Spectroscopic redshifts of selected flat-spectrum radio sources I

Dmitry Blinov; Alberto Floris; Andreas Zezas; Carolina Casadio; Elias Kyritsis; Valentina Missaglia; Vangelis Pantoulas; Avinash Kumar

arXiv · 2607.04959

Spectroscopic redshifts of selected flat-spectrum radio sources I

Dmitry Blinov·Alberto Floris·Andreas Zezas·Carolina Casadio·Elias Kyritsis·Valentina Missaglia·Vangelis Pantoulas·Avinash Kumar

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Abstract

We present the first results of a spectroscopic campaign carried out as part of the Search for Milli-Lenses (SMILE) program, which aims to constrain the prevalence of gravitational lens systems on milli-arcsecond angular scales (milli-lenses) using high-resolution Very Long Baseline Interferometry (VLBI) imaging. The SMILE parent sample contains ~ 5000 radio-loud active galaxies, selected as a flux-limited, complete subsample of CLASS (The Cosmic Lens All-Sky Survey) sources. We compiled redshift information for the full sample from multiple literature and catalog sources and found that 491 sources have no available redshift estimate, either spectroscopic or photometric. A further 948 sources have only photometric redshifts, many of which show substantial discrepancies between catalogs. Reliable redshifts are essential for VLBI radio-source studies because they convert angular measurements into physical linear scales, enable estimates of intrinsic luminosities and jet kinematics, and allow robust cosmological and population studies. To address this key limitation for lensing and population studies, we initiated a dedicated spectroscopic campaign to secure reliable redshifts for as many targets as possible. This paper focuses on the brightest sources in the SMILE sample. We report newly determined spectroscopic redshifts for 6 targets out of 15 observed with the Skinakas 1.3 m telescope.

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Dmitry Blinov, Alberto Floris, Andreas Zezas, Carolina Casadio, Elias Kyritsis, Valentina Missaglia, Vangelis Pantoulas, Avinash Kumar. 2026-07-06. Spectroscopic redshifts of selected flat-spectrum radio sources I. https://arxiv.org/abs/2607.04959

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