Methanol and water maser observations separate disc and outflow sources in IRAS 19410+2336

Darwish, M.S.; Edris, K. A.; Richards, A. M. S.; Etoka, S.; Saad, S. M.; Beheary, M. M.; Fuller, G. A.

doi:10.1093/mnras/staa574

Cited by 8 publications

(3 citation statements)

References 50 publications

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“…The most commonly-found masers in star-formation are CH 3 OH, OH and H 2 O. Rarer masers in this context include SiO, H 2 CO and NH 3 . In addition to the work described below, recent papers from the EVN [10,11], VLBA [12], VERA & ALMA [13], MERLIN [14,15] and modelling [16] are noted. Maser polarization in star-forming regions is reviewed by [17].…”

Section: Masers In Star-formationmentioning

confidence: 99%

Stellar Evolution Studies Using Masers

Humphreys¹

2023

Proceedings of 15th European VLBI Network Mini-Symposium and Users' Meeting — PoS(EVN2022)

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Masers probe a number of stages of stellar evolution including star-formation, asymptotic giant branch stars, pre-planetary nebulae, red supergiants and supernova remnants. High-angular resolution studies using VLBI are revealing information on the accretion process in high-mass stars, the mass-loss process of AGB stars and on the role of magnetic fields. In addition, large projects observing masers associated with star-formation and evolved stars are mapping out galactic structure and probing galactic dynamics. Here, I outline recent results for masers in the area of stellar evolution highlighting the contributions of VLBI and EVN observations, and the synergies of these with data from other telescopes such as ALMA.

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Section: Masers In Star-formationmentioning

confidence: 99%

Stellar Evolution Studies Using Masers

Humphreys¹

2023

Proceedings of 15th European VLBI Network Mini-Symposium and Users' Meeting — PoS(EVN2022)

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“…Water (H 2 O) masers are the predominant maser species found in star-forming regions, spanning low-, intermediate- (Furuya et al 2001(Furuya et al , 2003Bae et al 2011), and high-mass regions (Churchwell et al 1990;Palla et al 1991;Hofner & Churchwell 1996;Beuther et al 2002;Urquhart et al 2009Urquhart et al , 2011Volvach et al 2019;Darwish et al 2020;Hirota et al 2021;Kobak et al 2023). It is closely associated with outflows/jets (Felli et al 1992;Torrelles et al 1997;Patel et al 2000;Seth et al 2002;Goddi & Moscadelli 2006;Sanna et al 2010;Torrelles et al 2011, Torrelles 2012Moscadelli et al 2021), shocked gas (Claussen et al 1998;Furuya et al 2001), and circumstellar disks (Fiebig et al 1996;Torrelles et al 1998;Seth et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Large-scale Effect of an Accretion Burst in the High-Mass Young Stellar Object G358.93-0.03-MM1

Miao,

Chen,

Bayandina

et al. 2024

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The high-mass young stellar object G358.93-0.03-MM1 underwent a rapid accretion burst event from 2019 January to June, resulting in flares observed in most class II methanol maser transitions starting in mid-January. In contrast, the 22.235 GHz water maser flare started in mid-April. To investigate the physical origin of this significant difference, we made the Karl G. Jansky Very Large Array observations toward the G358.93-0.03 region on 2019 March 23 and April 4 and obtained the intensity and spatial distribution images of the water maser as well as the continuum emissions at Ku and K bands on the epoch close to the water maser flare. A comparative analysis, incorporating previously reported detections in February (pre-water maser flare) and June (post-water maser flare), reveals the time lag between the accretion burst and water maser flare. These observations confirm the variations of the propagation speed of a heatwave induced by the accretion burst in different directions: the heatwave is decelerated in dense regions (e.g., the disk and jet), whereas in directions from G358-MM1 to water maser components, the heatwave speed is supposed to be close to the speed of light. Variations in flux density and spatial positions were detected for water masers and continuum emissions, indicating that the accretion burst event originating from G358-MM1 affects not only the immediate environment within a dense structure of 0.″2 (1400 au at a source distance of 6.75 kpc) around MM1 itself, but also exerts influence on broader-scale regions extending up to approximately 3″ (21,000 au).

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“…Masers are also used to investigate the kinematics as well as the physical conditions surrounding massive protostellar objects from the onset of formation (e.g. Caswell 1997;Stahler et al 2000;Szymczak & Gérard 2004;Breen et al 2010b;Darwish et al 2020). Hydroxyl (OH), water (H2O) and methanol (CH3OH) masers are commonly used to investigate the kinematics as well as the physical conditions surrounding massive protostellar objects in the early stage(s) of their formation.…”

Section: Introductionmentioning

confidence: 99%

OH maser towards IRAS 06056+2131: polarization parameters and evolution status

Darwish

Richards

Etoka

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present high angular resolution observations of OH maser emission towards the high-mass star forming region IRAS 06056+2131. The observations were carried out using the UK radio interferometer array, Multi-Element Radio Linked Interferometer Network (MERLIN) in the OH main lines at 1665- and 1667-MHz, in addition to the OH satellite line at 1720-MHz. The results of this study reveal the small upper limit to the size of emission in the 1665-MHz line with an estimated total intensity of ∼4 Jy. We did not detect any emission from the 1667-MHz and 1720-MHz lines. The full polarization mode of MERLIN enables us to investigate the magnetic field in the OH maser region. In this transition, a Zeeman pair is identified from which a magnetic strength of ∼−1.5 mG is inferred. Our results show that IRAS 06056+2131 is highly polarized, with ∼ 96 % circular polarization and ∼ 6 % linear polarization. The linear polarization angle is ∼29○, implying a magnetic field which could be aligned with the outflow direction detected toward this region, but the actual magnetic field direction has an uncertainty of up to 110○ due to the possible effects of Faraday rotation. The star forming evolutionary status of the embedded proto-stellar object is discussed.

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Methanol and water maser observations separate disc and outflow sources in IRAS 19410+2336

Cited by 8 publications

References 50 publications

Stellar Evolution Studies Using Masers

Stellar Evolution Studies Using Masers

Large-scale Effect of an Accretion Burst in the High-Mass Young Stellar Object G358.93-0.03-MM1

OH maser towards IRAS 06056+2131: polarization parameters and evolution status

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