research10.1088/0004-6256/149/1/3

SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1

Abstract

International audienceWe present a new analysis of Hubble Space Telescope, Spitzer Space Telescope, and Very Large Telescope imaging and spectroscopic data of a bright lensed galaxy at z = 1.0334 in the lensing cluster A2667. Using this high-resolution imaging, we present an updated lens model that allows us to fully understand the lensing geometry and reconstruct the lensed galaxy in the source plane. This giant arc gives a unique opportunity to view the structure of a high-redshift disk galaxy. We find that the lensed galaxy of A2667 is a typical spiral galaxy with a morphology similar to the structure of its counterparts at higher redshift, z ∼ 2. The surface brightness of the reconstructed source galaxy in the z 850 band reveals the central surface brightness I (0) = 20.28 ± 0.22 mag arcsec −2 and a characteristic radius r s = 2.01 ± 0.16 kpc at redshift z ∼ 1. The morphological reconstruction in different bands shows obvious negative radial color gradients for this galaxy. Moreover, the redder central bulge tends to contain a metal-rich stellar population, rather than being heavily reddened by dust due to high and patchy obscuration. We analyze the VIMOS/integral field unit spectroscopic data and find that, in the given wavelength range (∼1800–3200 Å), the combined arc spectrum of the source galaxy is characterized by a strong continuum emission with strong UV absorption lines (Fe ii and Mg ii) and shows the features of a typical starburst Wolf–Rayet galaxy, NGC 5253. More specifically, we have measured the equivalent widths of Fe ii and Mg ii lines in the A2667 spectrum, and obtained similar values for the same wavelength interval of the NGC 5253 spectrum. Marginal evidence for [C iii] 1909 emission at the edge of the grism range further confirms our expectation

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oai:HAL:hal-01109685v1Last time updated on 11/11/2016

This paper was published in HAL-ENS-LYON.

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