Resolved millimeter-dust continuum cavity around the very low mass young star CIDA 1

Pinilla, P.; Natta, A.; Manara, C. F.; Ricci, Luca; Scholz, A.; Testi, L.

doi:10.1051/0004-6361/201832690

Cited by 25 publications

(39 citation statements)

References 73 publications

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“…If the overbrightness traces the tip of a spiral arm, we would expect it to not be co-radial, as observed for Ring #2. Interestingly, the continuum ALMA data (Barenfeld et al 2016;Pinilla et al 2018a) show a low contrast asymmetry (contrast less than a factor of two) along the same angle as the one observed in the scattered light data, supporting a density enhancement. However, it is located close to the outer ring (Ring #1), at large radii (in the ALMA image, peaking at 0.5 or 84 au), and does not coincide with the inner ring (Ring #2).…”

Section: Rings Gaps and Brightness Asymmetriessupporting

confidence: 61%

“…Modeling of the visibility data of ALMA observations reveals that there is a large cavity in the millimeter emission, surrounded by an asymmetric ring peaking at 84 au (0.5 , Pinilla et al 2018a). This location coincides with the outer edge of Ring #1 that extends from ∼0.3 to ∼0.5 and peaks approximately at ∼0.45 .…”

Section: Rings Gaps and Brightness Asymmetriesmentioning

confidence: 99%

“…Barenfeld et al (2016) observed ∼100 disk-host candidates in Upper Sco with ALMA, including HD 143006, and showed that, not only does Upper Sco have a lower fraction of disk-host stars than younger regions (such as Taurus or Lupus), but also that these disks have a lower dust mass to stellar mass ratio. The disk around HD 143006 (hereafter only referred to as HD 143006) is resolved at 0.88 mm with a ∼ 0.35 × 0.3 beam, and its continuum map shows a centrally depleted large cavity (∼84 au, Pinilla et al 2018a), and a low-contrast brightness asymmetry with an enhanced emission (by a factor 2) in the south-east (Barenfeld et al 2016). The innermost region, however, remains dust-and gas-rich as indicated by the high near infrared (IR) excess (∼21%, Garufi et al submitted), and by near IR interferometric observations that resolve hot dust at the sub-au scale (Lazareff et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Benisty

Juhász

Facchini

et al. 2018

A&A

115

113

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Context. While planet formation is thought to occur early in the history of a protoplanetary disk, the presence of planets embedded in disks, or of other processes driving disk evolution, might be traced from their imprints on the disk structure. Aims. We study the morphology of the disk around the T Tauri star HD 143006, located in the ∼5-11 Myr-old Upper Sco region, and we look for signatures of the mechanisms driving its evolution. Methods. We observed HD 143006 in polarized scattered light with VLT/SPHERE at near-infrared (J-band, 1.2 µm) wavelengths, reaching an angular resolution of ∼0.037 (∼6 au). We obtained two datasets, one with a 145 mas diameter coronagraph, and the other without, enabling us to probe the disk structure down to an angular separation of ∼0.06 (∼10 au). Results. In our observations, the disk of HD 143006 is clearly resolved up to ∼0.5 and shows a clear large-scale asymmetry with the eastern side brighter than the western side. We detect a number of additional features, including two gaps and a ring. The ring shows an overbrightness at a position angle (PA) of ∼140 • , extending over a range in position angle of ∼60 • , and two narrow dark regions. The two narrow dark lanes and the overall large-scale asymmetry are indicative of shadowing effects, likely due to a misaligned inner disk. We demonstrate the remarkable resemblance between the scattered light image of HD 143006 and a model prediction of a warped disk due to an inclined binary companion. The warped disk model, based on the hydrodynamic simulations combined with three-dimensional radiative transfer calculations, reproduces all major morphological features. However, it does not account for the observed overbrightness at PA∼140 • . Conclusions. Shadows have been detected in several protoplanetary disks, suggesting that misalignment in disks is not uncommon. However, the origin of the misalignment is not clear. As-yet-undetected stellar or massive planetary companions could be responsible for them, and naturally account for the presence of depleted inner cavities.

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Section: Rings Gaps and Brightness Asymmetriessupporting

confidence: 61%

Section: Rings Gaps and Brightness Asymmetriesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Benisty

Juhász

Facchini

et al. 2018

A&A

115

113

View full text Add to dashboard Cite

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“…We find that the disk of 2M0444 is best fit with a pre-transitional disk model with a gap in the disk from 0.02 au to 0.27 au. Transitional disks (i.e., disks with holes with large depletions of dust in the inner disk) have been previously inferred around one BD based on its SED (2MASS J03445771+3207416; Muzerolle et al 2006) and imaged around a very-low-mass star (CIDA 1; Pinilla et al 2018); 2M0444 would be the first inferred pre-transitional BD disk. Given that pretransitional and transitional disks are not uncommon around around T Tauri stars (e.g., Espaillat et al 2007;Muzerolle et al 2010;Kim et al 2013), BD disks may exhibit the same types of structures.…”

Section: Gap In the Disk Of 2m0444mentioning

confidence: 96%

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Rilinger

Espaillat

Macías

2019

ApJ

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Measuring the properties of protoplanetary disks around brown dwarfs is central to understanding the formation of brown dwarfs and their planetary companions. We present modeling of CFHT Tau 4 and 2M0444, two brown dwarfs with protoplanetary disks in the Taurus Molecular Cloud. By combining modeling of the spectral energy distributions and ALMA images, we obtain disk radii and masses for these objects; these parameters can be used to constrain brown dwarf formation and planet formation, respectively. We find that the disk around CFHT Tau 4 has a total mass of 0.42 M Jup and a radius of 80 au; we find 2M0444's disk to have a mass of 2.05 M Jup and a radius of 100 au. These radii are more consistent with those predicted by theoretical simulations of brown dwarf formation via undisturbed condensation from a mass reservoir than those predicted by ejection from the formation region. Furthermore, the disk mass of 2M0444 suggests that planet formation may be possible in this disk, although the disk of CFHT Tau 4 is likely not massive enough to form planets. The disk properties measured here provide constraints to theoretical models of brown dwarf formation and the formation of their planetary companions.

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“…Analysis of the gas kinematics can also be used as an indirect method to study embedded planets (Teague et al 2018;Pinte et al 2018). Other indirect indications, such as the the existence of gaps, spirals, assymmetries, and dust processing are observed frequently, and suggest that planets might already have formed (e.g., ALMA Partnership et al 2015;Zhang et al 2018;Lodato et al 2019;Pinilla et al 2018).…”

Section: Planet Formation Around Bdsmentioning

confidence: 99%

Demographics of disks around young very low-mass stars and brown dwarfs in Lupus

Sanchís

Testi

Natta

et al. 2020

A&A

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We present new 890 µm continuum ALMA observations of 5 brown dwarfs (BDs) with infrared excess in Lupus I and III -which, in combination with 4 BDs previously observed, allowed us to study the mm properties of the full known BD disk population of one star-forming region. Emission is detected in 5 out of the 9 BD disks. Dust disk mass, brightness profiles and characteristic sizes of the BD population are inferred from continuum flux and modeling of the observations. Only one source is marginally resolved, allowing for the determination of its disk characteristic size. We conduct a demographic comparison between the properties of disks around BDs and stars in Lupus. Due to the small sample size, we cannot confirm or disprove if the disk mass over stellar mass ratio drops for BDs, as suggested for Ophiuchus. Nevertheless, we find that all detected BD disks have an estimated dust mass between 0.2 and 3.2 M C ; these results suggest that the measured solid masses in BD disks can not explain the observed exoplanet population, analogous to earlier findings on disks around more massive stars. Combined with the low estimated accretion rates, and assuming that the mm-continuum emission is a reliable proxy for the total disk mass, we derive ratios of 9 M acc {M disk significantly lower than in disks around more massive stars. If confirmed with more accurate measurements of disk gas masses, this result could imply a qualitatively different relationship between disk masses and inward gas transport in BD disks.

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Resolved millimeter-dust continuum cavity around the very low mass young star CIDA 1

Cited by 25 publications

References 73 publications

Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Shadows and asymmetries in the T Tauri disk HD 143006: evidence for a misaligned inner disk

Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud

Demographics of disks around young very low-mass stars and brown dwarfs in Lupus

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