期刊
ASTROPHYSICAL JOURNAL
卷 764, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/764/2/186
关键词
galaxies: clusters: general; gravitational lensing: strong; quasars: individual (SDSS J102913.94+262317.9)
资金
- Smithsonian Astrophysical Observatory
- NSF [AST-1009756]
- FIRST program Subaru Measurements of Images and Redshifts (SuMIRe)
- World Premier International Research Center Initiative (WPI Initiative)
- MEXT, Japan
- JSPS [23740161]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009756] Funding Source: National Science Foundation
- Grants-in-Aid for Scientific Research [23740161] Funding Source: KAKEN
We present 279 epochs of optical monitoring data spanning 5.4 years from 2007 January to 2012 June for the largest image separation (22.'' 6) gravitationally lensed quasar, SDSS J1029+2623. We find that image A leads the images B and C by Delta t(AB) = (744 +/- 10) days (90% confidence); the uncertainty includes both statistical uncertainties and systematic differences due to the choice of models. With only a similar to 1% fractional error, the interpretation of the delay is limited primarily by cosmic variance due to fluctuations in the mean line-of-sight density. We cannot separate the fainter image C from image B, but since image C trails image B by only 2-3 days in all models, the estimate of the time delay between images A and B is little affected by combining the fluxes of images B and C. There is weak evidence for a low level of microlensing, perhaps created by the small galaxy responsible for the flux ratio anomaly in this system. Interpreting the delay depends on better constraining the shape of the gravitational potential using the lensed host galaxy, other lensed arcs, and the structure of the X-ray emission.
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