An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO

Rameau, Julien; Follette, Katherine B.; Pueyo, Laurent; Marois, Christian; Macintosh, Bruce; Millar-Blanchaer, Max; Wang, Jason; Vega, David; Doyon, René; Lafrenière, David; Nielsen, Eric L.; Bailey, Vanessa P.; Chilcote, Jeffrey; Close, Laird M.; Espósito, Thomas M.; Males, Jared R.; Metchev, Stanimir; Morzinski, Katie M.; Ruffio, Jean-Baptiste; Wolff, Schuyler; Ammons, S. Mark; Barman, Travis; Bulger, J.; Cotten, Tara; Rosa, Robert J. De; Duchêne, Gaspard; Fitzgerald, Michael P.; Goodsell, Stephen J.; Graham, James R.; Greenbaum, Alexandra Z.; Hibon, Pascale; Hung, Li‐Wei; Ingraham, Patrick; Kalas, Paul; Konopacky, Quinn; Larkin, James E.; Maire, Jérôme; Marchis, Franck; Oppenheimer, Ben R.; Palmer, David; Patience, Jennifer; Perrin, Marshall D.; Poyneer, Lisa; Rajan, Abhijith; Rantakyrö, Fredrik T.; Marley, Mark S.; Savransky, Dmitry; Schneider, Adam C.; Sivaramakrishnan, Anand; Song, Inseok; Soummer, Rémi; Thomas, Sandrine; Wallace, J. Kent; Ward-Duong, Kimberly; Wiktorowicz, Sloane

doi:10.3847/1538-3881/aa6cae

Cited by 87 publications

(67 citation statements)

References 78 publications

(111 reference statements)

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“…As we do not use spatial filtering now or in our previous paper, HD 100546 b's arXiv:1712.02819v1 [astro-ph.SR] 7 Dec 2017 point source-like appearance is not a filtering artifact as suggested in Rameau et al (2017). We also detect HD 100546 b in the 2016 GPIES data.…”

Section: Resultssupporting

confidence: 52%

“…However, HD 100546 has sub-au scale, optically-thin near-IR excess emission (J-K ∼ 1, over 50% of the system's H band flux) unresolvable by GPI (Benisty et al 2010;Tatulli et al 2011): the GPI stellar spectrum shown in Rameau et al (2017) is instead that of the star+inner disk. Furthermore, the light scattered by the outer disk is dominated by the 1500-1750 K inner disk; the disk comparison regions used by GPIES also lie on a thermal IR-bright spiral, which (if driven by a massive planet) can be heated well above local temperature (∼ 450 K; Lyra et al 2016).…”

Section: Resultsmentioning

confidence: 99%

“…• Rameau et al (2017) proposed that HD 100546 b's spectrum resembles the star's and the outer disk's and thus simply reveals scattered-light disk emission. However, HD 100546 has sub-au scale, optically-thin near-IR excess emission (J-K ∼ 1, over 50% of the system's H band flux) unresolvable by GPI (Benisty et al 2010;Tatulli et al 2011): the GPI stellar spectrum shown in Rameau et al (2017) is instead that of the star+inner disk.…”

Section: Resultsmentioning

confidence: 99%

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Clarifying the Status of HD 100546 as Observed by the Gemini Planet Imager

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Section: Resultssupporting

confidence: 52%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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Clarifying the Status of HD 100546 as Observed by the Gemini Planet Imager

et al. 2017

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“…Subsequent Ksband (2.15 μm) observations of the disk did not reveal a point source at the location of the b candidate (Boccaletti et al 2013), but rather faint extended emission (Garufi et al 2016). The nature of and physical relationship between the more compact L′ source and the extended Ks source is a subject for debate, and we discuss this in more detail in the companion to this paper (Rameau et al 2017), which is focused on the HD 100546 b planet candidate.…”

Section: Introductionmentioning

confidence: 91%

Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO

Follette

Rameau

Dong

et al. 2017

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106

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We present optical and near-infrared high-contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at Hα. The new GPI H-band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple data sets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 "c" varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD 100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images.

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“…This is especially the case as all these quantities are also available from global planet formation models as presented here, meaning that comprehensive comparisons covering many different aspects are possible. HD 100546 b This object was discovered by Quanz et al (2013), recovered by Currie et al (2014), and confirmed by Quanz et al (2015) (but see also Rameau et al 2017). The Herbig Ae/Be host star is a young, actively accreting intermediate-mass B9Vne star (M = 2.4 ± 0.1M , L ≈ 32L , T eff ≈ 10500 K).…”

Section: Comparison With Observed Forming Companions: Hd 100546 B Andmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

107

141

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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.

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An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO

Cited by 87 publications

References 78 publications

Clarifying the Status of HD 100546 as Observed by the Gemini Planet Imager

Clarifying the Status of HD 100546 as Observed by the Gemini Planet Imager

Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO

Characterization of exoplanets from their formation

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