PRODIGE – envelope to disk with NOEMA

Valdivia-Mena, M. T.; Pineda, Jaime E.; Segura-Cox, Dominique; Caselli, P.; Neri, R.; López-Sepulcre, A.; Cunningham, Nichol; Bouscasse, L.; Semenov, D.; Henning, Th.; Piétu, V.; Chapillon, E.; Dutrey, Anne; Fuente, A.; Guilloteau, S.; Hsieh, Tsung‐Hsin; Jiménez-Serra, Izaskun; Marino, Sebastián; Maureira, María José; Smirnov-Pinchukov, Grigorii V.; Tafalla, M.; Zhao, Bo

doi:10.1051/0004-6361/202243310

Cited by 55 publications

(23 citation statements)

References 83 publications

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“…In addition, anisotropic envelope accretion could also lead to bursts. Indeed, recent observations find infalling streamers at envelope scales, which are also suggested to change the protostellar accretion by funneling material into the inner region (Pineda et al 2020;Alves et al 2020;Ginski et al 2021;Murillo et al 2022;Cabedo et al 2021;Garufi et al 2022;Thieme et al 2022;Valdivia-Mena et al 2022;Pineda et al 2022). Such infalling streamers are also found in numerical simulation Seifried & Walch 2015;Zhao et al 2018).…”

Section: Introductionmentioning

confidence: 72%

“…By measuring the proper motion, Diaz-Rodriguez et al ( 2022) derive a total mass of VLA4A/B as 1 M from the orbital motion. Given the detected farthest projected distance of the DCN streamer ∼700 au, we derive a free-fall time of ∼3000 yr. We note that this can be taken as an upper limit since the initial velocity of DCN is ignored in the calculation (Valdivia-Mena et al 2022). As a result, we find a mass infalling rate of ≥ 1.4 × 10 −6 M yr −1 if this streamer is in a free-fall motion.…”

Section: Accretion Flow Traced By Dcn?mentioning

confidence: 81%

“…4, 700 au). This kind of streamers connecting inner and outer regions have been recently identified in embedded systems and are considered as infalling flows that provide the material supplying the growth of disks and central protostars Alves et al 2020;Murillo et al 2022;Cabedo et al 2021;Thieme et al 2022;Valdivia-Mena et al 2022).…”

Section: A Streamer In Dcn and C 18 O Emissionmentioning

confidence: 99%

“…During the embedded phase of a protostar, infall of material plays a crucial role in supplying material to the central source and protoplanetary disk. Recent studies have detected large infalling streamers at an early stage, which are believed to affect the protostellar accretion (Pineda et al 2020;Alves et al 2020;Cabedo et al 2021;Ginski et al 2021;Murillo et al 2022;Garufi et al 2022;Thieme et al 2022;Valdivia-Mena et al 2022).…”

Section: Accretion Flow Traced By Dcn?mentioning

confidence: 99%

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PRODIGE – envelope to disk with NOEMA

Hsieh¹,

Segura-Cox²,

Pineda³

et al. 2023

A&A

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Aims. We present high sensitivity and high-spectral resolution NOEMA observations of the Class 0/I binary system SVS13A, composed of the low-mass protostars VLA4A and VLA4B with a separation of ∼90 au. VLA4A is undergoing an accretion burst that enriches the chemistry of the surrounding gas. This gives us an excellent opportunity to probe the chemical and physical conditions as well as the accretion process. Methods. We observe the (12 K − 11 K ) lines of CH 3 CN and CH 3 13 CN, the DCN (3-2) line, and the C 18 O (2-1) line toward SVS13A using NOEMA. Results. We find complex line profiles at disk scales which cannot be explained by a single component or pure Keplerian motion. By adopting two velocity components to model the complex line profiles, we find that the temperatures and densities are significantly different between these two components. This suggests that the physical conditions of the emitting gas traced via CH 3 CN can change dramatically within the circumbinary disk. In addition, combining our observations of DCN (3-2) with previous ALMA high-angularresolution observations, we find that the binary system (or VLA4A) might be fed by an infalling streamer from envelope scales (∼700 au). If this is the case, this streamer contributes to the accretion of material onto the system with a rate of at least 1.4 × 10 −6 M yr −1 . Conclusions. We conclude that the CH 3 CN emission in SVS13A traces hot gas from a complex structure. This complexity might be affected by a streamer that is possibly infalling and funneling material into the central region.

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Section: Introductionmentioning

confidence: 72%

Section: Accretion Flow Traced By Dcn?mentioning

confidence: 81%

Section: A Streamer In Dcn and C 18 O Emissionmentioning

confidence: 99%

Section: Accretion Flow Traced By Dcn?mentioning

confidence: 99%

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PRODIGE – envelope to disk with NOEMA

Hsieh¹,

Segura-Cox²,

Pineda³

et al. 2023

A&A

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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%

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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Possible episodic infall towards a compact disk in B335

Bjerkeli¹,

Ramsey²,

Harsono³

et al. 2023

A&A

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Context. Previous observations of the isolated Class 0 source B335 have presented evidence of ongoing infall in various molecular lines, such as HCO+, HCN, and CO. There have been no confirmed observations of a rotationally supported disk on scales greater than ~12 au. Aims. The presence of an outflow in B335 suggests that a disk is also expected to be present or undergoing formation. To constrain the earliest stages of protostellar evolution and disk formation, we aim to map the region where gas falls inwards and observationally constrain its kinematics. Furthermore, we aim to put strong limits on the size and orientation of any disk-like structure in B335. Methods. We used high angular resolution 13CO data from the Atacama Large Millimeter/submillimeter Array (ALMA) and combined it with shorter-baseline archival data to produce a high-fidelity image of the infall in B335. We also revisited the imaging of high-angular resolution Band 6 continuum data to study the dust distribution in the immediate vicinity of B335. Results. Continuum emission shows an elliptical structure (10 by 7 au) with a position angle 5 degrees east of north, consistent with the expectation for a forming disk in B335. A map of the infall velocity (as estimated from the 13CO emission), shows evidence of asymmetric infall, predominantly from the north and south. Close to the protostar, infall velocities appear to exceed free-fall velocities. Three-dimensional (3D) radiative transfer models, where the infall velocity is allowed to vary within the infall region, may explain the observed kinematics. Conclusions. The data suggest that a disk has started to form in B335 and that gas is falling towards that disk. However, kinematically-resolved line data towards the disk itself is needed to confirm the presence of a rotationally supported disk around this young protostar. The high infall velocities we measured are not easily reconcilable with a magnetic braking scenario, suggesting that there is a pressure gradient that allows the infall velocity to vary in the region.

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PRODIGE – envelope to disk with NOEMA

Cited by 55 publications

References 83 publications

PRODIGE – envelope to disk with NOEMA

PRODIGE – envelope to disk with NOEMA

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

Possible episodic infall towards a compact disk in B335

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