<i>Chandra </i>X-ray observation of the young stellar cluster NGC 3293  in the Carina Nebula Complex

Preibisch, Thomas; Flaischlen, S.; Gaczkowski, B.; Townsley, Leisa K.; Broos, P. S.

doi:10.1051/0004-6361/201730874

Cited by 14 publications

(28 citation statements)

References 55 publications

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“…In contrast, X-rays can identify pre-main-sequence stars both with and without disks (Feigelson & Montmerle 1999;Feigelson 2018). Low-mass pre-main-sequence stars maintain high X-ray emission even after 10 Myr (e.g., Argiroffi et al 2016;Preibisch et al 2017), so X-ray selection should detect such a population if it exists.…”

Section: Appendix B Selection Effects Related To Stellar Agesmentioning

confidence: 99%

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

Kuhn

Hillenbrand

Carpenter

et al. 2020

ApJ

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We examine the clustering and kinematics of young stellar objects (YSOs) in the North America/Pelican Nebulae, as revealed by Gaia astrometry, in relation to the structure and motions of the molecular gas, as indicated in molecular-line maps. The Gaia parallaxes and proper motions allow us to significantly refine previously published lists of YSOs, demonstrating that many of the objects previously thought to form a distributed population turn out to be nonmembers. The members are subdivided into at least six spatio-kinematic groups, each of which is associated with its own molecular cloud component or components. Three of the groups are expanding, with velocity gradients of 0.3-0.5 km s −1 pc −1 , up to maximum velocities of ∼8 km s −1 away from the groups' centers. The two known O-type stars associated with the region, 2MASSJ20555125+4352246 and HD199579, are rapidly escaping one of these groups, following the same position-velocity relation as the low-mass stars. We calculate that a combination of gas expulsion and tidal forces from the clumpy distribution of molecular gas could impart the observed velocity gradients within the groups. However, on a global scale, the relative motions of the groups do not appear either divergent or convergent. The velocity dispersion of the whole system is consistent with the kinetic energy gained due to gravitational collapse of the complex. Most of the stellar population has ages similar to the freefall timescales for the natal clouds. Thus, we suggest the nearly freefall collapse of a turbulent molecular cloud as the most likely scenario for star formation in this complex.

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Section: Appendix B Selection Effects Related To Stellar Agesmentioning

confidence: 99%

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

Kuhn

Hillenbrand

Carpenter

et al. 2020

ApJ

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“…In contrast, X-rays can identify pre-mainsequence stars both with and without disks (Feigelson & Montmerle 1999;Feigelson 2018). Low-mass pre-mainsequence stars maintain high X-ray emission even after 10 Myr (e.g., Argiroffi et al 2016;Preibisch et al 2017), so X-ray selection should detect such a population if it exists.…”

Section: Star-formation Scenariosmentioning

confidence: 99%

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

Kuhn,

Hillenbrand,

Carpenter

et al. 2020

Preprint

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We examine the clustering and kinematics of young stellar objects (YSOs) in the North America/Pelican Nebulae, as revealed by Gaia astrometry, in relation to the structure and motions of the molecular gas, as indicated in molecular line maps. The Gaia parallaxes and proper motions allow us to significantly refine previously published lists of YSOs, demonstrating that many of the objects previously thought to form a distributed population turn out to be non-members. The members are subdivided into at least 6 spatio-kinematic groups, each of which is associated with its own molecular cloud component or components. Three of the groups are expanding, with velocity gradients of 0.3-0.5 km s −1 pc −1 , up to maximum velocities of ∼8 km s −1 away from the groups' centers. The two known O-type stars associated with the region, 2MASS J20555125+4352246 and HD 199579, are rapidly escaping one of these groups, following the same position-velocity relation as the low-mass stars. We calculate that a combination of gas expulsion and tidal forces from the clumpy distribution of molecular gas could impart the observed velocity gradients within the groups. However, on a global scale, the relative motions of the groups do not appear either divergent or convergent. The velocity dispersion of the whole system is consistent with the kinetic energy gained due to gravitational collapse of the complex. Most of the stellar population has ages similar to the free-fall timescales for the natal clouds. Thus, we suggest the nearly free-fall collapse of a turbulent molecular cloud as the most likely scenario for star formation in this complex.1. INTRODUCTION The way that stars and gas are distributed in a starforming region can provide useful constraints on the conditions in which the stars were formed (e.g., Elmegreen 2002;Parker et al. 2014;Gouliermis 2018;Feigelson 2018). For the nearest star-forming regions, astrometric measurements by ESA's Gaia spacecraft (Gaia Collaboration et al. 2016) can provide a multi-dimensional picture of how the young stars are clustered. Spatial and kinematic clustering has already been examined in several of the major star-forming regions within 1 kpc,

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“…Hence, X-ray surveys of star forming regions are used to uncover YSO populations. Particularly, for the detection of disk anemic YSOs, i.e., Class III sources, X-ray observations complement the YSO sources obtained from IR observations and a better census of the low-mass stellar content of clusters can be achieved (e.g., Preibisch & Feigelson 2005;Feigelson et al 2013;Broos et al 2013;Pandey et al 2013aPandey et al , 2014Preibisch et al 2017). Recently, Getman et al (2017) carried out the Star Formation in Nearby Clouds (SFiNCs) project to provide detailed studies of the young stellar populations and star cluster formation in nearby star forming regions (SFRs) including Be 59.…”

Section: Ysos From Infra-red and X-ray Observationsmentioning

confidence: 99%

Young Cluster Berkeley 59: Properties, Evolution, and Star Formation

Panwar

Pandey

Samal

et al. 2018

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Berkeley 59 is a nearby (∼1 kpc) young cluster associated with the Sh2-171 Hii region. We present deep optical observations of the central ∼ 2.5 × 2.5 pc 2 area of the cluster, obtained with the 3.58-m Telescopio Nazionale Galileo. The V /(V -I) color-magnitude diagram manifests a clear pre-mainsequence (PMS) population down to ∼ 0.2 M . Using the near-infrared and optical colors of the low-mass PMS members we derive a global extinction of A V = 4 mag and a mean age of ∼ 1.8 Myr, respectively, for the cluster. We constructed the initial mass function and found that its global slopes in the mass ranges of 0.2 -28 M and 0.2 -1.5 M are -1.33 and -1.23, respectively, in good agreement with the Salpeter value in the solar neighborhood. We looked for the radial variation of the mass function and found that the slope is flatter in the inner region than in the outer region, indicating mass segregation. The dynamical status of the cluster suggests that the mass segregation is likely primordial. The age distribution of the PMS sources reveals that the younger sources appear to concentrate close to the inner region compared to the outer region of the cluster, a phenomenon possibly linked to the time evolution of star-forming clouds is discussed. Within the observed area, we derive a total mass of ∼10 3 M for the cluster. Comparing the properties of Berkeley 59 with other young clusters, we suggest it resembles more to the Trapezium cluster.

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Chandra X-ray observation of the young stellar cluster NGC 3293 in the Carina Nebula Complex

Cited by 14 publications

References 55 publications

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

The Formation of a Stellar Association in the NGC 7000/IC 5070 Complex: Results from Kinematic Analysis of Stars and Gas

Young Cluster Berkeley 59: Properties, Evolution, and Star Formation

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