<i>SPITZER</i>IMAGING OF THE NEARBY RICH YOUNG CLUSTER, Cep OB3b

Allen, Thomas S.; Gutermuth, Robert; Kryukova, E.; Megeath, S. Thomas; Pipher, J. L.; Naylor, T.; Jeffries, R. D.; Wolk, S. J.; Spitzbart, B.; Muzerolle, James

doi:10.1088/0004-637x/750/2/125

Cited by 51 publications

(85 citation statements)

References 50 publications

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“…The extremely high extinction at VV CrA B is likely local, and a result of its nature as an IRC, rather than an indicator of a large amount of undetected material dimming the VV CrA system as a whole. There is also ample evidence that young stars at apparently distinct evolutionary stages appear to have similar ages (e.g., Allen et al 2012); although statistically clusters with lower disk fractions appear older than those with high disk fractions (Hernández et al 2008), the particulars and timeline for circumstellar disk evolution and dissipation around individual stars are still not completely understood.…”

Section: Age Approximationmentioning

confidence: 99%

S and VV Corona Australis: Spectroscopic Variability in Two Young Binary Star Systems

Sullivan

Prato

Edwards

et al. 2019

ApJ

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We used high-resolution near-infrared spectroscopy from the NIRSPEC instrument on the Keck II telescope, taken over multiple epochs spanning five years, to examine two young binary T Tauri star systems, S Corona Australis and VV Corona Australis. The stars in these 1-2" separation systems have optically thick circumstellar disks and high extinctions at optical and near-infrared wavelengths. Using a combination of new and archival data, we have determined the spectral types of all the stars in these two systems for the first time, examined the variable NIR veiling, measured the emission line equivalent widths, and created spectral energy distributions. They have similar spectral types (K7-M1) and are at approximately the same evolutionary stage, allowing comparison of the four stars in the two systems. We conclude that S CrA and VV CrA are young binary systems of stars bridging the Class I and Class II evolutionary stages, characterized by high accretion luminosities and variable emission lines.

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Section: Age Approximationmentioning

confidence: 99%

S and VV Corona Australis: Spectroscopic Variability in Two Young Binary Star Systems

Sullivan

Prato

Edwards

et al. 2019

ApJ

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“…For SFiNCs, both crowding and nebulosity are greatly reduced and we believe that published catalogs of disky YSOs have sufficient high quality to provide the basis for constructing our catalogs. The catalogs for 12 of the 22 SFiNCs regions have been reduced in a consistent way by Gutermuth et al (2009), and most of the other regions have catalogs derived using similar consistent procedures by Megeath et al (2012) and Allen et al (2012). Nevertheless, most of these published Spitzer catalogs are limited to disky YSOs.…”

Section: Spitzer-irac Datamentioning

confidence: 99%

Star Formation In Nearby Clouds (SFiNCs): X-Ray and Infrared Source Catalogs and Membership

Getman

Broos

Kuhn

et al. 2017

ApJS

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The Star Formation in Nearby Clouds (SFiNCs) project is aimed at providing a detailed study of the young stellar populations and of star cluster formation in thenearby 22 star-forming regions (SFRs) for comparison with our earlier MYStIX survey of richer, more distant clusters. As a foundation for the SFiNCs science studies, here, homogeneous data analyses of the Chandra X-ray and Spitzer mid-infrared archival SFiNCs data are described, and the resulting catalogs of over 15,300 X-ray and over 1,630,000 mid-infrared point sources are presented. On the basis of their X-ray/infrared properties and spatial distributions, nearly 8500 point sources have been identified as probable young stellar members of the SFiNCs regions. Compared to the existing X-ray/mid-infrared publications, the SFiNCs member list increases the census of YSO members by 6%-200% for individual SFRs and by 40% for the merged sample of all 22 SFiNCs SFRs.

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“…This suggests that some external factor has accelerated the disc dissipation. Possible mechanisms include stellar winds from nearby O stars, like in the Sco-Cen association, or intense UV radiation, either from the star itself (if sufficiently massive), or, again, from nearby O stars as in Orion -although this process generally requires several million years (Allen et al 2012).…”

Section: Spatial Distributionmentioning

confidence: 99%

Spectroscopic characterization of X-ray emitting young stars associated with the Sh 2-296 nebula★

Fernandes

Gregorio-Hetem

Montmerle

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We studied a sample of stars associated with the Sh 2-296 nebula, part of the reflection nebulae complex in the region of Canis Major (CMa R1). Our sample corresponds to optical counterparts of X-ray sources detected from observations with the XMMNewton satellite, which revealed dozens of possible low-mass young stars not yet known in this region.A sample of 58 young star candidates were selected based on optical spectral features, mainly Hα and lithium lines, observed with multi-objects spectroscopy performed by the Gemini South telescope. Among the candidates, we find 41 confirmed T Tauri and 15 very likely young stars. Based on the Hα emission, the T Tauri stars were distinguished between classical (17%) and weak-lined (83%), but no significant difference was found in the age and mass distribution of these two classes.The characterization of the sample was complemented by near-and mid-infrared data, providing an estimate of ages and masses from the comparison with pre-mainsequence evolutionary models. While half of the young stars have an age of 1-2 Myrs or less, only a small fraction (∼ 25%) shows evidence of IR excess revealing the presence of circumstellar discs. This low fraction is quite rare compared to most young star-forming regions, suggesting that some external factor has accelerated the disc dissipation.

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SPITZERIMAGING OF THE NEARBY RICH YOUNG CLUSTER, Cep OB3b

Cited by 51 publications

References 50 publications

S and VV Corona Australis: Spectroscopic Variability in Two Young Binary Star Systems

S and VV Corona Australis: Spectroscopic Variability in Two Young Binary Star Systems

Star Formation In Nearby Clouds (SFiNCs): X-Ray and Infrared Source Catalogs and Membership

Spectroscopic characterization of X-ray emitting young stars associated with the Sh 2-296 nebula★

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