MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANET<i>β</i>PIC b. II. 3–5<i>μ</i>m DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

Morzinski, Katie M.; Males, Jared R.; Skemer, Andrew J.; Close, Laird M.; Hinz, Philip M.; Rodigas, Timothy J.; Puglisi, Alfio; Esposito, Simone; Riccardi, Armando; Pinna, Enrico; Xompero, Marco; Briguglio, Runa; Bailey, Vanessa P.; Follette, Katherine B.; Kopon, Derek; Weinberger, Alycia J.; Wu, Yung‐Fu

doi:10.1088/0004-637x/815/2/108

Cited by 124 publications

(142 citation statements)

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“…centering (for SPHERE data) and via rotational centering (for MagAO), described in Sections 2.1 and 2.2, respectively, which are typically accurate to 0.25 pixels (Mesa et al 2015;Morzinski et al 2015). For both data sets, the position of HD 100453B is measured by fitting a 2D Gaussian to the source.…”

Section: Astrometric Error Budgetmentioning

confidence: 99%

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

Wagner

Dong

Sheehan

et al. 2018

ApJ

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HD 100453AB is a 10±2 Myr old binary whose protoplanetary disk was recently revealed to host a global twoarmed spiral structure. Given the relatively small projected separation of the binary (1 05, or ∼108 au), gravitational perturbations by the binary seemed to be a likely driving force behind the formation of the spiral arms. However, the orbit of these stars remained poorly understood, which prevented a proper treatment of the dynamical influence of the companion on the disk. We observed HD100453AB between 2015 and 2017, utilizing extreme adaptive optics systems on the Very Large Telescope and the Magellan Clay Telescope. We combined the astrometry from these observations with published data to constrain the parameters of the binary's orbit to a = 1 06±0 09, e=0.17±0.07, and i = 32°.5 ± 6°.5. We utilized publicly available ALMA 12 CO data to constrain the inclination of the disk,~ i 28 disk , which is relatively coplanar with the orbit of the companion and consistent with previous estimates from scattered light images. Finally, we input these constraints into hydrodynamic and radiative transfer simulations to model the structural evolution of the disk. We find that the spiral structure and truncation of the circumprimary disk in HD 100453 are consistent with a companion-driven origin. Furthermore, we find that the primary star's rotation, its outer disk, and the companion exhibit roughly the same direction of angular momentum, and thus the system likely formed from the same parent body of material.

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Section: Astrometric Error Budgetmentioning

confidence: 99%

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

Wagner

Dong

Sheehan

et al. 2018

ApJ

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“…The plate scale of the detector is 15.85 arcsec pixel −1 (Morzinski et al 2015). The target discussed in this paper to assess thecontrast performance ofthe vAPPis an A-type star with an L′-band magnitude between 0 and 1.…”

Section: Observationsmentioning

confidence: 99%

ON-SKY PERFORMANCE ANALYSIS OF THE VECTOR APODIZING PHASE PLATE CORONAGRAPH ON MagAO/Clio2

Otten

Snik

Kenworthy

et al. 2017

ApJ

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We report on the performance of a vector apodizing phase plate coronagraph that operates over a wavelength range of 2-5 μmand is installed in MagAO/Clio2 at the 6.5 m Magellan Clay telescope at Las Campanas Observatory, Chile. The coronagraph manipulates the phase in the pupil to produce three beams yielding two coronagraphic point-spread functions (PSFs) and one faint leakage PSF. The phase pattern is imposed through the inherently achromatic geometric phase, enabled by liquid crystal technology and polarization techniques. The coronagraphic optic is manufactured using a direct-write technique for precise control of the liquid crystal patternand multitwist retarders for achromatization. By integrating a linear phase ramp to the coronagraphic phase pattern, two separated coronagraphic PSFs are created with a single pupil-plane optic, which makes it robust and easy to install in existing telescopes. The two coronagraphic PSFs contain a 180°dark hole on each side of a star, and these complementary copies of the star are used to correct the seeing halo close to the star. To characterize the coronagraph, we collected a data set of a bright (m L =0-1) nearby star with ∼1.5 hr of observing time. By rotating and optimally scaling one PSFand subtracting it from the other PSF, we see a contrast improvement by 1.46 magnitudes at l D 3.5. With regular angular differential imaging at 3.9 μm, the MagAO vector apodizing phase plate coronagraph delivers a s D 5 mag contrast of 8.3 (= -10 3.3 ) at 2 l Dand 12.2 (= -10 4.8 ) at l D 3.5.

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“…Also, constraining the surface gravity of these objects has proven difficult since atmospheric properties are relatively insensitive to it. A more robust approach consists of using model atmospheres to derive a bolometric luminosity or, as in Morzinski et al (2015) for β Pic b, deriving it most empirically by combining photometry of a sufficiently large part of its spectrum. However, the issue is that to derive a mass from the bolometric luminosity, the postformation luminosity needs to be known; theoretical studies of the last decade have made clear that this is still an open issue, and in fact the single most important one in the field.…”

Section: Introductionmentioning

confidence: 99%

Characterization of exoplanets from their formation

Mordasini

Marleau

Mollière

2017

A&A

116

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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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MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANETβPIC b. II. 3–5μm DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

Cited by 124 publications

References 102 publications

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

ON-SKY PERFORMANCE ANALYSIS OF THE VECTOR APODIZING PHASE PLATE CORONAGRAPH ON MagAO/Clio2

Characterization of exoplanets from their formation

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