DIRECT IMAGING DISCOVERY OF A “SUPER-JUPITER” AROUND THE LATE B-TYPE STAR
                    <b>
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                    And

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

doi:10.1088/2041-8205/763/2/l32

Cited by 172 publications

(82 citation statements)

References 42 publications

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“…Comparing other young (<1 Gyr) substellar companions to the cooling models in Figure 4 shows that several known objects also fall in or very close to this region: 2MASS J01033563-5515561 ABb (Delorme et al 2013), AB Pic b (Chauvin et al 2005), κ And b (Carson et al 2013), G196-3 B (Rebolo et al 1998), SDSS J224953.47+004404.6 B (Allers et al 2010), LP261-75 B (Reid & Walkowicz 2006), HD 203030 B (Metchev & Hillenbrand 2006), and HN Peg B (Luhman et al 2007). For these objects, a luminosity and age do not translate into a unique mass prediction, instead being consistent with both ≈12-14 M Jup and ≈20-26 M Jup mass tracks.…”

Section: Discussionmentioning

confidence: 91%

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

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

131

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: Discussionmentioning

confidence: 91%

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

Bowler

Liu²,

Shkolnik

et al. 2013

ApJ

131

145

View full text Add to dashboard Cite

show abstract

“…Ages derived for early-type stars based on HR diagram measurements are extremely sensitive to rotation/ inclination effects. As shown for κ And, including rotation/ inclination effects can significantly reduce the star's estimated age and the interpretation of any imaged companions (Carson et al 2013;Jones et al 2016).…”

Section: Discussionmentioning

confidence: 99%

Subaru/SCExAO First-light Direct Imaging of a Young Debris Disk around HD 36546

Currie

Guyon

Tamura

et al. 2017

ApJL

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We present H-band scattered light imaging of a bright debris disk around the A0 star HD 36546 obtained from the Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system with data recorded by the HiCIAO camera using the vector vortex coronagraph. SCExAO traces the disk from r∼0 3 to r∼1″ (34-114 au). The disk is oriented in a near east-west direction (PA∼75°), is inclined by i∼70°-75°, and is strongly forward-scattering (g>0.5). It is an extended disk rather than a sharp ring; a second, diffuse dust population extends from the disk's eastern side. While HD 36546 intrinsic properties are consistent with a wide age range (t∼1-250 Myr), its kinematics and analysis of coeval stars suggest a young age (3-10 Myr) and a possible connection to TaurusAuriga's star formation history. SCExAO's planet-to-star contrast ratios are comparable to the first-light Gemini Planet Imager contrasts; for an age of 10 Myr, we rule out planets with masses comparable to HR 8799 b beyond a projected separation of 23 au. A massive icy planetesimal disk or an unseen super-Jovian planet at r>20 au may explain the disk's visibility. The HD 36546 debris disk may be the youngest debris disk yet imaged, is the first newly identified object from the now-operational SCExAO extreme AO system, is ideally suited for spectroscopic follow-up with SCExAO/CHARIS in 2017, and may be a key probe of icy planet formation and planet-disk interactions.

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“…Uncertainties in model-derived properties constitute the dominant systematic error for in-situ measurements of the IMF for young populations (Bastian et al 2010), determinations of star cluster ages (e.g., Preibisch et al 2001versus Pecaut et al 2012, comparison of protoplanetary disk properties to those of mature planetary systems (Andrews et al 2013), and binary formation studies (e.g., Kraus et al 2011a;Kraus & Hillenbrand 2012;Duchêne & Kraus 2013). Mass/age ambiguities strongly limit interpretations for directly imaged gas giant planets in young populations, where the host-star age and companion luminosity establish the planet mass (e.g., Lafrenière et al 2008versus Pecaut et al 2012, and also Carson et al 2013versus Hinkley et al 2013.…”

Section: Introductionmentioning

confidence: 99%

The Mass–radius Relation of Young Stars. I. Usco 5, an M4.5 Eclipsing Binary in Upper Scorpius Observed by K2

Kraus

Cody

Covey

et al. 2015

ApJ

140

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We present the discovery that UScoCTIO 5, a known spectroscopic binary in the Upper Scorpius star-forming region, is an eclipsing system with both primary and secondary eclipses apparent in K2 light curves obtained during Campaign 2. We have simultaneously fit the eclipse profiles from the K2 light curves and the existing RV data to demonstrate that UScoCTIO 5 consists of a pair of nearly identical M4.5 stars withThe radii are broadly consistent with pre-main-sequence ages predicted by stellar evolutionary models, but none agree to within the uncertainties. All models predict systematically incorrect masses at the 25%-50% level for the HR diagram position of these mid-M dwarfs, suggesting significant modifications to mass-dependent outcomes of star and planet formation. The form of the discrepancy for most model sets is not that they predict luminosities that are too low, but rather that they predict temperatures that are too high, suggesting that the models do not fully encompass the physics of energy transport (via convection and/or missing opacities) and/or a miscalibration of the SpT-T eff scale. The simplest modification to the models (changing T eff to match observations) would yield an older age for this system, in line with the recently proposed older age of Upper Scorpius (τ ∼ 11 Myr).

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DIRECT IMAGING DISCOVERY OF A “SUPER-JUPITER” AROUND THE LATE B-TYPE STAR κ And

Cited by 172 publications

References 42 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,

Subaru/SCExAO First-light Direct Imaging of a Young Debris Disk around HD 36546

The Mass–radius Relation of Young Stars. I. Usco 5, an M4.5 Eclipsing Binary in Upper Scorpius Observed by K2

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