Witnessing the Differential Evolution in Luminosity and Size of Disk Galaxies via Gravitational Lensing

Details Witnessing the Differential Evolution in Luminosity and Size of Disk Galaxies via Gravitational Lensing Witnessing the Differential Evolution in Luminosity and Size of Disk Galaxies via Gravitational Lensing

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21930705b&link_type=abstract

American Astronomical Society, AAS Meeting #219, #307.05

Astronomy and Astrophysics

Astrophysics

Scientific paper

We take advantage of the magnification in size and flux of a galaxy, provided by gravitational lensing, to analyze the properties of 62 strongly lensed galaxies of the Sloan Lens ACS (SLACS) Survey. The sample of lensed galaxies span a redshift range of 0.20 <= z <= 1.20 with a median redshift of z = 0.61. We use the lens modeling code LENSFIT to derive the luminosities, sizes and Sersic indices of the lensed galaxies. The measured properties of the lensed galaxies show a primarily compact, "disk"-like population with the peaks of the size and Sersic index distributions corresponding to ∼1.50 kpc and n∼1 respectively. Comparison of the SLACS lensed galaxies to a non-lensing, broad-band imaging based survey shows that a lensing survey allows us to probe a galaxy population that is typically ∼ 2 magnitudes fainter. Our analysis allows us to compare the = 0.61 disk galaxy sample (n <= 2.5) to an unprecedented local galaxy sample of 670,131 SDSS galaxies at z ∼ 0.1, which indicates that the evolution of the luminosity-size relation since z ∼ 1 cannot be explained fully in terms of pure size evolution but must be caused by a combination of luminosity and size evolution. Our observations are in excellent agreement with recent numerical simulations of disk galaxies since z ∼ 1 that show evidence of mass-dependent evolution where high-mass disk galaxies (stellar mass > 109 solar masses) evolve more in size and low-mass disk galaxies (stellar mass <= 109 solar masses) evolve more in luminosity. The authors gratefully acknowledge the support from the National Research Council of Canada and NSERC through Discovery grants. CYP is grateful for funding support through the Plaskett Fellowship of the Herzberg Institute of Astrophysics (National Research Council of Canada).

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