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dc.contributor.authorBirrer, S
dc.contributor.authorDhawan, S
dc.contributor.authorShajib, AJ
dc.date.accessioned2022-01-10T12:46:21Z
dc.date.available2022-01-10T12:46:21Z
dc.date.issued2022-01
dc.date.submitted2021-07-27
dc.identifier.issn0004-637X
dc.identifier.otherapjac323a
dc.identifier.otherac323a
dc.identifier.otheraas33719
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/332498
dc.description.abstract<jats:title>Abstract</jats:title> <jats:p>The dominant uncertainty in the current measurement of the Hubble constant (<jats:italic>H</jats:italic> <jats:sub>0</jats:sub>) with strong gravitational lensing time delays is attributed to uncertainties in the mass profiles of the main deflector galaxies. Strongly lensed supernovae (glSNe) can provide, in addition to measurable time delays, lensing magnification constraints when knowledge about the unlensed apparent brightness of the explosion is imposed. We present a hierarchical Bayesian framework to combine a data set of SNe that are not strongly lensed and a data set of strongly lensed SNe with measured time delays. We jointly constrain (i) <jats:italic>H</jats:italic> <jats:sub>0</jats:sub> using the time delays as an absolute distance indicator, (ii) the lens model profiles using the magnification ratio of lensed and unlensed fluxes on the population level, and (iii) the unlensed apparent magnitude distribution of the SN population and the redshift–luminosity relation of the relative expansion history of the universe. We apply our joint inference framework on a future expected data set of glSNe and forecast that a sample of 144 glSNe of Type Ia with well-measured time series and imaging data will measure <jats:italic>H</jats:italic> <jats:sub>0</jats:sub> to 1.5%. We discuss strategies to mitigate systematics associated with using absolute flux measurements of glSNe to constrain the mass density profiles. Using the magnification of SN images is a promising and complementary alternative to using stellar kinematics. Future surveys, such as the Rubin and Roman observatories, will be able to discover the necessary number of glSNe, and with additional follow-up observations, this methodology will provide precise constraints on mass profiles and <jats:italic>H</jats:italic> <jats:sub>0</jats:sub>.</jats:p>
dc.languageen
dc.publisherAmerican Astronomical Society
dc.subject310
dc.subjectGalaxies and Cosmology
dc.titleThe Hubble Constant from Strongly Lensed Supernovae with Standardizable Magnifications
dc.typeArticle
dc.date.updated2022-01-10T12:46:21Z
prism.issueIdentifier1
prism.publicationNameAstrophysical Journal
prism.volume924
dc.identifier.doi10.17863/CAM.79948
dcterms.dateAccepted2021-10-20
rioxxterms.versionofrecord10.3847/1538-4357/ac323a
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.contributor.orcidBirrer, S [0000-0003-3195-5507]
dc.contributor.orcidDhawan, S [0000-0002-2376-6979]
dc.contributor.orcidShajib, AJ [0000-0002-5558-888X]
dc.identifier.eissn1538-4357
cam.issuedOnline2022-01-04


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