A New Estimate of the Hubble Time with Improved Modeling of Gravitational Lenses

Coles, Jonathan P.

doi:10.1086/587635

Cited by 59 publications

(72 citation statements)

References 33 publications

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“…After accounting for the difference in the gravitational potential traversed by the light path for each multiple image (Shapiro 1964), the time delay can be used to directly constrain the Hubble constant (Refsdal 1964) and other cosmological parameters  (Linder 2004(Linder , 2011Coe & Moustakas 2009). Distant quasars multiply-imaged by foreground galaxies have been used for such time delay cosmography measurements, providing valuable cosmological constraints that can complement or validate other methods such as Type Ia SNe, baryon acoustic oscillations and the cosmic microwave background (e.g., Saha et al 2006;Oguri 2007;Coles 2008;Suyu et al 2010Suyu et al , 2013Suyu et al , 2014; and see Treu & Ellis 2014 for a recent review). Figure 9.…”

Section: Future Measurements Of Sn Time Delaysmentioning

confidence: 99%

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Rodney

Strolger

Kelly

et al. 2016

ApJ

102

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We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) "Refsdal," a gravitationally lensed SN at z=1.488±0.001 with multiple images behind the galaxy cluster MACS J1149.6 +2223. The first four observed images of SN Refsdal (images S1-S4) exhibited a slow rise (over ∼150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4±4 (for S2), 2±5 (S3), and 24±7 days (S4). The measured magnification ratios relative to S1 are 1.15±0.05 (S2), 1.01±0.04 (S3), and 0.34±0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7±2 (S2), 0.6±3 (S3), and 27±8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17±0.02 (S2), 1.00±0.01 (S3), and 0.38±0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements-both for SN Refsdal and for other strongly lensed SNe yet to come.

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Section: Future Measurements Of Sn Time Delaysmentioning

confidence: 99%

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Rodney

Strolger

Kelly

et al. 2016

ApJ

102

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“…Despite the many tests and successes of this technique (e.g. Saha et al 2006a,b;Read et al 2007;Coles 2008;Leier 2009;Leier et al 2011), it is unclear whether the uniform prior on the ellipticity used to sample the parameter space is not biasing the average pixelated mass profile derived by this method. These results suggest that the dark matter and baryon distribution in the central regions (typically 5 kpc) of lens galaxies do have similar shapes 7 .…”

Section: Position Angle and Ellipticitymentioning

confidence: 99%

“…Recently, Suyu et al (2009Suyu et al ( , 2010 showed that a detailed study of the lensed quasar CLASS B1608+656, combining different high-resolution data and advanced lens modeling techniques, could lead to an estimate of H 0 with very small random and systematic uncertainties: H 0 = 70.6 ± 3.1 km s −1 Mpc −1 . The determination of H 0 based on a large sample of lensed quasars can also reach a precision competitive with the one of standard methods (Oguri 2007;Coles 2008). …”

Section: Introductionmentioning

confidence: 99%

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Sluse

Chantry

Magain

et al. 2012

A&A

121

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Gravitationally lensed quasars can be used as powerful cosmological and astrophysical probes. We can (i) infer the Hubble constant H 0 based on the so-called time-delay technique, (ii) unveil substructures along the line-of-sight toward distant galaxies, and (iii) compare the shape and the slope of baryons and dark matter distributions in the inner regions of galaxies. To reach these goals, we need highaccuracy astrometry of the quasar images relative to the lensing galaxy and morphology measurements of the lens. In this work, we first present new astrometry for 11 lenses with measured time delays, namely, JVAS B0218+357, SBS 0909+532, RX J0911.4+0551, FBQS J0951+2635, HE 1104-1805, PG 1115+080, JVAS B1422+231, SBS 1520+530, CLASS B1600+434, CLASS B1608+656, and HE 2149-2745. These measurements proceed from the use of the Magain-Courbin-Sohy (MCS) deconvolution algorithm applied in an iterative way (ISMCS) to near-IR HST images. We obtain a typical astrometric accuracy of about 1-2.5 mas and an accurate shape measurement of the lens galaxy. Second, we combined these measurements with those of 14 other lensing systems, mostly from the COSMOGRAIL set of targets, to present new mass models of these lenses. The modeling of these 25 gravitational lenses led to the following results: 1) in four double-image quasars (HE0047-1746, J1226-006, SBS 1520+530, and HE 2149-2745), we show that the influence of the lens environment on the time delay can easily be quantified and modeled, hence putting these lenses with high priority for time-delay determination; 2) for quadruple-image quasars, the difficulty often encountered in reproducing the image positions to milli-arcsec accuracy (astrometric anomaly problem) is overcome by explicitly including the nearest visible galaxy/satellite in the lens model. However, one anomalous system (RXS J1131-1231) does not show any luminous perturber in its vicinity, and three others (WFI 2026-4536, WFI 2033, and B2045+265) have problematic modeling. These four systems are the best candidates for a pertubation by a dark matter substructure along the line-of-sight; 3) we revisit the correlation between the position angle (PA) and ellipticity of the light and of the mass distribution in lensing galaxies. As in previous studies, we find a significant correlation between the PA of the light and of the mass distributions. However, in contrast with these same studies, we find that the ellipticity of the light and of the mass also correlate well, suggesting that the overall spatial distribution of matter is not very different from the baryon distribution in the inner ∼5 kpc of lensing galaxies. This offers a new test for high-resolution hydrodynamical simulations.

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“…The lensing magnification also makes strong lenses natural cosmic telescopes in resolving high-redshift sources. In addition, strong lens systems involving time-variant sources such as quasars measure the Hubble constant (Refsdal 1964), applications of gravitationally lensed quasars such as time delay cosmography (e.g., Coles 2008;Suyu et al 2010) can constrain the quasar luminosity function (Richards et al 2006) and dark energy (e.g. Kochanek 1996;Oguri et al 2012).…”

Section: Introductionmentioning

confidence: 99%

SDSS J1640+1932: a spectacular galaxy–quasar strong lens system

Wang

Shu

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present Canada-France-Hawaii Telescope (CFHT) MegaCam observations of a galaxy-quasar strong gravitational lens system, SDSS J1640+1932. This system, located at z=0.195 (foreground elliptical galaxy) and z=0.778 (background quasar), was first visually identified by us in the Sloan Digital Sky Survey (SDSS) database. Our CFHT imaging with an angular resolution of 0.7 ′′ clearly resolves 4 lensed images and a nearly complete Einstein ring. Modeling the system with a singular isothermal ellipsoid (SIE) total mass distribution, we find an Einstein radius of 2.49 ′′+0.063 −0.049 enclosing a inferred mass of 7.25 +0.37 −0.29 × 10 11 M ⊙ . The quasar and its host galaxy have been magnified by a factor of 23, and the time delay relative to the leading image is determined to be 23.4-25.2 days. These parameters vary minimally when our model is fitted to the g-, r-or i-band images.

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A New Estimate of the Hubble Time with Improved Modeling of Gravitational Lenses

Cited by 59 publications

References 33 publications

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

SDSS J1640+1932: a spectacular galaxy–quasar strong lens system

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