Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations
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m, S500 ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnifications of the background sources are consistent with previous studies. However, the background source circularized radii (between 0.34 and 1.30 kpc) are ∼3 times smaller than the ones measured in the sub-millimetre/millimetre for a similarly selected and partially overlapping sample. We compare our lenses with those in the Sloan Lens Advanced Camera for Surveys (ACS) Survey confirming that our lens-independent selection is more effective at picking up fainter and diffuse galaxies and group lenses. This sample represents the first step towards characterizing the near-infrared properties and stellar masses of the gravitationally lensed dusty star-forming galaxies.
| Originalsprog | Engelsk |
|---|---|
| Tidsskrift | Monthly Notices of the Royal Astronomical Society |
| Vol/bind | 528 |
| Udgave nummer | 4 |
| Sider (fra-til) | 6222-6279 |
| Antal sider | 58 |
| ISSN | 0035-8711 |
| DOI | |
| Status | Udgivet - 2024 |
Bibliografisk note
Funding Information:
This work benefitted from the support of the project Z-GAL ANR-AAPG2019 of the French National Research Agency (ANR). EB acknowledges the School of Physics and Astronomy of Cardiff University for hospitality while this paper was in progress. EB, EMC, and GR are supported by Padua University grants Dotazione Ordinaria Ricerca (DOR) 2019–2021 and by the Italian Ministry for Education, University, and Research (MIUR) grant Progetto di Ricerca di Interesse Nazionale (PRIN) 2017 20173ML3WW-001. EMC is also funded by the Istituto Nazionale di Astrofisica (INAF) through grant PRIN 2022 C53D23000850006. LM and MV acknowledge financial support from the Inter-University Institute for Data Intensive Astronomy (IDIA), a partnership of the University of Cape Town, the University of Pretoria and the University of the Western Cape, and from the South African Department of Science and Innovation’s National Research Foundation under the ISARP RADIOSKY2020 and RADIOMAP + Joint Research Schemes (DSI-NRF grant nos 113121 and 150551) and the SRUG Projects (DSI-NRF grant nos 121291, SRUG22031677 and SRUG2204254729). DW acknowledges support from program number HST-GO-15242, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. AA is supported by the European Researc Council (ERC) Advanced Investigator grant, DMIDAS [GA 786910], to C. S. Frenk. PC acknowledges the support of the project Z-GAL ANR-AAPG2019 of the ANR. HD acknowledges financial support from the Agencia Estatal de Investigació n del Ministerio de Ciencia e Innovación (AEI-MCINN) under grant (La evolució n de los cíumulos de galaxias desde el amanecer hasta el mediodía có smico) with reference (PID2019-105776GB-I00/DOI:10.13039/501100011033) and acknowledge support from the ACIISI, Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant with reference PROID2020010107. JGN acknowledges financial support from the PGC projects PGC2018-101948-B-I00 and PID2021-125630NB-I00 from MICINN and Fondos Europeos de Desarrollo Regional (FEDER). SJ is supported by the European Union’s Horizon Europe research and innovation program under the Marie Skłodowska-Curie grant agreement no. 101060888. AL is partly supported by the PRIN MIUR 2017 prot. 20173ML3WW 002 ‘Opening the ALMA window on the cosmic evolution of gas, stars, and massive black holes’. IPF acknowledges support from the Spanish State Research Agency (AEI) under grant no. PID2019-105552RB-C43. SS was partly supported by ESCAPE – The European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures, which in turn received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement no. 824064. SS thanks the Science and Technology Facilities Council for support under grants ST/P000584/1. CY acknowledges the support from the ERC advanced grant 789410.
Funding Information:
This work benefitted from the support of the project Z-GAL ANRAAPG2019 of the French National Research Agency (ANR). EB acknowledges the School of Physics and Astronomy of Cardiff University for hospitality while this paper was in progress. EB, EMC, and GR are supported by Padua University grants Dotazione Ordinaria Ricerca (DOR) 2019–2021 and by the Italian Ministry for Education, University, and Research (MIUR) grant Progetto di Ricerca di Interesse Nazionale (PRIN) 2017 20173ML3WW-001. EMC is also funded by the Istituto Nazionale di Astrofisica (INAF) through grant PRIN 2022 C53D23000850006. LM and MV acknowledge financial support from the Inter-University Institute for Data Intensive Astronomy (IDIA), a partnership of the University of Cape Town, the University of Pretoria and the University of the Western Cape, and from the South African Department of Science and Innovation’s National Research Foundation under the ISARP RADIOSKY2020 and RADIOMAP + Joint Research Schemes (DSI-NRF grant nos 113121 and 150551) and the SRUG Projects (DSI-NRF grant nos 121291, SRUG22031677 and SRUG2204254729). DW acknowledges support from program number HST-GO-15242, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. AA is supported by the European Researc Council (ERC) Advanced Investigator grant, DMIDAS [GA 786910], to C. S. Frenk. PC acknowledges the support of the project Z-GAL ANRAAPG2019 of the ANR. HD acknowledges financial support from the Agencia Estatal de Investigació n del Ministerio de Ciencia e In-novación (AEI-MCINN) under grant (La evolució n de los cíumulos de galaxias desde el amanecer hasta el mediodía có smico) with reference (PID2019-105776GB-I00/DOI:10.13039/501100011033) and acknowledge support from the ACIISI, Consejería de Economía, Conocimiento y Empleo del Gobierno de Canarias and the European Regional Development Fund (ERDF) under grant with reference PROID2020010107. JGN acknowledges financial support from the PGC projects PGC2018-101948-B-I00 and PID2021-125630NBI00 from MICINN and Fondos Europeos de Desarrollo Regional (FEDER). SJ is supported by the European Union’s Horizon Europe research and innovation program under the Marie Skłodowska-Curie grant agreement no. 101060888. AL is partly supported by the PRIN MIUR 2017 prot. 20173ML3WW 002 ‘Opening the ALMA window on the cosmic evolution of gas, stars, and massive black holes’. IPF acknowledges support from the Spanish State Research Agency (AEI) under grant no. PID2019-105552RB-C43. SS was partly supported by ESCAPE – The European Science Cluster of Astronomy & Particle Physics ESFRI Research Infrastructures, which in turn received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement no. 824064. SS thanks the Science and Technology Facilities Council for support under grants ST/P000584/1. CY acknowledges the support from the ERC advanced grant 789410.
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© The Author(s) 2023.
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