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A Combined Very Large Telescope and Gemini Study of the Atmosphere of the Directly Imaged Planet, β Pictoris b

Author(s): Currie, Thayne; Burrows, Adam S.; Madhusudhan, Nikku; Fukagawa, Misato; Girard, Julien H.; et al

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dc.contributor.authorCurrie, Thayne-
dc.contributor.authorBurrows, Adam S.-
dc.contributor.authorMadhusudhan, Nikku-
dc.contributor.authorFukagawa, Misato-
dc.contributor.authorGirard, Julien H.-
dc.contributor.authorDawson, Rebekah-
dc.contributor.authorMurray-Clay, Ruth-
dc.contributor.authorKenyon, Scott-
dc.contributor.authorKuchner, Marc-
dc.contributor.authorMatsumura, Soko-
dc.contributor.authorJayawardhana, Ray-
dc.contributor.authorChambers, John-
dc.contributor.authorBromley, Ben-
dc.identifier.citationCurrie, Thayne, Burrows, Adam, Madhusudhan, Nikku, Fukagawa, Misato, Girard, Julien H, Dawson, Rebekah, Murray-Clay, Ruth, Kenyon, Scott, Kuchner, Marc, Matsumura, Soko, Jayawardhana, Ray, Chambers, John, Bromley, Ben. (2013). A Combined Very Large Telescope and Gemini Study of the Atmosphere of the Directly Imaged Planet, β Pictoris b. apj, 776 (15 - 15. doi:10.1088/0004-637X/776/1/15en_US
dc.description.abstractWe analyze new/archival VLT/NaCo and Gemini/NICI high-contrast imaging of the young, self-luminous planet β Pictoris b in seven near-to-mid IR photometric filters, using advanced image processing methods to achieve high signal-to-noise, high precision measurements. While β Pic b’s near-IR colors mimic those of a standard, cloudy early-to-mid L dwarf, it is overluminous in the mid-infrared compared to the field L/T dwarf sequence. Few substellar/planet-mass objects—i.e., κ And b and 1RXJ 1609B—match β Pic b’s JHKsL photometry and its 3.1μm and 5μm photometry are particularly difficult to reproduce. Atmosphere models adopting cloud prescriptions and large (∼60μm) dust grains fail to reproduce the β Pic b spectrum. However, models incorporating thick clouds similar to those found for HR 8799 bcde, but also with small (a few microns) modal particle sizes, yield fits consistent with the data within the uncertainties. Assuming solar abundance models, thick clouds, and small dust particles ( a = 4 μm), we derive atmosphere parameters of log(g) = 3.8 ± 0.2 and Teff = 1575–1650 K, an inferred mass of 7+4−3 MJ , and a luminosity of log(L/L ) ∼ −3.80 ± 0.02. The best-estimated planet radius, ≈1.65 ± 0.06 RJ , is near the upper end of allowable planet radii for hot-start models given the host star’s age and likely reflects challenges constructing accurate atmospheric models. Alternatively, these radii are comfortably consistent with hot-start model predictions if β Pic b is younger than ≈7 Myr, consistent with a late formation well after its host star’s birth ∼12+8 −4 Myr ago.en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.rightsFinal published version. This is an open access article.en_US
dc.titleA Combined Very Large Telescope and Gemini Study of the Atmosphere of the Directly Imaged Planet, β Pictoris ben_US
dc.typeJournal Articleen_US

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