Chandra X-ray Observations of the Young Stellar Cluster Berkeley 87 and its Oxygen-type Wolf-Rayet Star WR 142

Details Chandra X-ray Observations of the Young Stellar Cluster Berkeley 87 and its Oxygen-type Wolf-Rayet Star WR 142 Chandra X-ray Observations of the Young Stellar Cluster Berkeley 87 and its Oxygen-type Wolf-Rayet Star WR 142

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21547811s&link_type=abstract

American Astronomical Society, AAS Meeting #215, #478.11; Bulletin of the American Astronomical Society, Vol. 42, p.567

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Berkeley 87 is a heavily-reddened young open cluster lying in an obscured region of Cygnus. Age estimates for cluster members are typically in the range 1 - 3 Myr. Berkeley 87 is noteworthy as an example of a galactic open cluster harboring a rare oxygen-type Wolf-Rayet star, WR 142 (= Sand 5 = St 3; spectral type WO2). WO stars are the most highly-evolved WR stars and are likely supernova or gamma-ray burst (GRB) progenitors. The wind of WR 142 has a exceptionally high terminal speed in excess of 5000 km/s and may be producing shock waves in the surrounding cluster. We present results of a Chandra ACIS-I observation of Berkeley 87 centered on WR 142. The Chandra spectrum of WR 142 is exceptionally hard for a WR star, and shows excess low-energy absorption above that expected from its visual extinction. Some of this excess absorption likely arises in its powerful metal-rich wind. We compare its spectrum with the much softer X-ray spectra of cluster OB stars. We discuss the Chandra image of Berkeley 87, which reveals a large and diverse population of X-ray emitting young stars.

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