Direct Imaging of Multiple Planets Orbiting the Star HR 8799

By C. Marois, B. Macintosh, Travis S. Barman, B. Zuckerman, Inseok Song, J. Patience, D. Lafrèniere, R. Doyon. Science, 2008

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Direct imaging of exoplanetary systems is a powerful technique that can reveal Jupiter-like planets in wide orbits, can enable detailed characterization of planetary atmospheres, and is a key step toward imaging Earth-like planets. Imaging detections are challenging because of the combined effect of small angular separation and large luminosity contrast between a planet and its host star. High-contrast observations with the Keck and Gemini telescopes have revealed three planets orbiting the star HR 8799, with projected separations of 24, 38, and 68 astronomical units. Multi-epoch data show counter clockwise orbital motion for all three imaged planets. The low luminosity of the companions and the estimated age of the system imply planetary masses between 5 and 13 times that of Jupiter. This system resembles a scaled-up version of the outer portion of our solar system.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

DIRECT IMAGING OF FINE STRUCTURES IN GIANT PLANET-FORMING REGIONS OF THE PROTOPLANETARY DISK AROUND AB AURIGAE (2011, methodology): “…of companions with masses of a few up to a few tens of MJ at distances >20 AU, beyond what had been thought to be the planet-forming zone (Marois et al. 2008; Kalas et al. 2008; ∗ Based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory…”
EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, background): “The past few years have seen the first images that resolve exoplanets from their primary stars, most notably the three planets orbiting HR 8799 seen in thermal emission (Marois et al. 2008; Serabyn et al. 2010).”
A New High Contrast Imaging Program at Palomar Observatory (2010, background): “Moreover, recent results (Marois et al. 2008; Kalas et al. 2008; Lagrange et al. 2010) have demonstrated that direct imaging of planetary mass companions and disks (Oppenheimer et al. 2008; Hinkley et al. 2009; Mawet et al. 2009; Boccaletti et al. 2009) is a technique 1 Department of Astronomy,…”
LkCa 15: A YOUNG EXOPLANET CAUGHT AT FORMATION? (2011, background): “The same result has been found for moderately older direct-imaged exoplanets, such as Beta Pic b (Lagrange et al. 2009; Quanz et al. 2010; Currie et al. 2011a) and HR 8799 bcde (Marois et al. 2008; Bowler et al. 2010; Marois et al. 2010; Currie et al. 2011b; Madhusudhan et al. 2011).”
Photometric characterization of exoplanets using angular and spectral differential imaging (2010, background): “…(Itoh et al. 2005), GQ Lup b (Neuhäuser et al. 2005), AB Pic b (Chauvin et al. 2005), CHXR 73 B (Luhman et al. 2006), and more recently Fomalhaut b (Kalas et al. 2008), 1RXS J1609 b (Lafrenière et al. 2008), β Pic b (Lagrange et al. 2008) and the triple system around HR 8799 (Marois et al. 2008).”
The effects of fly‐bys on planetary systems (2010, background): “8 PL A N E T S O N V E RY W I D E O R B I T S A number of planets have been observed on very wide orbits around main-sequence dwarf stars by direct imaging techniques (e.g. Kalas et al. 2008; Marois et al. 2008).”
NEW DEBRIS DISKS AROUND YOUNG, LOW-MASS STARS DISCOVERED WITH THE SPITZER SPACE TELESCOPE (2009, neutral): “…primarily with the radial velocity technique, in the past decade, but also through direct imaging, transits, microlensing, and pulsar timing (Marois et al. 2008; Kalas et al. 2008; Butler et al. 2006; Marcy et al. 2005; Bond et al. 2004; Beaulieu et al. 2006; Wolszczan & Frail 1992, and…”
LATE ORBITAL INSTABILITIES IN THE OUTER PLANETS INDUCED BY INTERACTION WITH A SELF-GRAVITATING PLANETESIMAL DISK (2011, background): “Since it is locked in MMRs with Saturn and Jupiter, however, its orbital eccentricity should increase instead, which is exactly what we see in our simulations (Figure 5).”
Planet-Disk Interaction and Orbital Evolution (2012, background): “One application of the Masset-Snellgrove process refers to the formation of systems such as HR 8799 or Fomalhaut where the planets reside at very large distances from the star (Marois et al., 2008; Kalas et al., 2008).”
Wide-Field InfrarRed Survey Telescope-Astrophysics Focused Telescope Assets WFIRST-AFTA 2015 Report (2015, background): “They have produced a dozen notable successes (Kalas et al. 2008, Marois et al. 2008, Lagrange et al. 2010, Rameau et al. 2013, Kuzuhara et al. 2013, Currie et al. 2014, Kraus et al. 2014) but the systems discovered, with supermassive (3-10 MJ) young (<100 Myr) planets in wide (20-200 AU) orbits are…”
THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “The HR 8799 system has been particularly illuminating as it is the only directly imaged multi-planet system (Marois et al. 2008; Marois et al. 2010), and the planets possess extreme photospheric properties compared to previously known substellar objects.”
MASSES, RADII, AND CLOUD PROPERTIES OF THE HR 8799 PLANETS (2012, methodology): “These values are consistent with those reported by Marois et al. (2008) although they are 0.1 dex brighter for planet b, 0.2 dex fainter for planet c, and 0.1 dex fainter for planet d.”
EVIDENCE FOR A DISTANT GIANT PLANET IN THE SOLAR SYSTEM (2016, background): “While observational inference of extrasolar planetary systems such as HR 8799 (Marois et al. 2008) suggests that planets can indeed occupy exceptionally wide orbits, the solar nebula would have had to be exceptionally expansive to be compatible with in-situ formation of a planet on such a distant…”
The VAST Survey - III. The multiplicity of A-type stars within 75 pc (2013, background): “…the subject of deep AO imaging searches for extreme mass ratio planetary companions (e.g. Vigan et al. 2012; Nielsen et al. 2013), with several planetary systems discovered (Kalas et al. 2008; Marois et al. 2008; Lagrange et al. 2009; Marois et al. 2010; Carson et al. 2013; Rameau et al. 2013).”
Exoplanet Atmospheres: Physical Processes (2010, background): “Out of a dozen planet candidates, the most definitive planet detections are Fomalhaut b because of its mass (≤ 3 MJ) (Kalas et al. 2008) and the three planets orbiting HR 8799 (Marois et al. 2008).”
Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects (2019, background): “Firstly, robust detections of exoplanetary atmospheric spectra are routinely made today using a variety of techniques: transit spectroscopy (50), direct imaging (174), as well as Doppler spectroscopy (251), both from space as well as the ground.”