Pre-main sequence stars, emission stars and recent star formation in the Cygnus region

Bhavya, B. ; Mathew, Blesson ; Subramaniam, Annapurni (2007) Pre-main sequence stars, emission stars and recent star formation in the Cygnus region Bulletin of the Astronomical Society of India, 35 (3). pp. 383-411. ISSN 0304-9523

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The recent star formation history in the Cygnus region is studied using 5 clusters (IC 4996, NGC 6910, Berkeley 87, Biurakan 2 and Berkeley 86). The optical data from the literature are combined with the 2MASS data to identify the pre-main sequence (pre-MS) stars as stars with near IR excess. We identified 93 pre-MS stars and 9 stars with Hα emission spectra. The identified pre-MS stars are used to estimate the turn-on age of the clusters. The duration of star formation was estimated as the difference between the turn-on and the turn-off age. We find that, NGC 6910 and IC 4996 have been forming stars continuously for the last 6 – 7 Myr, Berkeley 86 and Biurakan 2 for 5 Myr and Berkeley 87 for the last 2 Myr. This indicates that the Cygnus region has been actively forming stars for the last 7 Myr, depending on the location. Nine emission line stars were identified in 4 clusters, using slit-less spectra (Be 87 - 4 stars; Be 86 - 2 stars, NGC 6910 - 2 stars and IC 4996 - 1 star). The individual spectra were obtained and analysed to estimate stellar as well as disk properties. All the emission stars are in the MS, well below the turn-off, in the core hydrogen burning phase. These stars are likely to be Classical Be (CBe)stars. Thus CBe phenomenon can be found in very young MS stars which are just a few (2–7) Myr old. This is an indication that CBe phenomenon need not be an evolutionary effect.

Item Type:Article
Source:Copyright of this article belongs to Astronomical Society of India.
Keywords:Stars : Emission-Line, Be; Pre-main Sequence – Stars : Formation – (Stars): Circumstellar Matter – (Galaxy): Open Clusters and Association
ID Code:106638
Deposited On:01 Feb 2018 12:01
Last Modified:01 Feb 2018 12:01

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