High-resolution ALMA observation of the 12CO(3–2) and 350 GHz continuum emissions of the debris disc of 49 Ceti

Nhung, P. T.; Hoai, D. T.; Tuan-Anh, P.; Diep, P. N.; Phượng, Nguyễn Thị Kim; Thảo, Nguyễn Thị Phương; Darriulat, P.

doi:10.1093/mnras/stx1125

Cited by 5 publications

(5 citation statements)

References 31 publications

(95 reference statements)

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“…These models yield CO masses of 10 −3.8 and 10 −3.5 M ⊕ , respectively, more than an order of magnitude smaller than our CO mass (10 −2.15 M ⊕ ). A similar discrepancy applies to the column density derived by Nhung et al (2017) based on 12 CO 3-2. We find that the 12 CO 2-1 and 3-2 emission is strongly optically thick (τ ∼ 120), while Hughes et al (2017) concluded…”

Section: Appendix a Continuum Fluxessupporting

confidence: 58%

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Cataldi

Aikawa

Iwasaki

et al. 2023

ApJ

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The origin and evolution of gas in debris disks are still not well understood. Secondary gas production from cometary material or a primordial origin have been proposed. So far, observations have mostly concentrated on CO, with only a few C observations available. We overview the C and CO content of debris disk gas and test state-of-the-art models. We use new and archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO and C i emission, complemented by C ii data from Herschel, for a sample of 14 debris disks. This expands the number of disks with ALMA measurements of both CO and C i by 10 disks. We present new detections of C i emission toward three disks: HD 21997, HD 121191, and HD 121617. We use a simple disk model to derive gas masses and column densities. We find that current state-of-the-art models of secondary gas production overpredict the C0 content of debris disk gas. This does not rule out a secondary origin, but might indicate that the models require an additional C removal process. Alternatively, the gas might be produced in transient events rather than a steady-state collisional cascade. We also test a primordial gas origin by comparing our results to a simplified thermochemical model. This yields promising results, but more detailed work is required before a conclusion can be reached. Our work demonstrates that the combination of C and CO data is a powerful tool to advance our understanding of debris disk gas.

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Section: Appendix a Continuum Fluxessupporting

confidence: 58%

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Cataldi

Aikawa

Iwasaki

et al. 2023

ApJ

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“…The 49 Cet debris disc system was subject to several modelling projects, either concentrating on the dust (e.g., Wahhaj et al 2007;Pawellek et al 2014;Choquet et al 2017), the gas (e.g., Roberge et al 2014;Miles et al 2016) or both components (e.g., Roberge et al 2013;Nhung et al 2017;Hughes et al 2017). In this study we focus on the dust component.…”

Section: Modelling Strategymentioning

confidence: 99%

A multiwavelength study of the debris disc around 49 Cet

Pawellek

Moór

Milli

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In a multiwavelength study of thermal emission and scattered light images we analyse the dust properties and structure of the debris disc around the A1-type main-sequence star 49 Cet. As a basis for this study, we present new scattered light images of the debris disc known to possess a high amount of both dust and gas. The outer region of the disc is revealed in former coronagraphic H-band and our new Y-band images from the Very Large Telescope SPHERE instrument. We use the knowledge of the disc’s radial extent inferred from ALMA observations and the grain size distribution found by spectral energy distribution fitting to generate semidynamical dust models of the disc. We compare the models to scattered light and thermal emission data and find that a disc with a maximum surface density at 110 au and shallow edges can describe both the thermal emission and the scattered light observations. This suggests that grains close to the blow-out limit and large grains stem from the same planetesimal population and are mainly influenced by radiation pressure. The influence of inward transport processes could not be analysed in this study.

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“…In particular one aims at identifying clearly which physico-chemical conditions need to be fulfilled for planets to start forming. We have studied several young stars [21][22][23], in particular a multiple stellar system, GG Tau A, which is presented below. GG Tau A, located at 150 pc in the Taurus molecular cloud [24,25], is considered to be an archetype of a T-Tauri  solar mass protostar multiple system.…”

Section: Young Starsmentioning

confidence: 99%

Astrophysics research at DAP

et al. 2020

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The research and training team of the Department of Astrophysics (DAP), Vietnam National Space Center, is some twenty years old. Currently, we work in the fields of stellar physics and high-redshift galaxies using mm/sub-mm data observed by world-leading radio interferometers such as ALMA and NOEMA. In this report, we present the research team and its activities and give illustrations of the research work with emphasis on the use of archival data.

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High-resolution ALMA observation of the 12CO(3–2) and 350 GHz continuum emissions of the debris disc of 49 Ceti

Cited by 5 publications

References 31 publications

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*

A multiwavelength study of the debris disc around 49 Cet

Astrophysics research at DAP

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