The giant pillars of the Carina Nebula

Rathborne, J. M.; Brooks, Kate; Burton, M. G.; Cohen, Martin; Bontemps, Sylvain

doi:10.1051/0004-6361:20031631

Cited by 40 publications

(74 citation statements)

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“…Vazquez et al (1996), DeGioia-Eastwood et al (2001), and Tapia et al (2003) suggest star formation started 5 to 10 Myr ago and has been active in the cluster since then, and other authors indeed find compelling evidence for ongoing star formation in the whole Carina complex (Megeath et al 1996;Brooks et al 1998;Smith et al 2003Smith et al , 2004Smith et al , 2005bRathborne et al 2004). In particular, the Car I dark cloud (de Graauw et al 1981;Brooks et al 1998) that borders Tr14 to the SW seems to be an active region of star formation judging by its clumpy structure (Brooks et al 2003;Tapia et al 2006) and the presence of deeply embedded (young) objects and ultra-compact HII regions, at least one of which is compatible with a B0-O9 star (Brooks et al 2001;Rathborne et al 2002;Tapia et al 2003).…”

Section: Introductionmentioning

confidence: 87%

NTT and VLT diffraction limited imaging of Trumpler 14: revealing a massive core-halo cluster

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2007

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Aims. We present the deepest and highest resolution near-infrared imaging to date of cluster Trumpler 14 in Carina. Our goal is to identify and characterise the young stellar population of this massive cluster. Methods. We made use of deep and wide-field NIR images from NTT and VLT observations, that were sensitive enough to detect substellar sources at the distance to this cluster, and at high enough resolution (VLT diffraction limited) to fully resolve the core of the cluster crowded with O stars. Results. We find that Tr14 has a well-defined core-halo structure, where less than 30% of the cluster's members reside in the core. The core is well characterised by a King function with a core radius of 0. 17 (0.14 pc at the adopted distance) and a constant baseline, the halo, of 125 sources/pc 2 . Despite the unusually large number of OB stars, the central number density at zero radius is ∼7.3 × 10 3 pc −3 , which is loose in comparison with similar clusters. We find a normal reddening law towards the cluster and derive a global reddening of A v = 2.6 ± 0.3 mag. We find convincing evidence of a sparse foreground population (∼5 sources/arcmin 2 ) reddened by about A v = 1.4 mag, which we suggest is not associated with Tr14 but is most likely an older population produced in the nearby young clusters of this complex. The colour-magnitude diagrams are compatible with ages between "zero" and ∼5 Myr, although the sources from the core of the cluster appear to concentrate on the youngest isochrones, suggesting that the halo population is, on average, slightly older than the core population. Using a set of simplistic, fixed-age, mass-luminosity relations, we derive a mass of 10 4 M for the cluster. From the NACO JHK s L data, we estimate a fraction of infrared-excess sources of 35%, although this is likely to be an underestimate given the bright completeness limits of the L band. Finally, we argue that the formerly identified proplyd candidates that fall inside our survey are not proplyds but remnants of the disrupted molecular cloud that surround the cluster. We also find a series of interesting objects in our field that are worthy of future attention: a candidate photoionised proplyd best seen in the L band, a compact nebula surrounding an early type star, and a tentative proplyd/small shock associated with a faint source.

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Section: Introductionmentioning

confidence: 87%

NTT and VLT diffraction limited imaging of Trumpler 14: revealing a massive core-halo cluster

Ascenso

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Lago

2007

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“…The possibility that this feature represents a supernova remnant was discussed -and ruled out -by Ward- Thompson & Robson (1991 Another prominent feature in the KOSMA 13 CO emission map (not as strong in mid-IR emission) are the DR17 pillars (clumps DR17-1, 2, 3, 4 in Fig. B.1), which closely resemble molecular "pillars" such as those seen in the Carina (Rathborne et al 2004) or Eagle nebula (Pound 1998). We suggest that they are shaped locally by the OB stars in the DR17 region and are associated with the DR17 loop/H II region.…”

Section: The Cyg Ob2 Globules and The Afgl2591 Cloudmentioning

confidence: 99%

A new view of the Cygnus X region

Schneider

Bontemps

Simon

et al. 2006

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Context. The Cygnus X region is one of the richest star formation sites in the Galaxy. There is a long-standing discussion about whether the region is a chance superposition of several complexes along the line of sight or a single coherent complex at a distance of 1.5 to 2 kpc. Aims. Combining a 13 CO 2 → 1 survey taken with the KOSMA 3 m telescope with mid-IR images from MSX provides a way to improve our understanding of the spatial structure of the complex. The physical properties of the molecular gas can be derived in more detail as it was done in former studies. Methods. Cygnus X has been mapped in 13 CO J = 2 → 1 (10.8 deg 2 ) at an angular resolution of 130 , as well as for smaller areas in 12 CO and 13 CO J = 3 → 2 (90 ), using the KOSMA 3 m submm-telescope. Results. We identified 91 clumps in 13 CO 2 → 1 that have a typical excitation temperature of 10−30 K, an average density of 1.3 × 10 3 cm −3 , radii of 1−8 pc, and masses of a few hundred to several ten thousand M . The main cloud complexes, the northern part (M 2.8 × 10 5 M ) including DR21 and W75N and the southern region (M 4.5 × 10 5 M ) with IC 1318 b/c and AFGL2591, show differences in their physical properties. The 13 CO emission is closely associated with mid-IR emission seen with MSX. We find evidence that Cygnus OB2 and Cygnus OB9 are affecting the molecular material in Cygnus X. Conclusions. Since essentially all molecular cloud complexes in Cygnus X form groups that are connected by molecular emission (visible in channel and position-velocity maps) and partly show evidence of interaction with UV radiation, we conclude that most of the objects seen in this region are located at the same distance, i.e., that of the OB2 cluster at ∼1.7 kpc, which is also consistent with the distances of other OB associations (OB9, OB1) in Cygnus X.

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“…The group of stars visible in the VISTA image includes the B1.5 star HD 303 313 and the young stellar objects PCYC 129 and PCYC 139 (Povich et al 2011), both of which are marked by small circles in the figure. The nominal position of the mid-infrared source MSX6C G287.22−00.53 (which is classified as an H ii region; see Rathborne et al 2004) corresponds to the crossing of the coordinate lines at the center of the clustering.…”

Section: Clusters and Groups Of Embedded Objectsmentioning

confidence: 99%