≡ Menu

Tight Constraints on Orbit of a Transiting ‘Super-Earth’

The super-Earth K2-3d orbits a red dwarf star in the constellation Leo, some 150 light years from Earth. The outermost of three planets discovered in the system, K2-3d was found in the K2 phase of the Kepler mission (K2 Second Light), following the issues with the spacecraft’s reaction wheels that led to the end of the primary mission. Interestingly, while the planet is large (with a radius 1.5 times that of Earth), its density is high and indicative of a solid surface (we can measure the radius of K2-3d by studying the transit light curve, while radial velocity methods yield the planet’s mass, allowing astronomers to calculate its density).

Given the right atmospheric parameters, liquid water could exist here, although most models show a tidally locked world receiving too much solar flux (1.4 times that of the Earth) to make habitable conditions likely. With an orbital period of 45 days, K2-3d’s transits are interesting because the planet is close enough to be a useful candidate for follow-up study with next generation telescopes. Transmission spectroscopy will allow us to study its atmosphere as starlight filters through it during a transit, opening up the possibility of searching for potential biosignatures.

But transits have to be observed to make such studies, and that means we must refine the transit ephemeris, which gives us needed parameters about when the planet will cross the face of its star as seen from Earth. The problem here is that we originally had only two transits to work with because the K2 mission surveys each area of the sky for a limited period of time. But an additional two transits were added soon after the planet’s discovery using data from the Spitzer Space Telescope, yielding a total of four measurements.

Now a team from the National Astronomical Observatory of Japan (NAOJ) and the University of Tokyo has used the MuSCAT (Multi-color Simultaneous Camera for studying Atmospheres of Transiting planets) instrument on the Okayama Astrophysical Observatory’s 188-cm telescope to produce the first transit data on K2-3d from a ground-based telescope. This fifth transit has refined the orbital period of K2-3d to within about 18 seconds, setting up future transit observations of a world on the inner edge of its star’s habitable zone.

k2-3d_fig3_en_s

Image: Predicted transit time deviation from the improved K2-3d transit ephemeris based on this research. The solid red line indicates the predicted times based on this research, the shaded area shows the uncertainty range. Squares, triangles, and circles are respectively the transit time data from the Kepler Telescope, Spitzer Space Telescope, and the latest observing instrument MuSCAT on the Okayama 188-cm Reflector Telescope. Gray marks show the values calculated in previous research and black marks represent the values re-calculated in this research. Purple and orange dotted lines are the transit ephemerides calculated in previous research using the K2 and the K2+Spitzer data, respectively. This research succeeded in correcting the predictions for the 2018 transit times by more than an hour. (credit: NAOJ).

The decrease in brightness of the host star as K2-3d transits is small, but the next generation of large telescopes should have plenty to work with. From the paper:

The transit depth of K2-3d is the second shallowest among those observed by ground-based telescopes, following 55 Cnc e (0.4 mmag transit observed by the 2.5m Nordic Optical Telescope, de Mooij et al. 2014). Our observation demonstrates that ground-based photometric observations can play an important role in improving the transit ephemeris of small-sized, long-period planets, including potentially habitable ones, discovered by ongoing and future space-based transit surveys such as K2 and the Transiting Exoplanet Survey Satellite (Ricker et al. 2015), whose survey durations are limited.

K2-3d will not be the last transiting planet discovered by K2, which continues its mission until at least February of 2018, and as the paper notes, we can look forward to the Transiting Exoplanet Survey Satellite (TESS), scheduled for launch in December of 2017. While K2-3d is a useful addition to the catalog, we will likely find numerous small planets even closer for follow-up studies of their atmosphere. Ground-based observations to measure the ephemerides of transiting planets will be crucial as we bulk up our catalog of nearby worlds.

The paper is Fukui et al., “Ground-based Transit Observation of the Habitable-zone Super-Earth K2-3d,” Astronomical Journal 21 November 2016 (abstract / preprint).

tzf_img_post

Comments on this entry are closed.

  • DJ Kaplan November 30, 2016, 13:11

    I wonder how we would – if at all – determine if any of these red dwarf exoplanets are actually tidally locked.

  • RobFlores November 30, 2016, 13:26

    What would be the most benign Tide Locked world orbiting a M type star, that we could encounter find out there? This world would not be that highly rated on a scale of such benigness.

    If a tide locked world was found with greenland sized continents at the poles and a tropical mid latitude ocean belt. My guess is that would be the closest to Earth like conditions these M star systems are likely to get.. But you would still have use substantial amount of shielding in habitats for humans to reside there, Food crops would have to withstand a few days of no sunlight and hard solar radiation. But at least at the poles the atmospheric differential heating would not cause such extreme winds compared to equatorial regions, but there would be strong winds.

  • Marshall Eubanks November 30, 2016, 14:12

    Now we can look for additional (non-transiting) planets through the timing of future transits by ground-based telescopes – additional planets will perturb the orbit of K2-3d and thus change the transit timings – see

    https://en.wikipedia.org/wiki/Transit-timing_variation

    for some references on this technique.

  • Ashley Baldwin November 30, 2016, 14:26

    It’s unlikely TESS with predominantly 40 day observation windows ( admittedly getting much longer the nearer to the ecliptic poles where windows overlap) can offer here but launched next year too ( hopefully for both ) 0.32 m ChEOPS is designed for just such work , though lying in a relatively low Earth orbit it won’t have continual viewing like Kepler so will miss some transits . It will certainly further refine the transit timing considerably though.

    The question now is will Hubble and/ or Spitzer be able to transit spectroscopy follow up ( especially the latter in its superior viewing Earth trailing orbit ) and /or will this planet be deemed worthy of JWST’s ideal but precious time ? With a shallow transit and only about 8 per year it’s going to take extended time to “bin” enough photons to make a meaningful analysis . Tempting target though.

  • Andrew LePage November 30, 2016, 16:05

    Not long after the discovery of K2-3d (known at the time as EPIC 201367065d) was announced almost two years ago, I did a “reality check” on the claims of the potential habitability of this world:

    http://www.drewexmachina.com/2015/01/20/habitable-planet-reality-check-keplers-new-k2-finds/

    Although this initial assessment was not all that promising, this world did deserve careful watching since it orbited a relatively bright star which could allow JWST to probe its atmosphere. Whether this world turns out to be habitable or not, such data would be valuable for probing the limits of planetary habitability. These new data that are helping to refine the ephemeris to make those studies possible.

  • Jim Strom November 30, 2016, 16:38

    Cool stuff.

    Will next gen telescopes be able to measure a star’s intensity with sufficient accuracy to estimate a transiting planet’s radius (or its radius relative to its star’s radius)? I am talking about the shape of the intensity curve as a planet begins a transit; the time between initially starting to occlude to the time of full occlusion.

    • Eniac November 30, 2016, 23:21

      Transit depth is proportional to the apparent area of the planet relative to the apparent area of the star. The radius is simply proportional to the square root. So, the answer is that planet radius comes out of any transit measurement, no need to wait for next gen telescopes.

      • Jim Strom December 1, 2016, 12:06

        Thank you; should have known.

      • DJ Kaplan December 1, 2016, 13:31

        Eniac, so this raises a question: if we don’t know the angle from which we are viewing the exoplanet’s transit across its star, then for instance just a little bit of the planet may be eclipsing the star, creating the appearance of a smaller planet, wouldn’t it? I’m sure this is factored in somewhere. Fascinating stuff!

        • Eniac December 2, 2016, 0:11

          Yes, this would happen, but rarely, because the planet is so much smaller than the star. It is easily detectable as a lack of a flat plateau in the light curve. The flat part of the light curve is when all of the planet is in full eclipse, the flanks are where it is in partial eclipse. The shape of the flanks could tells us something about the shape of the planet, but that is not very useful because all planets are round.