Faust

Vastel, C.; Alves, F. O.; Ceccarelli, C.; Bouvier, Mathilde; Jiménez-Serra, Izaskun; Sakai, Takeshi; Caselli, P.; Evans, Lucy; Fontani, F.; Gal, Romane Le; Chandler, Claire J.; Svoboda, Brian; Maud, L. T.; Codella, C.; Sakai, Nami; López-Sepulcre, A.; Moellenbrock, G.; Aikawa, Yuri; Balucani, Nadia; Bianchi, E.; Busquet, G.; Caux, E.; Charnley, Steven B.; Cuello, Nicolás; Simone, M. De; Dulieu, F.; Durán, Aurora; Fedele, D.; Feng, Siyi; Francis, Logan; Hama, Tetsuya; Hanawa, Tomoyuki; Herbst, Eric; Hirota, Tomoya; Imai, Muneaki; Isella, Andrea; Johnstone, D.; Leflóch, B.; Loinard, Laurent; Maureira, María José; Murillo, Nadia M.; Mercimek, S.; Mori, Shoji; Ménard, F.; Miotello, A.; Nakatani, Riouhei; Nomura, Hideko; Oba, Yasuhiro; Ohashi, Satoshi; Okoda, Yuki; Ospina-Zamudio, J.; Oya, Yoko; Pineda, Jaime E.; Podio, L.; Rimola, Albert; Cox, D. Segura; Shirley, Yancy L.; Testi, L.; Viti, S.; Watanabe, Naoki; Watanabe, Yoshimasa; Witzel, A.; Xue, Ci; Zhang, Yichen; Zhao, Bo; Yamamoto, Satoshi

doi:10.1051/0004-6361/202243414

Cited by 9 publications

(10 citation statements)

References 86 publications

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“…Given that nonradiative heating in the form of shocks is not only expected in binary interactions but also due to envelope/ disk and spiral arm/disk interactions (Ilee et al 2011;Miura et al 2017;Evans et al 2015), it might be generally important in the modeling of the inner regions in both multiple and single protostellar sources. This is supported by the increasing number of studies suggesting a shock origin for the unresolved emission from COMs and sulfur-bearing species showing complex line profiles and elevated gas temperatures in both class 0 and I sources (Artur de la Villarmois et al 2019;Oya et al 2019;Diaz-Rodriguez et al 2022;Hsieh et al 2022;Vastel et al 2022;Valdivia-Mena et al 2022). Moreover, in an unbiased chemical survey of 50 embedded protostars in Perseus (Yang et al 2021), 58% show emission from COMs.…”

Section: Mechanical Heating During the Embedded Protostellar Stagesmentioning

confidence: 83%

“…It has been difficult to unambiguously disentangle the heating mechanism in hot corinos because most observations do not resolve the compact COM-emitting region at disk scales (Jacobsen et al 2019;Belloche et al 2020;Bianchi et al 2020;Martín-Doménech et al 2021;Yang et al 2021;Vastel et al 2022). Although some observations have been able to identify COM and sulfur-bearing species arising preferentially in the transition between the disk and the infalling envelope material in which shocks are expected (Sakai et al 2014), evidence of elevated dust temperature is missing.…”

Section: Mechanical Heating In Hot Corinosmentioning

confidence: 99%

“…10 This class 0 binary is not the only known hot corino source in which high-resolution observations have suggested the presence of mechanical heating. Vastel et al (2022) argued that the hot methanol resolved down to 50 au around the class I binary BHB 2007-11 (separation of 28 au) is produced by shocks. In the case of the class 0/I SVS 13 A system (separation of 90 au), some COMs have been observed to emit in the circumstellar disks but also in a more extended region associated with the circumbinary gas (Diaz-Rodriguez et al 2022).…”

Section: Mechanical Heating In Hot Corinosmentioning

confidence: 99%

“…can be a crucial ingredient in modeling the temperature of both gas and dust at disk scales due to the higher densities and accretion rates at these stages. Considering such nonradiative heating mechanisms can have important implications for the estimations of embedded disk masses (Galvan-Madrid et al 2018;Zamponi et al 2021;Xu 2022), envelope and disk grain sizes (Li et al 2017;Zamponi et al 2021), and disk chemistry (Ilee et al 2011;Sakai et al 2014;Evans et al 2015;Harsono et al 2015;Ilee et al 2017;Evans et al 2019;Belloche et al 2020;Zamponi et al 2021;Vastel et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…In particular, shock and adiabatic compression heating can be present in regions where the infalling material is deposited into a disk (Sakai et al 2014;Miura et al 2017;Artur de la Villarmois et al 2019;Pineda et al 2022), near spiral arms in a gravitationally unstable disk (Boley & Durisen 2008;Boss 2001Boss , 2007Ilee et al 2011), or in the material around binaries (Mosta et al 2019;Vastel et al 2022). This type of heating can lead to local temperature enhancements and thus can be more easily decoupled from other types of heating such as irradiation or steady-state viscous heating, for which a smooth decrease of temperature with increasing distance to the protostar(s) is expected.…”

Section: Introductionmentioning

confidence: 99%

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Dust Hot Spots at 10 au Scales around the Class 0 Binary IRAS 16293–2422 A: A Departure from the Passive Irradiation Model

Maureira

Gong

Pineda

et al. 2022

ApJL

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Characterizing the physical conditions at disk scales in class 0 sources is crucial for constraining the protostellar accretion process and the initial conditions for planet formation. We use ALMA 1.3 and 3 mm observations to investigate the physical conditions of the dust around the class 0 binary IRAS 16293–2422 A down to ∼10 au scales. The circumbinary material’s spectral index, α, has a median of 3.1 and a dispersion of ∼0.2, providing no firm evidence of millimeter-sized grains therein. Continuum substructures with brightness temperature peaks of T b ∼ 60–80 K at 1.3 mm are observed near the disks at both wavelengths. These peaks do not overlap with strong variations of α, indicating that they trace high-temperature spots instead of regions with significant optical depth variations. The lower limits to the inferred dust temperature in the hot spots are 122, 87, and 49 K. Depending on the assumed dust opacity index, these values can be several times higher. They overlap with high gas temperatures and enhanced complex organic molecular emission. This newly resolved dust temperature distribution is in better agreement with the expectations from mechanical instead of the most commonly assumed radiative heating. In particular, we find that the temperatures agree with shock heating predictions. This evidence and recent studies highlighting accretion heating in class 0 disks suggest that mechanical heating (shocks, dissipation powered by accretion, etc.) is important during the early stages and should be considered when modeling and measuring properties of deeply embedded protostars and disks.

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Section: Mechanical Heating During the Embedded Protostellar Stagesmentioning

confidence: 83%

Section: Mechanical Heating In Hot Corinosmentioning

confidence: 99%

Section: Mechanical Heating In Hot Corinosmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dust Hot Spots at 10 au Scales around the Class 0 Binary IRAS 16293–2422 A: A Departure from the Passive Irradiation Model

Maureira

Gong

Pineda

et al. 2022

ApJL

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Spiers Memorial Lecture: Astrochemistry at high resolution

Ceccarelli¹

2023

Faraday Discuss.

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Faust

Evans,

Vastel,

Fontani

et al. 2023

A&A

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Context. Deuterium in H-bearing species is enhanced during the early stages of star formation. However, only a small number of high-spatial-resolution deuteration studies exist towards protostellar objects, leaving the small-scale structures of these objects unrevealed and understudied. Aims. We aim to constrain the deuterium fractionation ratios in a Class 0/I protostellar object in formaldehyde (H2CO), which has abundant deuterated isotopologues in this environment. Methods. We used the Atacama Large Millimeter Array (ALMA) within the context of the Large Program Fifty AU STudy of the chemistry in the disk/envelope system of Solar-like protostars (FAUST) to observe the Class 0/I protobinary system [BHB2007] 11, whose emission components are embedded in circumstellar disks that have radii of 2 to 3 au. The system is surrounded by a complex filamentary structure (the so-called streamers) connected to the larger circumbinary disk. In this work, we present the first study of formaldehyde D-fractionation towards this source with detections of H2CO 3(0,3)–2(0,2), combined with HDCO 4(2,2)–3(2,1), HDCO 4(1,4)–3(1,3) and D2CO 4(0,4)–3(0,3). These observations probe the structures of the protobinary system, enabling us to resolve multiple velocity components associated with the methanol hot spots also uncovered by FAUST data, as well as the colder external envelope. In addition, based on the kinematics seen in our observations of the H2CO emission, we propose the presence of a second large-scale outflow. Results. The results derived from our ALMA observations agree with the current literature in that we only find the deuterated species HDCO and D2CO in the central regions of the core, while undeuterated H2CO is found more ubiquitously. From our radiative transfer modelling, we the column density of H2CO to be in the range of (3-8) × 1014 cm−2 and that of HDCO to be within (0.8−2.9) × 1013 cm−2. The column density for the single detected velocity component of D2CO is within (2.6–1.3) × 1012 cm−2. This yields an average D/H ratio for formaldehyde in [BHB2007] 11 of $0.02_{ - 0.01}^{ + 0.02}$ from HDCO. The results of our kinematic model suggest that the dynamic feature is inconsistent with a streamer-like nature given the flat and outflowing velocity relation; we therefore tentatively conclude that the feature is an asymmetric molecular outflow launched by a wide-angle disk wind.

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Faust

Cited by 9 publications

References 86 publications

Dust Hot Spots at 10 au Scales around the Class 0 Binary IRAS 16293–2422 A: A Departure from the Passive Irradiation Model

Dust Hot Spots at 10 au Scales around the Class 0 Binary IRAS 16293–2422 A: A Departure from the Passive Irradiation Model

Spiers Memorial Lecture: Astrochemistry at high resolution

Faust

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