The VISTA Carina Nebula Survey

Zeidler, Peter; Preibisch, Thomas; Ratzka, Thorsten; Roccatagliata, V.; Petr-Gotzens, M. G.

doi:10.1051/0004-6361/201424376

Cited by 16 publications

(26 citation statements)

References 43 publications

(55 reference statements)

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“…Roughly 50% of the YSO population in Carina is found in sparse small groups that are widely distributed over an area of several square parsecs (Preibisch et al 2011b;Zeidler et al 2016). The newly detected Carina disks belong to this distributed population and are both located at larger distances from the ionizing sources where external evaporation will not threaten their survival over the next 10 million years.…”

Section: Discussionmentioning

confidence: 96%

Protoplanetary Disks in the Hostile Environment of Carina

Mesa‐Delgado

Zapata

Henney

et al. 2016

ApJL

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We report the first direct imaging of protoplanetary disks in the star-forming region of Carina, the most distant massive cluster in which disks have been imaged. Using the Atacama Large Millimeter/sub-millimeter Array (ALMA), the disks are observed around two young stellar objects (YSOs) that are embedded inside evaporating gaseous globules and exhibit jet activity. The disks have an average radius of 60 au and total masses of 30 and 50 M Jup . Given the measured masses, the minimum timescale required for planet formation (∼1-2 Myr) and the average age of the Carina population (∼1-4 Myr), it is plausible that young planets are present or their formation is currently ongoing in these disks. The non-detection of millimeter emission above the 4σ threshold (~M 7 Jup ) in the core of the massive cluster Trumpler 14, an area containing previously identified proplyd candidates, suggests evidence for rapid photo-evaporative disk destruction in the cluster's harsh radiation field. This would prevent the formation of giant gas planets in disks located in the cores of Carina's dense subclusters, whereas the majority of YSO disks in the wider Carina region remain unaffected by external photoevaporation.

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Section: Discussionmentioning

confidence: 96%

Protoplanetary Disks in the Hostile Environment of Carina

Mesa‐Delgado

Zapata

Henney

et al. 2016

ApJL

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“…the Carina star-forming region (e.g. Zeidler et al 2016) and the Tarantula Nebula (e.g. Sabbi et al 2016).…”

Section: Measurements Of Mass Segregationmentioning

confidence: 99%

Simulations of Fractal Star Cluster Formation. I. New Insights for Measuring Mass Segregation of Star Clusters with Substructure

Puzia

Lin

et al. 2017

ApJ

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We compare the existent methods including the minimum spanning tree based method and the local stellar density based method, in measuring mass segregation of star clusters. We find that the minimum spanning tree method reflects more the compactness, which represents the global spatial distribution of massive stars, while the local stellar density method reflects more the crowdedness, which provides the local gravitational potential information. It is suggested to measure the local and the global mass segregation simultaneously. We also develop a hybrid method that takes both aspects into account. This hybrid method balances the local and the global mass segregation in the sense that the predominant one is either caused either by dynamical evolution or purely accidental, especially when such information is unknown a priori. In addition, we test our prescriptions with numerical models and show the impact of binaries in estimating the mass segregation value.As an application, we use these methods on the Orion Nebula Cluster (ONC) observations and the Taurus cluster. We find that the ONC is significantly mass segregated down to the 20th most massive stars. In contrast, the massive stars of the Taurus cluster are sparsely distributed in many different subclusters, showing a low degree of compactness. The massive stars of Taurus are also found to be distributed in the high-density region of the subclusters, showing significant mass segregation at subcluster scales. Meanwhile, we also apply these methods to discuss the possible mechanisms of the dynamical evolution of the simulated substructured star clusters.

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“…A large number of pre-main-sequence stars have been identified from optical, infrared, and X-ray surveys (e.g. Tapia et al 2003;Ascenso et al 2007;Sanchawala et al 2007aSanchawala et al , 2007bPovich et al 2011;Gaczkowski et al 2013;Preibisch et al 2014;Kumar et al 2014;Beccari et al 2015), and Zeidler et al (2016) estimated the total number of pre-main-sequence objects in the region at 164 000. Hartigan et al (2015) presented candidate jets emanating from young stars in an area covering more than a square degree of the nebula.…”

Section: Introductionmentioning

confidence: 99%

Radio observations of globulettes in the Carina nebula

Haikala

Gahm

Grenman

et al. 2017

A&A

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Context. The Carina nebula hosts a large number of globulettes. An optical study of these tiny molecular clouds shows that the majority are of planetary mass, but there are also those with masses of several tens up to a few hundred Jupiter masses. Aims. We seek to search for, and hopefully detect, molecular line emission from some of the more massive objects; in case of successful detection we aim to map their motion in the Carina nebula complex and derive certain physical properties. Methods. We carried out radio observations of molecular line emission in 12 CO and 13 CO (2-1) and (3-2) of 12 globulettes in addition to positions in adjacent shell structures using APEX. Results. All selected objects were detected with radial velocities shifted relative to the emission from related shell structures and background molecular clouds. Globulettes along the western part of an extended dust shell show a small spread in velocity with small velocity shifts relative to the shell. This system of globulettes and shell structures in the foreground of the bright nebulosity surrounding the cluster Trumpler 14 is expanding with a few km s −1 relative to the cluster. A couple of isolated globulettes in the area move at similar speed. Compared to similar studies of the molecular line emission from globulettes in the Rosette nebula, we find that the integrated line intensity ratios and line widths are very different. The results show that the Carina objects have a different density/temperature structure than those in the Rosette nebula. In comparison the apparent size of the Carina globulettes is smaller, owing to the larger distance, and the corresponding beam filling factors are small. For this reason we were unable to carry out a more detailed modelling of the structure of the Carina objects in the way as performed for the Rosette objects. Conclusions. The Carina globulettes observed are compact and denser than objects of similar mass in the Rosette nebula. The distribution and velocities of these globulettes suggest that they have originated from eroding shells and elephant trunks. Some globulettes in the Trumpler 14 region are quite isolated and located far from any shell structures. These objects move at a similar speed as the globulettes along the shell, suggesting that they once formed from cloud fragments related to the same foreground shell.

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The VISTA Carina Nebula Survey

Cited by 16 publications

References 43 publications

Protoplanetary Disks in the Hostile Environment of Carina

Protoplanetary Disks in the Hostile Environment of Carina

Simulations of Fractal Star Cluster Formation. I. New Insights for Measuring Mass Segregation of Star Clusters with Substructure

Radio observations of globulettes in the Carina nebula

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