Outflows, Disks, and Stellar Content in a Region of High‐Mass Star Formation: G5.89−0.39 with Adaptive Optics

Puga, E.; Feldt, M.; Álvarez, Carlos; Henning, Th.; Apai, Dániel; Coarer, E. Le; Chalabaev, A.; Stecklum, B.

doi:10.1086/500389

Cited by 29 publications

(54 citation statements)

References 42 publications

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“…The 1.3 mm continuum source peaks in the centre of the H ii region (Sollins et al 2004). Moreover, NIR observations of the H 2 v = 1−0 S (1) rovibrational line and the Brγ emission show evidence of three outflows with distinct orientations and driving sources (Puga et al 2006 Thus it is unlikely that there exist a single central high-mass star in W28 A2 as was initially thought to be the case due to the symmetric morphology of the H ii region.…”

Section: W28 A2mentioning

confidence: 92%

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores

Miettinen

Harju

Haikala

et al. 2006

A&A

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Aims. We determine the fractional SiO abundance in high-mass star-forming cores, and investigate its dependence on physical conditions, to provide constraints on the chemistry models of the formation of SiO in the gas phase or via grain mantle evaporation. The work addresses also CH 3 CCH chemistry, as the kinetic temperature is determined using this molecule. Methods. We estimate the physical conditions of 15 high-mass star-forming cores and derive the fractional SiO and CH 3 CCH abundances using spectral line and dust continuum observations with the SEST. Results. The kinetic temperatures as derived from CH 3 CCH range from 25 to 39 K, the average being 33 K. The average gas density in the cores is 4.5 × 10 6 cm −3 . The SiO emission regions are extended and typically half of the integrated line emission comes from the velocity range traced out by CH 3 CCH emission. The upper limit of SiO abundance in this "quiescent" gas component is ∼10 −10 . The average CH 3 CCH abundance is about 7 × 10 −9 . It shows a shallow, positive correlation with the temperature, whereas SiO shows the opposite tendency. Conclusions. We suggest that the high CH 3 CCH abundance and its possible increase when the clouds become warmer is related to the intensified desorption of the chemical precursors of the molecule from grain surfaces. In contrast, the observed tendency of SiO does not support the idea that the evaporation of Si-containing species from the grain mantles would be important, and it contradicts models where neutral reactions with activation barriers dominate SiO production. A possible explanation for the decrease is that warmer cores represent more evolved stages of core evolution with fewer high-velocity shocks and thus less efficient SiO replenishment.

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Section: W28 A2mentioning

confidence: 92%

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores

Miettinen

Harju

Haikala

et al. 2006

A&A

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“…G5.89 also harbors a very energetic outflow with CO linewidths in excess of 150 km s −1 (Watson et al 2007). Puga et al (2006) recently attempted (1,2,6,10,14,18,22) Jy beam −1 , superposed with white 3.6 cm VLA contours 0.5× (1,5,10,20,30,40,50,60) mJy beam −1 . The beams are shown in the lower right corner to identify the ionizing source of the ultracompact H II region using deep near-IR observations.…”

Section: Ngc7538 Irs1mentioning

confidence: 96%

High resolution submillimeter observations of massive protostars

Brogan¹,

Hunter²,

Indebetouw

et al. 2007

Astrophys Space Sci

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We describe results from recent Submillimeter Array observations of massive protostellar objects (CepheusA-East, NGC7538 IRS1, and G5.89-0.39) with resolutions ranging from 0.8 to 2 . A wide range of spectral and continuum properties are observed, with one unifying theme: at these resolutions all of the studied sources reveal multiple submillimeter cores. Some are observed to have cm-wavelength counterparts, and others not, suggesting a range of evolutionary stages coexisting in close proximity. In the presence of such complexity and multiplicity of sources, these data suggest that the interpretation of diagnostics such as kinematic velocity gradients and temperatures that are strongly dependent on spatial resolution should be approached cautiously. C.L. Brogan ( ) · T.R. Hunter NRAO,

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“…Near-infrared spectroscopy, however, results in Vol. 713 a much less ambiguous identification and classification of the massive star content (e.g., Watson & Hanson 1997;Blum et al 2000;Hanson et al 2002;Kendall et al 2003;Bik et al 2005;Puga et al 2006). These studies demonstrate the diagnostic power of near-infrared spectroscopy in characterizing the young, massive, stellar population.…”

Section: Introductionmentioning

confidence: 99%

Sequential Star Formation in RCW 34: A Spectroscopic Census of the Stellar Content of High-Mass Star-Forming Regions

Bik

Puga

Waters

et al. 2010

ApJ

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In this paper, we present VLT/SINFONI integral field spectroscopy of RCW 34 along with Spitzer/IRAC photometry of the surroundings. RCW 34 consists of three different regions. A large bubble has been detected in the IRAC images in which a cluster of intermediate-and low-mass class II objects is found. At the northern edge of this bubble, an H ii region is located, ionized by 3 OB stars, of which the most massive star has spectral type O8.5V. Intermediate-mass stars (2-3 M ) are detected of G-and K-spectral type. These stars are still in the premain-sequence (PMS) phase. North of the H ii region, a photon-dominated region is present, marking the edge of a dense molecular cloud traced by H 2 emission. Several class 0/I objects are associated with this cloud, indicating that star formation is still taking place. The distance to RCW 34 is revised to 2.5 ± 0.2 kpc and an age estimate of 2 ± 1 Myr is derived from the properties of the PMS stars inside the H ii region. Between the class II sources in the bubble and the PMS stars in the H ii region, no age difference could be detected with the present data. The presence of the class 0/I sources in the molecular cloud, however, suggests that the objects inside the molecular cloud are significantly younger. The most likely scenario for the formation of the three regions is that star formation propagated from south to north. First the bubble is formed, produced by intermediate-and low-mass stars only, after that, the H ii region is formed from a dense core at the edge of the molecular cloud, resulting in the expansion similar to a champagne flow. More recently, star formation occurred in the rest of the molecular cloud. Two different formation scenarios are possible. (1) The bubble with the cluster of low-and intermediate-mass stars triggered the formation of the O star at the edge of the molecular cloud, which in its turn induces the current star formation in the molecular cloud. (2) An external triggering is responsible for the star formation propagating from south to north.

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Outflows, Disks, and Stellar Content in a Region of High‐Mass Star Formation: G5.89−0.39 with Adaptive Optics

Cited by 29 publications

References 42 publications

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores

High resolution submillimeter observations of massive protostars

Sequential Star Formation in RCW 34: A Spectroscopic Census of the Stellar Content of High-Mass Star-Forming Regions

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Outflows, Disks, and Stellar Content in a Region of High‐Mass Star Formation: G5.89−0.39 with Adaptive Optics

Cited by 29 publications

References 42 publications

SiO and CH3CCH abundances and dust emission in high-mass star-forming cores

SiO and CH3CCH abundances and dust emission in high-mass star-forming cores

High resolution submillimeter observations of massive protostars

Sequential Star Formation in RCW 34: A Spectroscopic Census of the Stellar Content of High-Mass Star-Forming Regions

Contact Info

Product

Resources

About

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores

SiO and CH₃CCH abundances and dust emission in high-mass star-forming cores