Infrared camera and spectrograph for the Subaru Telescope

Kobayashi, Naoto; Tokunaga, A. T.; Terada, Hiroshi; Goto, Miwa; Weber, M.; Potter, Robert D.; Onaka, Peter M.; Ching, Gregory K.; Young, Tony T.; Fletcher, Kent; Neil, Douglas M.; Robertson, Louis; Cook, Daniel; Imanishi, Masatoshi; Warren, David W.

doi:10.1117/12.317277

Cited by 121 publications

(17 citation statements)

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“…We first imaged 2MASS 0122-2439 with the Infrared Camera and Spectrograph (IRCS; Kobayashi et al 2000;Tokunaga et al 1998) combined with the AO188 adaptive optics system (Hayano et al 2010) at the Subaru Telescope on UT 2012 October 12. Natural guide star (NGS) AO was used with 2MASS 0122-2439 A (R = 13.2 mag) acting as the wavefront reference.…”

Section: Subaru/ircs Adaptive Optics Imagingmentioning

confidence: 99%

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

129

145

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We report the discovery of an L-type companion to the young M3.5V star 2MASS J01225093-2439505 at a projected separation of 1. 45 (≈52 AU) as part of our adaptive optics imaging search for extrasolar giant planets around young low-mass stars. 2MASS 0122-2439 B has very red near-infrared colors similar to the HR 8799 planets and the reddest known young/dusty L dwarfs in the field. Moderate-resolution (R ≈ 3800) 1.5-2.4 μm spectroscopy reveals a near-infrared spectral type of L4-L6 and an angular H-band shape, confirming its cool temperature and young age. The kinematics of 2MASS 0122-2439 AB are marginally consistent with members of the ∼120 Myr AB Dor young moving group based on the photometric distance to the primary (36 ± 4 pc) and our radial velocity measurement of 2MASS 0122-2439 A from Keck/HIRES. We adopt the AB Dor group age for the system, but the high energy emission, lack of Li i λ6707 absorption, and spectral shape of 2MASS 0122-2439 B suggest a range of ∼10-120 Myr is possible. The age and luminosity of 2MASS 0122-2439 B fall in a strip where "hot-start" evolutionary model mass tracks overlap as a result of deuterium burning. Several known substellar companions also fall in this region (2MASS J0103-5515 ABb, AB Pic b, κ And b, G196-3 B, SDSS 2249+0044 B, LP 261-75 B, HD 203030 B, and HN Peg B), but their dual-valued mass predictions have largely been unrecognized. The implied mass of 2MASS 0122-2439 B is ≈12-13 M Jup or ≈22-27 M Jup if it is an AB Dor member, or possibly as low as 11 M Jup if the wider age range is adopted. Evolutionary models predict an effective temperature for 2MASS 0122-2439 B that corresponds to spectral types near the L/T transition (≈1300-1500 K) for field objects. However, we find a mid-L near-infrared spectral type, indicating that 2MASS 0122-2439 B represents another case of photospheric dust being retained to cooler temperatures at low surface gravities, as seen in the spectra of young (8-30 Myr) planetary companions. Altogether, the low mass, low temperature, and red colors of 2MASS 0122-2439 B make it a bridge between warm planets like β Pic b and cool, very dusty ones like HR 8799 bcde.

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Section: Subaru/ircs Adaptive Optics Imagingmentioning

confidence: 99%

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

129

145

View full text Add to dashboard Cite

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“…The Infrared Camera and Spectrograph (IRCS; Tokunaga et al 1998;Kobayashi et al 2000) was used in its lowresolution spectrograph mode. The IRCS was equipped with an Aladdin-III 1024 × 1024 InSb array at the Infrared Nasmyth focus (Terada et al 2004).…”

Section: Observationsmentioning

confidence: 99%

High-Albedo C-Complex Asteroids in the Outer Main Belt: The Near-Infrared Spectra

Kasuga

Usui

Ootsubo

et al. 2013

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Primitive, outer-belt asteroids are generally of low albedo, reflecting carbonaceous compositions like those of CI and CM meteorites. However, a few outer-belt asteroids having high albedos are known, suggesting the presence of unusually reflective surface minerals or, conceivably, even exposed water ice. Here, we present near-infrared (1.1-2.5 μm) spectra of four outer-belt C-complex asteroids with albedos 0.1. We find no absorption features characteristic of water ice (near 1.5 and 2.0 μm) in the objects. Intimate mixture models set limits to the water ice by weight 2%. Asteroids (723) Hammonia and (936) Kunigunde are featureless and have (60%-95%) amorphous Mg pyroxenes that might explain the high albedos. Asteroid (1276) Ucclia also shows a featureless reflection spectrum with (50%-60%) amorphous Mg pyroxenes. Asteroid (1576) Fabiola shows a possible weak, broad absorption band (1.5-2.1 μm). The feature can be reproduced by (80%) amorphous Mg pyroxenes or orthopyroxene (crystalline silicate), either of which is likely to cause its high albedo. We discuss the origin of high-albedo components in primitive asteroids.

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“…We targeted HR 8799 in L on 2012 July 26 with the IRCS camera (Tokunaga et al 1998) using the narrow (20.43 mas pixel −1 ) camera with angular differential imaging/ pupil tracking mode (Marois et al 2006) and without a focal plane mask (Subaru Program S12A-051). We modified the IRCS software to record out 0.15 s short exposures and combine frames into data cubes every 200 frames for a cumulative integration time of 30 s. We "stared" at the star at a fixed position for four 10-20 minute sequences bracketed by a series of 5-10 dithered sky frames, sacrificing raw background-limited sensitivity for better PSF stability.…”

Section: Subaru/ircs Data (L )mentioning

confidence: 99%

DEEP THERMAL INFRARED IMAGING OF HR 8799 bcde: NEW ATMOSPHERIC CONSTRAINTS AND LIMITS ON A FIFTH PLANET

Currie

Burrows

Girard

et al. 2014

ApJ

109

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We present new L (3.8 μm) and Brα (4.05 μm) data and reprocessed archival L data for the young, planet-hosting star HR 8799 obtained with Keck/NIRC2, VLT/NaCo, and Subaru/IRCS. We detect all four HR 8799 planets in each data set at a moderate to high signal-to-noise ratio (S/N 6-15). We fail to identify a fifth planet, "HR 8799 f," at r < 15 AU at a 5σ confidence level: one suggestive, marginally significant residual at 0. 2 is most likely a pointspread function artifact. Assuming companion ages of 30 Myr and the Baraffe planet cooling models, we rule out an HR 8799 f with a mass of 5 M J (7 M J ), 7 M J (10 M J ), or 12 M J (13 M J ) at r proj ∼ 12 AU, 9 AU, and 5 AU, respectively. All four HR 8799 planets have red early T dwarf-like L − [4.05] colors, suggesting that their spectral energy distributions peak in between the L and M broadband filters. We find no statistically significant difference in HR 8799 cde's color. Atmosphere models assuming thick, patchy clouds appear to better match HR 8799 bcde's photometry than models assuming a uniform cloud layer. While non-equilibrium carbon chemistry is required to explain HR 8799 b and c's photometry/spectra, evidence for it from HR 8799 d and e's photometry is weaker. Future, deep-IR spectroscopy/spectrophotometry with the Gemini Planet Imager, SCExAO/CHARIS, and other facilities may clarify whether the planets are chemically similar or heterogeneous.

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Infrared camera and spectrograph for the Subaru Telescope

Cited by 121 publications

References 0 publications

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

High-Albedo C-Complex Asteroids in the Outer Main Belt: The Near-Infrared Spectra

DEEP THERMAL INFRARED IMAGING OF HR 8799 bcde: NEW ATMOSPHERIC CONSTRAINTS AND LIMITS ON A FIFTH PLANET

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