The Gaia space mission of the European Space Agency ESA is constructing an ultraprecise three-dimensional map of our Milky Way galaxy, observing almost two billion stars or roughly one percent of all the stars in our galaxy. Gaia was launched in December 2013 and has collected science data from July 2014. On Monday, June 13, ESA released Gaia data in Data Release 3 (DR3). Finnish researchers were strongly involved in the release.
Gaia data allows, for example, for the derivation of asteroid and exoplanet orbits and physical properties. The data helps unveil the origin and future evolution of the Solar System and the Milky Way and helps understand stellar and planetary-system evolution and our place in the cosmos.
Gaia revolves about its axis slowly in about six hours and is composed of two optical space telescopes. Three science instruments allow for accurate determination of stellar positions and velocities as well as the spectral properties. Gaia resides at about 1,5 million kilometers from the Earth in the anti-Sun direction, where it orbits the Sun together with the Earth in the proximity of the so-called Sun-Earth Lagrange L2-point.
Gaia DR3 on June 13, 2022 was significant across astronomy. Some 50 scientific articles are being published with DR3, of which nine articles have been devoted to underscoring the exceptionally significant potential of DR3 for future research.
The new DR3 data comprises, for example, the chemical compositions, temperatures, colors, masses, brightnesses, ages, and radial velocities of stars. DR3 includes the largest ever binary star catalog for the Milky Way, more than 150 000 Solar System objects, largely asteroids but also planetary satellites, as well as millions of galaxies and quasars beyond the Milky Way.
-There are so many revolutionary advances that it is difficult to pinpoint a single most significant advance. Based on Gaia DR3, Finnish researchers will change the conception of asteroids in our Solar System, exoplanets and stars in our Milky Way galaxy, as well as galaxies themselves, including the Milky Way and its surrounding satellite galaxies. Returning to our home planet, Gaia will produce an ultraprecise reference frame for navigation and positioning, says Academy Professor Karri Muinonen from the University of Helsinki.
Gaia and asteroids
The ten-fold increase in the number of asteroids reported in Gaia DR3 as compared to DR2 means that there is a significant increase in the number of close encounters between Gaia-detected asteroids. These close encounters can be utilized for asteroid mass estimation and we expect a significant increase in the number of asteroid masses to be derived by using Gaia DR3 astrometry, in particular, when combined with astrometry obtained by other telescopes.
In the conventional computation of an asteroid’s orbit, the asteroid is assumed to be a point-like object and its size, shape, rotation and surface light scattering properties are not taken into account. The Gaia DR3 astrometry is, however, so accurate that the angular offset between the asteroid’s center of mass and the center of the area illuminated by the Sun and visible to Gaia must be accounted for. Based on Gaia DR3, the offset has been certified for asteroid (21) Lutetia (Figure 2).
The ESA Rosetta space mission imaged Lutetia during the flyby on July 10, 2010. With the help of the Rosetta Lutetia imagery and ground-based astronomical observations, a rotation period, rotational pole orientation, and detailed shape model were derived. When the physical modeling is incorporated into orbit computation, the systematic errors are removed and, contrary to conventional computation, all observations can be incorporated into the orbit solution. Consequently, the Gaia astrometry provides information about the physical properties of asteroids. These properties need to be taken into account using physical models or empirical error models for the astrometry.
The Gaia DR3 includes, for the first time, spectral observations. The spectrum measures the color of the target, meaning the brightness at different wavelengths. One especially interesting feature is that the new release contains about 60 000 spectra of asteroids in our Solar System (Figure 3). The asteroid spectrum contains information on their composition and, thus, about their origin and the evolution of the whole Solar System. Before the Gaia DR3, there has been only few thousand asteroid spectra available, so Gaia will multiply the amount of data by more than an order of magnitude.
Gaia and exoplanets
Gaia is expected to produce detections of up to 20 000 giant exoplanets by measuring their gravitational effect on the movement of their host stars. This will enable finding virtually all Jupiter-like exoplanets in the Solar neighbourhood over the coming years and determining how common are Solar System -like architectures. The first such astrometric Gaia detection was a giant exoplanet around epsilon Indi A, that corresponds to the nearest Jupiter-like exoplanet only 12 light years away. The first such detections are possible because acceleration observed in radial velocity surveys can be combined with movement data from Gaia to determine the orbits and planetary masses.
Gaia and galaxies
The microarcsecond resolution of Gaia DR3 provides precise measurements of the motions of stars, not only within our own Milky Way galaxy, but also for the many satellite galaxies that surround it. From the motion of stars within the Milky Way itself, we can accurately measure its mass, and together with the proper motion of satellites, we can now accurately determine their orbits. This lets us look both into the past and into the future of the Milky Way galaxy system. For example, we can find out which of the galaxies that surround the Milky Way are true satellites, and which are just passing by. We can also investigate if the evolution of the Milky Way conforms to cosmological models, and in particular, whether the satellite orbits fit the standard dark matter model.
Gaia and reference frames
The International Celestial Reference Frame, ICRF3, is based on the position of a few thousand quasars determined by Very Long Baseline Interferometry (VLBI) at radio wavelengths. ICRF3 is used to obtain the coordinates of celestial objects and to determine the orbits of satellites. Quasars of ICRF3 are also fixed points on the sky that can be used to determine the precise orientation of the Earth in space at any time. Without this information, for example, satellite positioning would not work.
Gaia's data contain about 1,6 million quasars, which can be used to create a more accurate Celestial Reference Frame in visible light replacing the current one. In the future, this will have an impact on the accuracy of both satellite positioning and measurements of Earth-exploring satellites.
-The importance of DR3 and future data releases is in the improved accuracy due to increased data, summarizes Professor Markku Poutanen from the National Land Survey of Finland.
Academy Professor Karri Muinonen, University of Helsinki, firstname.lastname@example.org, +358 50 415 5474, Asteroids
Professor Markku Poutanen, National Land Survey of Finland, Finnish Geospatial Research Institute FGI, email@example.com, +358 40 7182152, Reference frames
Associate Professor Mikael Granvik, University of Helsinki and Luleå University of Technology, firstname.lastname@example.org, +358 50 521 7209, Asteroids
Docent, University Researcher Antti Penttilä, University of Helsinki, email@example.com, +358 50 524 0968, Asteroids
University Researcher Mikko Tuomi, University of Helsinki, firstname.lastname@example.org, +358 40 500 7454, Exoplanets and variable stars
Docent, Academy Research Fellow Till Sawala, University of Helsinki, email@example.com, +358 440 418000, Galaxies and cosmology
University of Helsinki Gaia DR3 press event, June 13, 2022
- 10.30 Opening, Gaia space mission, Karri Muinonen
- 10.35 Small Solar System bodies, Mikael Granvik
- 10.45 Discussion
- 11.00 ESA Central Event
- 12.00 Lunch
- 13.00 Gaia Data Release 3 highlights, Asteroid characterization from photometry, Karri Muinonen
- 13.20 Asteroid masses from astrometry, Mikael Granvik
- 13.30 Asteroid classifications from spectroscopy, Antti Penttilä
- 13.40 Exoplanets and variable stars, Mikko Tuomi
- 13.50 Galaxies, Till Sawala
- 14.00 Reference frames, Markku Poutanen
- 14.10 Questions and answers, discussion, Anne Virkki (chair)
- 15.00 Closing, Karri Muinonen
Recordings of the University of Helsinki Gaia DR3 press event
Full overview of the Gaia DR3 contents
Figure 1. Mass estimate for main-belt asteroid (445) Edna based on ground-based astrometry (blue), Gaia DR2 astrometry (red), and their combination (green). The combination of ground-based and Gaia data provides the most accurate estimate for Edna's mass and the low density suggest that its carbonaceous interior has not been fully compacted. Reference and image credit: Siltala, L. & Granvik, M. 2022, Astronomy & Astrophysics 658, A65.
Figure 2. Asteroid (21) Lutetia’s photocenter (brown bullet) and center of mass (blue bullet) as projected in the direction of Gaia for three viewing geometries. The vertical axis (green bars) is in the direction of the z-axis of the equatorial reference frame (north is upwards) and the illumination by the Sun is in the direction of the red bar. The angle between Gaia and the Sun (the so-called phase angle) is, from the left to the right, 16.7, 24.2 and 20.9 degrees and the photocenter-barycenter distance is 7.42, 5.96 and 10.91 km, respectively. Reference and image credit: Tanga, P., Muinonen, K., Penttilä, A., et al., 2022, Astronomy & Astrophysics, in press.
Figure 3. Histogram of the asteroids with spectra in Gaia Data Release 3. The number of asteroids is in the vertical axis, and the horizontal axis shows the distance of the asteroid to the Sun in astronomical units (au). One au is the average distance between the Earth and the Sun. Reference and image credit: Gaia Collaboration, Galluccio, L., Muinonen, K., Fedorets, G., Granvik, M. Penttilä, A., Siltala, L., et al., 2022, Astronomy & Astrophysics, in press.
Figure 4. A: Radial velocity observations of epsilon Indi A demonstrating acceleration caused by the gravitational pull of a giant exoplanet. B(C): Observed proper motion (position) that changed significantly between Gaia observations and earlier measurements verifying the planetary nature of the star's companion by enabling the determination of its mass. Reference and image credit: Feng, F., Anglada-Escudé, G., Tuomi, M. et al., 2019, MNRAS 490, 5002.
Figure 5. Orbits of seven Milky Way satellite galaxies, integrated numerically for 1 billion years into the past and future, using proper motions from Gaia DR2 (left) and Gaia DR3 (right). While the Gaia DR2 proper motions have considerable uncertainty, the much more precise Gaia DR3 proper motions allow us to reconstruct the past and predict the future evolution with high precision. Image credit: Till Sawala.