The Trends High-Contrast Imaging Survey. I. Three Benchmark M Dwarfs Orbiting Solar-Type Stars

Crepp, Justin R.; Johnson, John Asher; Howard, Andrew W.; Marcy, G. W.; Fischer, Debra A.; Hillenbrand, Lynne A.; Yantek, Scott; Delaney, Colleen R.; Wright, Jason T.; Isaacson, Howard; Montet, Benjamin T.

doi:10.1088/0004-637x/761/1/39

Cited by 72 publications

(72 citation statements)

References 48 publications

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“…Standard AO imaging reduction methods were used to flatfield the images, correct for bad pixels, and subtract the sky background (Crepp et al 2012). Upon noticing the companions from the NIRC2 automated pipeline, we performed several experiments to confirm their nature, including studying how the signal-to-noise ratio improved with increasing number of processed frames from different detector quadrants.…”

Section: High-contrast Ao Imagingmentioning

confidence: 99%

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

Johnson

Rodriguez

Zhou

et al. 2018

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We present the discovery of KELT-21b, a hot Jupiter transiting the V=10.5 A8V star HD 332124. The planet has an orbital period of P=3.6127647±0.0000033 days and a radius of 1.586 0.040 0.039 -+ R J . We set an upper limit on the 1 planetary mass of M 3.91 P < M J at 3s confidence. We confirmed the planetary nature of the transiting companion using this mass limit and Doppler tomographic observations to verify that the companion transits HD 332124. These data also demonstrate that the planetary orbit is well-aligned with the stellar spin, with a sky-projected spinorbit misalignment of 5.6 1.91.7 . High-resolution imaging observations revealed the presence of a pair of stellar companions to KELT-21, located at a separation of 1 2 and with a combined contrast of K 6.39 0.06 S D =  with respect to the primary. Although these companions are most likely physically associated with KELT-21, we cannot confirm this with our current data. If associated, the candidate companions KELT-21 B and C would each have masses of ∼0.12 M ☉ , a projected mutual separation of ∼20 au, and a projected separation of ∼500 au from KELT-21. KELT-21b may be one of only a handful of known transiting planets in hierarchical triple stellar systems.

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Section: High-contrast Ao Imagingmentioning

confidence: 99%

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

Johnson

Rodriguez

Zhou

et al. 2018

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“…The TRENDS (TaRgetting bENchmark-objects with Doppler Spectroscopy) high-contrast imaging program uses precise radial velocity (RV) measurements obtained over a long time baseline to identify promising targets for follow-up observations using adaptive optics (AO; Crepp et al 2012bCrepp et al , 2013. In addition to diffraction-limited imaging, TRENDS also uses coronagraphy, point-spread function (PSF) subtraction, and ≈1 hr integration times to achieve deep contrast at near-infrared wavelengths (Marois et al 2006;Lafrenière et al 2007;Crepp et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The Trends High-Contrast Imaging Survey. Iii. A Faint White Dwarf Companion Orbiting Hd 114174

Crepp

Johnson

Howard

et al. 2013

ApJ

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The nearby Sun-like star HD 114174 exhibits a strong and persistent Doppler acceleration indicating the presence of an unseen distant companion. We have acquired high-contrast imaging observations of this star using NIRC2 at Keck and report the direct detection of the body responsible for causing the "trend." HD 114174 B has a projected separation of 692 ± 9 mas (18.1 AU) and is 10.75 ± 0.12 mag (contrast of 5 × 10 −5 ) fainter than its host in the K-band, requiring aggressive point-spread function subtraction to identify. Our astrometric time baseline of 1.4 yr demonstrates physical association through common proper motion. We find that the companion has absolute magnitude, M J = 13.97 ± 0.11, and colors, J − K = 0.12 ± 0.16 mag. These characteristics are consistent with an ≈T3 dwarf, initially leading us to believe that HD 114174 B was a substellar object. However, a dynamical analysis that combines radial velocity measurements with available imaging data indicates a minimum mass of 0.260 ± 0.010 M . We conclude that HD 114174 B must be a white dwarf. Assuming a hydrogen-rich composition, atmospheric and evolutionary model fits yield an effective temperature T eff = 8200 ± 4000 K, surface gravity log g = 8.90 ± 0.02, and cooling age of t c ≈ 3.4 Gyr, which is consistent with the 4.7 +2.3 −2.6 Gyr host star isochronal age estimate. HD 114174 B is a benchmark object located only 26.14 ± 0.37 pc from the Sun. It may be studied at a level of detail comparable to Sirius and Procyon, and used to understand the link between the mass of white dwarf remnants with that of their progenitors.

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“…It would also be interesting to collect additional RV data to see if there is an RV acceleration caused by the stellar companion. This approach has been fruitful in discovering low mass companions (Crepp et al 2012;Knutson et al 2014). An RV acceleration would further constrain the orbit.…”

Section: Discussionmentioning

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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The Trends High-Contrast Imaging Survey. I. Three Benchmark M Dwarfs Orbiting Solar-Type Stars

Cited by 72 publications

References 48 publications

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

KELT-21b: A Hot Jupiter Transiting the Rapidly Rotating Metal-poor Late-A Primary of a Likely Hierarchical Triple System

The Trends High-Contrast Imaging Survey. Iii. A Faint White Dwarf Companion Orbiting Hd 114174

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

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