Abstract
The dynamical modelling of integral field unit (IFU) stellar kinematics is a powerful tool to unveil the dynamical structure and mass build-up of galaxies in the local Universe, while gravitational lensing is nature’s cosmic telescope to explore the properties of galaxies beyond the local Universe. We present a new approach, which unifies dynamical modelling of galaxies with the magnification power of strong gravitational lensing, to reconstruct the structural and dynamical properties of high-redshift galaxies. By means of axisymmetric Jeans modelling, we create a dynamical model of the source galaxy, assuming a surface brightness and surface mass density profile. We then predict how the source’s surface brightness and kinematics would look when lensed by the foreground mass distribution and compare with the mock observed arcs of strong gravitational lensing systems. For demonstration purposes, we created and also analysed mock data of the strong lensing system RX J1131−1231. By modelling both the lens and source, we recover the dynamical mass within the effective radius of strongly lensed high-redshift sources within 5% uncertainty, and we improve the constraints on the lens mass parameters by up to 50%. This machinery is particularly well-suited for future observations from large segmented-mirror telescopes, such as the James Webb Space Telescope, which will yield high sensitivity and angular-resolution IFU data for studies on distant and faint galaxies.
Highlights
IntroductionThe progenitors of today’s massive galaxy population are thought to be small and dense (Daddi et al 2005; Trujillo et al 2006; Zirm et al 2007; van der Wel et al 2008, 2014; van Dokkum et al 2008; Szomoru et al 2010, 2012), discy (Toft et al 2005; Trujillo et al 2006; van der Wel et al 2011; Chang et al 2013), with quenched star formation and old stellar populations (Kriek et al 2006, 2008, 2009; Toft et al 2007; Cimatti et al 2008; van Dokkum et al 2010), small Sérsic indices, and high stellar velocity dispersion (van Dokkum et al 2009; Bezanson et al 2011; Toft et al 2012; van de Sande et al 2013) (see Cappellari 2016, for a review)
By computing the deflection produced by the lens mass profile, these quantities are mapped to the image plane
We obtain a lensed kinematic map and a surface brightness map that we compare to the input kinematic and
Summary
The progenitors of today’s massive galaxy population are thought to be small and dense (Daddi et al 2005; Trujillo et al 2006; Zirm et al 2007; van der Wel et al 2008, 2014; van Dokkum et al 2008; Szomoru et al 2010, 2012), discy (Toft et al 2005; Trujillo et al 2006; van der Wel et al 2011; Chang et al 2013), with quenched star formation and old stellar populations (Kriek et al 2006, 2008, 2009; Toft et al 2007; Cimatti et al 2008; van Dokkum et al 2010), small Sérsic indices, and high stellar velocity dispersion (van Dokkum et al 2009; Bezanson et al 2011; Toft et al 2012; van de Sande et al 2013) (see Cappellari 2016, for a review). GLaD is able to model the source stellar kinematics using axisymmetric Jeans modelling, assuming a source surface brightness and surface mass density profile, and predict how these maps will look like when lensed and distorted by a strong gravitational lens. This allows us to compare the predicted arcs and images directly to the observed strong gravitational lensing systems, in order to provide improved constraints for both the source and the deflector. From the redshifts of the lens and the source galaxies in Sect. 3, one arcsecond at the lens (source) plane in RX J1131−1231 corresponds to 4.43 (7.04) kpc
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