G287.84-0.82: an infrared star cluster in the Carina nebula

Hägele, G. F.; Colombo, J. F. Albacete; Barbá, R. H.; Bosch, G.

doi:10.1111/j.1365-2966.2004.08403.x

Cited by 10 publications

(9 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A very similar morphology was found in the submillimetre regime by Preibisch et al (2011). This structure is reminiscent of other ‘pillars’ in the southern part of the nebula (Rathborne et al 2004), and notably of G287.84−0.82 (Dutra & Bica 2001; Hägele et al 2004; Smith, Stassun & Bally 2005).…”

Section: Observationssupporting

confidence: 73%

Imaging study of NGC 3372, the Carina nebula - III. The properties of G287.47−0.54 (Tr 14-N4), an embedded young cluster and its associated H2 emission★

Tapia¹,

Roth²,

Bohigas³

et al. 2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

New deep broad‐ and narrow‐band (JHK and Br γ at 2.17 μm and H2 at 2.12 μm) near‐infrared (near‐IR) images of the mid‐IR source G287.47−0.54 (Tr14‐N4) taken with the Baade Magellan telescope are presented and analysed along with archive 3.6–8 μ m Spitzer images. The analysis of these data demonstrates the presence of a compact (r∼ 23 arcsec, 0.3 pc), embedded IR cluster with at least 72 young members. The colour–magnitude diagram of the cluster suggests an age of approximately 105 years, consistent with the large fraction (≥32 per cent) of embedded sources found to show significant excess emission at λ > 2 μ m. The two youngest and most luminous sources are located close to the cluster nucleus. The properties of their spectral energy distributions (SEDs) indicate that these are Class I young stellar objects (YSOs) with masses in the range 7–9 M⊙ and luminosities between 400 and 800 L⊙. We derive the presence of a tilted (i∼ 40°–70°) disc of size ≥0.05 pc around one of these YSOs, #902. This object is seen directly through the dust disc only at λ≥ 2.2, with most of the observed near‐IR radiation being scattered light from lobes on both sides of the disc. In contrast, the second bright YSO, #438, is seen directly even in the near‐IR and also shows symmetrically elongated features that seem to be caused by scattering. The young cluster G287.47−0.54 is embedded at the head of a dust pillar and is another example of a photodissociation region (PDR) where triggered star formation occurs as a consequence of the interaction of a very massive developed cluster, in this case Tr 16, with a dense molecular core. It appears that the dense cloudlet is sticking out of the remnant giant molecular cloud located at the far side of the northern Carina nebula. Five small molecular hydrogen emission knots at 2.12 μ m with no Brγ counterpart are found in the vicinity of a CO peak, some 0.4 pc north‐west of the cluster nucleus. Most probably, these are shock excited, suggesting the presence of mass outflows in the region. At present, it is unclear whether the engine of this outflow is a member of the cluster or rather it is an undetected, younger YSO deeply embedded in the molecular core.

show abstract

Section: Observationssupporting

confidence: 73%

Imaging study of NGC 3372, the Carina nebula - III. The properties of G287.47−0.54 (Tr 14-N4), an embedded young cluster and its associated H2 emission★

Tapia¹,

Roth²,

Bohigas³

et al. 2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…An 8.6 µm MSX image of the Carina Nebula is shown in Figure 1. The presence of active, ongoing star formation in this region has since been confirmed by obervations of embedded young clusters like the "Treasure Chest" and others (Smith et al 2005;Rathborne et al 2002Rathborne et al , 2004Hägele et al 2004) and a large number of outflows in the form of irradiated Herbig-Haro (HH) jets throughout the region (Smith et al 2004a(Smith et al , 2010. There are many dense cores detected in C 18 O that are spread across the region, providing sites of ongoing and potential future star formation, with some evidence for molecular outflow activity (Yonekura et al 2005).…”

Section: Introductionmentioning

confidence: 83%

Spitzer Space Telescope observations of the Carina nebula: the steady march of feedback-driven star formation

Smith¹,

Povich²,

Whitney³

et al. 2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We report the first results of imaging the Carina nebula (NGC 3372) with the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope, providing a photometry catalogue of over 44 000 point sources as well as a catalogue of over 900 candidate young stellar objects (YSOs) based on fits to their spectral energy distributions (SEDs). We discuss several aspects of the extended emission, including the structure of dozens of dust pillars that result when a clumpy molecular cloud is shredded by feedback from massive stars. There are surprisingly few of the ‘extended green objects’ (EGOs) that are normally taken as signposts of outflow activity in Spitzer data, and not one of the dozens of Herbig‐Haro jets detected optically are seen as EGOs. EGOs are apparently poor tracers of outflow activity in strongly irradiated environments, due to the effects of massive star feedback. A population of ‘extended red objects’ tends to be found around late O‐type and early B‐type stars, some with clear bow‐shock morphology. These are dusty shocks where stellar winds collide with photoevaporative flows off nearby clouds. Finally, the relative distributions of O‐type stars, small star clusters and subclusters of YSOs as compared to the dust pillars show that while some YSOs are located within dust pillars, many more stars and YSOs reside just outside pillar heads. We suggest that pillars are transient phenomena, part of a continuous outwardly propagating wave of star formation driven by feedback from massive stars. As the pillars are destroyed, they leave newly formed stars in their wake, and these are then subsumed into the young OB association. The YSOs are found predominantly in the cavity between pillars and massive stars, arguing that their formation was in fact triggered. Altogether, the current generation of YSOs shows no strong deviation from a normal initial mass function (IMF). The number of YSOs is consistent with a roughly constant star‐formation rate over the past ∼3 Myr, implying that propagating star formation in pillars constitutes an important mechanism to construct unbound OB associations. These accelerated pillars may give birth to massive O‐type stars that, after several million years, could appear to have formed in isolation.

show abstract

“…First, CCCP-Cl 17 is the Treasure Chest, a compact cluster with bright mid-infrared emission dominated by an O9.5 star producing the compact HII region MSX G287.84-0.82 (Hägele et al 2004;Smith et al 2005). About 100 members are in the full X-ray sample.…”

Section: Obscured and Embedded Clustersmentioning

confidence: 99%

X-Ray Star Clusters in the Carina Complex

Feigelson

Getman

Townsley

et al. 2011

ApJS

View full text Add to dashboard Cite

The distribution of young stars found in the Chandra Carina Complex Project (CCCP) is examined for clustering structure. X-ray surveys are advantageous for identifying young stellar populations compared to optical and infrared surveys in suffering less contamination from nebular emission and Galactic field stars. The analysis is based on smoothed maps of a spatially complete subsample of ∼ 3000 brighter X-ray sources classified as Carina members, and ∼ 10, 000 stars from the full CCCP sample. The principal known clusters are recovered, and some

show abstract

G287.84-0.82: an infrared star cluster in the Carina nebula

Cited by 10 publications

References 30 publications

Imaging study of NGC 3372, the Carina nebula - III. The properties of G287.47−0.54 (Tr 14-N4), an embedded young cluster and its associated H2 emission★

Imaging study of NGC 3372, the Carina nebula - III. The properties of G287.47−0.54 (Tr 14-N4), an embedded young cluster and its associated H2 emission★

Spitzer Space Telescope observations of the Carina nebula: the steady march of feedback-driven star formation

X-Ray Star Clusters in the Carina Complex

Contact Info

Product

Resources

About