@article{TownsleyBroosCorcoranetal.2011,
  author    = {Townsley, Leisa K. and Broos, Patrick S. and Corcoran, Michael F. and Feigelson, Eric D. and Gagne, Marc and Montmerle, Thierry and Oey, M. S. and Smith, Nathan and Garmire, Gordon P. and Getman, Konstantin V. and Povich, Matthew S. and Evans, Nancy Remage and Naze, Yael and Parkin, E. R. and Preibisch, Thomas and Wang, Junfeng and Wou, Scott J. and Chu, You-Hua and Cohen, David H. and Gruendl, Robert A. and Hamaguchi, Kenji and King, Robert R. and Mac Low, Mordecai-Mark and McCaughrean, Mark J. and Moffat, Anthony F. J. and Oskinova, Lida and Pittard, Julian M. and Stassun, Keivan G. and Ud-Doula, Asif and Walborn, Nolan R. and Waldron, Wayne L. and Churchwell, Ed and Nictiols, J. S. and Owocki, Stanley P. and Schulz, Norbert S.},
  title     = {An introduction to the chandra carina complex project},
  series = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Supplement series},
  volume    = {194},
  journal   = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Supplement series},
  number    = {1},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0067-0049},
  doi       = {10.1088/0067-0049/194/1/1},
  pages     = {28},
  year      = {2011},
  abstract  = {The Great Nebula in Carina provides an exceptional view into the violent massive star formation and feedback that typifies giant H II regions and starburst galaxies. We have mapped the Carina star-forming complex in X-rays, using archival Chandra data and a mosaic of 20 new 60 ks pointings using the Chandra X-ray Observatory's Advanced CCD Imaging Spectrometer, as a testbed for understanding recent and ongoing star formation and to probe Carina's regions of bright diffuse X-ray emission. This study has yielded a catalog of properties of > 14,000 X-ray point sources;> 9800 of them have multiwavelength counterparts. Using Chandra's unsurpassed X-ray spatial resolution, we have separated these point sources from the extensive, spatially-complex diffuse emission that pervades the region; X-ray properties of this diffuse emission suggest that it traces feedback from Carina's massive stars. In this introductory paper, we motivate the survey design, describe the Chandra observations, and present some simple results, providing a foundation for the 15 papers that follow in this special issue and that present detailed catalogs, methods, and science results.},
  language  = {en}
}
@article{JaniakScharmannGreenetal.1996,
  author    = {Janiak, Chr. and Scharmann, T. G. and Green, J. C. and Parkin, R. P. G. and Kolm, M. J. and Riedel, E. and Mickler, Wulfhard and Elguero, J. and Claramunt, R. M. and Sanz, D.},
  title     = {Effects of nitrogen substitution in Poly(pyrazolyl)borato Ligands : from orbital energy levels to C-H...O Hydrogen Bonding},
  year      = {1996},
  language  = {en}
}
@article{ParkinBroosTownsleyetal.2011,
  author    = {Parkin, E. R. and Broos, Patrick S. and Townsley, L. K. and Pittard, J. M. and Moffat, Anthony F. J. and Naze, Y. and Rauw, G. and Oskinova, Lida and Waldron, W. L.},
  title     = {X-RAY EMISSION FROM THE DOUBLE-BINARY OB-STAR SYSTEM QZ CAR (HD 93206)},
  series = {ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES},
  volume    = {194},
  journal   = {ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES},
  number    = {1},
  publisher = {IOP PUBLISHING LTD},
  address   = {BRISTOL},
  issn      = {0067-0049},
  doi       = {10.1088/0067-0049/194/1/8},
  pages     = {11},
  year      = {2011},
  abstract  = {X-ray observations of the double-binary OB-star system QZ Car (HD 93206) obtained with the Chandra X-ray Observatory over a period of roughly 2 years are presented. The respective orbits of systems A (O9.7 I+b2 v, P-A = 21 days) and B (O8 III+o9 v, P-B = 6 days) are reasonably well sampled by the observations, allowing the origin of the X-ray emission to be examined in detail. The X-ray spectra can be well fitted by an attenuated three-temperature thermal plasma model, characterized by cool, moderate, and hot plasma components at kT similar or equal to 0.2, 0.7, and 2 keV, respectively, and a circumstellar absorption of similar or equal to 0.2 x 10(22) cm(-2). Although the hot plasma component could be indicating the presence of wind-wind collision shocks in the system, the model fluxes calculated from spectral fits, with an average value of similar or equal to 7x10(-13) erg s(-1) cm(-2), do not show a clear correlation with the orbits of the two constituent binaries. A semi-analytical model of QZ Car reveals that a stable momentum balance may not be established in either system A or B. Yet, despite this, system B is expected to produce an observed X-ray flux well in excess of the observations. If one considers the wind of the O8 III star to be disrupted by mass transfer, the model and observations are in far better agreement, which lends support to the previous suggestion of mass transfer in the O8 III+o9 v binary. We conclude that the X-ray emission from QZ Car can be reasonably well accounted for by a combination of contributions mainly from the single stars and the mutual wind-wind collision between systems A and B.},
  language  = {en}
}