Star formation in the outer Galaxy: coronal properties of NGC 1893
Abstract
Context. The outer Galaxy, where the environmental conditions are different from the solar neighborhood, is a laboratory in which it is possible to investigate the dependence of star formation process on the environmental parameters. Aims. We investigate the X-ray properties of NGC 1893, a young cluster (~1–2 Myr) in the outer part of the Galaxy (galactic radius ≥11 kpc) where we expect differences in the disk evolution and in the mass distribution of the stars, to explore the X-ray emission of its members and compare it with that of young stars in star-forming regions near to the Sun. Methods. We analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, we derive X-ray luminosities and compare the respective properties of Class II and Class III members. We also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. Results. The X-ray luminosity of NGC 1893 X-ray members is in the range 10^(29.5)−10^(31.5) erg s^(-1). Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. We found that 34% of the 1021 lightcurves appear variable and that they show 0.16 flare per source, on average. Comparing our results with those relative to the Orion Nebula Cluster, we find that, by accounting for observational biases, the X-ray properties of NGC 1893 and the Orion ones are very similar. Conclusions. The X-ray properties in NGC 1893 are not affected by the environment and the stellar population in the outer Galaxy may have the same coronal properties of nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.
Additional Information
© 2012 ESO. Article published by EDP Sciences. Received 13 May 2011; Accepted 2 December 2011. This research made use of data obtained from the Chandra X-ray Observatory and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. We acknowledge financial contributions from ASI-INAF agreement I/009/10/0, from the European Commission (contract N. MRTN-CT-2006-035890) and PRIN-INAF (P.I. Lanza). S.J.W. is supported by NASA contract NAS8-03060 (Chandra). We thank the referee for helpful suggestions and comments that improved this work.Attached Files
Published - Caramazza2012p18474Astron_Astrophys.pdf
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Additional details
- Eprint ID
- 31882
- Resolver ID
- CaltechAUTHORS:20120612-133229601
- I/009/10/0
- Agenzia Spaziale Italiana (ASI)
- MRTN-CT-2006-035890
- Marie Curie Fellowship
- Istituto Nazionale di Astrofisica (INAF)
- NAS8-03060
- NASA
- Created
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2012-06-14Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field