J/A+A/673/A9 TDCOSMO XII. Resolved kinematics of lens galaxy (Shajib+, 2023)
TDCOSMO. XII. Improved Hubble constant measurement from lensing time delays
using spatially resolved stellar kinematics of the lens galaxy.
Shajib A.J., Mozumdar P., Chen G.C.-F., Treu T., Cappellari M., Knabel S.,
Suyu S.H., Bennert V.N., Frieman J.A., Sluse D., Birrer S., Courbin F.,
Fassnacht C.D., Villafana L., Williams P.R.
<Astron. Astrophys. 673, A9 (2023)>
=2023A&A...673A...9S 2023A&A...673A...9S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Spectra, infrared
Keywords: distance scale - gravitational lensing: strong -
Galaxy: kinematics and dynamics -
galaxies: elliptical and lenticular, cD -
galaxies: individual: RXJ1131-1231
Abstract:
Strong-lensing time delays enable the measurement of the Hubble
constant (H0) independently of other traditional methods. The main
limitation to the precision of time-delay cosmography is mass-sheet
degeneracy (MSD). Some of the previous TDCOSMO analyses broke the MSD
by making standard assumptions about the mass density profile of the
lens galaxy, reaching 2% precision from seven lenses. However, this
approach could potentially bias the H0 measurement or underestimate
the errors. For this work, we broke the MSD for the first time using
spatially resolved kinematics of the lens galaxy in RXJ1131-1231
obtained from the Keck Cosmic Web Imager spectroscopy, in combination
with previously published time delay and lens models derived from
Hubble Space Telescope imaging. This approach allowed us to robustly
estimate H0, effectively implementing a maximally flexible mass model.
Following a blind analysis, we estimated the angular diameter distance
to the lens galaxy Dd=865-81+85Mpc and the time-delay
distance D{DELTA}t=2180-271+472Mpc, giving
H0=77.1-7.1+7.3km/s/Mpc for a flat {LAMBDA} cold dark matter
cosmology. The error budget accounts for all uncertainties, including
the MSD inherent to the lens mass profile and line-of-sight effects,
and those related to the mass-anisotropy degeneracy and projection
effects. Our new measurement is in excellent agreement with those
obtained in the past using standard simply parametrized mass profiles
for this single system (H0=78.3-3.3+3.4km/s/Mpc) and for seven
lenses (H0=74.2-1.6+1.6km/s/Mpc), or for seven lenses
using single-aperture kinematics and the same maximally flexible
models used by us (H0=73.3-5.8+5.8km/s/Mpc). This agreement
corroborates the methodology of time-delay cosmography.
Description:
The data included in the Fits file is the reduced, drizzled, and
cropped 3D datacube from KCWI integral field spectrograph on the Keck
Observatory for the lensing galaxy in RXJ1131-1231. The cropped field
of view is 6.3x6.3 square arcseconds. The observed wavelength range is
3600-5600 Angstrom. The dimension of the datacube is (5215, 43, 43).
The spectral resolution is R∼3600. Each spaxel's width is 0.1457
arcsecond and the reciprocal dispersion is 0.5 Angstrom/pixel.
Objects:
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RA (2000) DE Designation(s)
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11 31 51.46 -12 31 58.44 lensing galaxy in RXJ1131-1231 = [SSC2003] J1131GL
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 289 1 Informations on fits datacude
fits/* . 1 fits datacude
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 24 F5.3 arcsec/pix scale Scale of the image
26- 27 I2 --- Nx Number of pixels along X-axis
29- 30 I2 --- Ny Number of pixels along Y-axis
32- 35 I4 --- Nz Number of pixels along Z-axis
37- 46 A10 "datime" Obs.date Observation date
48- 51 I4 0.1nm bWAVE Lower value of wavelength interval
53- 56 I4 0.1nm BWAVE Upper value of wavelength interval
58- 60 F3.1 0.1nm dWAVE Wavelength resolution
62- 66 I5 Kibyte size Size of FITS file
68-100 A33 --- FileName Name of FITS file, in subdirectory fits
102-289 A188 --- Title Title of the FITS file
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History:
From Anowar Shajib, ajshajib(at)uchicago.edu
Acknowledgements:
The data presented herein were obtained at the W. M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California and
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W. M. Keck
Foundation. The authors wish to recognize and acknowledge the very
significant cultural role and reverence that the summit of Maunakea
has always had within the indigenous Hawaiian community.
We are most fortunate to have the opportunity to conduct observations
from this mountain.
References:
Millon et al., Paper I 2020A&A...639A.101M 2020A&A...639A.101M
Millon et al., Paper II 2020A&A...642A.193M 2020A&A...642A.193M
GilmaN et al., Paper III 2020A&A...642A.194G 2020A&A...642A.194G
Birrer et al., Paper IV 2020A&A...643A.165B 2020A&A...643A.165B
Birrer & Treu, Paper V 2021A&A...649A..61B 2021A&A...649A..61B
Chem et al., Paper VI 2021A&A...652A...7C 2021A&A...652A...7C
van de Vyvere et al., Paper VII 2022A&A...659A.127V 2022A&A...659A.127V
Gomer et al., Paper VIII 2022A&A...667A..86G 2022A&A...667A..86G
Shajib et al., Paper IX 2022A&A...667A.123S 2022A&A...667A.123S
(End) Patricia Vannier [CDS] 01-Mar-2023