Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager

Macintosh, Bruce; Graham, James R.; Barman, Travis; Rosa, Robert J. De; Konopacky, Quinn; Marley, Mark S.; Marois, Christian; Nielsen, Eric L.; Pueyo, Laurent; Rajan, Abhijith; Rameau, Julien; Saumon, D.; Wang, Jason; Patience, J.; Ammons, Mark; Arriaga, Pauline; Artigau, Étienne; Beckwith, S.; Brewster, James T.; Bruzzone, Sebastian; Bulger, J.; Burningham, B.; Burrows, Adam; Chen, C.; Chiang, Eugene; Chilcote, Jeffrey; Dawson, Rebekah I.; Dong, Ruobing; Doyon, René; Draper, Zachary H.; Duchêne, Gaspard; Espósito, Thomas M.; Fabrycky, Daniel C.; Fitzgerald, Michael P.; Follette, Katherine B.; Fortney, Jonathan J.; Gerard, Benjamin L.; Goodsell, Stephen J.; Greenbaum, Alexandra Z.; Hibon, Pascale; Hinkley, Sasha; Cotten, Tara; Hung, Li Wei; Ingraham, Patrick; Johnson-Groh, Mara; Kalas, Paul; Lafrenière, David; Larkin, James E.; Lee, J.; Line, Michael R.; Long, Douglas; Maire, Jérôme; Marchis, Franck; Matthews, Brenda C.; Max, C. E.; Metchev, Stanimir; Millar-Blanchaer, Max; Mittal, Tushar; Morley, Caroline; Morzinski, Katie M.; Murray-Clay, Ruth; Oppenheimer, Ben R.; Palmer, David; Patel, Rahul; Perrin, Marshall D.; Poyneer, Lisa; Rafikov, Roman R.; Rantakyrö, Fredrik T.; Rice, Emily L.; Rojo, P.; Rudy, Alexander R.; Ruffio, Jean-Baptiste; Ruíz, M. T.; Sadakuni, Naru; Saddlemyer, Les; Salama, M.S.; Savransky, Dmitry; Schneider, Adam C.; Sivaramakrishnan, Anand; Song, Inseok; Soummer, Rémi; Thomas, Sandrine; Vasisht, Gautam; Wallace, J. Kent; Ward-Duong, Kimberly; Wiktorowicz, Sloane; Wolff, Schuyler; Zuckerman, B.

doi:10.1126/science.aac5891

Cited by 548 publications

(421 citation statements)

References 83 publications

Supporting

Mentioning

407

Contrasting

Order By: Relevance

“…8, the gray lines and shaded regions indicate synthetic planets that have a luminosity compatible with measurements of two important directly imaged extrasolar planets at 20 Myr, namely β Pictoris b (Lagrange et al 2009 and 51 Eridani b (Macintosh et al 2015). Both stars are members of the β Pic moving group with an age estimate of 21 ± 4 Myr (Binks & Jeffries 2014), while Macintosh et al (2015) adopt 20 ± 6 Myr for 51 Eri. It is interesting to study the properties of the synthetic analogs of the two planets, but it should be kept in mind that we only selected them based on a compatible luminosity.…”

Section: Comparison With β Pic B and 51 Eri Bmentioning

confidence: 99%

“…Direct imaging discoveries include the well-studied β Pic b ) and HR 8799 bcde objects (Marois et al 2008(Marois et al , 2010, but also a handful of exciting recent additions: HD 95086 b and 51 Eri b with small lower mass limits of a few Jupiter masses, and HIP 65426 b (Rameau et al 2013a,c;De Rosa et al 2016;Macintosh et al 2015;Samland et al 2017;Chauvin et al 2017). As advances both in observational and data-reduction techniques make it possible to probe closer in to the host stars, one could expect an increasing number of discoveries N if the radial-velocity result that dN/dP ≈ −0.7 < 0 (Cumming et al 2008), derived for masses M = 0.3-10 M and periods P = 2-2000 days, holds also at separations relevant for direct imaging.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

116

142

View full text Add to dashboard Cite

Context. This paper continues a series in which we predict the main observable characteristics of exoplanets based on their formation. In Paper I we described our global planet formation and evolution model that is based on the core accretion paradigm. In Paper II we studied the planetary mass-radius relationship with population syntheses. Aims. In this paper we present an extensive study of the statistics of planetary luminosities during both formation and evolution. Our results can be compared with individual directly imaged extrasolar (proto)planets and with statistical results from surveys. Methods. We calculated three populations of synthetic planets assuming different efficiencies of the accretional heating by gas and planetesimals during formation. We describe the temporal evolution of the planetary mass-luminosity relation. We investigate the relative importance of the shock and internal luminosity during formation, and predict a statistical version of the post-formation mass vs. entropy "tuning fork" diagram. Because the calculations now include deuterium burning we also update the planetary mass-radius relationship in time.Results. We find significant overlap between the high post-formation luminosities of planets forming with hot and cold gas accretion because of the core-mass effect. Variations in the individual formation histories of planets can still lead to a factor 5 to 20 spread in the post-formation luminosity at a given mass. However, if the gas accretional heating and planetesimal accretion rate during the runaway phase is unknown, the post-formation luminosity may exhibit a spread of as much as 2-3 orders of magnitude at a fixed mass. As a key result we predict a flat log-luminosity distribution for giant planets, and a steep increase towards lower luminosities due to the higher occurrence rate of low-mass (M 10-40 M ⊕ ) planets. Future surveys may detect this upturn. Conclusions. Our results indicate that during formation an estimation of the planetary mass may be possible for cold gas accretion if the planetary gas accretion rate can be estimated. If it is unknown whether the planet still accretes gas, the spread in total luminosity (internal+accretional) at a given mass may be as large as two orders of magnitude, therefore inhibiting the mass estimation. Due to the core-mass effect even planets which underwent cold accretion can have large post-formation entropies and luminosities, such that alternative formation scenarios such as gravitational instabilities do not need to be invoked. Once the number of self-luminous exoplanets with known ages and luminosities increases, the resulting luminosity distributions may be compared with our predictions.

show abstract

Section: Comparison With β Pic B and 51 Eri Bmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

116

142

View full text Add to dashboard Cite

show abstract

“…The Gemini instrument launched a multiyear search for Jupiter-like planets orbiting hot, young stars in November 2014. Early observations of 51 Eridani, a 20-million-year-old star about 30 parsecs away, spotted a Jupiter-like world 2.5 times farther from the star than Jupiter is from the Sun 10 . The spectrum showed that this exoplanet, dubbed 51 Eridani b, has an atmosphere containing more methane -a known component of Jupiter's atmosphere -than any other exoplanet.…”

Section: Spectrum C Dmentioning

confidence: 99%

The truth about exoplanets

Hecht¹

2016

Nature

View full text Add to dashboard Cite

“…With present-day instrumentation, this technique is mostly limited to young self-luminous giant planets in very long-period orbits ( 10 AU) around nearby young stars (e.g., Macintosh et al 2015). The next generation of exoplanet imaging efforts on the ground and in space will target long-period, mature Jovian planets similar to GJ 676A b (Traub et al 2016;Kasper 2015) and will pave the path towards observing the spectrum of a potential Earth-twin, which will require a large space observatory.…”

Section: Prospects For Directly Imaging the Gas Giants Around Gj 676amentioning

confidence: 99%

The mass of planet GJ 676A b from ground-based astrometry

Sahlmann

Lazorenko

Ségransan

et al. 2016

A&A

View full text Add to dashboard Cite

GJ 676A is an M0 dwarf hosting both gas-giant and super-Earth-type planets discovered with radial-velocity measurements. Using FORS2/VLT, we obtained position measurements of the star in the plane of the sky that tightly constrain its astrometric reflex motion caused by the super-Jupiter planet 'b' in a 1052-day orbit. This allows us to determine the mass of this planet to M b = 6.7 +1.8 −1.5 M J , which is ∼40 % higher than the minimum mass inferred from the radial-velocity orbit. Using new HARPS radial-velocity measurements, we improve upon the orbital parameters of the inner low-mass planets 'd' and 'e' and we determine the orbital period of the outer giant planet 'c' to P c = 7340 days under the assumption of a circular orbit. The preliminary minimum mass of planet 'c' is M c sin i = 6.8 M J with an upper limit of ∼39 M J that we set using NACO/VLT high-contrast imaging. We also determine precise parallaxes and relative proper motions for both GJ 676A and its wide M3 companion GJ 676B. Despite the probably mature age of the system, the masses and projected separations (∼0 . 1 -0 . 4) of planets 'b' and 'c' make them promising targets for direct imaging with future instruments in space and on extremely large telescopes. In particular, we estimate that GJ 676A b and GJ 676A c are promising targets for directly detecting their reflected light with the WFIRST space mission. Our study demonstrates the synergy of radial-velocity and astrometric surveys that is necessary to identify the best targets for such a mission.

show abstract

Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager

Cited by 548 publications

References 83 publications

Characterization of exoplanets from their formation

Characterization of exoplanets from their formation

The truth about exoplanets

The mass of planet GJ 676A b from ground-based astrometry

Contact Info

Product

Resources

About