Measuring H0 with Quasar Time Delays
Frédéric Courbin (EPFL, Switzerland)
For the COSMOGRAIL, H0LiCOW, STRIDES and SHARP collaborations

COSMICLENS

Laboratoire d’astrophysique http://lastro.epfl.ch
Ecole Polytechnique Fédérale de Lausanne (EPFL)

Chicago - October 2019

Time Delays in Strongly Lensed Quasars

ImageAA
Lensedimage

Quasar
SourcequasarObserverLensed image B

Image B

Lens
galaxy“Lens”

ObserverTime Delays Measure the Hubble Constant H0H0Lens potentialat the images

H0Source position(unconstrained)
Astrometryof the images{1 + zL D L D S
t=·cDLS✓/ 1/H01 ⌅|⇥2⌅ |2⇤(⇥⌅ )Time delays provide a single-step and independent constraint on H0.

◆

Example of RX J1131-123

Image: NASA/STScIExample of RX J1131-123

Mass in the Einstein ring
Mass slope at image position

Image: NASA/STScIExample of RX J1131-123

Mass in the Einstein ring
Mass slope at image position

Mass contribution of intervening galaxies
along the line-of-sight (mass sheet)

Image: NASA/STScIWhat’s Needed and State of the ArtPASTTime delays measurements

15-30%

Mass model for the lens- Simplistic models- Few constraints

Environment of the lens

- External shear

Line of Sight contribution- External shear

What’s Needed and State of the Art

Time delays measurements

PASTNOW

15-30%

1-5%

Mass model for the lens

- Simplistic models- Few constraints- Flexible elliptical models- Deep sharp HST/AO images- Lens dynamics

Environment of the lens

- External shear- Include nearby companions- Multiplane lensing- Photo and spectro z

Line of Sight contribution- External shear- Galaxy counts- Cosmological simulations- Weak lensing- BLIND Analysis !

Time Delay Measurements

Past Measurements of Time Delays (1989-1992)

Q0957+561 « controversy » in the early 90s

Vanderriest et al. 1989, A&A, 215, 1: opticalmonitoring: Δt = 415 ± 20 days
Schild 1990, AJ, 100, 1771: optical monitoring:Δt = 405 days
Lehar et al. 1992, ApJ, 384, 453: radio
monitoring at the VLA
Δt = 513 ± 40 days

Past Measurements of Time Delays (1989-1992)

Vanderriest et al. (1989, A&A, 215, 1)

COSMOGRAIL Light Curves of WFI2033-4723

1.2m Euler telescope (La Silla)

Bonvin et al. 2019, arXiv:1905.08260

MPIA 2.2m Light Curves of WFI2033-4723

1.2m Euler telescope (La Silla)

2.2m MPIA telescope (La Silla)

Bonvin et al. 2019, arXiv:1905.08260

2- Constraining the Mass SlopeImaging Data for RX J1131-123
HSTNOW
PAST

Keck AO+ MUSE @VLT
+ OSIRIS @Keck
Ground-based seeing-limited
Lensing constraints restricted
to astrometry of the lensed
imagesFor detailed analyses of Keck AO imaging see
Chen et al. (2019, arXiv1907.02533)

Mass Slope of Lens Galaxy

Arrival time surfaces
in the image plane

Image positions unchanged

Normalized mass profileκ = projected mass density
in units of the critical massTime delays changed

Figure adapted from Saha, 2000, AJ 120, 1654

Constraining Models with Thick Rings !

RX J1131-123 (HST)

Lensing constraints come from all pixels covered by the Einstein ring formed by the quasar host.
Suyu et al. (2014, ApJ, 788, L35)

Blind Analysis !
Results of the unblinding process are published as they are !

A vast family of models is used

Chen et al. (2019, arXiv1907.02533)

3- Effect of Line of Sight

Mass-sheet Degeneracy (Line-of-Sight Contribution)
Mass along the line of sight brings extra mass inside the Einstein radius.
This can be estimated in different ways:
Using galaxy counts in lens fields and compare with the general field (Fassnacht et al.
2006, ApJ, 642, 30)
Using weighted galaxy counts (Collett et al. 2013, MNRAS 432, 679; Greene et al.
2013, ApJ, 768, 39)
Calibrating with cosmological simulations (e.g. Suyu et al. 2013, ApJ, 766, 70)
Using weak lensing maps (e.g. Tihhonova et al. 2018, MNRAS, 477, 5657)

LoS contribution: Galaxy Counts and Weak Lensing

30 arcmin

From weak lensing
Tihhonova et al. (2018, MNRAS 477, 5657)

From galaxy counts
Chen et al. (2019, arXiv1907.02533)

LoS contribution: Galaxy Counts and Weak Lensing
HST F606W

Galaxy counts and weak lensing agree !
Field of B1608: HST and Subaru imaging

HST F814W

Tihhonova et al. 2019, submitted

Current Values of External Convergence
No obvious correlation between H0 and external convergence among the 6 fields analyzed so far.

Before correction

After correction

Millon et al. 2019, in prep

Cosmology Results for 1 Lens in flat lambda-CMD

Cosmology Results for 2 Lenses in flat lambda-CMD

Cosmology Results for 3 Lenses in flat lambda-CMD

Cosmology Results for 4 Lenses in flat lambda-CMD

Cosmology Results for 5 Lenses in flat lambda-CMD

Cosmology Results for 6 Lenses in flat lambda-CMD

H0LiCOW XIII: milestone paper (Wong et al. 2019, arXiv1907.04869)

Are these statistically compatible with each other ?

Random Realizations with 6 Lenses (fiducial: 73.3)

Random Realizations with 6 Lenses (fiducial: 73.3)

Random Realizations with 6 Lenses (fiducial: 73.3)

Random Realizations with 6 Lenses (fiducial: 73.3)

Random Realizations with 6 Lenses (fiducial: 73.3)

Latest Object from the Collaboration: DES J0408-5354

DES J0408-5354: Data
HST color image

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sha1_base64="VvODso1peFFb6KMkRjYlMjP7juQ=">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</latexit>
sha1_base64="p5lh9qLNQEk4YViUw3UAWg8qsoc=">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</latexit>t(AB) = 112.1 ± 2.1 days (1.8%)

z=1.032z=0.769

MPIA 2.2m light curveand image
z=0.771

Time delays: Courbin et al. (2018)
Discovery: Lin et al. 2017

Shajib et al. (2019 arXiv1910.06306)

DES J0408-5354: Modeling with Lenstronomy

Shajib et al. (2019 arXiv1910.06306)

New Cosmology Results for 7 Lenses in flat lambda-CMD

Unblinding of
DES 0408-5354

Preliminary

See also poster from Anowar Shajib

Cosmology Results for 6 Lenses in flat lambda-CMDPreliminary

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SHOES
6 lenses
6 lenses+ SHOES

H0LiCOW XIII milestone paper by Wong et al. (2019, arXiv1907.04869)

Cosmology Results for 7 Lenses in flat lambda-CMD

Preliminary
1.573.7+1.4<latexit sha1_base64="wv8WBSnktio/jMITyF5eQouSuP8=">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</latexit>

7 lenses

5.3<latexit sha1_base64="jB1LA9P+aysE2Tc5yv07iVw9KlM=">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</latexit>

SHOES
6 lenses
6 lenses+ SHOES

Adding DES0408-5354 by Shajib et al. (2019, arXiv1910.06306)

Cosmology Results for 7 Lenses in flat lambda-CMD

Preliminary

5.7
5.3

1.5
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SHOES
6 lenses
6 lenses+ SHOESNow combining SHOES with 7 lenses

Summary
Strong lensing time delays consist in an absolute distance indicatorTime delays are measured to a few percents within 1 single season
DES, KIDS, HSC, PanSTARSS EUCLID, LSST, Gaia, will discoverhundreds of new suitable targets
7 lenses give H0 with accuracy and precision comparable tosupernovae and are independent
In flat lambda-CDM H0 = 73.7 +/- 2.9 km.s-1.Mpc-1
A dozen of additional objects already « in the pipeline »All analysis done blind!

More strong lensing results on posters by Akin Yildirim, Anowar Shajib & Chih-Fan Chen