Scientists detect and validate the longest-period exoplanet found with TESS

Scientists from The University of New Mexico (UNM), and Massachusetts Institute of Technology (MIT) have detected and validated two of the longest-period exoplanets found by TESS to date. These long period large exoplanets orbit a K dwarf star and belong to a class of planets known as warm Jupiters, which have orbital periods of 10-200 days and are at least six times Earth's radius. This recent discovery offers exciting research opportunities for the future of finding long-period planets that resemble those in our own solar system.

The research titled, TOI-4600 b and c: Two long-period giant planets orbiting an early K dwarf will be published in a future issue of The Astrophysical Journal Letters. The exoplanets, TOI-4600 b and c, were detected using photometric data from the Transiting Exoplanet Survey Satellite (TESS) and followed up with observations using the telescopes on the ground since they provide better resolution.

The observing strategy adopted by NASA's TESS, which divides each hemisphere into 13 sectors that are surveyed for roughly 28 days, is producing the most comprehensive all-sky search for transiting planets. This approach has already proven its capability to detect both large and small planets around different kinds of stars. In the case of TOI-4600, the star is a K dwarf star, also known as an orange dwarf, which are stars slightly smaller and cooler than the Sun.

Exoplanets must transit their host stars at least twice within TESS 's observing span to be detected with the correct period by the Science Processing Operations Center (SPOC) pipeline and the Quick Look Pipeline (QLP), which search the 2-minute and 30-minute cadence TESS data, respectively. Because 74 percent of TESS' total sky coverage is only observed for 28 days, the majority of TESS exoplanets detected have periods less than 40 days. Therefore, TOI-4600 b's 82.69-day, or nearly 3-month, and TOI-4600 c's 482.82-day, or 16-month, periods make their discoveries even more valuable.

The University of New Mexico's Ismael Mireles, the lead author of the paper, along with collaborators including Diana Dragomir, an assistant professor in UNM's Department of Physics and Astronomy, and collaborators from Massachusetts Institute of Technology and University of Bern, analyzed the data in order to measure the periods and sizes of these planets.

After initially detecting the transits, Mireles and team had to confirm that these were actual planets and to determine which signal the star was coming from. The diagnostic tools with TESS indicated that the signals coming from the target site were indeed on point. With help from TESS-Follow-up Observing Program (TFOP) Subgroup 1 (SG1), a global network of professional and amateur astronomers with access to telescopes small and large, they observed and watched a transit happen thus confirming for the researchers that this planet is indeed on target. Another factor that Mireles and his team had to consider were the masses and sizes of the planets. In order to achieve this they substituted the velocity measurements to observe how much the host star wobbles because the host star will pull on the planet.

"When we got the measurements, we were seeing very little movement in the target star. So when you start, you could be responsible for what we were seeing. Those two things together pretty much ruled it out. At that point we were sure that we had two planets," Mireles stated.

The researchers found these two planets and the inner planet TOI-4600 b is 82.69 days with a radius that is around just under seven times Earth's radius. It is between the size of Neptune and Saturn. This planet, TOI-4600 b,has an estimated temperature of about 170 degrees Fahrenheit, which is hot, but colder than a lot of the planets that astronomers have found. The second planet found, TOI-4600 c, is about nine and a half times Earth's radius, meaning it is roughly Saturn sized. It initially transited only once the first time TESS observed the star before transiting a second time almost three years later.

"Once you have two transits, you have an idea of what the periods can be. It could be the 965 days separating them, half of that, a third, a quarter, etc. The shorter periods could be ruled out because TESS had observed the star for a long time, so it only left two periods: 965 days or half of that," explained Mireles. The researchers used a model developed by collaborator Hugh Osborn at the University of Bern to compare the possible orbital periods and determine which one was most likely, and found that half of 965, or 482.82 days to be precise, was more likely. TOI-4600 c's 482.82 day period makes it the longest-period planet found by TESS to date and with a temperature of around -110 degrees Fahrenheit, it is one of the coldest planets found by TESS.

Katharine Hesse, TOI & Vetting Lead at MIT, collaborated with Mireles and team on the data analysis from TESS. Hesse helped process and analyze the large amount of data and placed the system into the context of other multiple-planet systems that have been found by missions including TESS. The comparison of the TOI-4600 system with other discovered exoplanet systems helps explore features like the formation time and processes and helped the researchers begin to place this system in the broader context of exoplanet systems.

"The main thing is trying to uncover more about planet formation because based on what we know about the exoplanets we found, so far, nothing really looks like the solar system. The interesting thing is that we want to learn about this planet formation. We have over 5,000 exoplanets now, but none of these systems really look like the solar system. And so we want to find out how these different types of systems formed and migrated," Mireles said.

Mireles and researchers are interested in these findings because of the discovery of two long period giant planets, which is a configuration that astronomers don't often see, even though the solar system found had four giant long distances or a long period one. This prompts further research discussions and questions as Mireles points out, "We want to find out how these are formed? Are there other planets in this system? Does that tell us anything about how these giant planets affect smaller planets that might be in there or might not be in there and why they're not there? There's still things that we want to find out and that will tell us a lot about planet formation."

In closing, Mireles promotes a call to action for citizen scientists, and hobbyists in astronomy, to participate and get involved in this research discovery. On Monday, Oct. 16, there will be another possible transit opportunity coming up for those who are interested and want to observe it to further confirm that the period of the outer planet is indeed 482 days. People with even smaller telescopes could participate if they have the right tools. "There are definitely people that are citizen scientists or amateur astronomers that have their own telescopes and help us with all these observations. There is a group of people with access to telescopes that are essentially confirming that a transit event is occurring on the star of interest," said Mireles.

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NASA's TESS tunes into an all-sky 'symphony' of red giant stars

Using observations from NASA's Transiting Exoplanet Survey Satellite (TESS), astronomers have identified an unprecedented collection of pulsating red giant stars all across the sky. These stars, whose rhythms arise from internal sound waves, provide the opening chords of a symphonic exploration of our galactic neighborhood.

TESS primarily hunts for worlds beyond our solar system, also known as exoplanets. But its sensitive measurements of stellar brightness make TESS ideal for studying stellar oscillations, an area of research called asteroseismology.

Hon presented the research during the second TESS Science Conference, an event supported by the Massachusetts Institute of Technology in Cambridge -- held virtually from Aug. 2 to 6 -- where scientists discuss all aspects of the mission. The Astrophysical Journal has accepted a paper describing the findings, led by Hon.

Sound waves traveling through any object -- a guitar string, an organ pipe, or the interiors of Earth and the Sun -- can reflect and interact, reinforcing some waves and canceling out others. This can result in orderly motion called standing waves, which create the tones in musical instruments.

Just below the surfaces of stars like the Sun, hot gas rises, cools, and then sinks, where it heats up again, much like a pan of boiling water on a hot stove. This motion produces waves of changing pressure -- sound waves -- that interact, ultimately driving stable oscillations with periods of a few minutes that produce subtle brightness changes. For the Sun, these variations amount to a few parts per million. Giant stars with masses similar to the Sun's pulsate much more slowly, and the corresponding brightness changes can be hundreds of times greater.

Oscillations in the Sun were first observed in the 1960s. Solar-like oscillations were detected in thousands of stars by the French-led Convection, Rotation and planetary Transits (CoRoT) space telescope, which operated from 2006 to 2013. NASA's Kepler and K2 missions, which surveyed the sky from 2009 to 2018, found tens of thousands of oscillating giants. Now TESS extends this number by another 10 times.

"With a sample this large, giants that might occur only 1% of the time become pretty common," said co-author Jamie Tayar, a Hubble Fellow at the University of Hawaii. "Now we can start thinking about finding even rarer examples."

The physical differences between a cello and a violin produce their distinctive voices. Similarly, the stellar oscillations astronomers observe depend on each star's interior structure, mass, and size. This means asteroseismology can help determine fundamental properties for large numbers of stars with accuracies not achievable in any other way.

"Our initial result, using stellar measurements across TESS's first two years, shows that we can determine the masses and sizes of these oscillating giants with precision that will only improve as TESS goes on," said Marc Hon, a NASA Hubble Fellow at the University of Hawaii in Honolulu. "What's really unparalleled here is that TESS's broad coverage allows us to make these measurements uniformly across almost the entire sky."

When stars similar in mass to the Sun evolve into red giants, the penultimate phase of their stellar lives, their outer layers expand by 10 or more times. These vast gaseous envelopes pulsate with longer periods and larger amplitudes, which means their oscillations can be observed in fainter and more numerous stars.

TESS monitors large swaths of the sky for about a month at a time using its four cameras. During its two-year primary mission, TESS covered about 75% of the sky, each camera capturing a full image measuring 24-by-24 degrees every 30 minutes. In mid-2020, the cameras began collecting these images at an even faster pace, every 10 minutes.

The images were used to develop light curves -- graphs of changing brightness -- for nearly 24 million stars over 27 days, the length of time TESS stares at each swath of the sky. To sift through this immense accumulation of measurements, Hon and his colleagues taught a computer to recognize pulsating giants. The team used machine learning, a form of artificial intelligence that trains computers to make decisions based on general patterns without explicitly programming them.

To train the system, the team used Kepler light curves for more than 150,000 stars, of which some 20,000 were oscillating red giants. When the neural network finished processing all of the TESS data, it had identified a chorus of 158,505 pulsating giants.

Next, the team found distances for each giant using data from ESA's (the European Space Agency's) Gaia mission, and plotted the masses of these stars across the sky. Stars more massive than the Sun evolve faster, becoming giants at younger ages. A fundamental prediction in galactic astronomy is that younger, higher-mass stars should lie closer to the plane of the galaxy, which is marked by the high density of stars that create the glowing band of the Milky Way in the night sky.

"Our map demonstrates for the first time empirically that this is indeed the case across nearly the whole sky," said co-author Daniel Huber, an assistant professor for astronomy at the University of Hawaii. "With the help of Gaia, TESS has now given us tickets to a red giant concert in the sky."

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Not just for finding planets: Exoplanet-hunter TESS telescope spots bright gamma-ray burst

NASA has a long tradition of unexpected discoveries, and the space program's TESS mission is no different. SMU astrophysicist and her team have discovered a particularly bright gamma-ray burst using a NASA telescope designed to find exoplanets -- those occurring outside our solar system -- particularly those that might be able to support life.

It's the first time a gamma-ray burst has been found this way.

Gamma-ray bursts are the brightest explosions in the universe, typically associated with the collapse of a massive star and the birth of a black hole. They can produce as much radioactive energy as the sun will release during its entire 10-billion-year existence.

Krista Lynne Smith, an assistant professor of physics at Southern Methodist University, and her team confirmed the blast -- called GRB 191016A -- happened on Oct. 16 and also determined its location and duration. A study on the discovery has been published in The Astrophysical Journal.

"Our findings prove this TESS telescope is useful not just for finding new planets, but also for high-energy astrophysics," said Smith, who specializes in using satellites like TESS (Transiting Exoplanet Survey Satellite) to study supermassive black holes and gas that surrounds them. Such studies shed light on the behavior of matter in the deeply warped spacetime around black holes and the processes by which black holes emit powerful jets into their host galaxies.

Smith calculated that GRB 191016A had a peak magnitude of 15.1, which means it was 10,000 times fainter than the faintest stars we can see with the naked eyes.

That may sound quite dim, but the faintness has to do with how far away the burst occurred. It is estimated that light from GRB 191016A's galaxy had been travelling 11.7 billion years before becoming visible in the TESS telescope.

Most gamma ray bursts are dimmer -- closer to 160,000 times fainter than the faintest stars.

The burst reached its peak brightness sometime between 1,000 and 2,600 seconds, then faded gradually until it fell below the ability of TESS to detect it some 7000 seconds after it first went off.

This gamma-ray burst was first detected by a NASA's satellite called Swift-BAT, which was built to find these bursts. But because GRB 191016A occurred too close to the moon, the Swift-BAT couldn't do the necessary follow-up it normally would have to learn more about it until hours later.

NASA's TESS happened to be looking at that same part of the sky. That was sheer luck, as TESS turns its attention to a new strip of the sky every month.

While exoplanet researchers at a ground-base for TESS could tell right away that a gamma-ray burst had happened, it would be months before they got any data from the TESS satellite on it. But since their focus was on new planets, these researchers asked if any other scientists at a TESS conference in Sydney, Australia were interested in doing more digging on the blast.

Smith was one of the few high-energy astrophysics specialists there at that time and quickly volunteered.

"The TESS satellite has a lot of potential for high-energy applications, and this was too good an example to pass up," she said. High-energy astrophysics studies the behavior of matter and energy in extreme environments, including the regions around black holes, powerful relativistic jets, and explosions like gamma-ray bursts.

TESS is an optical telescope that collects light curves on everything in its field of view, every half hour. Light curves are a graph of light intensity of a celestial object or region as a function of time. Smith analyzed three of these light curves to be able to determine how bright the burst was.

She also used data from ground-based observatories and the Swift gamma-ray satellite to determine the burst's distance and other qualities about it.

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Surprise! TESS shows ancient north star undergoes eclipses

Astronomers using data from NASA's Transiting Exoplanet Survey Satellite (TESS) have shown that Alpha Draconis, a well-studied star visible to the naked eye, and its fainter companion star regularly eclipse each other. While astronomers previously knew this was a binary system, the mutual eclipses came as a complete surprise.

"The first question that comes to mind is 'how did we miss this?'" said Angela Kochoska, a postdoctoral researcher at Villanova University in Pennsylvania who presented the findings at the 235th meeting of the American Astronomical Society in Honolulu on Jan. 6. "The eclipses are brief, lasting only six hours, so ground-based observations can easily miss them. And because the star is so bright, it would have quickly saturated detectors on NASA's Kepler observatory, which would also mask the eclipses."

The system ranks among the brightest-known eclipsing binaries where the two stars are widely separated, or detached, and only interact gravitationally. Such systems are important because astronomers can measure the masses and sizes of both stars with unrivaled accuracy.

Alpha Draconis, also known as Thuban, lies about 270 light-years away in the northern constellation Draco. Despite its "alpha" designation, it shines as Draco's fourth-brightest star. Thuban's fame arises from a historical role it played some 4,700 years ago, back when the earliest pyramids were being built in Egypt.

At that time, it appeared as the North Star, the one closest to the northern pole of Earth's spin axis, the point around which all of the other stars appear to turn in their nightly motion. Today, this role is played by Polaris, a brighter star in the constellation Ursa Minor. The change happened because Earth's spin axis performs a cyclic 26,000-year wobble, called precession, that slowly alters the sky position of the rotational pole.

TESS monitors large swaths of the sky, called sectors, for 27 days at a time. This long stare allows the satellite to track changes in stellar brightness. While NASA's newest planet hunter mainly seeks dimmings caused by planets crossing in front of their stars, TESS data can be used to study many other phenomena as well.

A 2004 report suggested that Thuban displayed small brightness changes that cycled over about an hour, suggesting the possibility that the system's brightest star was pulsating.

To check this, Timothy Bedding, Daniel Hey, and Simon Murphy at the University of Sydney, Australia, and Aarhus University, Denmark, turned to TESS measurements. In October, they published a paper that described the discovery of eclipses by both stars and ruling out the existence of pulsations over periods less than eight hours.

Now Kochoska is working with Hey to understand the system in greater detail.

"I've been collaborating with Daniel to model the eclipses and advising on how to bring together more data to better constrain our model." Kochoska explained. "The two of us took different approaches to modeling the system, and we hope our efforts will result in its full characterization."

As known from earlier studies, the stars orbit every 51.4 days at an average distance of about 38 million miles (61 million kilometers), slightly more than Mercury's distance from the Sun. The current preliminary model shows that we view the system about three degrees above the stars' orbital plane, which means neither star completely covers the other during the eclipses. The primary star is 4.3 times bigger than the Sun and has a surface temperature around 17,500 degrees Fahrenheit (9,700 C), making it 70% hotter than our Sun. Its companion, which is five times fainter, is most likely half the primary's size and 40% hotter than the Sun.

Kochoska says she is planning ground-based follow-up observations and anticipating additional eclipses in future TESS sectors.

"Discovering eclipses in a well-known, bright, historically important star highlights how TESS impacts the broader astronomical community," said Padi Boyd, the TESS project scientist at NASA's Goddard Space Flight Center in Greenbelt, Maryland. "In this case, the high precision, uninterrupted TESS data can be used to help constrain fundamental stellar parameters at a level we've never before achieved."

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Confirmation of toasty TESS planet leads to surprising find of promising world

This diagram shows the layout of the GJ 357 system. Planet d orbits within the star’s so-called habitable zone, the orbital region where liquid water can exist on a rocky planet’s surface. If it has a dense atmosphere, which will take future studies to determine, GJ 357 d could be warm enough to permit the presence of liquid water.

A piping hot planet discovered by NASA's Transiting Exoplanet Survey Satellite (TESS) has pointed the way to additional worlds orbiting the same star, one of which is located in the star's habitable zone. If made of rock, this planet may be around twice Earth's size.

The new worlds orbit a star named GJ 357, an M-type dwarf about one-third the Sun's mass and size and about 40% cooler that our star. The system is located 31 light-years away in the constellation Hydra. In February, TESS cameras caught the star dimming slightly every 3.9 days, revealing the presence of a transiting exoplanet -- a world beyond our solar system -- that passes across the face of its star during every orbit and briefly dims the star's light.

"In a way, these planets were hiding in measurements made at numerous observatories over many years," said Rafael Luque, a doctoral student at the Institute of Astrophysics of the Canary Islands (IAC) on Tenerife who led the discovery team. "It took TESS to point us to an interesting star where we could uncover them."

The transits TESS observed belong to GJ 357 b, a planet about 22% larger than Earth. It orbits 11 times closer to its star than Mercury does our Sun. This gives it an equilibrium temperature -- calculated without accounting for the additional warming effects of a possible atmosphere -- of around 490 degrees Fahrenheit (254 degrees Celsius).

"We describe GJ 357 b as a 'hot Earth,'" explains co-author Enric Pallé, an astrophysicist at the IAC and Luque's doctoral supervisor. "Although it cannot host life, it is noteworthy as the third-nearest transiting exoplanet known to date and one of the best rocky planets we have for measuring the composition of any atmosphere it may possess."

But while researchers were looking at ground-based data to confirm the existence of the hot Earth, they uncovered two additional worlds. The farthest-known planet, named GJ 357 d, is especially intriguing.

"GJ 357 d is located within the outer edge of its star's habitable zone, where it receives about the same amount of stellar energy from its star as Mars does from the Sun," said co-author Diana Kossakowski at the Max Planck Institute for Astronomy in Heidelberg, Germany. "If the planet has a dense atmosphere, which will take future studies to determine, it could trap enough heat to warm the planet and allow liquid water on its surface."

Without an atmosphere, it has an equilibrium temperature of -64 F (-53 C), which would make the planet seem more glacial than habitable. The planet weighs at least 6.1 times Earth's mass, and orbits the star every 55.7 days at a range about 20% of Earth's distance from the Sun. The planet's size and composition are unknown, but a rocky world with this mass would range from about one to two times Earth's size.

Even through TESS monitored the star for about a month, Luque's team predicts any transit would have occurred outside the TESS observing window.

GJ 357 c, the middle planet, has a mass at least 3.4 times Earth's, orbits the star every 9.1 days at a distance a bit more than twice that of the transiting planet, and has an equilibrium temperature around 260 F (127 C). TESS did not observe transits from this planet, which suggests its orbit is slightly tilted -- perhaps by less than 1 degree -- relative to the hot Earth's orbit, so it never passes across the star from our perspective.

To confirm the presence of GJ 357 b and discover its neighbors, Luque and his colleagues turned to existing ground-based measurements of the star's radial velocity, or the speed of its motion along our line of sight. An orbiting planet produces a gravitational tug on its star, which results in a small reflex motion that astronomers can detect through tiny color changes in the starlight. Astronomers have searched for planets around bright stars using radial velocity data for decades, and they often make these lengthy, precise observations publicly available for use by other astronomers.

Luque's team examined ground-based data stretching back to 1998 from the European Southern Observatory and the Las Campanas Observatory in Chile, the W.M. Keck Observatory in Hawaii, and the Calar Alto Observatory in Spain, among many others.

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