Protostellar Outflows at the EarliesT Stages (POETS)

Sanna, A.; Moscadelli, L.; Goddi, C.; Beltrán, M. T.; Brogan, C. L.; Garatti, A. Caratti o; Carrasco-González, Carlos; Hunter, T. R.; Massi, F.; Padovani, M.

doi:10.1051/0004-6361/201834551

Cited by 36 publications

(33 citation statements)

References 37 publications

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“…19). Observations of non-thermal components in jets from high-mass YSOs are still rare, although good examples have been recently discovered thanks to high-angular resolution, sensitive radio survey (for instance, the POETS source G035.02+0.35, Sanna et al 2019). The observational evidence for point 2, as already discussed in Moscadelli et al (2019, see Sect.…”

Section: The Magnetized and Rotating Jetmentioning

confidence: 88%

Multi-scale view of star formation in IRAS 21078+5211: from clump fragmentation to disk wind

Moscadelli

Beuther

Ahmadi

et al. 2021

A&A

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Section: The Magnetized and Rotating Jetmentioning

confidence: 88%

Multi-scale view of star formation in IRAS 21078+5211: from clump fragmentation to disk wind

Moscadelli

Beuther

Ahmadi

et al. 2021

A&A

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“…However, some of these may arise from strong side-lobe patterns from incomplete uv sampling in the VLA observation. As shown in Figure 1f, some regions have negative spectral indices of −0.5 < α ν < −0.2, inconsistent with pure free-free emission or dust emission, indicating possible contributions from nonthermal synchrotron emission, which is occasionally found associated with massive protostellar jets (e.g., Garay et al 1996;Carrasco-González et al 2010;Moscadelli et al 2013;Rosero et al 2016;Beltrán et al 2016;Sanna et al 2019). Thus, detection of negative spectral indices is also consistent with a jet being embedded inside the wide-angle ionized outflow.…”

Section: 3 and 7 MM Continuummentioning

confidence: 94%

“…In the region with negative spectral indices indicating synchrotron emission, we estimate the minimum-energy magnetic filed strength, B min , which minimizes the total energy of the synchrotron source by assuming equipartition between the magnetic field energy and the particle energy. Following the classical formula for estimating minimumenergy magnetic field strength (e.g., Carrasco-González et al 2010;Sanna et al 2019)…”

Section: Estimating the Magnetic Field Strength From Synchrotron Ementioning

confidence: 99%

Discovery of a Photoionized Bipolar Outflow toward the Massive Protostar G45.47+0.05

Zhang¹,

Tanaka²,

Rosero³

et al. 2019

ApJL

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Massive protostars generate strong radiation feedback, which may help set the mass they achieve by the end of the accretion process. Studying such feedback is therefore crucial for understanding the formation of massive stars. We report the discovery of a photoionized bipolar outflow towards the massive protostar G45.47+0.05 using high-resolution observations at 1.3 mm with the Atacama Large Millimeter/Submillimeter Array (ALMA) and at 7 mm with the Karl G. Jansky Very Large Array (VLA). By modeling the free-free continuum, the ionized outflow is found to be a photoevaporation flow with an electron temperature of 10, 000 K and an electron number density of ∼ 1.5 × 10 7 cm −3 at the center, launched from a disk of radius of 110 au. H30α hydrogen recombination line emission shows strong maser amplification, with G45 being one of very few sources to show such millimeter recombination line masers. The mass of the driving source is estimated to be 30 − 50 M based on the derived ionizing photon rate, or 30 − 40 M based on the H30α kinematics. The kinematics of the photoevaporated material is dominated by rotation close to the disk plane, while accelerated to outflowing motion above the disk plane. The mass loss rate of the photoevaporation outflow is estimated to be ∼ (2 − 3.5) × 10 −5 M yr −1 . We also found hints of a possible jet embedded inside the wide-angle ionized outflow with non-thermal emissions. The possible co-existence of a jet and a massive photoevaporation outflow suggests that, in spite of the strong photoionization feedback, accretion is still on-going.

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“…upper-limits) data. Coloured circles represent YSOs from the literature for comparison which are, DG Tau A (blue marker;Purser et al 2018), the Serpens triple radio source (yellow marker;Rodríguez-Kamenetzky et al 2016), G035.02+0.35N (red marker;Sanna, A. et al 2019), HOPS 370 (purple marker;Osorio et al 2017) and HH 80-81 (green marker;Marti et al 1993).…”

mentioning

confidence: 99%

A Galactic survey of radio jets from massive protostars

Purser

Lumsden

Hoare

et al. 2021

Monthly Notices of the Royal Astronomical Society

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In conjunction with a previous southern-hemisphere work, we present the largest radio survey of jets from massive protostars to date with high-resolution, ($\sim 0{_{.}^{\prime\prime}}04$) Jansky Very Large Array (VLA) observations towards two subsamples of massive star-forming regions of different evolutionary statuses: 48 infrared-bright, massive, young, stellar objects (MYSOs) and 8 infrared dark clouds (IRDCs) containing 16 luminous (${\, L_{\rm {bol}}}>10^3{{\rm \, L_{\odot }}}$) cores. For $94{{\ \rm per\ cent}}$ of the MYSO sample we detect thermal radio (α ≥ −0.1 whereby Sν∝να) sources coincident with the protostar, of which $84{{\ \rm per\ cent}}$ (13 jets and 25 candidates) are jet-like. Radio luminosity is found to scale with ${\, L_{\rm {bol}}}$ similarly to the low-mass case supporting a common mechanism for jet production across all masses. Associated radio lobes tracing shocks are seen towards $52{{\ \rm per\ cent}}$ of jet-like objects and are preferentially detected towards jets of higher radio and bolometric luminosities, resulting from our sensitivity limitations. We find jet mass loss rate scales with bolometric luminosity as ${\dot{m}_{\rm jet}}\propto {\, L_{\rm {bol}}}^{0.9\pm 0.2}$, thereby discarding radiative, line-driving mechanisms as the dominant jet-launching process. Calculated momenta show that the majority of jets are mechanically capable of driving the massive, molecular outflow phenomena since pjet > poutflow. Finally, from their physical extent we show that the radio emission can not originate from small, optically-thick Hii regions. Towards the IRDC cores, we observe increasing incidence rates/radio fluxes with age using the proxy of increasing luminosity-to-mass (L/M) and decreasing infrared flux ratios (S70 μm/S24 μm). Cores with $L/M\, <\, 40\, L_\odot \, M_\odot ^{-1}$ are not detected above (5.8 GHz) radio luminosities of ∼1 mJy kpc2.

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Protostellar Outflows at the EarliesT Stages (POETS)

Cited by 36 publications

References 37 publications

Multi-scale view of star formation in IRAS 21078+5211: from clump fragmentation to disk wind

Multi-scale view of star formation in IRAS 21078+5211: from clump fragmentation to disk wind

Discovery of a Photoionized Bipolar Outflow toward the Massive Protostar G45.47+0.05

A Galactic survey of radio jets from massive protostars

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