A hot compact dust disk around a massive young stellar object

Kraus, Stefan; Hofmann, K.-H.; Menten, K. M.; Schertl, D.; Weigelt, G.; Wyrowski, F.; Meilland, A.; Perraut, K.; Petrov, R.; Robbe-Dubois, S.; Schilke, P.; Testi, L.

doi:10.1038/nature09174

Cited by 146 publications

(212 citation statements)

References 26 publications

(23 reference statements)

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“…However, direct observations of accretion disks in high-mass star-forming regions are still limited to few cases, mostly around YSOs with masses ≤20 M and luminosities ≤10 4 L (e.g., Kraus et al 2010). The situation is less clear for more luminous objects (Cesaroni et al 2007), although recently Zapata et al (2009recently Zapata et al ( , 2010 suggested the presence of a Keplerian infalling ring around a central object of at least 60 M .…”

Section: Introductionmentioning

confidence: 99%

On the kinematics of massive star forming regions: the case of IRAS 17233–3606

Leurini

Codella

Zapata

et al. 2011

A&A

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Context. Direct observations of accretion disks around high-mass young stellar objects would help to discriminate between different models of formation of massive stars. However, given the complexity of massive star forming regions, such studies are still limited in number. Additionally, there is still no general consensus on the molecular tracers to be used for such investigations. Aims. Because of its close distance and high luminosity, IRAS 17233−3606 is a potential laboratory to search for traces of rotation in the inner gas around the protostar(s). Therefore, we selected the source for a detailed analysis of its molecular emission at 230 GHz with the SMA. Methods. We systematically investigated the velocity fields of transitions in the SMA spectra which are not affected by overlap with other transitions, and searched for coherent velocity gradients to compare them to the distribution of outflows in the region. Beside CO emission we also used high-angular H 2 images to trace the outflow motions driven by the IRAS 17233−3606 cluster. Results. We find linear velocity gradients in many transitions of the same molecular species and in several molecules. We report the first detection of HNCO in molecular outflows from massive YSOs. We discuss the CH 3 CN velocity gradient taking into account various scenarios: rotation, presence of multiple unresolved sources with different velocities, and outflow(s). Although other interpretations cannot be ruled out, we propose that the CH 3 CN emission might be affected by the outflows of the region. Higher angular observations are needed to discriminate between the different scenarios.Conclusions. The present observations, with the possible association of CH 3 CN with outflows in a few thousands AU around the YSOs' cluster, (i) question the choice of the tracer to probe rotating structures, and (ii) show the importance of the use of H 2 images for detailed studies of kinematics.

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Section: Introductionmentioning

confidence: 99%

On the kinematics of massive star forming regions: the case of IRAS 17233–3606

Leurini

Codella

Zapata

et al. 2011

A&A

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“…Images of stellar surfaces (e.g., Haubois et al 2009), binaries (e.g., Zhao et al 2008), and circumstellar shells around evolved stars (e.g., Le Bouquin et al 2009) have been obtained. Two circumstellar disks have been imaged, around an intermediate-mass young star (Renard et al 2010) and around a massive young star (Kraus et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A low optical depth region in the inner disk of the Herbig Ae star HR 5999

Benisty

Renard

Natta

et al. 2011

A&A

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Context. Circumstellar disks surrounding young stars are known to be the birthplaces of planetary systems, and the innermost astronomical unit is of particular interest. Near-infrared interferometric studies have revealed a complex morphology for the close environment surrounding Herbig Ae stars. Aims. We present new long-baseline spectro-interferometric observations of the Herbig Ae star, HR 5999, obtained in the H and K bands with the AMBER instrument at the VLTI, and aim to produce near-infrared images at the sub-AU spatial scale. Methods. We spatially resolve the circumstellar material and reconstruct images in the H and K bands using the MiRA algorithm. In addition, we interpret the interferometric observations using models that assume that the near-infrared excess is dominated by the emission of a circumstellar disk. We compare the images reconstructed from the VLTI measurements to images obtained using simulated model data.Results. The K-band image reveals three main elements: a ring-like feature located at ∼0.65 AU, a low surface brightness region inside 0.65 AU, and a central spot. At the maximum angular resolution of our observations (B/λ ∼ 1.3 mas), the ring is resolved while the central spot is only marginally resolved, preventing us from revealing the exact morphology of the circumstellar environment. We suggest that the ring traces silicate condensation, i.e., an opacity change, in a circumstellar disk around HR 5999. We build a model that includes a ring at the silicate sublimation radius and an inner disk of low surface brightness responsible for a large amount of the near-infrared continuum emission. The model successfully fits the SED, visibilities, and closure phases in the H and K bands, and provides evidence of a low surface brightness region inside the silicate sublimation radius. Conclusions. This study provides milli-arcsecond resolution images of the environment of HR 5999 and additional evidence that in Herbig Ae stars, there is material in a low surface brightness region, probably a low optical depth region, located inside the silicate sublimation radius and of unknown nature. The possibility that the formation of such a region in a thick disk is related to disk evolution should be investigated.

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“…In this scenario all massive stars should belong to multiple systems. The first very massive young stars observed with the VLTI/AMBER (Kraus et al 2010) showed no clue of binarity and a disk-like structure compatible with the first scenario (see Fig. 3).…”

Section: The Formation Of Massive Starsmentioning

confidence: 61%

An interferometric journey around massive stars

Meilland¹,

Stee²

2014

Proc. IAU

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Abstract. Since the construction in the late nineties of modern facilities such as the VLTI or CHARA, interferometry became a key technique to probe massive stars and their oftencomplex circumstellar environments. Over the last decade, the development of a new generation of beam combiners for these facilities enabled major breakthroughs in the understanding of the formation and evolution of massive stars. In this short review, we will present few of these advances concerning young stellar objects, binarity, mass loss, and stellar surfaces.

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A hot compact dust disk around a massive young stellar object

Cited by 146 publications

References 26 publications

On the kinematics of massive star forming regions: the case of IRAS 17233–3606

On the kinematics of massive star forming regions: the case of IRAS 17233–3606

A low optical depth region in the inner disk of the Herbig Ae star HR 5999

An interferometric journey around massive stars

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