X-Ray Star Clusters in the Carina Complex

Feigelson, E. D.; Getman, Konstantin V.; Townsley, Leisa K.; Broos, P. S.; Povich, Matthew S.; Garmire, G. P.; King, Robert R.; Montmerle, T.; Preibisch, Thomas; Smith, Nathan; Stassun, Keivan G.; Wang, Junfeng; Wolk, S. J.; Zinnecker, H.

doi:10.1088/0067-0049/194/1/9

Cited by 79 publications

(93 citation statements)

References 58 publications

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“…This result agrees with the results on the spatial distribution of the X-ray selected YSOs in the CCCP (Feigelson et al 2011;Preibisch et al 2011a), which established that about half of the young stars are members of clusters or stellar groups, while the other half constitutes the "widely-distributed population", which is spread out through the entire CCCP area. Our findings extend this result from the 1.4 sq.…”

Section: Portion Of Cysos In Clusterssupporting

confidence: 92%

“…Based on an estimate of the total young stellar population in the area of the CCCP X-ray survey (Feigelson et al 2011), we can estimate a total number of ∼164 000 YSOs for the full area of the Carina nebula complex that includes the region NGC 3324. Appendix B: The catalog of infrared excess objects in the VCNS survey area …”

Section: Discussionmentioning

confidence: 99%

“…Based on the size of the X-ray selected YSO sample, Feigelson et al (2011) estimated that the total stellar population (i.e., down to stellar masses of ∼0.1 M ) in the 1.4 sq. deg CCCP field should be ∼104 000.…”

Section: An Estimate Of the Full Young Stellar Population In The Cncmentioning

confidence: 99%

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The VISTA Carina Nebula Survey

Zeidler

Preibisch

Ratzka

et al. 2015

A&A

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We performed a deep wide-field (6.76 sq. deg) near-infrared survey with the VISTA telescope that covers the entire extent of the Carina nebula complex (CNC). The point-source catalog created from these data contains around four million individual objects down to masses of 0.1 M . We present a statistical study of the large-scale spatial distribution and an investigation of the clustering properties of infrared-excesses objects, which are used to trace disk-bearing young stellar objects (YSOs). A selection based on a near-infrared (J − H) versus (H − K s ) color-color diagram shows an almost uniform distribution over the entire observed area. We interpret this as a result of the very high degree of background contamination that arises from the Carina Nebula's location close to the Galactic plane. Complementing the VISTA near-infrared catalog with Spitzer IRAC mid-infrared photometry improves the situation of the background contamination considerably. We find that a (J − H) versus (K s − [4.5]) color-color diagram is well suited to tracing the population of YSO-candidates (cYSOs) by their infrared excess. We identify 8781 sources with strong infrared excess, which we consider as cYSOs. This sample is used to investigate the spatial distribution of the cYSOs with a nearest-neighbor analysis. The surface density distribution of cYSOs agrees well with the shape of the clouds as seen in our Herschel far-infrared survey. The strong decline in the surface density of excess sources outside the area of the clouds supports the hypothesis that our excess-selected sample consists predominantly of cYSOs with a low level of background contamination. This analysis allows us to identify 14 groups of cYSOs outside the central area.Our results suggest that the total population of cYSOs in the CNC comprises about 164 000 objects, with a substantial fraction (∼35%) located in the northern, still not well studied parts. Our cluster analysis suggests that roughly half of the cYSOs constitute a non-clustered, dispersed population.

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Section: Portion Of Cysos In Clusterssupporting

confidence: 92%

Section: Discussionmentioning

confidence: 99%

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The VISTA Carina Nebula Survey

Zeidler

Preibisch

Ratzka

et al. 2015

A&A

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“…1 presents this star cluster aggregate (hereafter Perseus 1 cluster aggregate) formed by ECs with similar ages. Such groups were predicted or observed by Efremov (1995); Guillout et al (1998);Fellhauer & Kroupa (2005); de la Fuente Marcos & de la Fuente Marcos (2008, 2009a, 2010Feigelson et al (2011);Camargo et al (2011Camargo et al ( , 2012Camargo et al ( , 2013Camargo et al ( , 2015a. Several large dust emission bubbles in WISE images connect these clusters, suggesting second generation effects (Camargo et al 2015a).…”

Section: Discussionmentioning

confidence: 60%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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In the present work we investigate the properties of 18 embedded clusters (ECs). The sample includes 11 previously known clusters and we report the discovery of 7 ECs on WISE images, thus complementing our recent list of 437 new clusters. The main goal is to use such clusters to shed new light on the Galactic structure by tracing the spiral arms with cluster distances. Our results favour a four-armed spiral pattern tracing three arms, Sagitarius-Carina, Perseus, and the Outer arm. The SagitariusCarina spiral arm is probed in the borderline of the third and fourth quadrants at a distance from the Galactic centre of d 1 ∼ 6.4 kpc adopting R ⊙ = 7.2 kpc, or d 2 ∼ 7.2 kpc for R ⊙ = 8.0 kpc. Most ECs in our sample are located in the Perseus arm that is traced in the second and third quadrants and appear to be at Galactocentric distances in the range d 1 = 9 − 10.5 kpc or d 2 = 9.8 − 11.3 kpc. Dolidze 25, Bochum 2, and Camargo 445 are located in the Outer arm that extends along the second and third Galactic quadrants with a distance from the Galactic centre in the range of d 1 = 12.5 − 14.5 kpc or d 2 = 13.5 − 15.5 kpc. We find further evidence that in the Galaxy ECs are predominantly located within the thin disc and along spiral arms. They are excellent tools for tracing these Galactic features and therefore new searches for ECs can contribute to a better understanding of the Galactic structure. We also report an EC aggregate located in the Perseus arm.

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“…Similar differences are found in Classical versus Weak T-Tauri stars ). However, this effect is minor when comparing entire populations (Kuhn et al 2015;Feigelson et al 2011) and cannot rule out the hypothesis of an universal X-ray luminosity function for PMS stars as proposed by Feigelson et al (2005).…”

Section: X-ray Luminositiesmentioning

confidence: 94%

First stars of theρOphiuchi dark cloud

Pillitteri

Wolk

Chen

et al. 2016

A&A

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Star formation in molecular clouds can be triggered by the dynamical action of winds from massive stars. Furthermore, X-ray and UV fluxes from massive stars can influence the life time of surrounding circumstellar disks. We present the results of a 53 ks XMMNewton observation centered on the ρ Ophiuchi A+B binary system. ρ Ophiuchi lies in the center of a ring of dust, likely formed by the action of its winds. This region is different from the dense core of the cloud (L1688 Core F) where star formation is at work. X-rays are detected from ρ Ophiuchi as well as a group of surrounding X-ray sources. We detected 89 X-ray sources, 47 of them have at least one counterpart in 2MASS+All-WISE catalogs. Based on IR and X-ray properties, we can distinguish between young stellar objects (YSOs) belonging to the cloud and background objects. Among the cloud members, we detect three debris-disk objects and 22 disk-less − Class III young stars. We show that these stars have ages in 5−10 Myr, and are significantly older than the YSOs in L1688. We speculate that they are the result of an early burst of star formation in the cloud. An X-ray energy of ≥5 × 10 44 erg has been injected into the surrounding medium over the past 5 Myr, we discuss the effects of such energy budget in relation to the cloud properties and dynamics.

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X-Ray Star Clusters in the Carina Complex

Cited by 79 publications

References 58 publications

The VISTA Carina Nebula Survey

The VISTA Carina Nebula Survey

Tracing the Galactic spiral structure with embedded clusters

First stars of theρOphiuchi dark cloud

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