Gaps in the Hd 169142 Protoplanetary Disk Revealed by Polarimetric Imaging: Signs of Ongoing Planet Formation?

Quanz, Sascha P.; Avenhaus, H.; Buenzli, E.; Garufi, A.; Schmid, Hans Martin; Wolf, S.

doi:10.1088/2041-8205/766/1/l2

Cited by 177 publications

(227 citation statements)

References 43 publications

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“…The companion location also fits well with the extent and the location of cavities/gaps/spirals in young structured (or transition) disks (Andrews et al 2011;Grady et al 2013;Quanz et al 2013b) discovered around Herbig Ae stars. κ And b's separation is close to that of the candidate substellar embryo (Quanz et al 2013a) around the 2.4 M star HD 100546, whose mass might extend inside the "brown-dwarf" regime.…”

Section: Discussionsupporting

confidence: 79%

“…Nevertheless, the subsequent formation pathway remains unclear. Core accretion (CA) could eventually explain the properties of directly imaged planets with the narrowest orbits (HR 8799 e and d, β Pictoris b; Kennedy & Kenyon 2008;Mordasini et al 2009a;Rafikov 2011). But associated CA formation timescales become too long compared to the mean lifetime of primordial disks and require higher disk surface density for an in-situ formation at more than ∼15 AU (Boley 2009;Dodson-Robinson et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Characterization of the gaseous companionκAndromedae b

Bonnefoy¹,

Currie²,

Marleau³

et al. 2014

A&A

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Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 ± 2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (K s ), 3.776 (L ), 4.052 (NB_4.05), and 4.78 µm (M ) obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15.86 ± 0.21, H = 14.95 ± 0.13, K s = 14.32 ± 0.09 mag for κ And b. We detect the companion in all our high-contrast observations. We confirm previous contrasts obtained at K s and L band. We derive NB_4.05 = 13.0 ± 0.2, and M = 13.3 ± 0.3 mag and estimate log 10 (L/L ) = −3.76 ± 0.06. Atmospheric models yield T eff = 1900 +100 −200 K. They do not set any constraint on the surface gravity. "Hotstart" evolutionary models predict masses of 14 +25 −2 M Jup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30 +120 −10 Myr), "warm-start" evolutionary tracks constrain the mass to M ≥ 10 M Jup . Conclusions. The mass of κ Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.

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Section: Discussionsupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Characterization of the gaseous companionκAndromedae b

Bonnefoy¹,

Currie²,

Marleau³

et al. 2014

A&A

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“…They mark a crucial phase in disk evolution, intermediate between fully gas-rich and gas-depleted systems. Their existence was first suggested by the distinctive near-tomid-infrared (NIR-MIR) dips in their spectral energy distributions (SEDs; e.g., Strom et al 1989;Skrutskie et al 1990;Calvet et al 2005;Espaillat et al 2007Espaillat et al , 2008, and later confirmed by resolved images in NIR scattered light (e.g., Thalmann et al 2010;Hashimoto et al 2012;Mayama et al 2012;Garufi et al 2013;Quanz et al 2013;Avenhaus et al 2014aAvenhaus et al , 2014bTsukagoshi et al 2014) and by resolved mm wave maps of dust continuum and gas line emission (e.g., Andrews et al 2011;Mathews et al 2012;Tang et al 2012;Fukagawa et al 2013;Isella et al 2013;van der Marel et al 2013van der Marel et al , 2014van der Marel et al , 2015aPérez et al 2014;Zhang et al 2014;Canovas et al 2015;Hashimoto et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Sizes and Depletions of the Dust and Gas Cavities in the Transitional Disk J160421.7-213028

Dong

Marel

Hashimoto

et al. 2017

ApJ

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We report ALMA Cycle 2 observations of 230 GHz (1.3 mm) dust continuum emission, and 12 CO, 13 CO, and C 18 O J=2-1 line emission, from the Upper Scorpius transitional disk [PZ99] J160421.7-213028, with an angular resolution of ∼  0. 25 (35 au). Armed with these data and existing H-band scattered light observations, we measure the size and depth of the disk's central cavity, and the sharpness of its outer edge, in three components: sub-μm-sized "small" dust traced by scattered light, millimeter-sized "big" dust traced by the millimeter continuum, and gas traced by line emission. Both dust populations feature a cavity of radius ∼70 au that is depleted by factors of at least 1000 relative to the dust density just outside. The millimeter continuum data are well explained by a cavity with a sharp edge. Scattered light observations can be fitted with a cavity in small dust that has either a sharp edge at 60 au, or an edge that transitions smoothly over an annular width of 10 au near 60 au. In gas, the data are consistent with a cavity that is smaller, about 15 au in radius, and whose surface density at 15 au is  10 3 1 times smaller than the surface density at 70 au; the gas density grades smoothly between these two radii. The CO isotopologue observations rule out a sharp drop in gas surface density at 30 au or a double-drop model, as found by previous modeling. Future observations are needed to assess the nature of these gas and dust cavities (e.g., whether they are opened by multiple as-yet-unseen planets or photoevaporation).

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“…Dust imaging of a protoplanetary disks enables studying the spatial distribution of dust grains for different sizes in the disk. High spatial resolution observations of transitional disks reveal complex disk structures and can be used to study the interaction between dust gaps and protoplanets (e.g., van der Marel et al 2013;Casassus et al 2013;Quanz et al 2013). Characterizing the connection between the radial structure and the SED is thus important to gain insight into the role of planet formation in the evolution of protoplanetary disks.…”

Section: Introductionmentioning

confidence: 99%

Large dust gaps in the transitional disks of HD 100453 and HD 34282

Khalafinejad

Maaskant

Mariñas

et al. 2016

A&A

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Context. The formation of dust gaps in protoplanetary disks is one of the most important signs of disk evolution and might indicate the formation of planets. Aims. We aim to characterize the flaring disk structure around the Herbig Ae/Be stars HD 100453 and HD 34282. Their spectral energy distributions (SEDs) show an emission excess between 15−40 µm, but very weak (HD 100453) and no (HD 34282) signs of the 10 and 20 µm amorphous silicate features. We investigate whether this implies the presence of large dust gaps. Methods. We investigated spatially resolved mid-infrared Q-band images taken with Gemini North/MICHELLE. We performed radiative transfer modeling and examined the radial distribution of dust. We simultaneously fit the Q-band images and SEDs of HD 100453 and HD 34282. Results. Our solutions require that the inner halos and outer disks be separated by large dust gaps that are depleted with respect to the outer disk by a factor of 1000 or more. The inner edges of the outer disks of HD 100453 and HD 34282 have temperatures of ∼160 ± 10 K and ∼60 ± 5 K, respectively. Because of the high surface brightness of these walls, they dominate the emission in the Q band. Their radii are constrained at 20 +2 −2 AU and 92 +31 −17 AU, respectively. Conclusions. HD 100453 and HD 34282 most likely have disk dust gaps. The upper limit of the dust mass in each gap is estimated to be about 10 −7 M . We find that the locations and sizes of disk dust gaps are connected to the SED, as traced by the mid-infrared flux ratio F 30 /F 13.5 . We propose a new classification scheme for the Meeus groups based on the F 30 /F 13.5 ratio. The absence of amorphous silicate features in the observed SEDs is caused by the depletion of small ( 1 µm) silicate dust at temperatures above 160 K, which could be related to the presence of a dust gap in that region of the disk.

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Gaps in the Hd 169142 Protoplanetary Disk Revealed by Polarimetric Imaging: Signs of Ongoing Planet Formation?

Cited by 177 publications

References 43 publications

Characterization of the gaseous companionκAndromedae b

Characterization of the gaseous companionκAndromedae b

The Sizes and Depletions of the Dust and Gas Cavities in the Transitional Disk J160421.7-213028

Large dust gaps in the transitional disks of HD 100453 and HD 34282

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