The Flying Saucer:   Tomography of the thermal and density gas structure   of an edge-on protoplanetary disk

Dutrey, Anne; Guilloteau, S.; Piétu, V.; Chapillon, E.; Wakelam, Valentine; Folco, E. Di; Stoecklin, Thierry; Denis-Alpizar, Otoniel; Gorti, Uma; Teague, Richard; Henning, Th.; Semenov, D.; Grosso, N.

doi:10.1051/0004-6361/201730645

Cited by 70 publications

(104 citation statements)

References 31 publications

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“…The CO(2-1) emission being optically thick, the peak brightness is representative of the gas temperature while the integrated area is more complex to interpret. This suggests that the observed spirals correspond to warmer gas located well above the mid-plane (at 2 to 3 scale heights, as directly observed in the "Flying Saucer" by Dutrey et al 2017). An increase in surface density, as occurs in the spiral density waves created by a planet, will result in a higher CO opacity, and thus in the τ = 1 layer located at higher altitude, where the temperature is higher because of the moderate vertical temperature gradient (Phuong et al 2020).…”

Section: Resultssupporting

confidence: 66%

Planet-induced spirals in the circumbinary disk of GG Tauri A

Phượng

Dutrey

Folco

et al. 2020

A&A

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Context. ALMA high angular resolution observations of the dust and CO emission have already revealed signatures of protoplanets embedded in protoplanetary disks. These detections are around single T Tauri stars, while exoplanet surveys reveal that planets can also form in binary (or multiple) systems, either in circumstellar or circumbinary orbits. Aims. We searched for indirect evidence for planet formation in the multiple system GG Tau A, which harbors the most massive circumbinary disk among T Tauri stars. Methods. We performed CO(2–1) ALMA Cycle 6 observations of GG Tau A at 0.3″ resolution. The images confirm the “hot spot” detected at higher frequencies, but also reveal prominent spiral-like features. We modeled these features using the analytic prescription for the linear perturbation regime induced by low-mass planets. Results. The brightest spiral is well reproduced by a density wave excited by a protoplanet (GG Tau Ac) at the hot-spot location (290 au), just outside the dust ring. The absence of a clear gap (in gas or dust) at the planet location implies that its mass is significantly lower than that of Jupiter, i.e., of about the mass of Neptune or lower. Furthermore, other prominent (trailing) spiral patterns can be represented by adding one (or more) planet(s) at larger orbital radii, with the most obvious candidate located near the 2:1 mean-motion resonance with GG Tau Ac. Conclusions. The (proto-)planet GG Tau Ac appears to externally confine the ring in a stable configuration, explaining its high mass. Our results also suggest that planets similar in mass to Neptune may form in dense circumbinary disks orbiting (wide) binary stars. In the GG Tau case, orbital resonances appear to play an important role in shaping this multiple circumbinary planet system.

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Section: Resultssupporting

confidence: 66%

Planet-induced spirals in the circumbinary disk of GG Tauri A

Phượng

Dutrey

Folco

et al. 2020

A&A

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“…In our models, the molecular layer is very thin and situated high above the disk plane at three scale heights. This is at odds with the observations of CS in the Flying Saucer (Dutrey et al 2017), where CS appears closer to one scale height. The difference may be due to the larger mass of the GG Tau disk (0.15 M ).…”

Section: Sulfur-bearing Speciescontrasting

confidence: 79%

First detection of H₂S in a protoplanetary disk

Phượng

Chapillon

Majumdar

et al. 2018

A&A

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Context. Studying molecular species in protoplanetary disks is very useful to characterize the properties of these objects, which are the site of planet formation. Aims. We attempt to constrain the chemistry of S-bearing molecules in the cold parts of circumstellar disk of GG Tau A. Methods. We searched for H2S, CS, SO, and SO2 in the dense disk around GG Tau A with the NOrthem Extended Millimeter Array (NOEMA) interferometer. We analyzed our data using the radiative transfer code DiskFit and the three-phase chemical model Nautilus. Results. We detected H2S emission from the dense and cold ring orbiting around GG Tau A. This is the first detection of H2S in a protoplanetary disk. We also detected HCO+, H13CO+, and DCO+ in the disk. Upper limits for other molecules, CCS, SO2, SO, HC3N, and c-C3H2 are also obtained. The observed DCO+/HCO+ ratio is similar to those in other disks. The observed column densities, derived using our radiative transfer code DiskFit, are then compared with those from our chemical code Nautilus. The column densities are in reasonable agreement for DCO+, CS, CCS, and SO2. For H2S and SO, our predicted vertical integrated column densities are more than a factor of 10 higher than the measured values. Conclusions. Our results reinforce the hypothesis that only a strong sulfur depletion may explain the low observed H2S column density in the disk. The H2S detection in GG Tau A is most likely linked to the much larger mass of this disk compared to that in other T Tauri systems.

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“…This is not a valid assumption in the uppermost layers of the disk (Bergin et al 2007), but is a reasonable simplification in this study focusing on S-chemistry in the molecular disk layers (e.g. Woitke et al 2009;Akimkin et al 2013;Dutrey et al 2017;Semenov et al 2018). For instance, in the Flying Saucer edge-on T Tauri disk, the CS emission is observed to be less vertically extended than the CO one (Dutrey et al 2017).…”

Section: Temperature Profilementioning

confidence: 93%

Sulfur Chemistry in Protoplanetary Disks: CS and H₂CS

Gal

Öberg

Loomis

et al. 2019

ApJ

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The nature and abundance of sulfur chemistry in protoplanetary disks (PPDs) may impact the sulfur inventory on young planets and therefore their habitability. PPDs also present an interesting test bed for sulfur chemistry models, since each disk present a diverse set of environments. In this context, we present new sulfur molecule observations in PPDs, and new S-disk chemistry models. With ALMA we observed the CS 5 − 4 rotational transition toward five PPDs (DM Tau, DO Tau, CI Tau, LkCa 15, MWC 480), and the CS 6 − 5 transition toward three PPDs (LkCa 15, MWC 480 and V4046 Sgr). Across this sample, CS displays a range of radial distributions, from centrally peaked, to gaps and rings. We also present the first detection in PPDs of 13 CS 6 − 5 (LkCa 15 and MWC 480), C 34 S 6 − 5 (LkCa 15), and H 2 CS 8 17 − 7 16 , 9 19 − 8 18 and 9 18 − 8 17 (MWC 480) transitions. Using LTE models to constrain column densities and excitation temperatures, we find that either 13 C and 34 S are enhanced in CS, or CS is optically thick despite its relatively low brightness temperature. Additional lines and higher spatial resolution observations are needed to distinguish between these scenarios. Assuming CS is optically thin, CS column density model predictions reproduce the observations within a factor of a few for both MWC 480 and LkCa 15. However, the model underpredicts H 2 CS by 1-2 orders of magnitude. Finally, comparing the H 2 CS/CS ratio observed toward the MWC 480 disk and toward different ISM sources, we find the closest match with prestellar cores. two of the Taurus disks: the Herbig Ae disk MWC 480, and the T Tauri disk LkCa 15. The spectral resolution for these lines was ∼ 975 kHz, i.e. corresponding to a velocity resolution of ∼ 1 km/s. The 12 CS 6 − 5 transition was observed in three execution blocks on January 17, 2016, April 23, 2016 and December 12, 2016. For the first execution block 31 antennas were included and covered baselines from 15 to 331 m. 36 antennas were included for the two other execution blocks, covering baselines from 15 to 463 m and 15 to 650 m, respectively. The first and third blocks used the source J0510+1800 as band-pass and flux calibrators, and the source J0438+3004 as phase calibrator. The second block of execution used the source J0238+1636 as band-pass calibrator, the source J0433+2905 as phase calibrator, and the source J0510+1800 as flux calibrator. The total on-source integration time were 17.6, 12.6 and 20.7 min., respectively.The 13 CS and C 34 S 6−5, and H 2 CS 8 17 −7 16 rotational transitions were observed in a single execution block, on January 17, 2016, with the same calibrator sources as those used for the first and second execution blocks used for 12 CS 6 − 5 (see above) but with 36 antennas and a total on-source integration time of ∼ 19.2 min.

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The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk

Cited by 70 publications

References 31 publications

Planet-induced spirals in the circumbinary disk of GG Tauri A

Planet-induced spirals in the circumbinary disk of GG Tauri A

First detection of H₂S in a protoplanetary disk

Sulfur Chemistry in Protoplanetary Disks: CS and H₂CS

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The Flying Saucer: Tomography of the thermal and density gas structure of an edge-on protoplanetary disk

Cited by 70 publications

References 31 publications

Planet-induced spirals in the circumbinary disk of GG Tauri A

Planet-induced spirals in the circumbinary disk of GG Tauri A

First detection of H2S in a protoplanetary disk

Sulfur Chemistry in Protoplanetary Disks: CS and H2CS

Contact Info

Product

Resources

About

First detection of H₂S in a protoplanetary disk

Sulfur Chemistry in Protoplanetary Disks: CS and H₂CS