A Close Companion Search Around L Dwarfs Using Aperture Masking Interferometry and Palomar Laser Guide Star Adaptive Optics

Bernat, David; Bouchez, Antonin H.; Ireland, Michael; Tuthill, P. G.; Martinache, Frantz; Angione, John; Burruss, Rick; Cromer, John; Dekany, Richard; Guiwits, Stephen R.; Henning, John; Hickey, Jason; Kibblewhite, E. J.; McKenna, D.; Moore, Anna; Petrie, Harold L.; Roberts, J. T.; Shelton, J. C.; Thicksten, R.; Trinh, Thang; Tripathi, Renu; Troy, Mitchell; Truong, Trieu‐Kien; Velur, V.; Lloyd, James P.

doi:10.1088/0004-637x/715/2/724

Cited by 50 publications

(41 citation statements)

References 26 publications

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“…4 Now at Department of Astronomy, Cornell University, Ithaca, NY 14853, USA. (Bernat et al 2010), and three years of solid-state sum-frequency 589 nm laser guide star operations (Velur et al 2004;Bouchez et al 2007;Roberts et al 2008) including the demonstration of back pumping and frequency chirping techniques that increase the efficiency of photoreturn from Earth's mesospheric sodium layer (Kibblewhite 2008(Kibblewhite , 2009). PALM-241 achieved infrared K-band imaging Strehl ratios under median seeing conditions of 1.…”

Section: Introductionmentioning

confidence: 99%

PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE

Dekany

Roberts

Burruss

et al. 2013

ApJ

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167

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We describe and report first results from PALM-3000, the second-generation astronomical adaptive optics (AO) facility for the 5.1 m Hale telescope at Palomar Observatory. PALM-3000 has been engineered for high-contrast imaging and emission spectroscopy of brown dwarfs and large planetary mass bodies at near-infrared wavelengths around bright stars, but also supports general natural guide star use to V ≈ 17. Using its unique 66 × 66 actuator deformable mirror, PALM-3000 has thus far demonstrated residual wavefront errors of 141 nm rms under ∼1 seeing conditions. PALM-3000 can provide phase conjugation correction over a 6. 4 × 6. 4 working region at λ = 2.2 μm, or full electric field (amplitude and phase) correction over approximately one-half of this field. With optimized back-end instrumentation, PALM-3000 is designed to enable 10 −7 contrast at 1 angular separation, including post-observation speckle suppression processing. While continued optimization of the AO system is ongoing, we have already successfully commissioned five back-end instruments and begun a major exoplanet characterization survey, Project 1640.

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Section: Introductionmentioning

confidence: 99%

PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE

Dekany

Roberts

Burruss

et al. 2013

ApJ

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167

113

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“…However, various radial velocity and high spatial resolution imaging works in the literature (see also Sect. 5.5) have not revealed the presence of a second, massive object in relatively close orbits around J0045+1634, J0355+1133, J1726+1538, and J2208+2921 (Reid et al , 2006Bouy et al 2003;Bernat et al 2010;Blake et al 2010;Stumpf et al 2010). Our age estimate for J0355+1133 (120 As explained in Kirkpatrick (2005) and Cruz et al (2009), the β and γ appended to the L subtypes indicate intermediateand very low-gravity spectra, respectively.…”

Section: Hr Diagram: Ages and Massesmentioning

confidence: 65%

“…Using aperture masking interferometry and laser guide star adaptive optics of the 200-inch telescope on the Palomar Observatory, Bernat et al (2010) reported the detection of a companion candidate around J0355+1133 at a separation of 82.5 mas and 2.1:1 contrast in the K s -band, suggesting that both companion and primary have similar masses. At the distance of J0355+1133, the projected physical separation would result in 0.74 AU, and each component would have a mass of about 0.04-0.05 M (after splitting the object luminosity into two sources in Fig.…”

Section: Minimum Detectable Mass Of Astrometric Companionsmentioning

confidence: 99%

Trigonometric parallaxes of young field L dwarfs

Osorio

Béjar

Miles-Páez

et al. 2014

A&A

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Aims. We aim to determine the trigonometric parallaxes and proper motions of a sample of ten field L0-L5 dwarfs with spectroscopic evidence for low-gravity atmospheres. The ten sources were located in color-absolute magnitude diagrams and in the HertzsprungRussell (HR) diagram for age and mass derivations and were compared with field and star cluster dwarfs of related spectral classification and with state-of-the-art solar-metallicity evolutionary models. Methods. We obtained J and K s imaging data using 2-4 m class telescopes with a typical cadence of one image per month between 2010 January and 2012 December, in which the data cover a time baseline of nearly three years. We also obtained low resolution optical spectra (R ∼ 300, 500-1100 nm) using the 10 m Gran Telescopio de Canarias to assess the presence of lithium absorption in four targets and confirm their young age. The derived parallaxes and proper motions were combined with data from the literature to determine T eff , luminosity, and space velocities. All this information along with the lithium observations was used to assess the ages and masses of the sample. The astrometric curves were also examined for periodic perturbations indicative of unseen companions. Results. Trigonometric parallaxes and proper motions were derived to typical accuracies of a milliarcsecond (mas) and ±10 mas yr −1 , respectively. All ten L dwarfs have large motions (μ ≥ 70 mas yr −1 ) and are located at distances between 9 and 47 pc. They lie above and on the sequence of field dwarfs in the diagrams of absolute J and K s magnitude versus spectral type and luminosity versus effective temperature, which implies ages similar to or smaller than those typical of the field. In the HR diagram, 2MASS J00332386−1521309 (L4), 2MASS J00452143+1634446 (L2), 2MASS J03552337+1133437 (L5), 2MASS J05012406−0010452 (L4), G 196-3B (L3), 2MASS J17260007+1538190 (L3), and 2MASS J22081363+2921215 (L3) occupy locations that are compatible with the most likely ages in the interval ≈10-500 Myr if they are single objects. All of these dwarfs (except for 2MASS J00332386−1521309) show strong lithium absorption at 670.8 nm, thus confirming the young ages and masses ranging from ≈11 through ≈45 M Jup for this subsample. The detection of atomic lithium in the atmosphere of 2MASS J00452143+1634446 (L2) is reported for the first time. The lack of lithium in 2MASS J00332386−1521309 (L4) is not compatible with its position in the HR diagram, suggesting a spectral type earlier than L4. The remaining three dwarfs, 2MASS J02411151−0326587 (L0), 2MASS J10224821+5825453 (L1), and 2MASS J15525906+2948485 (L0) have locations in the HR diagram indicative of older ages and higher masses consistent with the observed lithium depletion previously published. The dynamical studies based on space velocities derived from our parallaxes and proper motions fully support the aforementioned results for 2MASS J00452143+1634446, 2MASS J03552337+1133437, G 196-3B, 2MASS J10224821+5825453, and 2MASS J15525906+2948485. We did ...

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“…Next, we subtracted the mean κ CrB closure phase set from the mean β CrB closure phase set, to remove systematic errors presumably present in both data sets. From here, we fitted a binary star model to the β CrB data in two stages, following an approach similar to that of Ireland et al and Bernat et al 24,27 First, we performed a "brute force" search over a coarse parameter grid. We explore a range of three parameters: radial separation (r), position angle (θ), and contrast (η).…”

Section: Results Of the β Crb Closure Phase Modelmentioning

confidence: 99%

“…Besides unique resolved measurements of individual binary and multiple star systems, 18,24,25 there has been one high-contrast survey of stars in the Upper Scorpius moving group, 26 and another survey for companions of L-dwarfs. 27 A large portion of the first survey and all of the latter survey were carried out at with the Palomar Hale Telescope's adaptive optics system (PALAO) in the near-infrared. 28 Both have yielded new sub-stellar companion candidates.…”

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confidence: 99%

Aperture mask interferometry with an integral field spectrograph

Zimmerman

Sivaramakrishnan

Bernat

et al. 2012

Optical and Infrared Interferometry III

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A non-redundant pupil mask placed in front of a low-resolution integral field spectrograph (IFS) adds a spectral dimension to high angular resolution imaging behind adaptive optics systems. We demonstrate the first application of this technique, using the spectroscopic binary star system β CrB as our target. The mask and IFS combination enabled us to measure the first low-resolution spectrum of the F3-F5 dwarf secondary component of β CrB, at an angular separation 141 mas from its A5-A7Vp primary star. To record multi-wavelength closure phases, we collected interferograms simultaneously in 23 spectral channels spanning the J and H bands (1.1 µm-1.8 µm), using the Project 1640 IFS behind the 249-channel PalAO adaptive optics system on the Hale telescope at Palomar Observatory. In addition to providing physical information about the source, spectrallyresolved mask fringes have the potential to enhance detection limits over single filter observations. While the overall dynamic range of our observation suffers from large systematic calibration errors, the information gleaned from the full channel range improves the dynamic range by a factor of 3 to 4 over the best single channel.

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A Close Companion Search Around L Dwarfs Using Aperture Masking Interferometry and Palomar Laser Guide Star Adaptive Optics

Cited by 50 publications

References 26 publications

PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE

PALM-3000: EXOPLANET ADAPTIVE OPTICS FOR THE 5 m HALE TELESCOPE

Trigonometric parallaxes of young field L dwarfs

Aperture mask interferometry with an integral field spectrograph

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