First Light Adaptive Optics Images from the Keck II Telescope: A New Era of High Angular Resolution Imagery

Wizinowich, Peter; Acton, D. Scott; Shelton, Chris; Stomski, Paul J.; Gathright, J.; Ho, Kevin; Lupton, William; Tsubota, K.; Lai, Olivier; Max, C. E.; Brase, James M.; An, Jong R.; Avicola, K.; Olivier, Scot S.; Gavel, Donald T.; Macintosh, Bruce; Ghez, A. M.; Larkin, James E.

doi:10.1086/316543

Cited by 374 publications

(200 citation statements)

References 5 publications

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“…02 pix −1 and a field of view of 20 . We used the R = 14.1 USNO B star 1444−0306431 (Monet et al 2003) for the input of the Natural Guide Star (Wizinowich et al 2000) wavefront sensor. Five images were taken in the H bb filter (a broad-band H filter) with single frame exposure times of 120 s. WISE 2005+5424 has a FWHM of 0.…”

Section: Mosfirementioning

confidence: 99%

The Exemplar T8 Subdwarf Companion of Wolf 1130

Mace

Kirkpatrick

Cushing

et al. 2013

ApJ

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We have discovered a wide separation (188. 5) T8 subdwarf companion to the sdM1.5+WD binary Wolf 1130. Companionship of WISE J200520.38+542433.9 is verified through common proper motion over a ∼3 yr baseline. Wolf 1130 is located 15.83 ± 0.96 pc from the Sun, placing the brown dwarf at a projected separation of ∼3000 AU. Near-infrared colors and medium resolution (R ≈ 2000-4000) spectroscopy establish the uniqueness of this system as a high-gravity, low-metallicity benchmark. Although there are a number of low-metallicity T dwarfs in the literature, WISE J200520.38+542433.9 has the most extreme inferred metallicity to date with [Fe/H] = −0.64 ± 0.17 based on Wolf 1130. Model comparisons to this exemplar late-type subdwarf support it having an old age, a low metallicity, and a small radius. However, the spectroscopic peculiarities of WISE J200520.38+542433.9 underscore the importance of developing the low-metallicity parameter space of the most current atmospheric models.

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Section: Mosfirementioning

confidence: 99%

The Exemplar T8 Subdwarf Companion of Wolf 1130

Mace

Kirkpatrick

Cushing

et al. 2013

ApJ

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“…The data presented here were collected in 2003 and 2004 using the Keck II AO system (Wizinowich et al, 2000) and the near-infrared NIRC-2 camera (1024 × 1024 Aladdin-3 InSb array). All observations were recorded in the narrow field of view (with a 9.942 mas pixel scale) in Kp broad-band filter (λ 0 = 2.124 μm; Δλ = 0.351 μm).…”

Section: Collected Datamentioning

confidence: 99%

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

106

101

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This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × R Hill (1/4 × R Hill ) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6-8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450-464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.

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“…We used the Keck II telescope, its AO system (Wizinowich et al 2000), and the NIRC2 instrument to observe the system at three epochs in 2011 and 2012. Each time, we collected data in multiple filters with multiple coadds.…”

Section: Keck II Observationsmentioning

confidence: 99%

KNOW THE STAR, KNOW THE PLANET. IV. A STELLAR COMPANION TO THE HOST STAR OF THE ECCENTRIC EXOPLANET HD 8673b

Roberts

Mason

Neyman

et al. 2015

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HD 8673 hosts a massive exoplanet in a highly eccentric orbit (e = 0.723). Based on two epochs of speckle interferometry a previous publication identified a candidate stellar companion. We observed HD 8673 multiple times with the 10 m Keck II telescope, the 5 m Hale telescope, the 3.63 m Advanced Electro-Optical System telescope, and the 1.5 m Palomar telescope in a variety of filters with the aim of confirming and characterizing the stellar companion. We did not detect the candidate companion, which we now conclude was a false detection, but we did detect a fainter companion. We collected astrometry and photometry of the companion on six epochs in a variety of filters. The measured differential photometry enabled us to determine that the companion is an early M dwarf with a mass estimate of 0.33-0.45 M  . The companion has a projected separation of 10 AU, which is one of the smallest projected separations of an exoplanet host binary system. Based on the limited astrometry collected, we are able to constrain the orbit of the stellar companion to a semimajor axis of 35-60 AU, an eccentricity ⩽0.5, and an inclination of 75°-85°. The stellar companion has likely strongly influenced the orbit of the exoplanet and quite possibly explains its high eccentricity.

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First Light Adaptive Optics Images from the Keck II Telescope: A New Era of High Angular Resolution Imagery

Cited by 374 publications

References 5 publications

The Exemplar T8 Subdwarf Companion of Wolf 1130

The Exemplar T8 Subdwarf Companion of Wolf 1130

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

KNOW THE STAR, KNOW THE PLANET. IV. A STELLAR COMPANION TO THE HOST STAR OF THE ECCENTRIC EXOPLANET HD 8673b

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