From AAS NOVA: “Identifying a Slow Planet from a Single TESS Transit”



10 August 2020
Susanna Kohler

Artist’s illustration of a gas giant exoplanet on a wide orbit around its host star. [NASA/JPL-Caltech]

Over the past 25 years, we’ve found thousands of worlds beyond our solar system. Nonetheless, some categories of exoplanets remain elusive — for instance, planets that orbit their hosts on long, slow paths. A new study shows how we might hunt these worlds down.

Observational Limits

Since the first exoplanet discovery a quarter century ago, we’ve found more than 4,000 confirmed planets orbiting other stars. A large number of these discoveries are planets that transit across the face of their host star — most identified by the Kepler Space Telescope or, more recently, by the Transiting Exoplanet Survey Satellite (TESS).

NASA/Kepler Telescope, and K2 March 7, 2009 until November 15, 2018

NASA/MIT TESS replaced Kepler in search for exoplanets

Planet transit. NASA/Ames.

These exoplanets are valuable targets because we can use the transits to measure properties like their radii, densities, bulk compositions, and even their atmospheres.

Unfortunately, due to the nature of transit detections, our observations are inherently biased: it’s easier to detect and confirm short-period, large planets, which means we know a lot about hot Jupiters, but relatively little about wide-orbit, cooler planets.

Because the TESS spacecraft observes a typical region for less than a month, planets on wide orbits longer than 30 days will register — at most — a single transit in TESS data before the telescope moves on to the next section of sky. But can we somehow leverage these single transits to learn more about slow, wide-orbit planets?

Avoiding Overbooking

A planet candidate with only one transit detection could be confirmed with radial-velocity measurements of its host star. But high-precision radial-velocity instruments are in high demand! Without precise knowledge of a planet’s period, confirming that planet’s existence and measuring its properties would require a huge observational time investment from already overbooked radial-velocity instruments.

Fortunately, a team of scientists led by Samuel Gill (University of Warwick, UK) has now demonstrated a more efficient way of pinning down a planet after just one TESS transit.

Light curve showing the best fit to the transit photometry of NGTS-11 from TESS and NGTS. [Gill et al. 2020]

Two Transits, Fewer Options

Gill and collaborators followed up on a planet candidate that had registered a single TESS transit in September 2018. The team conducted an intense photometric monitoring campaign of the candidate’s host star using the economical telescopes of the Next-Generation Transit Survey (NGTS) facility in Chile — and with 79 nights of observations, they detected a second transit of the candidate 390 days after the initial TESS transit.

ESO NGTS an array of twelve 20-centimetre telescopes at Cerro Paranel, 2,635 metres (8,645 ft) above sea level

From the combined photometric observations, the authors were able to narrow down the possible periods for the planet to just 13 options. Using these constraints, they could then wrap up with brief and efficient radial-velocity measurements to identify the properties of the planet.

Radial Velocity Method-Las Cumbres Observatory

A Cool Discovery

The result? NGTS-11 b (or TOI-1847 b), as the confirmed planet is now named, is a Saturn-mass planet on a wide, ~35-day orbit. With an equilibrium temperature of just 435 K, NGTS-11 b is one of the coolest known transiting gas giants and a valuable target for future transmission spectroscopy to explore its atmosphere.

Gill and collaborators’ identification of NGTS-11 b from just a single TESS transit shows the power of using ground-based photometry to pin down wide-orbit planets. This approach could help us to dramatically expand our understanding of the slower, long-period worlds beyond our solar system.


“NGTS-11 b (TOI-1847 b): A Transiting Warm Saturn Recovered from a TESS Single-transit Event,” Samuel Gill et al 2020 ApJL 898 L11.

See the full article here .


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