki ‘Brown Dwarfs’ says the term is used for objects greater than 13 MJ, and implies the separation is that these objects can fuse deuterium. The object mentioned here is 5 MJ. Did the definition change when I wasn’t looking?

    • Paul Gilster July 11, 2016, 13:55

      The authors give a nod to this: “Deuterium is expected to be quickly depleted by fusion in objects more massive than ∼13 Mjup, a boundary commonly used to separate planets from brown dwarfs.”

      The other distinguishing factor, though, seems to be how the object developed, with WISE 0855 believed to have formed as a solitary brown dwarf rather than as a planet around a star in a system from which it was ejected. In other words, it would have formed from a collapsing cloud of interstellar materials rather than, as a planet, by accumulating gas and dust inside a star’s circumstellar disk. I assume that’s the distinction being used to call this a ‘brown dwarf.’

      • Joy July 11, 2016, 14:40

        I understand their argument but find it quite thin. This is an old cold object. Any assertions about the formation history of this object are nothing more than unsupported speculations. It has a gas giant planetary mass, that much is clear.

        • Michael T July 13, 2016, 22:54

          I have the same issue with the terminology.
          Brown dwarfs fuse deuterium. This object doesn’t fuse anything. It is less than half the theoretical size minimum for a brown dwarf. The very adjective “Brown” indicates (to me) some active energy production producing a glow, and a linguistic extension from “red” dwarfs. Yes I know gravitation can do this too, but then ANY planet could be called a “dwarf star”.

          It would be better to call this a lone planet IMO.

  • Michael July 11, 2016, 13:16

    Just wondering if techaliens inhabitated a moon around a massive BD if they could cause pulsed fusion with a high powered laser as the density of BD can get quite high.

    • Harry R Ray July 11, 2016, 16:00

      Just wondering if we could TEASE OUT a moon*(more on this later)transiting WISE 0855 by COMBINING ALL OF THE EXISTING DATA! If we CAN, and we DO, would a sattilite orbiting a BELOW THE 13MJ BDTHRESHOLD be called a planet, moon, or SOMETHING ELSE! The way the IAU usually COMPROMISES with this kind of sticky situation, it would probably be called something in the line of “planetoid”!

      • Moebius July 12, 2016, 8:08

        Let’s call that a “Ploon”

  • Hop David July 11, 2016, 14:46

    Top of my wish list is a WISE 2.0 parked at Sun-Earth L2.

    At L2 a small shade suffices to block heat from the sun earth and moon. It is much less difficult to keep cold.

    A wide field infra red scope is not only good for hunting brown dwarfs, but also finding and characterizing the smaller near earth asteroids in our immediate neighborhood. Observing a rock with infra red and visual wavelengths at the same time gives us a notion of the body’s albedo. When we know albedo, the rock’s apparent magnitude allows us to estimate the asteroid’s size.

    It’d be good to get a good inventory of the potential city killers (Tunguska to Chelyabinsk sized rocks). The info would also be helpful to companies who hoped to utilize asteroids (Planetary Resources and Deep Space Industries).