Classical T-Tauri stars with VPHAS+: II: NGC 6383 in Sh 2-012★

Kalari, V.

doi:10.1093/mnras/stz250

Cited by 9 publications

(5 citation statements)

References 51 publications

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“…While X-ray observations require space missions (e.g., Chandra or XMM-Newton), the optical and NIR observations can also be obtained from the ground, and with extreme AO even at similar spatial resolutions as HST provides. Combining these broad-band observations with narrow-band observations such as the Hα or Paβ filter allows to detect pre-main sequence stars with active mass accretion (e.g., De Marchi et al 2011;Beccari et al 2015;Zeidler et al 2016a;Kalari 2019) revealing protoplanetary disks. NUV and FUV photometry and spectroscopy from space is necessary to study and classify the most massive OB-stars.…”

Section: Observing Young Star-forming Regionsmentioning

confidence: 99%

Star Clusters Near and Far

et al. 2020

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Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e. detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.

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Section: Observing Young Star-forming Regionsmentioning

confidence: 99%

Star Clusters Near and Far

et al. 2020

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“…The equivalent width (EW Hα ) of each star was calculated by means of the code 5 of Kalari (2019). Following De Marchi et al (2010), the author defined EW Hα as:…”

Section: Vphas Photometrymentioning

confidence: 99%

A CCD Search for Variable Stars in the Open Cluster NGC 6611

Michalska,

Kołaczkowski,

Leiton

et al. 2023

Preprint

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We present the results of the U BV I C variability survey in the young open cluster NGC 6611 based on observations obtained during 34 nights spanning one year. In total, we found 95 variable stars. Most of these stars are classified as periodic and irregular pre-main sequence (PMS) stars. The analysis of the JHK S 2MASS photometry and fourcolour IRAC photometry revealed 165 Class II young stellar sources, 20 of which are irregular variables and one is an eclipsing binary. These classifications, complemented by JHK UKIDSS photometry and riHα VPHAS photometry, were used to identify 24 candidates for classical T Tauri stars and 30 weak-lined T Tauri stars. In addition to the PMS variables, we discovered eight δ Scuti candidates. None of these were previously known. Furthermore, we detected 17 eclipsing binaries where two were previously known. Based on the proper motions provided by the Gaia EDR3 catalogue, we calculated the cluster membership probabilities for 91 variable stars. For 61 variables, a probability higher than 80% was determined, which makes them cluster members. Only 25 variables with a probability less than 20% were regarded to be non-members.

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“…It is through this excess Hα emission that accreting young PMS stars can be readily identified. in Kalari (2019) for VPHAS+ photometry to estimate the Hα equivalent width of all VPHAS+ sources, adopting the average absolute visual extinction value (A V ) of 1.3 mag from Rho et al (2008).…”

Section: Pre-main Sequence Starsmentioning

confidence: 99%

The Young Stellar Population, Distance, and Cloud-Cloud Collision Induced Star Formation Scenario of the Trifid Nebula

Kalari

2021

Preprint

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The Trifid Nebula is a young, nearby star-forming region where star formation is proposed to have been triggered by cloud-cloud collision (CCC), based on observations of molecular clouds. It offers a unique opportunity to test whether the CCC hypothesis is supported by the spatial distribution and star formation chronology of young stars.We present the first study of the optically visible pre-main sequence (PMS) population of the region using riHα imaging and Gaia astrometry. Combined with an analysis of young stellar objects (YSOs) using infrared imaging, we capture the spatial distribution and star formation chronology of the young stellar population. From the analysis, 15 Flat/Class I YSOs, 46 Class II YSOs, and 41 accreting PMS stars are identified (diskless/non-accreting sources are not included in the analysis). The distance based on Gaia parallaxes is ∼1250 pc, significantly closer than previously reported. The Class II YSOs and PMS stars (∼1.5 Myr old) are spread toward the edge of the molecular clouds. They are slightly younger than the estimated crossing time of ∼2.7 Myr and closer to the estimated dynamical age ∼0.85 Myr. Younger Class I YSOs are more concentrated spatially. There exists a cavity devoid of young stars where the two clouds overlap. This evidence suggests that the current generation of stars formed after the collision of two clouds ∼1 Myr ago, and this result can be corroborated using future spectroscopic studies.

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Classical T-Tauri stars with VPHAS+: II: NGC 6383 in Sh 2-012★

Cited by 9 publications

References 51 publications

Star Clusters Near and Far

Star Clusters Near and Far

A CCD Search for Variable Stars in the Open Cluster NGC 6611

The Young Stellar Population, Distance, and Cloud-Cloud Collision Induced Star Formation Scenario of the Trifid Nebula

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