Dark halo response and the stellar initial mass function in early-type and late-type galaxies

We present a blind time-delay strong lensing (TDSL) cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 . We combine the relative time delay between the quasar images, Hubble Space Telescope imaging, the Keck stellar velocity dispersion of the lensing galaxy, and wide-field photometric and spectroscopic data of the field to constrain two angular diameter distance relations. The combined analysis is performed by forward modelling the individual data sets through a Bayesian hierarchical framework, and it is kept blind until the very end to prevent experimenter bias. After unblinding, the inferred distances imply a Hubble constant H 0 = 68.8 +5.4 −5.1 km s −1 Mpc −1 , assuming a flat Λ cold dark matter cosmology with uniform prior on Ω m in [0.05, 0.5]. The precision of our cosmographic measurement with the doubly imaged quasar SDSS 1206+4332 is comparable with those of quadruply imaged quasars and opens the path to perform on selected doubles the same analysis as anticipated for quads. Our analysis is based on a completely independent lensing code than our previous three H0LiCOW systems and the new measurement is fully consistent with those. We provide the analysis scripts paired with the publicly available software to facilitate independent analysis. The consistency between blind measurements with independent codes provides an important sanity check on lens modelling systematics. By combining the likelihoods of the four systems under the same prior, we obtain H 0 = 72.5 +2.1 −2.3 km s −1 Mpc −1 . This measurement is independent of the distance ladder and other cosmological probes.

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“…(ii) Option COMPOSITE: We split the luminous and dark component of the lens model into two composite parts (see, e.g., Dutton et al 2011…”

Section: Main Deflector Galaxy G0mentioning

confidence: 99%

H0LiCOW – IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant

Birrer

Treu

Rusu

et al. 2019

Monthly Notices of the Royal Astronomical Society

377

334

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“…Numerous physical mechanisms, such as the mass accretion history, the initial mass function, dynamical instabilities, and adiabatic contraction determine the relative contribution of baryons and dark matter E-mail: frizzo@mpa-garching.mpg.de within a galaxy (e.g. Blumenthal et al 1986;Dutton et al 2011;Courteau & Dutton 2015;Zolotov et al 2015). For this reason, quantifying the amount of dark matter from kinematical measurements provides a strong constraints on galaxy formation models (Rubin et al 1978;van Albada et al 1985).…”

Section: Introductionmentioning

confidence: 99%

A novel 3D technique to study the kinematics of lensed galaxies

Rizzo

Vegetti

Fraternali

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a 3D Bayesian method to model the kinematics of strongly lensed galaxies from spatially-resolved emission-line observations. This technique enables us to simultaneously recover the lens-mass distribution and the source kinematics directly from the 3D data cube. We have tested this new method with simulated OSIRIS observations for nine star-forming lensed galaxies with different kinematic properties. The simulated rotation curves span a range of shapes which are prototypes of different morphological galaxy types, from dwarf to massive spiral galaxies. We have found that the median relative accuracy on the inferred lens and kinematic parameters are at the level of 1 and 2 per cent, respectively. We have also tested the robustness of the technique against different inclination angles, signal-to-noise ratios, the presence of warps or non-circular motions and we have found that the accuracy stays within a few per cent in most cases. This technique represents a significant step forward with respect to the methods used until now, as the lens parameters and the kinematics of the source are derived from the same 3D data. This enables us to study the possible degeneracies between the two and estimate the uncertainties on all model parameters consistently.

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“…Proxy for the spin parameter l Re vs. ellipticity  e for galaxies with * > M 10 10 M e . For each galaxy we show its velocity map aligned to 45°using the kinematic position angle, with the velocity range set by the stellar mass Tully-Fisher relation (Dutton et al 2011). A regularization algorithm is applied to avoid overlap of the velocity maps.…”

Section: Kinemetry: Regular and Non Regular Rotatorsmentioning

confidence: 99%

“…The size of the grid and velocity maps are chosen such that no galaxy is offset by more than one grid point from its original position. The stellar mass Tully-Fisher (Dutton et al 2011) relation is used for the velocity scale: for a galaxy with stellar mass * > M 10 10 M e the velocity scale of the velocity map ranges from −95<V[ km s…”

Section: Separating Fast and Slow Rotatorsmentioning

confidence: 99%

The Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics

Sande

Bland-Hawthorn

Fogarty

et al. 2017

ApJ

131

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Recent cosmological hydrodynamical simulations suggest that integral field spectroscopy can connect the highorder stellar kinematic moments h 3 (∼skewness) and h 4 (∼kurtosis) in galaxies to their cosmological assembly history. Here, we assess these results by measuring the stellar kinematics on a sample of 315 galaxies, without a morphological selection, using two-dimensional integral field data from the SAMI Galaxy Survey. Proxies for the spin parameter (l R e ) and ellipticity ( e ) are used to separate fast and slow rotators; there exists a good correspondence to regular and non-regular rotators, respectively, as also seen in earlier studies. We confirm that regular rotators show a strong h 3 versus s V anti-correlation, whereas quasi-regular and non-regular rotators show a more vertical relation in h 3 and s V . Motivated by recent cosmological simulations, we develop an alternative approach to kinematically classify galaxies from their individual h 3 versus s V signatures. Within the SAMI Galaxy Survey, we identify five classes of high-order stellar kinematic signatures using Gaussian mixture models. Class 1 corresponds to slow rotators, whereas Classes 2-5 correspond to fast rotators. We find that galaxies with similar  l R e e -values can show distinctly different s h V 3 -signatures. Class 5 objects are previously unidentified fast rotators that show a weak h 3 versus s V anti-correlation. From simulations, these objects are predicted to be disk-less galaxies formed by gas-poor mergers. From morphological examination, however, there is evidence for large stellar disks. Instead, Class 5 objects are more likely disturbed galaxies, have counter-rotating bulges, or bars in edge-on galaxies. Finally, we interpret the strong anti-correlation in h 3 versus s V as evidence for disks in most fast rotators, suggesting a dearth of gas-poor mergers among fast rotators.

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Dark halo response and the stellar initial mass function in early-type and late-type galaxies

Cited by 101 publications

References 161 publications

H0LiCOW – IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant

H0LiCOW – IX. Cosmographic analysis of the doubly imaged quasar SDSS 1206+4332 and a new measurement of the Hubble constant

A novel 3D technique to study the kinematics of lensed galaxies

The Sami Galaxy Survey: Revisiting Galaxy Classification Through High-Order Stellar Kinematics

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