ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Garufi, A.; Podio, L.; Codella, C.; Rygl, K. L. J.; Bacciotti, F.; Facchini, Stefano; Fedele, D.; Miotello, A.; Teague, Richard; Testi, L.

doi:10.1051/0004-6361/201937247

Cited by 29 publications

(53 citation statements)

References 78 publications

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“…In this work, we report on new images of IRAS 04302 at ∼0 . 3 (∼48 au) taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in the context of the ALMA-DOT program (ALMA chemical survey of Disk-Outflow sources in Taurus, see Garufi et al 2020, and in prep. ).…”

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confidence: 99%

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Podio

Garufi

Codella

et al. 2020

A&A

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The chemical composition of planets is inherited from that of the natal protoplanetary disk at the time of planet formation. Increasing observational evidence suggests that planet formation occurs in less than 1−2 Myr. This motivates the need for spatially resolved spectral observations of young Class I disks, as carried out by the ALMA chemical survey of Disk-Outflow sources in Taurus (ALMA-DOT). In the context of ALMA-DOT, we observe the edge-on disk around the Class I source IRAS 04302+2247 (the butterfly star) in the 1.3 mm continuum and five molecular lines. We report the first tentative detection of methanol (CH3OH) in a Class I disk and resolve, for the first time, the vertical structure of a disk with multiple molecular tracers. The bulk of the emission in the CO 2−1, CS 5−4, and o–H2CO 31, 2 − 21, 1 lines originates from the warm molecular layer, with the line intensity peaking at increasing disk heights, z, for increasing radial distances, r. Molecular emission is vertically stratified, with CO observed at larger disk heights (aperture z/r ∼ 0.41−0.45) compared to both CS and H2CO, which are nearly cospatial (z/r ∼ 0.21−0.28). In the outer midplane, the line emission decreases due to molecular freeze-out onto dust grains (freeze-out layer) by a factor of > 100 (CO) and 15 (CS). The H2CO emission decreases by a factor of only about 2, which is possibly due to H2CO formation on icy grains, followed by a nonthermal release into the gas phase. The inferred [CH3OH]/[H2CO] abundance ratio is 0.5−0.6, which is 1−2 orders of magnitude lower than for Class 0 hot corinos, and a factor ∼2.5 lower than the only other value inferred for a protoplanetary disk (in TW Hya, 1.3−1.7). Additionally, it is at the lower edge but still consistent with the values in comets. This may indicate that some chemical reprocessing occurs in disks before the formation of planets and comets.

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Section: ) Inmentioning

confidence: 99%

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Podio

Garufi

Codella

et al. 2020

A&A

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“…Recent high-resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) of H 2 CO transitions in 20 protoplanetary disks suggest that both gas-phase and solid-state formation of formaldehyde occurs, with their relative contributions varying across different disks (van der Marel et al 2014;Loomis et al 2015;Carney et al 2017;Öberg et al 2017;Guzmán et al 2018;Kastner et al 2018;Podio et al 2019;Garufi et al 2020;Pegues et al 2020). Parametric model fits to resolved observations of H 2 CO 3 12 -2 11 and 5 15 -4 14 in the disk of TTauri star TWHya find both warm and cold H 2 CO components in compact and extended regions, respectively (Öberg et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The TW Hya Rosetta Stone Project. II. Spatially Resolved Emission of Formaldehyde Hints at Low-temperature Gas-phase Formation

Scheltinga

Hogerheijde

Cleeves

et al. 2021

ApJ

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Formaldehyde (H 2 CO) is an important precursor to organics like methanol (CH 3 OH). It is important to understand the conditions that produce H 2 CO and prebiotic molecules during star and planet formation. H 2 CO possesses both gas-phase and solid-state formation pathways, involving either UV-produced radical precursors or CO ice and cold (20 K) dust grains. To understand which pathway dominates, gaseous H 2 COʼs ortho-to-para ratio (OPR) has been used as a probe, with a value of 3 indicating "warm" conditions and <3 linked to cold formation in the solid state. We present spatially resolved Atacama Large Millimeter/submillimeter Array observations of multiple ortho-and para-H 2 CO transitions in the TWHya protoplanetary disk to test H 2 CO formation theories during planet formation. We find disk-averaged rotational temperatures and column densities of 33±2 K, (1.1±0.1)× 10 12 cm −2 and 25±2 K, (4.4±0.3)×10 11 cm −2 for ortho-and para-H 2 CO, respectively, and an OPR of 2.49±0.23. A radially resolved analysis shows that the observed H 2 CO emits mostly at rotational temperatures of 30-40 K, corresponding to a layer with z/R0.25. The OPR is consistent with 3 within 60 au, the extent of the pebble disk, and decreases beyond 60 au to 2.0±0.5. The latter corresponds to a spin temperature of 12 K, well below the rotational temperature. The combination of relatively uniform emitting conditions, a radial gradient in the OPR, and recent laboratory experiments and theory on OPR ratios after sublimation, led us to speculate thatgas-phase formation is responsible for the observed H 2 CO across the TWHya disk.

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“…[51,[219][220][221][222][223]), as well as a few S-bearing species, e.g. CS, H 2 CS, H 2 S (e.g., [224][225][226][227][228][229][230][231]). The content of complex organic molecules (COMs), on the contrary, is still only poorly known because of their lower gas-phase abundances (< 10 −8 with respect to the abundance of atomic hydrogen).…”

Section: Organics As C-o-n Carriersmentioning

confidence: 99%

Exploring the link between star and planet formation with Ariel

et al. 2021

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The goal of the Ariel space mission is to observe a large and diversified population of transiting planets around a range of host star types to collect information on their atmospheric composition. The planetary bulk and atmospheric compositions bear the marks of the way the planets formed: Ariel’s observations will therefore provide an unprecedented wealth of data to advance our understanding of planet formation in our Galaxy. A number of environmental and evolutionary factors, however, can affect the final atmospheric composition. Here we provide a concise overview of which factors and effects of the star and planet formation processes can shape the atmospheric compositions that will be observed by Ariel, and highlight how Ariel’s characteristics make this mission optimally suited to address this very complex problem.

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ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Cited by 29 publications

References 78 publications

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

The TW Hya Rosetta Stone Project. II. Spatially Resolved Emission of Formaldehyde Hints at Low-temperature Gas-phase Formation

Exploring the link between star and planet formation with Ariel

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