The SOUL view of IRAS 20126+4104

Massi, F.; Garatti, A. Caratti o; Cesaroni, R.; Sridharan, T. K.; Ghose, Essna; Pinna, Enrico; Beltrán, M. T.; Leurini, S.; Moscadelli, L.; Sanna, A.; Agapito, Guido; Briguglio, Runa; Christou, Julian C.; Esposito, Simone; Mazzoni, Tommaso; Miller, Douglas L.; Plantet, Cédric; Power, J.; Puglisi, Alfio; Rossi, Fabio; Rothberg, Barry; Taylor, Gary; Veillet, Christian

doi:10.1051/0004-6361/202245235

Cited by 7 publications

(14 citation statements)

References 59 publications

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“…This velocity is consistent with previously measured jet knots ejected by massive protostars (e.g. Fedriani et al 2019;Massi et al 2023). This interpretation is supported by the fact that the other jet tracers in the radio regime align with the NIR NE knot.…”

Section: Episodic Ejection As a Response To Episodic Accretionsupporting

confidence: 91%

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The sharpest view on the high-mass star-forming region S255IR

Fedriani¹,

Garatti²,

Cesaroni³

et al. 2023

A&A

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Context. Massive stars have an impact on their surroundings from early in their formation until the end of their lives. However, very little is known about their formation. Episodic accretion may play a crucial role, but observations of these events have only been reported towards a handful of massive protostars. Aims. We aim to investigate the outburst event from the high-mass star-forming region S255IR where recently the protostar NIRS3 underwent an accretion outburst. We follow the evolution of this source both in photometry and morphology of its surroundings. Methods. We perform near-infrared adaptive optics observations on the S255IR central region using the Large Binocular Telescope in the K s broad-band and the H 2 and Brγ narrow-band filters with an angular resolution of ∼ 0 ′′ . 06, close to the diffraction limit.Results. We discover a new near-infrared knot north-east from NIRS3 that we interpret as a jet knot that was ejected during the last accretion outburst and observed in the radio regime as part of a follow-up after the outburst. We measure a mean tangential velocity for this knot of 450 ± 50 km s −1 . We analyse the continuum-subtracted images from H 2 which traces jet shocked emission, and Brγ which traces scattered light from a combination of accretion activity and UV radiation from the central massive protostar. We observe a significant decrease in flux at the location of NIRS3, with K=13.48 mag being the absolute minimum in the historic series. Conclusions. Our observations strongly suggest a scenario where the episodic accretion is followed by an episodic ejection response in the near-infrared, as it was seen in the earlier radio follow-up. The 30 years of ∼ 2 µm photometry suggests that NIRS3 might have undergone another outburst in the late 1980s, being the first massive protostar with such evidence observed in the near-infrared.

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Section: Episodic Ejection As a Response To Episodic Accretionsupporting

confidence: 91%

“…From our AO imaging data, we can estimate the ejection time scale of these H 2 knots. It has been observed that H 2 knots driven by HMYSOs can have velocities exceeding 100 km s −1 (see, e.g., Fedriani et al 2018;Massi et al 2023). This would imply that the dynamic age of the NIRS3 H 2 knots is ∼ 400 − 700 years.…”

Section: Resultsmentioning

confidence: 99%

The sharpest view on the high-mass star-forming region S255IR

Fedriani¹,

Garatti²,

Cesaroni³

et al. 2023

A&A

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“…In our case, n H 2 < 5 × 10 4 cm −3 , as shown in Fig. 13, and sh < ∼ 100 km s −1 , which was obtained from proper motion measurements of the H 2 O masers (Moscadelli et al 2005(Moscadelli et al , 2011 and H 2 knots (Massi et al 2023). Therefore, n H 2 sh < 5 × 10 11 cm −2 s −1 , which satisfies the previous condition.…”

Section: Shocked Regionsupporting

confidence: 81%

“…The (proto)star is powering a outflow undergoing precession about the disk axis (Shepherd et al 2000;Cesaroni et al 2005;Caratti o Garatti et al 2008). This outflow has been imaged on scales from a few 100 au (Moscadelli et al 2005;Cesaroni et al 2013) to 0.5 pc (Shepherd et al 2000;Lebrón et al 2006) and its 3D expansion velocity has been measured through maser and H 2 -knot proper motions (Moscadelli et al 2005;Massi et al 2023). The distance to IRAS 20126+4104 (1.64±0.05 kpc) has been accurately determined from parallax measurements of the H 2 O masers (Moscadelli et al 2011), which prove this to be one of the closest disks around B-type (proto)stars, thus allowing for excellent linear resolution.…”

Section: Introductionmentioning

confidence: 99%

A Herschel study of the high-mass protostar IRAS 20126+4104

Cesaroni

Faustini

Galli

et al. 2023

A&A

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We performed Herschel observations of the continuum and line emission from the high-mass star-forming region IRAS 20126+4104, which hosts a well-studied B-type (proto)star powering a bipolar outflow and is associated with a Keplerian circumstellar disk. The continuum images at six wavelengths allowed us to derive an accurate estimate of the bolometric luminosity and mass of the molecular clump enshrouding the disk. The same region has been mapped in 12 rotational transitions of carbon monoxide, which were used in synergy with the continuum data to determine the temperature and density distribution inside the clump and improve upon the mass estimate. The maps of two fine structure oxygen far-IR lines were used to estimate the volume density of the shocked region at the surface of the southern lobe of the outflow and the mass-loss rate. Our findings lend further support to the scenario previously proposed by various authors, confirming that at the origin of the bolometric luminosity and bipolar outflow from IRAS 20126+4104 is a B-type star located at the centre of the Keplerian disk.

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“…These two types of models can be applied to the jet and knot positions, directly relating periodicity in the knot positions to the binary period or precession period (e.g., Raga et al 2002). Most prior work focuses on molecular jets with small wiggles and opening angles (i.e., the angular width of the jet) of <10°; these are usually interpreted in terms of binary motion (Gueth et al 1996;Zinnecker et al 1998;Woitas et al 2002;Chandler et al 2005;Sahai et al 2005;Ybarra et al 2006;Seale & Looney 2008;Phillips & Pérez-Grana 2009;Lee et al 2010Lee et al , 2015Whelan et al 2010;Agra-Amboage et al 2011;Noriega-Crespo et al 2011, 2020Estalella et al 2012;Fernández-López et al 2013;Velázquez et al 2014;Kwon et al 2015;Beltrán et al 2016;Moraghan et al 2016;Choi et al 2017;Louvet et al 2018;Hara et al 2021;Jhan & Lee 2021;Murphy et al 2021;Massi et al 2022Massi et al , 2023.…”

Section: Introductionmentioning

confidence: 99%

HOPS 361-C’s Jet Decelerating and Precessing through NGC 2071 IR

Karnath

Quillen

et al. 2023

ApJ

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We present a two-epoch Hubble Space Telescope study of NGC 2071 IR highlighting HOPS 361-C, a protostar producing an arced 0.2 parsec-scale jet. The proper motions for the brightest knots decrease from 350 to 100 km s−1 with increasing distance from the source. The [Fe ii] and Paβ emission line intensity ratio gives a velocity jump through each knot of 40–50 km s−1. A new [O i] 63 μm spectrum, taken with the German REciever for Astronomy at Terahertz frequencies instrument aboard Stratospheric Observatory for Infrared Astronomy, shows a low line-of-sight velocity indicative of high jet inclination. Proper motions and jump velocities then estimate 3D flow speed for knots. Subsequently, we model knot positions and speeds with a precessing jet that decelerates. The measurements are matched with a precession period of 1000–3000 yr and half opening angle of 15°. The [Fe ii] 1.26-to-1.64 μm line intensity ratio determines visual extinction to each knot from 5 to 30 mag. Relative to ∼14 mag of extinction through the cloud from C18O emission maps, the jet is embedded at a 1/5–4/5 fractional cloud depth. Our model suggests the jet is dissipated over a 0.2 pc arc. This short distance may result from the jet sweeping through a wide angle, allowing the cloud time to fill cavities opened by the jet. Precessing jets contrast with nearly unidirectional protostellar jets that puncture host clouds and can propagate significantly farther.

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The SOUL view of IRAS 20126+4104

Cited by 7 publications

References 59 publications

The sharpest view on the high-mass star-forming region S255IR

The sharpest view on the high-mass star-forming region S255IR

A Herschel study of the high-mass protostar IRAS 20126+4104

HOPS 361-C’s Jet Decelerating and Precessing through NGC 2071 IR

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