A<i>WISE</i>CENSUS OF YOUNG STELLAR OBJECTS IN THE PERSEUS OB2 ASSOCIATION

Azimlu, Mohaddesseh; Martínez-Galarza, Juan Rafael; Muench, August

doi:10.1088/0004-6256/150/3/95

Cited by 28 publications

(39 citation statements)

References 30 publications

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“…We identified 17 and 14 MYSO candidates (L ≥ 10 3 L ) in W51 and W43, respectively, according to both the SED Fitting tool by Robitaille et al (2007) and the Bayesian method by Azimlu et al (2015). The clustered fraction of MYSOs are ∼94% and ∼79% in W51 and W43, respectively.…”

Section: 4mentioning

confidence: 99%

Young Stellar Objects in the Massive Star-forming Regions W51 and W43

Saral

Hora

Audard

et al. 2017

ApJ

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We present the results of our investigation of the star-forming complexes W51 and W43, two of the brightest in the first Galactic quadrant. In order to determine the young stellar object (YSO) populations in W51 and W43 we used color-magnitude relations based on Spitzer mid-infrared and 2MASS/UKIDSS near-infrared data. We identified 302 Class I YSOs and 1178 Class II/transition disk candidates in W51, and 917 Class I YSOs and 5187 Class II/transition disk candidates in W43. We also identified tens of groups of YSOs in both regions using the Minimal Spanning Tree (MST) method. We found similar cluster densities in both regions, even though Spitzer was not able to probe the densest part of W43. By using the Class II/I ratios, we traced the relative ages within the regions, and based on the morphology of the clusters, we argue that several sites of star formation are independent of one another in terms of their ages and physical conditions. We used spectral energy distribution-fitting to identify the massive YSO (MYSO) candidates since they play a vital role in the star formation process, and then examined them to see if they are related to any massive star formation tracers such as UCH II regions, masers, or dense fragments. We identified 17 MYSO candidates in W51, and 14 in W43, respectively, and found that groups of YSOs hosting MYSO candidates are positionally associated with H II regions in W51, though we do not see any MYSO candidates associated with previously identified massive dense fragments in W43.

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Section: 4mentioning

confidence: 99%

Young Stellar Objects in the Massive Star-forming Regions W51 and W43

Saral

Hora

Audard

et al. 2017

ApJ

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“…Orion A is approximately 400 pc away Schlafly et al (2014) and has a diameter of roughly 40 pc Da . Orion A has a large stellar density of 2 × 10 4 /pc 3 Palla & Stahler (1999 Küçük & Akkaya (2010) [3] Erickson et al (2011) [4] Azimlu et al (2015) stars. Using the published mass and ages of these stars ) that were obtained using the evolutionary model of Siess et al (2000), we plot the SFE in the ONC as a function of time in Figure 1(a) and find a power-law fit of t 2.31 .…”

Section: Superlinear Star Formation Efficiencymentioning

confidence: 99%

The accelerating pace of star formation

Caldwell

Chang

2017

Monthly Notices of the Royal Astronomical Society

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We study the temporal and spatial distribution of star formation rates in four wellstudied star-forming regions in local molecular clouds(MCs): Taurus, Perseus, ρ Ophiuchi, and Orion A. Using published mass and age estimates for young stellar objects in each system, we show that the rate of star formation over the last 10 Myrs has been accelerating and is (roughly) consistent with a t 2 power law. This is in line with previous studies of the star formation history of molecular clouds and with recent theoretical studies. We further study the clustering of star formation in the Orion Nebula Cluster(ONC). We examine the distribution of young stellar objects as a function of their age by computing an effective half-light radius for these young stars subdivided into age bins. We show that the distribution of young stellar objects is broadly consistent with the star formation being entirely localized within the central region. We also find a slow radial expansion of the newly formed stars at a velocity of v = 0.17 km s −1 , which is roughly the sound speed of the cold molecular gas. This strongly suggests the dense structures that form stars persist much longer than the local dynamical time. We argue that this structure is quasi-static in nature and is likely the result of the density profile approaching an attractor solution as suggested by recent analytic and numerical analysis.

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“…Simpson et al 2012;Azimlu, Martínez-Galarza & Muench 2015) but fits involving submillimetre data have tended to focus on more distant, massive YSOs (e.g. Mottram et al 2011;Faimali et al 2012).…”

Section: Model Sedsmentioning

confidence: 99%