Other
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21347001r&link_type=abstract
American Astronomical Society, AAS Meeting #213, #470.01; Bulletin of the American Astronomical Society, Vol. 41, p.420
Other
Scientific paper
The ChaMPlane Survey is designed to identify the many serendipitous X-ray sources detected in Galactic Plane fields to investigate the spatial distribution of accretion-powered X-ray sources within the Galaxy. Archival Chandra images are combined with deep NOAO 4m Mosaic photometry to generate lists of likely targets, for which spectra are then acquired at WIYN and CTIO. We report results of WIYN/Hydra multi-object spectroscopy for Chandra and Hα-excess targets in 22 northern ChaMPlane fields. Our spectrograph setup covers 4000 Å -- 6800 Å, with resolution of 2.8 Å (FWHM). We generally cover 60 objects per setup, with 1-3 setups per field. Spectroscopic identification of targeted objects is >90% complete to a magnitude of R=21, with reasonable success identifying sources down to R=22.5. Classified objects include 12 Hα-selected cataclysmic variables (CVs), 4 Be stars, over 670 M stars (about half of which have clear Hα emission), and 31 active galactic nuclei of redshift 0.02--4.25. The apparent CVs have R magnitudes ranging from 14.8 to 21.7, and typically show Hα, Hβ, and He I lines. A few CVs also show the He II 4686 Å line and/or M-star secondary profiles. Clear rotational splitting is seen in several CVs as well. Three other objects might be CVs, including one X-ray source, but the spectra are not conclusive.
We discuss trends seen in this sample of ChaMPlane objects, and examine the implications of our CV detections for the space density of CVs within the context of a model of expected CV detections. The model uses Monte-Carlo techniques to create and sample an exponential-disk CV distribution. Detection is set by limiting magnitude, computed using a model for CV absolute magnitude distribution, a gas/dust model for the disk, and heliocentric distance.
This work is supported in part by NSF grant AST-0098683 and NASA/Chandra grants AR1-2001X, AR2-3002B, AR3-4002B, and AR4-5003B.
Cohn Haldan N.
Grindlay Jonathon E.
Lugger Phyllis Minnie
Rogel Allen B.
van den Berg Maureen
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