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 (rhymes with fluid) is a high-precision  spectrograph that is designed to measure the extremely minute wobble of nearby stars using the . This effect results from the mutual gravitational force between a planet and its host star which causes the star’s position to shift very slightly as the planet travels around it. With this powerful capability, one of NEID’s main science goals is to confirm exoplanet candidates found by other exoplanet missions.

NEID is funded by the  (NN-EXPLORE) and is mounted on the  at the U.S. National Science Foundation Kitt Peak National Observatory (), a Program of NSF NOIRLab.

One mission that NEID is complementing is the European Space Agency’s () spacecraft. Through its precise monitoring of the positions and motions of stars in our galaxy, Gaia is revolutionizing our understanding of many areas of astrophysics. With its exquisite precision, Gaia is expected to be able to detect thousands of exoplanets in orbit around nearby stars.

Unlike the radial velocity method used by NEID, Gaia uses a technique known as  to detect a star’s motion. This technique involves measuring the subtle motion of a star as it is tugged by the gravity of an orbiting planet by looking at how the star moves compared to background or nearby stars.

Recently, as part of the latest Gaia data release, a list of stars that appear to be moving as though pulled by an exoplanet — the list of Gaia AStrometric Objects of Interest (Gaia-ASOIs) — was published. “However, the motion of these stars is not necessarily due to a planet,” said Guðmundur Stefánsson, assistant professor at the University of Amsterdam and lead author of the  appearing in The Astrophysical Journal. “Instead, the ‘star’ might be a pair of stars that are too close together for Gaia to recognize them as separate objects. The tiny shifts in position that appear to be due to a planet might actually result from the nearly perfect cancellation of the larger shifts in position of the two stars.” 

To weed out these binary stars and harvest the true planets, it is necessary to conduct follow-up observations with spectroscopy. To do so, the team used observations from NEID and two other spectrographs: the Habitable-zone Planet Finder () on the  at  in Texas, and the  on the  at La Palma in the Canary Islands.

With these powerful instruments the team conducted follow-up observations of 28 star systems with planet candidates identified by Gaia. They found that of the 28 candidate systems 21 were false positives and were actually binary star systems — two stars that orbit a common center of mass. They also confirmed that one system is a star hosting a   — an object with a mass in between those of planets and stars — but one was a star hosting a giant planet.

The newly discovered exoplanet, named Gaia-4b, has an orbital period of 570 days and a mass of 12 Jupiter masses and orbits a star 64% of the mass of the Sun. Not only is Gaia-4b the first planet ever detected by Gaia using the astrometric technique whose orbital solution is fully and independently confirmed, but it is also one of the most massive planets known to orbit a low-mass star.

“It is an exciting time for both NEID and Gaia,” says Jayadev Rajagopal, scientist at NSF NOIRLab and a co-author of the paper. “Gaia is more than living up to its promise of detecting planetary companions to stars with highly precise astrometry, and NEID is demonstrating that its long-term radial velocity precision is capable of detecting low-mass planets around those stars. With more candidate planets to come as roughly the last year of data is analyzed, this work is a harbinger of the future where Gaia discoveries of planets and brown dwarfs will need to be confirmed, or rejected, by NEID data.”

In addition to the detection of Gaia-4b and Gaia-5b, the authors provide a first glimpse of the ‘false positive rate’ of the Gaia Astrometric Exoplanet catalog, which is in the range 30–80% in their sample. This highlights the importance of ground-based observations like those possible with NEID in confirming planetary candidates in the Gaia-planet-detection era.

Notes

[1] The newly discovered brown dwarf, named Gaia-5b, is a 21-Jupiter-mass brown dwarf in a 358-day eccentric orbit around a star with 34% of the mass of the Sun.

More information

This research was presented in a paper titled “Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars” to appear in The Astrophysical Journal. DOI: 

The team is composed of Guðmundur Stefánsson (University of Amsterdam), Suvrath Mahadevan (The Pennsylvania State University), Joshua Winn (Princeton University), Marcus Marcussen (Aarhus University), Shubham Kanodia (Carnegie Institution for Science), Simon Albrecht (Aarhus University), Evan Fitzmaurice (The Pennsylvania State University, Institute for Computational and Data Sciences Scholar), OnÄ— Mikulskitye (University of Amsterdam), Caleb Cañas (NASA Postdoctoral Fellow, NASA Goddard Space Flight Center), Juan Ignacio Espinoza-Retamal (Pontificia Universidad Católica de Chile, Millennium Institute for Astrophysics, University of Amsterdam), Yiri Zwart (University of Amsterdam), Daniel Krolikowski (Steward Observatory, The University of Arizona), Andrew Hotnisky (The Pennsylvania State University), Paul Robertson (The University of California), Jaime A. Alvarado-Montes (Macquarie University), Chad Bender (Steward Observatory, The University of Arizona), Cullen Blake (University of Pennsylvania), Joe Callingham (Leiden University, Netherlands Institute for Radio Astronomy), William Cochran (The University of Texas at Austin), Megan Delamer (The Pennsylvania State University), Scott Diddams (University of Colorado), Jiayin Dong (Flatiron Institute, University of Illinois at Urbana-Champaign), Rachel Fernandes (The Pennsylvania State University), Mark Giovanazzi (Amherst College), Samuel Halverson (California Institute of Technology), Jessica Libby-Roberts (The Pennsylvania State University), Sarah E. Logsdon (NSF NOIRLab), Michael McElwain (NASA Goddard Space Flight Center), Joe Ninan (Tata Institute of Fundamental Research), Jayadev Rajagopal (NSF NOIRLab), Varghese Reji (Tata Institute of Fundamental Research), Arpita Roy (Schmidt Sciences), Christian Schwab (Macquarie University), and Jason Wright (The Pennsylvania State University).

The  is a partnership between Indiana University, University of Wisconsin–Madison, Pennsylvania State University, Princeton University, Purdue University (until 2025), NSF NOIRLab, and NASA.

, the U.S. National Science Foundation center for ground-based optical-infrared astronomy, operates the  (a facility of , , , , , and ), NSF Kitt Peak National Observatory (), NSF Cerro Tololo Inter-American Observatory (), the Community Science and Data Center (), and NSF–DOE  (in cooperation with ’s  National Accelerator Laboratory). It is managed by the Association of Universities for Research in Astronomy () under a cooperative agreement with  and is headquartered in Tucson, Arizona. 

The scientific community is honored to have the opportunity to conduct astronomical research on I’oligam Du’ag (Kitt Peak) in Arizona, on Maunakea in Hawai‘i, and on Cerro Tololo and Cerro Pachón in Chile. We recognize and acknowledge the very significant cultural role and reverence of I’oligam Du’ag to the Tohono O’odham Nation, and Maunakea to the Kanaka Maoli (Native Hawaiians) community.

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Contacts

Jayadev Rajagopal
Scientist
NSF NOIRLab
Email: [email protected]

Josie Fenske
Jr. Public Information Officer
NSF NOIRLab
Email: [email protected]