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DISSECTING THE GRAVITATIONAL LENS B1608+656. II. PRECISION MEASUREMENTS OF THE HUBBLE CONSTANT, SPATIAL CURVATURE, AND THE DARK ENERGY EQUATION OF STATE
Open accessAbstract
Strong gravitational lens systems with measured time delays between the multiple images provide a method for measuring the "time-delay distance" to the lens, and thus the Hubble constant. We present a Bayesian analysis of the strong gravitational lens system B1608+656, incorporating (1) new, deep Hubble Space Telescope ( HST ) observations, (2) a new velocity-dispersion measurement of 260 ± 15 km s −1 for the primary lens galaxy, and (3) an updated study of the lens' environment. Our analysis of the HST images takes into account the extended source surface brightness, and the dust extinction and optical emission by the interacting lens galaxies. When modeling the stellar dynamics of the primary lens galaxy, the lensing effect, and the environment of the lens, we explicitly include the total mass distribution profile logarithmic slope γ' and the external convergence κ ext ; we marginalize over these parameters, assigning well-motivated priors for them, and so turn the major systematic errors into statistical ones. The HST images provide one such prior, constraining the lens mass density profile logarithmic slope to be γ' = 2.08 ± 0.03; a combination of numerical simulations and photometric observations of the B1608+656 field provides an estimate of the prior for κ ext : 0.10 +0.08 −0.05 . This latter distribution dominates the final uncertainty on H 0 . Fixing the cosmological parameters at Ω m = 0.3, Ω Λ = 0.7, and w = −1 in order to compare with previous work on this system, we find H 0 = 70.6 +3.1 −3.1 km s −1 Mpc −1 . The new data provide an increase in precision of more than a factor of 2, even including the marginalization over κ ext . Relaxing the prior probability density function for the cosmological parameters to that derived from the Wilkinson Microwave Anisotropy Probe ( WMAP ) five-year data set, we find that the B1608+656 data set breaks the degeneracy between Ω m and Ω Λ at w = −1 and constrains the curvature parameter to be −0.031 < Ω k < 0.009 (95% CL), a level of precision comparable to that afforded by the current Type Ia SNe sample. Asserting a flat spatial geometry, we find that, in combination with WMAP , H 0 = 69.7 +4.9 −5.0 km s −1 Mpc −1 and w = −0.94 +0.17 −0.19 (68% CL), suggesting that the observations of B1608+656 constrain w as tightly as the current Baryon Acoustic Oscillation data do.
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“Time delays of galaxy-scale lensed quasars will allow one to measure Hubble ' s constant ( e.g., Suyu et al. 2010; Bonvin et al. 2017 ) in hundreds of systems; subpercentlevel precision in H ( z ) should be achievable ( Coe & Moustakas 2009; Treu & Marshall 2016 ) , providing a further independent dark energy probe.”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Suyu et al. 2010
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Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
Riess, A. G., Filippenko, A. V., Challis, P., Clocchiatti, A., Diercks, A., Garnavich, P. M., Gilliland, R. L., Hogan, C. J., Jha, S., Kirshner, R. P., et al. (1998) · The Astronomical Journal · doi:10.1086/300499 · Cited by 19,704
Measurements of Ω and Λ from 42 High‐Redshift Supernovae
Perlmutter, S., Aldering, G., Goldhaber, G., Knop, R. A., Nugent, P., Castro, P. G., Deustua, S., Fabbro, S., Goobar, A., Groom, D. E., et al. (1999) · The Astrophysical Journal · doi:10.1086/307221 · Cited by 18,062
Three‐Year Wilkinson Microwave Anisotropy Probe ( WMAP ) Observations: Implications for Cosmology
Spergel, D. N., Bean, R., Dore, O., Nolta, M. R., Bennett, C. L., Dunkley, J., Hinshaw, G., Jarosik, N., Komatsu, E., Page, L., et al. (2007) · The Astrophysical Journal Supplement Series · doi:10.1086/513700 · Cited by 6,778
FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION
Komatsu, E., Dunkley, J., Nolta, M. R., Bennett, C. L., Gold, B., Hinshaw, G., Jarosik, N., Larson, D., Limon, M., Page, L., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/180/2/330 · Cited by 5,786
Simulations of the formation, evolution and clustering of galaxies and quasars
Springel, V., White, S. D. M., Jenkins, A. R., Frenk, C. S., Yoshida, N., Gao, L., Navarro, J. F., Thacker, R. J., Croton, D., Helly, J. C., et al. (2005) · Nature · doi:10.1038/nature03597 · Cited by 5,060
Eisenstein, D. J., Zehavi, I., Hogg, D. W., Scoccimarro, R., Blanton, M. R., Nichol, R. C., Scranton, R., Seo, H., Tegmark, M., Zheng, Z., et al. (2005) · The Astrophysical Journal · doi:10.1086/466512 · Cited by 4,641
Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant
Freedman, W. L., Madore, B. F., Gibson, B. K., Ferrarese, L., Kelson, D. D., Sakai, S., Mould, J. R., Robert C. Kennicutt, Jr., Ford, H. C., Graham, J. A., et al. (2001) · The Astrophysical Journal · doi:10.1086/320638 · Cited by 3,543
Cosmological parameters from CMB and other data: A Monte Carlo approach
Lewis, A., & Bridle, S. (2002) · Physical Review D · doi:10.1103/physrevd.66.103511 · Cited by 3,495
An analytical model for spherical galaxies and bulges
Hernquist, L. (1990) · The Astrophysical Journal · doi:10.1086/168845 · Cited by 3,166
The Keck Low-Resolution Imaging Spectrometer
Oke, J. B., Cohen, J., Carr, M., Cromer, J. L., Dingizian, A., Harris, F. H., Labrecque, S., Lucinio, R., Schaal, W., Epps, H. W., et al. (1995) · Publications of the Astronomical Society of the Pacific · doi:10.1086/133562 · Cited by 2,100
Research works printed but not linked: 10
- Binney, 1987, Galactic dynamics, 747
- Fadely, 2009, ApJ
- Fassnacht, 2009, MNRAS
- Hu, 2005, Observing Dark Energy, 215
- MacKay, 2003, Information Theory, Inference and Learning Algorithms
- McKean, 2009, MNRAS
- Osipkov, 1979, Pis'ma Astron. Zh., 5, 77
- Schneider, 2006, Gravitational Lensing: Strong, Weak and Micro
- Sivia, 1996, Data Analysis: A Bayesian Tutorial
- Tammann, 1979, IAU Coll. 54, Scientific Research with the Space Telescope, 263
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SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
Komatsu, E., Smith, K. M., Dunkley, J., Bennett, C. L., Gold, B., Hinshaw, G., Jarosik, N., Larson, D., Nolta, M. R., Page, L., et al. (2011) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/192/2/18 · Cited by 8,802
“Using WMAP+BAO+H0, we find w = −1.10 ± 0.14 (68% CL), which improves to w = −1.08 ± 0.13 (68% CL) if we add the time-delay distance out to the lens system B1608+656 (Suyu et al. 2010, see Section 3.2.5).”
BackgroundInfluentialLSST: From Science Drivers to Reference Design and Anticipated Data Products
Ivezić, Ž., Kahn, S. M., Tyson, J. A., Abel, B., Acosta, E., Allsman, R., Alonso, D., AlSayyad, Y., Anderson, S. F., Andrew, J., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab042c · Cited by 4,357
“• Time delays of galaxy-scale lensed quasars will allow one to measure Hubble’s constant (e.g. Suyu et al. 2010) in hundreds or thousands of systems; subpercent level precision in H(z) should be achievable (Coe & Moustakas 2009), providing a further independent dark energy probe.”
BackgroundSelf-citationObservational probes of cosmic acceleration
Weinberg, D. H., Mortonson, M. J., Eisenstein, D. J., Hirata, C. M., Riess, A. G., & Rozo, E. (2013) · Physics Reports · doi:10.1016/j.physrep.2013.05.001 · Cited by 1,520
“In the best cases, distance scale constraints at the ∼ 5% level, after marginalizing over uncertainties in the mass distribution, are achievable for an individual lens (e.g., Suyu et al. 2010, 2012a).”
Wong, K., Suyu, S., Chen, G., Rusu, C., Millon, M., Sluse, D., Bonvin, V., Fassnacht, C., Taubenberger, S., Auger, M., et al. (2019) · Monthly notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3094 · Cited by 966
“Lens name D t (Mpc) Dd (Mpc) Blind analysis References B1608+656 5156+296−236 1228+177−151 No Suyu et al. (2010), Jee et al. (2019) RXJ1131−1231 2096+98−83 804+141−112 Yesa Suyu et al. (2014), Chen et al. (2019) HE 0435−1223 2707+183−168 —”
BackgroundMethodInfluentialSelf-citationChallenges for Λ CDM: An update
Perivolaropoulos, L., & Skara, F. (2022) · New Astronomy Reviews · doi:10.1016/j.newar.2022.101659 · Cited by 1,130
Metadata
- Authors
- Suyu, S. H., Marshall, P. J., Auger, M. W., Hilbert, S., Blandford, R. D., Koopmans, L. V. E., Fassnacht, C. D., & Treu, T.
- Affiliations
- University of Bonn (DE)
- University of California, Santa Barbara (US)
- Kavli Institute for Particle Astrophysics and Cosmology (US)
- University of Groningen (NL)
- University of California, Davis (US)
- Corresponding author
- Suyu, S. H.
- ORCID
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2010-02-10
- Volume
- 711
- Issue
- 1
- Pages
- 201-221
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2143112358
- Cited by
- 454
- References
- 80
- Citations by year
- 2026: 19 · 2025: 39 · 2024: 32 · 2023: 26 · 2022: 29 · 2021: 22 · 2020: 30 · 2019: 34 · 2018: 25 · 2017: 24 · 2016: 37 · 2015: 28 · 2014: 16 · 2013: 29 · 2012: 23
- FWCI
- 16.62
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- University of Groningen research database (University of Groningen / Centre for Information Technology) (submittedVersion, other-oa)
- arXiv (Cornell University)
- Funders
- National Science Foundation (0444059, 0642621, DE-AC02-76SF00515, CAREER, NAS 5-26555)
- U.S. Department of Energy (76SF00515, DE–AC02–76SF00515, AC02‐76SF00515, NAS 5-26555, DE-AC02-)
- National Aeronautics and Space Administration (NAS 526555, 526555)
- Alfred P. Sloan Foundation
- Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
- Deutsche Forschungsgemeinschaft (DE-AC02-76SF00515, NAS 5-26555)
- Nederlandse Organisatie voor Wetenschappelijk Onderzoek (10158)
- Science and Technology Facilities Council (ST/H00243X/1)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- strong gravitational lensing, Hubble constant, time-delay distance, dark energy equation of state, spatial curvature, lens mass profile, external convergence, velocity dispersion, interstellar extinction, cosmological parameter constraints, Bayesian analysis
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