The Seeds Direct Imaging Survey for Planets and Scattered Dust Emission in Debris Disk Systems

Janson, Markus; Brandt, Timothy D.; Moro‐Martín, Amaya; Usuda, Tomonori; Thalmann, Christian; Carson, J.; Goto, Miwa; Currie, Thayne; McElwain, Michael W.; Itoh, Yoichi; Fukagawa, Misato; Crepp, Justin R.; Kuzuhara, Masayuki; Hashimoto, Jun; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Abe, Lyu; Brandner, W.; Egner, Sebastian; Feldt, M.; Grady, C. A.; Guyon, Olivier; Hayano, Yutaka; Hayashi, M.; Hayashi, Saeko S.; Henning, Thomas; Hodapp, Klaus W.; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Knapp, G. R.; Kwon, Jungmi; Matsuo, Taro; Miyama, Shoken M.; Morino, Jun-Ichi; Nishimura, Tetsuro; Pyo, Tae‐Soo; Serabyn, Eugene; Suenaga, Takuya; Shimada, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro; Miki, Takami; Takato, Naruhisa; Terada, Hiroshi; Tomono, D.; Turner, Edwin L.; Watanabe, Makoto; Wisniewski, John P.; Yamada, Tōru; Takami, Hideki; Tamura, Motohide

doi:10.1088/0004-637x/773/1/73

Cited by 89 publications

(84 citation statements)

References 116 publications

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“…For this study, we use the previously published data sets comprised of debris disk hosts (Janson et al 2013b), proposed members of nearby MGs (Brandt et al 2014), and Pleiades members (Yamamoto et al 2013). The Pleiades targets are young, with ages that are betterconstrained than those of typical field stars.…”

Section: Seedsmentioning

confidence: 99%

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A Statistical Analysis of Seeds and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?

Brandt¹,

McElwain²,

Turner³

et al. 2014

ApJ

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135

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We conduct a statistical analysis of a combined sample of direct imaging data, totalling nearly 250 stars. The stars cover a wide range of ages and spectral types, and include five detections (κ And b, two ∼60 M J brown dwarf companions in the Pleiades, PZ Tel B, and CD−35 2722B). For some analyses we add a currently unpublished set of SEEDS observations, including the detections GJ 504b and GJ 758B. We conduct a uniform, Bayesian analysis of all stellar ages using both membership in a kinematic moving group and activity/rotation age indicators. We then present a new statistical method for computing the likelihood of a substellar distribution function. By performing most of the integrals analytically, we achieve an enormous speedup over brute-force Monte Carlo. We use this method to place upper limits on the maximum semimajor axis of the distribution function derived from radialvelocity planets, finding model-dependent values of ∼30-100 AU. Finally, we model the entire substellar sample, from massive brown dwarfs to a theoretically motivated cutoff at ∼5 M J , with a single power-law distribution. We find that p(M, a) ∝ M −0.65±0.60 a −0.85±0.39 (1σ errors) provides an adequate fit to our data, with 1.0%-3.1% (68% confidence) of stars hosting 5-70 M J companions between 10 and 100 AU. This suggests that many of the directly imaged exoplanets known, including most (if not all) of the low-mass companions in our sample, formed by fragmentation in a cloud or disk, and represent the low-mass tail of the brown dwarfs.

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Section: Seedsmentioning

confidence: 99%

“…The debris disk sample has its stellar properties listed in Table 4 of Janson et al (2013b). For this work, we revisit the ages using the Bayesian techniques presented in Brandt et al (2014) and summarized in Section 4.…”

Section: Seedsmentioning

confidence: 99%

A Statistical Analysis of Seeds and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?

Brandt¹,

McElwain²,

Turner³

et al. 2014

ApJ

Self Cite

135

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show abstract

“…While alternative possibilities exist for explaining these structures (e.g., Lyra & Kuchner 2013), such rings may be shaped by planets orbiting near the ring edges (e.g., Quillen 2006). It is therefore interesting to study the regions close to the edges in particular detail (e.g., Apai et al 2008;Janson et al 2013a). While many planetary imaging surveys are performed at JHK-band (∼1-2.5 μm) wavelengths (e.g.…”

Section: Introductionmentioning

confidence: 99%

High-contrast imaging withSpitzer: deep observations of Vega, Fomalhaut, andϵEridani

Janson

Quanz

Carson

et al. 2015

A&A

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Stars with debris disks are intriguing targets for direct-imaging exoplanet searches, owing both to previous detections of wide planets in debris disk systems, and to commonly existing morphological features in the disks themselves that may be indicative of a planetary influence. Here we present observations of three of the most nearby young stars, which are also known to host massive debris disks: Vega, Fomalhaut, and Eri. The Spitzer Space Telescope is used at a range of orientation angles for each star to supply a deep contrast through angular differential imaging combined with high-contrast algorithms. The observations provide the opportunity to probe substantially colder bound planets (120-330 K) than is possible with any other technique or instrument. For Vega, some apparently very red candidate point sources detected in the 4.5 μm image remain to be tested for common proper motion. The images are sensitive to ∼2 M jup companions at 150 AU in this system. The observations presented here represent the first search for planets around Vega using Spitzer. The upper 4.5 μm flux limit on Fomalhaut b could be further constrained relative to previous data. In the case of Eri, planets below both the effective temperature and the mass of Jupiter could be probed from 80 AU and outward, although no such planets were found. The data sensitively probe the regions around the edges of the debris rings in the systems where planets can be expected to reside. These observations validate previous results showing that more than an order of magnitude improvement in performance in the contrast-limited regime can be acquired with respect to conventional methods by applying sophisticated high-contrast techniques to space-based telescopes, thanks to the high degree of PSF stability provided in this environment.

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“…The main objectives of these surveys were to populate the mass vs. semi-major axis diagram at large separations, and to clarify the mechanisms of planetary formation. Among the most recent of these surveys we can cite the NACO-Large Program at the Very Large Telescope (Desidera et al 2014;Chauvin et al 2014), the Strategic Exploration of Exoplanets and Disk with Subaru (SEEDS) at the Subaru Telescope (Janson et al 2013;Brandt et al 2014), the Near-Infrared Coronagraphic Imager (NICI) campaign at the Gemini South Telescope (Nielsen et al 2013;Biller et al 2013), the International Deep Planet Survey (Vigan et al 2012) at the Very Large Telescope (VLT) and Gemini North, and a survey of young, nearby, and dusty stars to understand the formation of wide-orbit giant planets (Rameau et al 2013b) at VLT.…”

Section: Introductionmentioning

confidence: 99%

Performance of the VLT Planet Finder SPHERE

Zurlo

Vigan

Mesa

et al. 2014

A&A

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Context. The new planet finder for the Very Large Telescope (VLT), the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), just had its first light in Paranal. A dedicated instrument for the direct detection of planets, SPHERE, is composed of a polametric camera in visible light, the Zurich IMager POLarimeter (ZIMPOL), and two near-infrared sub-systems: the Infra-Red Dual-beam Imager and Spectrograph (IRDIS), a multi-purpose camera for imaging, polarimetry, and long-slit spectroscopy, and the integral field spectrograph (IFS), an integral field spectrograph. Aims. We present the results obtained from the analysis of data taken during the laboratory integration and validation phase, after the injection of synthetic planets. Since no continuous field rotation could be performed in the laboratory, this analysis presents results obtained using reduction techniques that do not use the angular differential imaging (ADI) technique. Methods. To perform the simulations, we used the instrumental point spread function (PSF) and model spectra of L and T-type objects scaled in contrast with respect to the host star. We evaluated the expected error in astrometry and photometry as a function of the signal to noise of companions, after spectral differential imaging (SDI) reduction for IRDIS and spectral deconvolution (SD) or principal component analysis (PCA) data reductions for IFS. Results. We deduced from our analysis, for example, that β Picb, a 12 Myr old planet of ∼10 M Jup and semi-major axis of 9-10 AU, would be detected with IRDIS with a photometric error of 0.16 mag and with a relative astrometric position error of 1.1 mas. With IFS, we could retrieve a spectrum with error bars of about 0.15 mag on each channel and astrometric relative position error of 0.6 mas. For a fainter object such as HR 8799d, a 13 M Jup planet at a distance of 27 AU, IRDIS could obtain a relative astrometric error of 3 mas.

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The Seeds Direct Imaging Survey for Planets and Scattered Dust Emission in Debris Disk Systems

Cited by 89 publications

References 116 publications

A Statistical Analysis of Seeds and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?

A Statistical Analysis of Seeds and Other High-Contrast Exoplanet Surveys: Massive Planets or Low-Mass Brown Dwarfs?

High-contrast imaging withSpitzer: deep observations of Vega, Fomalhaut, andϵEridani

Performance of the VLT Planet Finder SPHERE

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