A photometric and spectroscopic investigation of star formation in the very young open cluster NGC 6383

Rauw, Grégor; Manfroid, Jean; Becker, M. De

doi:10.1051/0004-6361/200912780

Cited by 6 publications

(18 citation statements)

References 35 publications

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“…IRAS sources embedded in clouds have also been reported by Sugitani & Ogura (1994) and Yamaguchi et al (1999): none of the SFO sources of Sugitani & Ogura (1994) are located in our Table 4): six objects, including one B-star and one F-star, have a clear emission in this line, i.e., a very small fraction of our sources. The lack of simultaneous Hα and X-ray emissions is not surprising and has been remarked on several times (e.g., NGC 6383, Rauw et al 2010): indeed, Hα traces the accreting gas, whereas strong X-ray emission is mostly a marker of coronal activity; weak-line TTs often show the latter but not the former, while classical TTs display the opposite behavior.…”

Section: Young Starsmentioning

confidence: 84%

X-ray properties of the young open clusters HM1 and IC 2944/2948

Nazé

Rauw

Sana

et al. 2013

A&A

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Using XMM-Newton data, we study for the first time the X-ray emission of HM1 and IC 2944/2948. Low-mass, pre-main-sequence objects with an age of a few Myr are detected, as well as a few background or foreground objects. Most massive stars in both clusters display the usual high-energy properties of that type of objects, though with log [L X /L BOL ] apparently lower in HM1 than in IC 2944/2948. Compared with studies of other clusters, it seems that a low signal-to-noise ratio at soft energies, due to the high extinction, may be the main cause of this difference. In HM1, the two Wolf-Rayet stars show contrasting behaviors: WR89 is extremely bright, but much softer than WR87. It remains to be seen whether wind-wind collisions or magnetically confined winds can explain these emissions. In IC 2944/2948, the X-ray sources concentrate around HD 101205; a group of massive stars to the north of this object is isolated, suggesting that there exist two subclusters in the field-of-view.

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Section: Young Starsmentioning

confidence: 84%

X-ray properties of the young open clusters HM1 and IC 2944/2948

Nazé

Rauw

Sana

et al. 2013

A&A

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“…The diffuse shell is resplendent with numerous bright pillars, and rims, which may be the site of current and future star formation. The region is dotted with small optically dark clouds, indicating regions of possibly higher extinction (Rauw et al 2010). Although approximately circular in shape, the HII region is not uniformly ionised.…”

Section: Sh 2-012 and The Central Cluster Ngc 6383mentioning

confidence: 98%

“…Most likely, the diffuse shell is ionised by the central star of NGC 6383, HD 159176. An O7 V binary, HD 159176, has an age of 2.3-2.8 Myr (Rauw et al 2010). The diffuse shell is resplendent with numerous bright pillars, and rims, which may be the site of current and future star formation.…”

Section: Sh 2-012 and The Central Cluster Ngc 6383mentioning

confidence: 99%

“…A significant number of stars identified as CTTS based on their photometric EWHα have kinematic properties statistically different from the mean of the population. These stars are very likely contaminant non-members that are found further in the spiral arm or located in front of the region (Rauw et al 2010), although a small fraction might be runaway or dynamically ejected stars that might be true members. However, we remain conservative in our choice and exclude all kinematic outliers as non-members.…”

Section: Removal Of Kinematic Outliersmentioning

confidence: 99%

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

Kalari

2019

Monthly Notices of the Royal Astronomical Society

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This paper presents optical (ugriHα)-infrared (JHKs,3.6-8.0µm) photometry, and Gaia astrometry of 55 Classical T-Tauri stars (CTTS) in the star-forming region Sh 2-012, and it's central cluster NGC 6383. The sample was identified based on photometric Hα emission line widths, and has a median age of 2.8±1.6 Myr, with a mass range between 0.3-1 M . 94% of CTTS with near-infrared cross-matches fall on the near-infrared T-Tauri locus, with all stars having mid-infrared photometry exhibiting evidence for accreting circumstellar discs. CTTS are found concentrated around the central cluster NGC 6383, and towards the bright rims located at the edges of Sh 2-012. Stars across the region have similar ages, suggestive of a single burst of star formation. Mass accretion rates (Ṁ acc ) estimated via Hα and u-band line intensities show a scatter (0.3 dex) similar to spectroscopic studies, indicating the suitability of Hα photometry to estimateṀ acc . Examining the variation ofṀ acc with stellar mass (M * ), we find a smaller intercept in theṀ acc -M * relation than oft-quoted in the literature, providing evidence to discriminate between competing theories of protoplanetary disc evolution.

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“…The Hα filter at WFI has a special passband, therefore it cannot be directly linked to any existing standard photometric system (see also Rauw et al 2010). By selecting ten stars observed with EMMI (see Sect.…”

Section: On the Basis Of Hα Emissionmentioning

confidence: 99%

Investigation of the stellar content in the western part of the Carina nebula

Kumar¹,

Sharma²,

Manfroid³

et al. 2014

A&A

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Context. The low obscuration and proximity of the Carina nebula make it an ideal place to study the ongoing star formation process and impact of massive stars on low-mass stars in their surroundings. Aims. To investigate this process, we generated a new catalog of the pre-main-sequence stars in the Carina west (CrW) region and studied their nature and spatial distribution. We also determined various parameters (reddening, reddening law, age, mass), which are used further to estimate the initial mass function and K-band luminosity function for the region under study. Methods. We obtained deep UBVRI Hα photometric data of the field situated to the west of the main Carina nebula and centered on WR 22. Medium-resolution optical spectroscopy of a subsample of X-ray selected objects along with archival data sets from Chandra, XMM-Newton and 2MASS surveys were used for the present study. Different sets of color-color and color-magnitude diagrams are used to determine reddening for the region and to identify young stellar objects (YSOs) and estimate their age and mass. Results. Our spectroscopic results indicate that the majority of the X-ray sources are late spectral type stars. The region shows a large amount of differential reddening with minimum and maximum values of E(B − V) as 0.25 and 1.1 mag, respectively. Our analysis reveals that the total-to-selective absorption ratio R V is ∼3.7 ± 0.1, suggesting an abnormal grain size in the observed region. We identified 467 YSOs and studied their characteristics. The ages and masses of the 241 optically identified YSOs range from ∼0.1 to 10 Myr and ∼0.3 to 4.8 M , respectively. However, the majority of them are younger than 1 Myr and have masses below 2 M . The high mass star WR 22 does not seem to have contributed to the formation of YSOs in the CrW region. The initial mass function slope, Γ, in this region is found to be −1.13 ± 0.20 in the mass range of 0.5 < M/M < 4.8. The K-band luminosity function slope (α) is also estimated as 0.31 ± 0.01. We also performed minimum spanning tree analysis of the YSOs in this region, which reveals that there are at least ten YSO cores associated with the molecular cloud, and that leads to an average core radius of 0.43 pc and a median branch length of 0.28 pc.

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A photometric and spectroscopic investigation of star formation in the very young open cluster NGC 6383

Cited by 6 publications

References 35 publications

X-ray properties of the young open clusters HM1 and IC 2944/2948

X-ray properties of the young open clusters HM1 and IC 2944/2948

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

Investigation of the stellar content in the western part of the Carina nebula

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