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arXiv · 1305.6924

Constraining the Minimum Luminosity of High Redshift Galaxies through Gravitational Lensing

Natalie Mashian·Abraham Loeb
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Abstract

We simulate the effects of gravitational lensing on the source count of high redshift galaxies as projected to be observed by the Hubble Frontier Fields program and the James Webb Space Telescope (JWST) in the near future. Taking the mass density profile of the lensing object to be the singular isothermal sphere (SIS) or the Navarro-Frenk-White (NFW) profile, we model a lens residing at a redshift of z_L = 0.5 and explore the radial dependence of the resulting magnification bias and its variability with the velocity dispersion of the lens, the photometric sensitivity of the instrument, the redshift of the background source population, and the intrinsic maximum absolute magnitude (M_{max}) of the sources. We find that gravitational lensing enhances the number of galaxies with redshifts z >= 13 detected in the angular region θ_E/2 <= θ<= 2θ_E (where θ_E is the Einstein angle) by a factor of ~ 3 and 1.5 in the HUDF (df/dν_0 ~ 9 nJy) and medium-deep JWST surveys (df/dν_0 ~ 6 nJy). Furthermore, we find that even in cases where a negative magnification bias reduces the observed number count of background sources, the lensing effect improves the sensitivity of the count to the intrinsic faint-magnitude cut-off of the Schechter luminosity function. In a field centered on a strong lensing cluster, observations of z >= 6 and z >= 13 galaxies with JWST can be used to infer this cut-off magnitude for values as faint as M_{max} ~ -14.4 and -16.1 mag (L_{min} ~ 2.5*10^{26} and 1.2*10^{27} erg s^{-1} Hz^{-1}) respectively, within the range bracketed by existing theoretical models. Gravitational lensing may therefore offer an effective way of constraining the low-luminosity cut-off of high-redshift galaxies.

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Natalie Mashian, Abraham Loeb. 2013-11-25. Constraining the Minimum Luminosity of High Redshift Galaxies through Gravitational Lensing. https://doi.org/10.1088/1475-7516%2F2013%2F12%2F017

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