A Refined QSO Selection Method Using Diagnostics Tests: 663 QSO Candidates in the LMC
arXiv:1110.5632 · doi:10.1088/0004-637X/747/2/107
Abstract
We present 663 QSO candidates in the Large Magellanic Cloud (LMC) selected using multiple diagnostics. We started with a set of 2,566 QSO candidates from our previous work selected using time variability of the MACHO LMC lightcurves. We then obtained additional information for the candidates by crossmatching them with the Spitzer SAGE, the MACHO UBVI, the 2MASS, the Chandra and the XMM catalogs. Using this information, we specified six diagnostic features based on mid-IR colors, photometric redshifts using SED template fitting, and X-ray luminosities in order to further discriminate high confidence QSO candidates in the absence of spectra information. We then trained a one-class SVM (Support Vector Machine) model using the diagnostics features of the confirmed 58 MACHO QSOs. We applied the trained model to the original candidates and finally selected 663 high confidence QSO candidates. Furthermore, we crossmatched these 663 QSO candidates with the newly confirmed 144 QSOs and 275 non-QSOs in the LMC fields. On the basis of the counterpart analysis, we found that the false positive rate is less than 1%.
13 pages, 17 figures. accepted for publication in ApJ
References in corpus (7)
- Modeling the Time Variability of SDSS Stripe 82 Quasars as a Damped Random Walk
- The XMM-Newton Serendipitous Survey. V. The Second XMM-Newton Serendipitous Source Catalogue
- Photometric redshifts in the SWIRE Survey
- QSO Selection Algorithm Using Time Variability and Machine Learning: Selection of 1,620 QSO Candidates from MACHO LMC Database
- Discovery of 5000 Active Galactic Nuclei behind the Magellanic Clouds
- Constraining Warm Dark Matter using QSO gravitational lensing
- The Magellanic Quasars Survey. II. Confirmation of 144 New Active Galactic Nuclei Behind the Southern Edge of the Large Magellanic Cloud
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- A Deep Chandra Observation of the Giant HII Region N11 I. X-ray Sources in the Field
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