The DIVING3D survey – Deep Integral Field Spectrograph View of Nuclei of Galaxies – I. Definition and sample presentation

Steiner, J. E.; Menezes, R. B.; Ricci, T. V.; Silva, Patrícia da; Fernandes, R. Cid; Asari, N. Vale; Carvalho, M. S.; May, D.; Coelho, P.; Amorim, A. L. de

doi:10.1093/mnras/stac034

Cited by 7 publications

(3 citation statements)

References 126 publications

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“…NGC 6868 was observed on 2013 May 04 with the Gemini South Telescope using the Gemini Multi-Object Spectrograph (GMOS) in the IFU mode (Allington-Smith et al 2002 ;Hook et al 2004 ). This object is part of the DIVING 3D surv e y, which made observations of the central regions of all 170 galaxies in the Southern hemisphere with B < 12.0 and | b | > 15 • (see Steiner et al 2022 for more details). The one slit set-up was used for the observations, resulting in an FoV of 5.0 × 3.5 arcsec 2 .…”

Section: O B S E Rvat I O N a N D Data R E D U C T I O Nmentioning

confidence: 99%

Digging deeper into NGC 6868 I: Stellar population

Benedetti

Riffel

Ricci

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We use Gemini integral field unit observations to map the stellar population properties in the inner region (∼680 × 470 pc2) of the galaxy NGC 6868. In order to understand the physical and chemical properties of the stellar content of this galaxy, we performed stellar population synthesis using the starlight code with the MILES simple stellar population models. We measured the absorption line indices Fe4383, Mg2, Mgb, Fe5270, Fe5335 for the whole FoV, and used them to derive Fe3 and [MgFe]’. These indices were used to derive [α/Fe]. This galaxy is dominated by old metal-rich populations (12.6 Gyr; 1.0 and 1.6 Z⊙) with a negative metallicity gradient. We also found a recent (∼63 Myr) metal-rich (1.6 Z⊙) residual star formation in the centre of the galaxy. A dust lane with a peak extinction in the V band of 0.65 mag is seen. No signs of ordered stellar motion are found and the stellar kinematics is dispersion dominated. All indices show a spatial profile varying significantly along the FoV. Mg2 shows a shallow gradient, compatible with the occurrence of mergers in the past. Mgb and Fe3 profiles suggest different enrichment processes for these elements. We observe three distinct regions: for R<100 pc and R>220 pc, Mg2, Mgb anti correlate with respect to Fe3 and [MgFe]’, and for 100 pc<R<220 pc, they correlate, hinting at different enrichment histories. The [α/Fe] profile is really complex and has a central value of ∼0.2 dex. We interpret this as the result of a past merger with another galaxy with a different [α/Fe] history, thus explaining the [α/Fe] maps.

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Section: O B S E Rvat I O N a N D Data R E D U C T I O Nmentioning

confidence: 99%

Digging deeper into NGC 6868 I: Stellar population

Benedetti

Riffel

Ricci

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…The DIVING 3D project is a survey designed to unveil the central regions of galaxies with IFU spectroscopy (Steiner et al, 2022). Inspired on the Palomar survey, the DIVING 3D has a statistically complete sample of galaxies, all objects with B < 12.0 mag, δ < 0 • and |b| > 15 • .…”

Section: The Diving 3d Surveymentioning

confidence: 99%

“…Additionally, aims to study the kinematics and properties of the stellar populations. Besides the complete sample, another strength of the survey is the high angular resolution, under seeing limited conditions, and high signal-to-noise ratio (SNR) observations (Steiner et al, 2021;Steiner et al, 2022). The data used in the project consist of a optical and two NIR IFU data cubes.…”

Section: The Diving 3d Surveymentioning

confidence: 99%

The many faces of the Seyfert galaxy NGC 5643

Macedo¹

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Primeiramente, agradeço à Natureza pela oportunidade de estar vivo e me sentir mais vivo ainda ao vislumbrar a sua beleza.Agradeço a minha família pelo apoio e compreensão. Principalmente a minha mãe Neiva e minha avó Inês, que nunca desacreditaram a minha jornada.Agradeço ao meu orientador, João Evangelista Steiner por confiar a mim esse projeto, me orientar e me inspirar. Agradeço também a oportunidade das monitorias nas suas disciplinas de "Astronomia -Uma Visão Geral". Eu cresci muito nesse tempo. Agradeço ao meu orientador Rodrigo Nemmen por ter me acolhido em seu grupo de pesquisa, me orientado e mentorado na pesquisa e na vida acadêmica. Seu apoio foi fundamental. Aproveito para agradecer aos membros doGrupo de Buracos Negros da USP, pelo acolhimento e apoio, em especial ao Fábio Cafardo, Ivan Almeida, Roberta Duarte e Raniere de Menezes. Agradeço imensamente o apoio e a orientação dos membros do grupo de pesquisa do meu orientador, João Steiner, que lideram o DIV IN G 3D survey. A orientação de vocês foi essencial para que eu seguisse nesse projeto e hoje possa defendê-lo. Agradeço a Tiago Vecchi Ricci pela suas ideias, feedbacks, orientação e mentoria. A Roberto Bertoldo Menezes as diversas ajudas e apoio na pesquisa e na vida acadêmica. A Daniel May as ideias, apoio e momentos de descontração. A Patrícia da Silva pelas suas ideias, feedbacks e em especial a revisão desse manuscrito, agradeço de coração. A Catarina Aydar por me receber na USP, pela parceria nas disciplinas e na pesquisa, por todo apoio e ajuda nos momentos difíceis.Agradeço também a outros pesquisadores que também foram essenciais nessa minha jornada. A Roderik Overzier pelas suas ideias e mentoria, direcionamentos na pesquisa e na vida acadêmica, apoio nos momentos difíceis e suas aulas sobre AGNs.A Laerte Sodré Júnior pelos direcionamentos e apoio na pesquisa e na vida acadêmica.Agradeço a Victoria Reynaldi pela sua disponibilidade, apoio, ideias sobre a pesquisa e a vida, e sua colaboração. A Alberto Rodríguez Ardila pelas nossas conversas e ideias sobre a pesquisa. A Oli Dors pelo seu apoio, ideias e aulas. Agradeço o apoio e troca de ideias às e aos pesquisadores Daniel Ruschel Dutra,

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The DIVING3D Survey – Deep IFS view of nuclei of galaxies – II. First results: nuclear emission-line properties of the mini-DIVING3D sample

Menezes

Steiner

Ricci

et al. 2022

Monthly Notices of the Royal Astronomical Society

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This work presents the first results of the Deep IFS View of Nuclei of Galaxies (DIVING3D) survey. We analysed the nuclear emission-line spectra of a sub-sample we call mini-DIVING3D, which includes all Southern galaxies with B < 11.2 and |b| > 15○. We verified that $23{{\ \rm per\ cent}} \pm 4{{\ \rm per\ cent}}$ of the galaxies show nuclear emission-line properties characteristic of Low Ionization Nuclear Emission-Line Regions (LINERs). Diagnostic diagram analysis reveals an apparent dichotomy, not detected in previous studies, between objects classified as H II regions and as LINERs or Seyferts, with very few galaxies classified as transition objects. A possible explanation for this result is that at least part of the transition objects are composite systems, with a central LINER contaminated by the emission from circumnuclear H II regions. The higher spatial resolution of the DIVING3D survey, in comparison with previous studies, allowed us to isolate the nuclear emission from circumnuclear contaminations, reducing the number of transition objects. We also propose an alternative scenario, in which the emission-line spectra of some transition objects are the result of shock heating by central outflows, together with photoionization by young stars. Clear evidence of Active Galactic Nuclei, in the optical and X-ray spectral bands, were detected in 69 per cent of the LINERs in the mini-DIVING3D sample. Considering the entire mini-DIVING3D sample, evidence of AGNs were detected in 65 per cent of the objects.

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The DIVING3D survey – Deep Integral Field Spectrograph View of Nuclei of Galaxies – I. Definition and sample presentation

Cited by 7 publications

References 126 publications

Digging deeper into NGC 6868 I: Stellar population

Digging deeper into NGC 6868 I: Stellar population

The many faces of the Seyfert galaxy NGC 5643

The DIVING3D Survey – Deep IFS view of nuclei of galaxies – II. First results: nuclear emission-line properties of the mini-DIVING3D sample

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