Large-Scale Structure of the Carina Nebula

Smith, Nathan; Egan, M. P.; Carey, Sean; Price, S. D.; Morse, Jon A.; Price, P. A.

doi:10.1086/312578

Cited by 92 publications

(154 citation statements)

References 21 publications

Supporting

Mentioning

149

Contrasting

Order By: Relevance

“…We can see many of them in the southern part of the image. We also observe large bubbles in the northern region, probably caused by the gusts of hot gas leaking from the powerful stars at the center of the nebula (Smith et al 2000). The central clusters Tr 14 and Tr 16 tend to be devoid of star formation (Smith & Brooks 2008), but there are active sites of ongoing star formation in the outer regions of the nebula.…”

Section: Introductionmentioning

confidence: 85%

“…However, following the detection of several embedded IR sources, Smith et al (2000) showed that star formation is still going on in this region. Later, Brooks et al (2001) also identified two compact Hii regions possibly linked with very young O-type stars.…”

Section: Introductionmentioning

confidence: 99%

“…Approximate locations of different star clusters (Tr 14,15,16;Bo 9,10;Cr 228,232,and NGC 3324) are denoted by white boxes. η Carinae is marked by an arrow and in the lower left part of the image, south pillars (Smith et al 2000) are shown. The region covered in the present study is shown by the green box.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Investigation of the stellar content in the western part of the Carina nebula

Kumar¹,

Sharma²,

Manfroid³

et al. 2014

A&A

View full text Add to dashboard Cite

Context. The low obscuration and proximity of the Carina nebula make it an ideal place to study the ongoing star formation process and impact of massive stars on low-mass stars in their surroundings. Aims. To investigate this process, we generated a new catalog of the pre-main-sequence stars in the Carina west (CrW) region and studied their nature and spatial distribution. We also determined various parameters (reddening, reddening law, age, mass), which are used further to estimate the initial mass function and K-band luminosity function for the region under study. Methods. We obtained deep UBVRI Hα photometric data of the field situated to the west of the main Carina nebula and centered on WR 22. Medium-resolution optical spectroscopy of a subsample of X-ray selected objects along with archival data sets from Chandra, XMM-Newton and 2MASS surveys were used for the present study. Different sets of color-color and color-magnitude diagrams are used to determine reddening for the region and to identify young stellar objects (YSOs) and estimate their age and mass. Results. Our spectroscopic results indicate that the majority of the X-ray sources are late spectral type stars. The region shows a large amount of differential reddening with minimum and maximum values of E(B − V) as 0.25 and 1.1 mag, respectively. Our analysis reveals that the total-to-selective absorption ratio R V is ∼3.7 ± 0.1, suggesting an abnormal grain size in the observed region. We identified 467 YSOs and studied their characteristics. The ages and masses of the 241 optically identified YSOs range from ∼0.1 to 10 Myr and ∼0.3 to 4.8 M , respectively. However, the majority of them are younger than 1 Myr and have masses below 2 M . The high mass star WR 22 does not seem to have contributed to the formation of YSOs in the CrW region. The initial mass function slope, Γ, in this region is found to be −1.13 ± 0.20 in the mass range of 0.5 < M/M < 4.8. The K-band luminosity function slope (α) is also estimated as 0.31 ± 0.01. We also performed minimum spanning tree analysis of the YSOs in this region, which reveals that there are at least ten YSO cores associated with the molecular cloud, and that leads to an average core radius of 0.43 pc and a median branch length of 0.28 pc.

show abstract

Section: Introductionmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Investigation of the stellar content in the western part of the Carina nebula

Kumar¹,

Sharma²,

Manfroid³

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…These HII regions are seen in many massive molecular clouds and are the object of a great number of observational studies: in the Rosette nebula (Schneider et al 2010), M16 (Andersen et al 2004), 30 Doradus (Walborn et al 2002), Carina nebula (Smith et al 2000), the Elephant Trunk nebula (Reach et al 2004), the Trifid nebula (Lefloch et al 2002), M17 (Jiang et al 2002), or the Horsehead nebula (Bowler et al 2009). Spitzer observations also provide a wide range of HII regions, which were studied in detail by Deharveng et al (2010).…”

Section: Introductionmentioning

confidence: 99%

3D simulations of pillar formation around HII regions: the importance of shock curvature

Tremblin

Audit

Minier

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. Radiative feedback from massive stars is a key process for understanding how HII regions enhance or inhibit star formation in pillars and globules at the interface with molecular clouds. We aim to contribute by modelling the interactions between ionization and gas clouds to better understand the processes at work. We study in detail the impact of modulations on the cloud-HII region interface and density modulations inside the cloud. Methods. We ran 3D hydrodynamical simulations based on Euler equations coupled with gravity using the HERACLES code. We implemented a method to solve ionization/recombination equations and took into account typical heating and cooling processes at work in the interstellar medium that are caused by ionization/recombination physics. Results. UV radiation creates a dense shell compressed between an ionization front and a shock ahead. Interface modulations produce a curved shock that collapses on itself, which leads to stable growing pillar-like structures. The narrower the initial interface modulation, the longer the resulting pillar. We interpret pillars resulting from density modulations in terms of the ability of these density modulations to curve the shock ahead of the ionization front. Conclusions. The shock curvature is a key process for understanding the formation of structures at the edge of HII regions. Interface and density modulations at the edge of the cloud have a direct impact on the morphology of the dense shell during its formation. Deeper inside the cloud, structures have less influence because of the high densities reached by the shell during its expansion.

show abstract

“…through jets from obscured proto-stars piercing through the surface into the HII region (e.g. in Eta Carina, Smith et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Pillars, Jets and Dynamical Features

et al. 2010

View full text Add to dashboard Cite

Abstract. We present high resolution simulations on the impact of ionizing radiation on turbulent molecular clouds. The combination of hydrodynamics, gravitational forces and ionization in the tree-SPH code iVINE naturally leads to the formation of elongated filaments and clumps, which are in excellent agreement with the pillars observed around HII regions. Including gravity the formation of a second generation of low-mass stars with surrounding protostellar disks is triggered at the tips of the pillars, as also observed. A parameter study allows us to determine the physical conditions under which irregular structures form and whether they resemble large pillars or a system of small, isolated globules.

show abstract

Large-Scale Structure of the Carina Nebula

Cited by 92 publications

References 21 publications

Investigation of the stellar content in the western part of the Carina nebula

Investigation of the stellar content in the western part of the Carina nebula

3D simulations of pillar formation around HII regions: the importance of shock curvature

Pillars, Jets and Dynamical Features

Contact Info

Product

Resources

About