A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

Baume, G.; Rodríguez, María Margarita; Corti, Mariela Alejandra; Carraro, G.; Panei, J. A.

doi:10.1093/mnras/stu1108

Cited by 9 publications

(7 citation statements)

References 48 publications

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“…Consistently with its high reddening, Population C lies far behind the other two. We note that the three groups of young stars found in this work present a scenario similar to that revealed from other studies on closer Galactic directions (see, e.g., Carraro & Costa 2009, Baume et al 2014or Mohr-Smith et al 2015.…”

Section: Stellar Populationssupporting

confidence: 88%

Stellar populations in the Carina region: The Galactic plane at l = 291

Molina-Lera,

Baume,

Gamen

et al. 2016

Preprint

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Context. Previous studies of the Carina region have revealed its complexity and richness as well as a significant number of early-type stars. However, in many cases, these studies only concentrated on the central region (Trumpler 14/16) or were not homogeneous. This latter aspect, in particular, is crucial because very different ages and distances for key clusters have been claimed in recent years. Aims. The aim of this work is to study in detail an area of the Galactic plane in Carina, eastward η Carina. We analyze the properties of different stellar populations and focus on a sample of open clusters and their population of YSOs and highly reddened early stars. We also studied the stellar mass distribution in these clusters and the possible scenario of their formation. Finally, we outline the Galactic spiral structure in this direction. Methods. We obtained deep and homogeneous photometric data (U BV I KC ) for six young open clusters: NGC 3752, Trumpler 18, NGC 3590, Hogg 10, 11, and 12, located in Carina at l ∼ 291 • , and their adjacent stellar fields, which we complemented with spectroscopic observations of a few selected targets. We also culled additional information from the literature, which includes stellar spectral classifications and near-infrared photometry from 2MAS S . We finally developed a numerical code that allowed us to perform a homogeneous and systematic analysis of the data. Our results provide more reliable estimates of distances, color excesses, masses, and ages of the stellar populations in this direction. Results. We estimate the basic parameters of the studied clusters and find that they identify two overdensities of young stellar populations located at about 1.8 kpc and 2.8 kpc, with E B−V ∼ 0.1 − 0.6. We find evidence of pre-main-sequence populations inside them, with an apparent coeval stellar formation in the most conspicuous clusters. We also discuss apparent age and distance gradients in the direction NW-SE. We study the mass distributions of the covered clusters and several others in the region (which we took form the literature). They consistently show a canonical IMF slope (the Salpeter one). We discover and characterise an abnormally reddened massive stellar population, scattered between 6.6 and 11 kpc. Spectroscopic observations of ten stars of this latter population show that all selected targets were massive OB stars. Their location is consistent with the position of the Carina-Sagittarius spiral arm.

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Section: Stellar Populationssupporting

confidence: 88%

Stellar populations in the Carina region: The Galactic plane at l = 291

Molina-Lera,

Baume,

Gamen

et al. 2016

Preprint

Self Cite

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show abstract

Section: Stellar Populationssupporting

confidence: 87%

“…For better visualisation, the whole fourth quadrant (270 • ≤ l ≤ 360 • ) is shown. We complement the result of the present study with data from previous papers (see, e.g., Baume et al 2014), such as young open clusters and HII regions, to provide a more comprehensive picture of the fourth quadrant. The figure also includes the four-arm Galactic model from Vallée Vallée (2008).…”

Section: Spiral Structure Toward Carinamentioning

confidence: 70%

Stellar populations in the Carina region

Molina-Lera

Baume

Gamen

et al. 2016

A&A

Self Cite

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Context. Previous studies of the Carina region have revealed its complexity and richness as well as a significant number of early-type stars. However, in many cases, these studies only concentrated on the central region (Trumpler 14/16) or were not homogeneous. This latter aspect, in particular, is crucial because very different ages and distances for key clusters have been claimed in recent years. Aims. The aim of this work is to study in detail an area of the Galactic plane in Carina, eastward η Carina. We analyze the properties of different stellar populations and focus on a sample of open clusters and their population of young stellar objects and highly reddened early stars. We also studied the stellar mass distribution in these clusters and the possible scenario of their formation. Finally, we outline the Galactic spiral structure in this direction. Methods. We obtained deep and homogeneous photometric data (U BV I KC ) for six young open clusters: NGC 3752, Trumpler 18, NGC 3590, Hogg 10, 11, and 12, located in Carina at l ∼ 291• , and their adjacent stellar fields, which we complemented with spectroscopic observations of a few selected targets. We also culled additional information from the literature, which includes stellar spectral classifications and near-infrared photometry from 2MASS. We finally developed a numerical code that allowed us to perform a homogeneous and systematic analysis of the data. Our results provide more reliable estimates of distances, color excesses, masses, and ages of the stellar populations in this direction. Results. We estimate the basic parameters of the studied clusters and find that they identify two overdensities of young stellar populations located at about 1.8 kpc and 2.8 kpc, with E B−V ∼ 0.1−0.6. We find evidence of pre-main-sequence populations inside them, with an apparent coeval stellar formation in the most conspicuous clusters. We also discuss apparent age and distance gradients in the direction NW-SE. We study the mass distributions of the covered clusters and several others in the region (which we took form the literature). They consistently show a canonical IMF slope (the Salpeter one). We discover and characterise an abnormally reddened massive stellar population, scattered between 6.6 and 11 kpc. Spectroscopic observations of ten stars of this latter population show that all selected targets were massive OB stars. Their location is consistent with the position of the Carina-Sagittarius spiral arm.

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“…Employed methods for determining the fundamental parameters of the young stellar clusters, (sizes, extinctions, distances, ages, members and masses) have already been described in several previous papers (see e.g. Chené et al 2012Chené et al , 2013Baume et al 2014). Here, we provide a brief summary and highlight what we have done differently in this study.…”

Section: Discussionmentioning

confidence: 95%

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

Corti

Baume

Panei

et al. 2016

A&A

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Aims. We report on a study of the global properties of some embedded clusters that are found in the fourth quadrant of the Milky Way. We aim to clarify some issues that relate to their location in the Galaxy and their stellar formation processes. Methods. We performed BVI photometric observations in the region of DBS 77, 78, 102, 160, and 161 clusters, and infrared spectroscopy in the DBS 77 region. These were complemented with JHK data from the VVV survey combined with the 2MASS catalogue, and used mid-infrared information from the GLIMPSE catalogue. We also searched for HI data from the SGPS and PMN radio surveys, and previous spectroscopic stellar classifications. The spectroscopic and photometric information enabled us to estimate the spectral classification of the brightest stars for each of the studied regions. On the other hand, we used radio data to investigate the interstellar material parameters and the continuum sources that are probably associated with the respective stellar components. Results. We estimated the basic physical parameters of the clusters (reddening, distance, age, and initial mass function). We searched for HII regions located near to the studied clusters and we analyzed the possible links between them. In the particular case of the DBS 160−161 clusters, we identified the HI bubble B332.5-0.1-42 that is located around them. We found that the mechanical energy injected in to the interstellar medium by the more massive stars of this couple of clusters was enough to generate the bubble.

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A deep and wide-field view at the IC 2944/2948 complex in Centaurus*

Cited by 9 publications

References 48 publications

Stellar populations in the Carina region: The Galactic plane at l = 291

Stellar populations in the Carina region: The Galactic plane at l = 291

Stellar populations in the Carina region

The embedded clusters DBS 77, 78, 102, and 160−161, and their link with the interstellar medium

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