Near-infrared imaging of RAFGL7009S

Zavagno, A.; Deharveng, L.; Nadeau, Daniel; Caplan, J.

doi:10.1051/0004-6361:20021129

Cited by 24 publications

(24 citation statements)

References 37 publications

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“…This object is also known as RAFGL 7009S and is a well-known embedded massive YSO associated with an UC Hii region and displaying strong midinfrared ice absorption features and a powerful molecular outflow (Zavagno et al 2002;Dartois et al 2000;Shepherd & Churchwell 1996;McCutcheon et al 1995). We identify a single strongly peaked sub-mm clump in the SCUBA 450 and 850 µm images, positionally coincident with the UC Hii region of KCW94 and with flux levels consistent with those quoted in McCutcheon et al (1995), allowing for the different filter bandwidths used.…”

Section: G2565+105: Panels 30s and 30lsupporting

confidence: 56%

“…Field centre (J2000) Mehringer et al (1998); (2) Wood & Churchwell (1989a); (3) Acord et al (1998); (4) Churchwell et al (1990); (5) Fish et al (2003); (6) Hofner et al (1994); (7) Kurtz et al (1994);(8) van der Tak et al (2000); (9) kinematic distance evaluated from CH 3 OH maser velocity given by Szymczak et al (2000); (10) Harju et al (1998); (11) kinematic distance evaluated from CH 3 OH maser velocity given by Caswell et al (1995); (12) kinematic distance evaluated from Hydrogen radio recombination line velocity given by Kuchar & Clarke (1997); (13) Blum et al (2000); (14) Zavagno et al (2002); (15) Motte et al (2003); (16) Palagi et al (1993); (17) Araya et al (2002); (18) Watson et al (2003); (19) Codella et al (1994). etc.) we are confident that there is little selection bias within our final list of UC Hii regions.…”

Section: Uc Hiimentioning

confidence: 99%

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A SCUBA imaging survey of ultracompact HII regions

Thompson

Hatchell

Walsh

et al. 2006

A&A

107

120

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We present a SCUBA submillimetre (450 and 850 µm) survey of the environment of 105 IRAS point sources, selected from the Wood & Churchwell (1989a) and Kurtz et al. (1994) radio ultracompact (UC) Hii region surveys. We detected a total of 155 sub-mm clumps associated with the IRAS point sources and identified three distinct types of object: ultracompact cm-wave sources that are not associated with any sub-mm emission (sub-mm quiet objects), sub-mm clumps that are associated with ultracompact cm-wave sources (radio-loud clumps); and sub-mm clumps that are not associated with any known ultracompact cm-wave sources (radio-quiet clumps). 90% of the sample of IRAS point sources were found to be associated with strong sub-mm emission. We consider the sub-mm colours, morphologies and distance-scaled fluxes of the sample of sub-mm clumps and show that the sub-mm quiet objects are unlikely to represent embedded UC Hii regions unless they are located at large heliocentric distances. Many of the 2. 5 SCUBA fields contain more than one sub-mm clump, with an average number of companions (the companion clump fraction) of 0.90. The clumps are more strongly clustered than other candidate HMPOs and the mean clump surface density exhibits a broken power-law distribution with a break at 3 pc. We demonstrate that the sub-mm and cm-wave fluxes of the majority of radio-loud clumps are in excellent agreement with the standard model of ultracompact Hii regions. We speculate on the nature of the radio-quiet sub-mm clumps and, whilst we do not yet have sufficient data to conclude that they are in a pre-UC Hii region phase, we argue that their characteristics are suggestive of such a stage.

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Section: G2565+105: Panels 30s and 30lsupporting

confidence: 56%

Section: Uc Hiimentioning

confidence: 99%

A SCUBA imaging survey of ultracompact HII regions

Thompson

Hatchell

Walsh

et al. 2006

A&A

107

120

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“…The region is associated with a weak and irregular compact radio source that was initially classified as an ultracompact (UC) H ii region (Kurtz et al 1994;Walsh et al 1998). The radio source spatially coincides with an unresolved infrared source (Zavagno et al 2002;Varricatt et al 2010) and with submillimeter emissions at 350 μm, 450 μm, and 850 μm (Hunter et al 2000;Walsh et al 2003).…”

Section: G2565+105mentioning

confidence: 69%

“…Furthermore, four 6.7 GHz CH 3 OH masers were detected near the continuum peak of the radio source; they are linearly distributed southward (Walsh et al 1998). The CH 3 OH maser velocities suggest an association with the radio source, possibly with a disk and not with the bipolar outflow (Zavagno et al 2002).…”

Section: G2565+105mentioning

confidence: 88%

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Surcis

Vlemmings

Langevelde

et al. 2015

A&A

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Context. Theoretical simulations and observations at different angular resolutions have shown that magnetic fields have a central role in massive star formation. Like in low-mass star formation, the magnetic field in massive young stellar objects can either be oriented along the outflow axis or randomly. Aims. Measuring the magnetic field at milliarcsecond resolution (10-100 au) around a substantial number of massive young stellar objects permits determining with a high statistical significance whether the direction of the magnetic field is correlated with the orientation of the outflow axis or not. Methods. In late 2012, we started a large VLBI campaign with the European VLBI Network to measure the linearly and circularly polarized emission of 6.7 GHz CH 3 OH masers around a sample of massive star-forming regions. This paper focuses on the first seven observed sources, G24.78+0.08, G25.65+1.05, G29.86-0.04, G35.03+0.35, G37.43+1.51, G174.20-0.08, and G213.70-12.6. For all these sources, molecular outflows have been detected in the past. Results. We detected a total of 176 CH 3 OH masing cloudlets toward the seven massive star-forming regions, 19% of which show linearly polarized emission. The CH 3 OH masers around the massive young stellar object MM1 in G174.20-0.08 show neither linearly nor circularly polarized emission. The linear polarization vectors are well ordered in all the other massive young stellar objects. We measured significant Zeeman splitting toward both A1 and A2 in G24.78+0.08, and toward G29.86-0.04 and G213.70-12.6. Conclusions. By considering all the 19 massive young stellar objects reported in the literature for which both the orientation of the magnetic field at milliarcsecond resolution and the orientation of outflow axes are known, we find evidence that the magnetic field (on scales 10-100 au) is preferentially oriented along the outflow axes.

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“…It is located at a distance of 3.2 kpc (Molinari et al 1996). The radio peak is coincident with an unresolved infrared source, identified as a young B1 V star with a large K ‐band excess (Zavagno et al 2002), and is also closely associated with methanol (Molinari et al 1996) and ammonia maser emission (Szymczak, Hrynek & Kus 2000; Walsh et al 2003). Submillimetre continuum observations at 350 μm (Hunter et al 2000), 450 μm and 850 μm (Walsh et al 2003) are all peaked at the position of the radio and maser sources.…”

Section: Introductionmentioning

confidence: 96%

Imaging and integral-field spectroscopy of shocked H2 around G25.65+1.05

Todd

Ramsay

2006

Monthly Notices of the Royal Astronomical Society

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Near‐infrared imaging of the emission from molecular hydrogen is a powerful method for discovering outflows in star‐forming regions. We present new near‐infrared images, and long‐slit and integral‐field spectroscopy of the ultracompact H ii region G25.65+1.05. These new observations reveal shocked H2 emission associated with a bipolar outflow from a young high‐mass star at the centre of the source. The physical parameters of the outflow are discussed and compared with those of outflows from lower mass stars.

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Near-infrared imaging of RAFGL7009S

Cited by 24 publications

References 37 publications

A SCUBA imaging survey of ultracompact HII regions

A SCUBA imaging survey of ultracompact HII regions

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Imaging and integral-field spectroscopy of shocked H2 around G25.65+1.05

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