The Hubble Time Inferred from 10 Time Delay Lenses

Saha, Prasenjit; Coles, Jonathan P.; Macciò, Andrea V.; Williams, Liliya L. R.

doi:10.1086/507583

Cited by 90 publications

(121 citation statements)

References 38 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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“…Simultaneous modeling has been done in the past by e.g. Saha et al (2006) -with 10 lenses and Coles (2008) -with 11 lenses. Figure 22 shows the result of the simultaneous modeling of 5 systems with time delays obtained at the NOT.…”

Section: Simultanous Modelingmentioning

confidence: 99%

Results of optical monitoring of 5 SDSS double QSOs with the Nordic Optical Telescope

Paraficz¹,

Hjorth²,

Elíasdóttir

2009

A&A

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We present optical R-band light curves of five SDSS double QSOs (SDSS J0903+5028, SDSS J1001+5027, SDSS J1206+4332, SDSS J1353+1138, SDSS J1335+0118) obtained from monitoring at the Nordic Optical Telescope (NOT) between September 2005 and September 2007. We also present analytical and pixelated modeling of the observed systems. For SDSS J1206+4332, we measured the time delay to be Δτ = 116 +4 −5 days, which, for a singular isothermal ellipsoid model, corresponds to a Hubble constant of 73 +3 −4 km s −1 Mpc −1 . Simultaneous pixelated modeling of five other systems for which a time delay has now been previously measured at the NOT leads to H 0 = 61.5 +8 −4 km s −1 Mpc −1 . Finally, by comparing light curves of the two images of each system, suitably shifted by the predicted or observed time-delays, we found no evidence of microlensing variability over the course of the monitoring period.

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“…The important point about equation (2) is its dependence on a 2 , leading to a standard deviation (a) $ . This zeroth-order contribution to , although large, has no observational consequence because it depicts a coherent delay (2a) ¼ 2 (a) which, as is explained in x 2 (see also Bar-Kana 1996;Seljak 1994), simply causes a global absolute shift in the angular positions of images without changing relative positions. The next-order contribution to (a) would come from the second integral in equation (1), i.e., (a) $ a 2 .…”

Section: Introduction: Time Delay Anisotropy From Primordial Matter Dmentioning

confidence: 95%

“…Now the objective of this paper is to investigate whether time delay measurements can probe the mass distribution in the near (z P 1) universe where nonlinear matter clumping is important, because similar considerations in the context of primordial matter that fills the high-redshift universe have already been made, with the conclusion that such forms of matter cause negligible additional delays (Surpi et al 1996;Bar-Kana 1996;Seljak 1994). One could persist with the approach of equation (1) by adopting a modified primordial matter spectrum P(k) that includes an ''extension'' to the nonlinear, or large-k, regime ( Peacock & Dodds 1994;Smith et al 2003), except that concerning the effect of widely spaced and compact clumps on two closely separated light rays it actually makes more sense to calculate directly the time delay induced by the gravitational perturbation of a random ensemble of clumps.…”

Section: Time Delay Anisotropy From a Statistical Ensemble Of Galaxiesmentioning

confidence: 99%

Strong‐Lensing Time Delay: A New Way of Measuring Cosmic Shear

Lieu

2008

ApJ

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The phenomenon of cosmic shear, or distortion of images of distant sources unaccompanied by magnification, is an effective way of probing the content and state of the foreground universe, because light rays do not have to pass through matter clumps in order to be sheared. It is shown that the delay in the arrival times between two simultaneously emitted photons that appear to be arriving from a pair of images of a strongly lensed cosmological source contains not only information about the Hubble constant, but also the long-range gravitational effect of galactic-scale mass clumps located away from the light paths in question. This is therefore also a method of detecting shear. Data on time delays among a sample of strongly lensed sources can provide crucial information about whether extra dynamics beyond gravity and dark energy are responsible for the global flatness of space. If the standard ÃCDM model is correct, there should be a large dispersion in the value of H 0 as inferred from the delay data by (the usual procedure of ) ignoring the shear from all other mass clumps except the strong lens itself. The fact that there has not been any report of a significant deviation from the h ¼ 0:7 mark during any of the H 0 determinations by this technique may already be pointing to the absence of the random effect discussed here.

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The Hubble Time Inferred from 10 Time Delay Lenses

Cited by 90 publications

References 38 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

Results of optical monitoring of 5 SDSS double QSOs with the Nordic Optical Telescope

Strong‐Lensing Time Delay: A New Way of Measuring Cosmic Shear

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