Accretion Bursts from Young Stars

Garatti, A. Caratti o; Eislöffel, J.

doi:10.1007/978-3-030-14128-8_16

Cited by 2 publications

(2 citation statements)

References 27 publications

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“…If accretion and outflows are linked together, this would in fact agree with the morphology of many optical and near-infrared (NIR) jets that appear composed of aligned knots (emitting in several optical and NIR spectral lines), which, in this view, would be relics of past accretion bursts. In this scenario, both protostars and very young stars should also exhibit photometric variability with augmented luminosity A&A 672, A113 (2023) occurring during phases of intense accretion, which has actually been observed in both low-mass (see, e. g. Yoo et al 2017;Caratti o Garatti & Eislöffel 2019), intermediate-mass (Benisty et al 2010) and high-mass young stars (see, e. g. Caratti o Garatti et al 2017;Hunter et al 2017).…”

Section: Introductionmentioning

confidence: 97%

The SOUL view of IRAS 20126+4104

Massi

Garatti

Cesaroni

et al. 2023

A&A

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Context. We exploit the increased sensitivity of the recently installed adaptive optics SOUL at the LBT to obtain new high-spatial-resolution near-infrared images of the massive young stellar object IRAS20126+4104 and its outflow. Aims. We aim to derive the jet proper motions and kinematics, as well as to study its photometric variability by combining the novel performances of SOUL together with previous near-infrared images. Methods. We used both broad-band (Ks, K′) and narrow-band (Brγ, H2) observations from a number of near-infrared cameras (UKIRT/UFTI, SUBARU/CIAO, TNG/NICS, LBT/PISCES, and LBT/LUCI1) to derive maps of the continuum and the H2 emission in the 2.12 µm line. Three sets of images, obtained with adaptive optics (AO) systems (CIAO, in 2003; FLAO, in 2012; SOUL, in 2020), allowed us to derive the proper motions of a large number of H2 knots along the jet. Photometry from all images was used to study the jet variability. Results. We derived knot proper motions in the range of 1.7–20.3 mas yr−1 (i.e. 13–158 km s−1 at 1.64 kpc), implying an average outflow tangential velocity of ~80 km s−1. The derived knot dynamical age spans a ~200–4000 yr interval. A ring-like H2 feature near the protostar location exhibits peculiar kinematics and may represent the outcome of a wide-angle wind impinging on the outflow cavity. Both H2 geometry and velocities agree with those inferred from proper motions of the H2O masers, located at a smaller distance from the protostar. Although the total H2 line emission from the knots does not exhibit time variations at a ⪞0.3 mag level, we have found a clear continuum flux variation (radiation scattered by the dust in the cavity opened by the jet) which is anti-correlated between the blue-shifted and red-shifted lobes and may be periodic (with a period of ~12–18 yr). We suggest that the continuum variability might be related to inner-disc oscillations which have also caused the jet precession. Conclusions. Our analysis shows that multi-epoch high-spatial-resolution imaging in the near-infrared is a powerful tool to unveil the physical properties of highly embedded massive protostars.

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Section: Introductionmentioning

confidence: 97%

The SOUL view of IRAS 20126+4104

Massi

Garatti

Cesaroni

et al. 2023

A&A

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“…Here, HH 216 is seen as a bright bow shock-shaped feature in all of the emission line maps shown in Section 3. In the [O ii] emission lines, HH 216 shows two distinct components (Figure 2), where the double-peaked line profile is a consequence of the bow-shock geometry of HH 216 (Caratti o Garatti & Eislöffel 2009).…”

Section: A Multi-wavelength Analysis Of Hh 216mentioning

confidence: 99%

Wide field-of-view study of the Eagle Nebula with the Fourier transform imaging spectrograph SITELLE at CFHT

Flagey

McLeod

Aguilar

et al. 2020

A&A

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Context. We present the very first wide-field, 11 by 11 , optical spectral mapping of M 16, one of the most famous star-forming regions in the Galaxy. The data were acquired with the new imaging Fourier transform spectrograph SITELLE mounted on the Canada-France-Hawaii Telescope (CFHT). We obtained three spectral cubes with a resolving power of 10'000 (SN1 filter), 1500 (SN2 filter) and 600 (SN3 filter), centered on the iconic Pillars of Creation and the HH 216 flow, covering the main optical nebular emission lines, namelyAims. We validate the performance, calibration, and data reduction of SITELLE, and analyze the structures in the large field-of-view in terms of their kinematics and nebular emission. Methods. We compared the SITELLE data to MUSE integral field observations and other spectroscopic and narrow-band imaging data to validate the performance of SITELLE. We computed gas-phase metallicities via the strong-line method, performed a pixelby-pixel fit to the main emission lines to derive kinematics of the ionized gas, computed the mass-loss rate of the Eastern pillar (also known as the Spire), and combined the SITELLE data with near-infrared narrow-band imaging to characterize the HH 216 flow. Results. The comparison with previously published fluxes demonstrates very good agreement. We disentangle the dependence of the gas-phase metallicities (derived via abundance-tracing line ratios) on the degree of ionization and obtain metallicities that are in excellent agreement with the literature. We confirm the bipolar structure of HH 216, find evidence for episodic accretion from the source of the flow, and identify its likely driving source. We compute the mass-loss rateṀ of the Spire pillar on the East side of the Hii region and find excellent agreement with the correlation between the mass-loss rate and the ionizing photon flux from the nearby cluster NGC 6611.

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Accretion Bursts from Young Stars

Cited by 2 publications

References 27 publications

The SOUL view of IRAS 20126+4104

The SOUL view of IRAS 20126+4104

Wide field-of-view study of the Eagle Nebula with the Fourier transform imaging spectrograph SITELLE at CFHT

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