The<i>Herschel</i>/PACS view of the Cep OB2 region: Global protoplanetary disk evolution and clumpy star formation

Sicilia‐Aguilar, A.; Roccatagliata, V.; Getman, Konstantin V.; Rivière-Marichalar, P.; Birnstiel, T.; Merın, Bruno; Fang, Min; Henning, Thomas; Eiroa, C.; Currie, Thayne

doi:10.1051/0004-6361/201424669

Cited by 19 publications

(28 citation statements)

References 76 publications

(142 reference statements)

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“…This behavior might arise because it is hard to stop viscous accretion of gas through the disk unless the mass of the (outer) disk is very low. This seems to be the case for transition disks around low-mass/solar-type stars (Sicilia-Aguilar et al 2015). If trapping of mm-dust grains occurs at the inner rim of the outer disk, then a mm-dust depletion higher than the gas depletion would be expected inside the dust cavity (e.g., Pinilla et al 2016).…”

Section: Comparison To Other Transition Disks With Quantified Gas Surmentioning

confidence: 95%

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A gas density drop in the inner 6 AU of the transition disk around the Herbig Ae star HD 139614

Carmona

Thi

Kamp³

et al. 2017

A&A

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Context. Quantifying the gas surface density inside the dust cavities and gaps of transition disks is important to establish their origin. Aims. We seek to constrain the surface density of warm gas in the inner disk of HD 139614, an accreting 9 Myr Herbig Ae star with a (pre-)transition disk exhibiting a dust gap from 2.3±0.1 to 5.3±0.3 AU. Methods. We observed HD 139614 with ESO/VLT CRIRES and obtained high-resolution (R∼90 000) spectra of CO ro-vibrational emission at 4.7 µm. We derived constraints on the disk's structure by modeling the CO isotopolog line-profiles, the spectroastrometric signal, and the rotational diagrams using grids of flat Keplerian disk models. Results. We detected υ = 1 → 0 12 CO, 2→1 12 CO, 1→0 13 CO, 1→0 C 18 O, and 1→0 C 17 O ro-vibrational lines. Lines are consistent with disk emission and thermal excitation. 12 CO υ = 1 → 0 lines have an average width of 14 km s −1 , T gas of 450 K and an emitting region from 1 to 15 AU. 13 CO and C 18 O lines are on average 70 and 100 K colder, 1 and 4 km s −1 narrower than 12 CO υ = 1 → 0, and are dominated by emission at R≥ 6 AU. The 12 CO υ = 1 → 0 composite line-profile indicates that if there is a gap devoid of gas it must have a width narrower than 2 AU. We find that a drop in the gas surface density (δ gas ) at R < 5 − 6 AU is required to be able to simultaneously reproduce the line-profiles and rotational diagrams of the three CO isotopologs. Models without a gas density drop generate 13 CO and C 18 O emission lines that are too broad and warm. The value of δ gas can range from 10 −2 to 10 −4 depending on the gas-to-dust ratio of the outer disk. We find that the gas surface density profile at 1 < R < 6 AU is flat or increases with radius. We derive a gas column density at 1 < R < 6 AU of N H = 3 × 10 19 − 10 21 cm −2 (7 × 10 −5 − 2.4 × 10 −3 g cm −2 ) assuming N CO = 10 −4 N H . We find a 5σ upper limit on the CO column density N CO at R≤1 AU of 5 × 10 15 cm −2 (N H ≤ 5 × 10 19 cm −2 ). Conclusions. The dust gap in the disk of HD 139614 has molecular gas. The distribution and amount of gas at R≤ 6 AU in HD 139614 is very different from that of a primordial disk. The gas surface density in the disk at R ≤ 1 AU and at 1 < R < 6 AU is significantly lower than the surface density that would be expected from the accretion rate of HD 139614 (10 −8 M yr −1 ) assuming a standard viscous α-disk model. The gas density drop, the non-negative density gradient in the gas inside 6 AU, and the absence of a wide (> 2 AU) gas gap, suggest the presence of an embedded < 2 M J planet at around 4 AU. A. Carmona et al.: CO ro-vibrational emission in the transition disk HD 139614. 12 CO 1-0 P(6) 12 CO 1-0 P(7) 12 CO 1-0 P(9) 2.0 2.2 2.4 2.6 12 CO 1-0 P(10) -40 -20 0 20 40 0.2 0.6 1.0 12 CO 1-0 P(11) 12 CO 1-0 P(12) 12 CO 1-0 P(13) 12 CO 1-0 P(15) 13 CO 1-0 R(6) 13 CO 1-0 R(5) 13 CO 1-0 R(4) 2.0 2.2 13 CO 1-0 R(2) -40 -20 0 20 40 0.2 0.6 1.0 13 CO 1-0 R(0) 13 CO 1-0 P(1) 13 CO 1-0 P(2) 13 CO1-0P4 12 CO2-1P9 C 18 O 1-0 R(7) C 18 O 1-0 R(6) C 18 O 1-0 R(5)

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Section: Comparison To Other Transition Disks With Quantified Gas Surmentioning

confidence: 95%

“…A dust cavity can have a dust gap inside it. tween accreting and non-accreting transition disks, with the nonaccreting disks being significantly more evolved (lower masses, flatter disks) as seen with Herschel (Sicilia-Aguilar et al 2015).…”

Section: Introductionmentioning

confidence: 97%

A gas density drop in the inner 6 AU of the transition disk around the Herbig Ae star HD 139614

Carmona

Thi

Kamp³

et al. 2017

A&A

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“…The shape of A&A proofs: manuscript no. ms the disk is defined by the combination of H p (R 0 ) and ξ, which determine the emission at all wavelengths once all other parameters are fixed (Bulger et al 2014;Sicilia-Aguilar et al 2015). In summary, a disk model is defined by six parameters: the disk mass M d , inner and outer radii R i and R out , the slope of the surface density profile p, and the two parameters H p (R 0 ), ξ.…”

Section: Disk Modelsmentioning

confidence: 99%

Brown dwarf disks withHerschel: Linking far-infrared and (sub)-mm fluxes

Daemgen

Natta

Scholz

et al. 2016

A&A

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Brown dwarf disks are excellent laboratories to test our understanding of disk physics in an extreme parameter regime. In this paper we investigate a sample of 29 well-characterized brown dwarfs and very low-mass stars, for which Herschel far-infrared fluxes and (sub)-mm fluxes are available. We measured new Herschel PACS fluxes for 11 objects and complement these with (sub)-mm data and Herschel fluxes from the literature. We analyze their spectral energy distributions in comparison with results from radiative transfer modeling. Fluxes in the far-infrared are strongly affected by the shape and temperature of the disk (and hence stellar luminosity), whereas the (sub)-mm fluxes mostly depend on disk mass. Nevertheless, there is a clear correlation between far-infrared and (sub)mm fluxes. We argue that the link results from the combination of the stellar mass-luminosity relation and a scaling between disk mass and stellar mass. We find strong evidence of dust settling to the disk midplane. The spectral slopes between near-and far-infrared are mostly between −0.5 and −1.2 in our sample, which is comparable to more massive T Tauri stars; this may imply that the disk shapes are similar as well, although highly flared disks are rare among brown dwarfs. We find that dust temperatures in the range of 7-15 K, calculated with T ≈ 25 (L/L ⊙ ) 0.25 K, are appropriate for deriving disk masses from (sub)-mm fluxes for these low luminosity objects. About half of our sample hosts disks with at least one Jupiter mass, confirming that many brown dwarfs harbor sufficient material for the formation of Earth-mass planets in their midst.

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“…In addition to evolved disks, other disks are intrinsically faint, such as disks around BD. For these cases, the mid- and far-IR data may be a good option to set strong constraints to the total dust content (Currie & Sicilia-Aguilar 2011; Harvey et al 2012a; Sicilia-Aguilar et al 2011, 2013a, 2015a; Daemgen et al 2016), even though the degeneracy between disk scale height and total disk mass cannot be broken unless long-wavelength data is included.…”

Section: The Disk Massmentioning

confidence: 99%

A ‘Rosetta Stone’ for Protoplanetary Disks: The Synergy of Multi-Wavelength Observations

Sicilia‐Aguilar

Banzatti

Carmona

et al. 2016

Publ. Astron. Soc. Aust.

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The recent progress in instrumentation and telescope development has brought us different ways to observe protoplanetary disks, including interferometers, space missions, adaptive optics, polarimetry, and time-and spectrally-resolved data. While the new facilities have changed the way we can tackle the existing open problems in disk structure and evolution, there is a substantial lack of interconnection between different observing techniques and their user communities. Here, we explore the complementarity of some of the stateof-the-art observing techniques, and how they can be brought together in a collective effort to understand how disks evolve and disperse at the time of planet formation.This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh, 2016. Its goal is to clarify where multi-wavelength observations of disks converge in unveiling disk structure and evolution, and where they diverge and challenge our current understanding. We discuss caveats that should be considered when linking results from different observations, or when drawing conclusions based on limited datasets (in terms of wavelength or sample). We focus on disk properties that are currently being revolutionized by multi-wavelength observations. Specifically: the inner disk radius, holes and gaps and their link to large-scale disk structures, the disk mass, and the accretion rate. We discuss how the links between them, as well as the apparent contradictions, can help us to disentangle the disk physics and to learn about disk evolution.

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TheHerschel/PACS view of the Cep OB2 region: Global protoplanetary disk evolution and clumpy star formation

Cited by 19 publications

References 76 publications

A gas density drop in the inner 6 AU of the transition disk around the Herbig Ae star HD 139614

A gas density drop in the inner 6 AU of the transition disk around the Herbig Ae star HD 139614

Brown dwarf disks withHerschel: Linking far-infrared and (sub)-mm fluxes

A ‘Rosetta Stone’ for Protoplanetary Disks: The Synergy of Multi-Wavelength Observations

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