TY - JOUR
T1 - CAVITY, Calar Alto Void Integral-field Treasury surveY and project extension
AU - Pérez, I.
AU - Verley, S.
AU - Sánchez-Menguiano, L.
AU - Ruiz-Lara, T.
AU - García-Benito, R.
AU - Puertas, S. Duarte
AU - Jiménez, A.
AU - Domínguez-Gómez, J.
AU - Espada, D.
AU - Peletier, R. F.
AU - Román, J.
AU - Rodríguez, M. I.
AU - Argudo-Fernández, M.
AU - Torres-Ríos, G.
AU - Bidaran, B.
AU - Alcázar-Laynez, M.
AU - Weygaert, R. van de
AU - Lisenfeld, U.
AU - Zurita, A.
AU - Florido, E.
AU - Hulst, J. M. van der
AU - Blázquez-Calero, G.
AU - Villalba-González, P.
AU - Moral-Castro, I. del
AU - Alarcón, P. Sánchez
AU - Lugo-Aranda, A.
AU - Walo-Martín, D.
AU - Conrado, A.
AU - Delgado, R. González
AU - Falcón-Barroso, J.
AU - Ferré-Mateu, A.
AU - Hernández-Sánchez, M.
AU - Awad, P.
AU - Kreckel, K.
AU - Courtois, H.
AU - Espada-Miura, R.
AU - Relaño, M.
AU - Galbany, L.
AU - Sánchez-Blázquez, P.
AU - Pérez-Montero, E.
AU - Sánchez-Portal, M.
AU - Bongiovanni, A.
AU - Planelles, S.
AU - Quilis, V.
AU - Weijmans, A. M.
AU - Raj, M. A.
AU - Aragón-Calvo, M. A.
AU - Azzaro, M.
AU - Bergond, G.
AU - Blazek, M.
AU - Cikota, S.
AU - Fernández-Martín, A.
AU - Gardini, A.
AU - Guijarro, A.
AU - Hermelo, I.
AU - Martin, P.
AU - Linares, J. I. Vico
N1 - Funding: We acknowledge financial support by the research projects AYA2017-84897-P, PID2020-113689GB-I00, and PID2020-114414GB-I00, financed by MCIN/AEI/10.13039/501100011033, the project A-FQM-510-UGR20 financed from FEDER/Junta de Andalucía-Consejería de Transformación Económica, Industria, Conocimiento y Universidades/Proyecto and by the grants P20-00334 and FQM108, financed by the Junta de Andalucía (Spain). TRL acknowledges support from Juan de la Cierva fellowship (IJC2020-043742-I). LSM acknowledges support from Juan de la Cierva fellowship (IJC2019-041527-I). DE acknowledges support from a Beatriz Galindo senior fellowship (BG20/00224) from the Spanish Ministry of Science and Innovation. RGD, RGB, and AC acknowledge financial support from the State Agency for Research of the Spanish MCIU through ‘Center of Excellence Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía, CEX2021-001131-S, funded by MCIN/AEI/10.13039/501100011033, and to financial support from the projects PID-2019-109067-GB100 and PID2022-141755NB-I00. HC also acknowledges support from the Institut Universitaire de France and from the CNES. IMC acknowledges support from ANID programme FONDECYT Postdoctorado 3230653. JF-B acknowledges support from the PID2022-140869NB-I00 grant from the Spanish Ministry of Science and Innovation. VQ,SP, and MH acknowledge that this work has been supported by the Agencia Estatal de Investigación Española (AEI; grant PID2022-138855NB-C33), by the Ministerio de Ciencia e Innovación (MCIN) within the Plan de Recuperación, Transformación y Resiliencia del Gobierno de España through the project ASFAE/2022/001, with funding from European Union NextGenerationEU (PRTR-C17.I1), and by the Generalitat Valenciana (grant PROMETEO CIPROM/2022/49). PSB acknowledges financial support from the from the Spanish Ministry of Science under the projects with references: PID2019-107427GB-C31 and PID2022-138855NB-C31. PVG acknowledges that the project that gave rise to these results received the support of a fellowship from “la Caixa” Foundation (ID 100010434). The fellowship code is B005800. AFM acknowledges support from RYC2021-031099-I and PID2021-123313NA-I00 of MICIN/AEI/10.13039/501100011033/FEDER, UE, NextGenerationEU/PRT. M.A-F. acknowledges support from the Emergia program (EMERGIA20-38888) from Consejería de Universidad, Investigación e Innovación de la Junta de Andalucía. JR acknowledges funding from University of La Laguna through the Margarita Salas Program from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation. BB acknowledges financial from the Grant AST22_4.4, funded by Consejería de Universidad, Investigación e Innovación and Gobierno de España and Unión Europea – NextGenerationEU, and by the research project PID2020-113689GB-I00 financed by MCIN/AEI/10.13039/501100011033. GTR acknowledges financial support from the research project PRE2021-098736, funded by MCIN/AEI/10.13039/501100011033 and FSEs.
PY - 2024/9/13
Y1 - 2024/9/13
N2 - We have learnt in the last decades that the majority of galaxies belong to high density regions interconnected in a sponge-like fashion. This large-scale structure is characterised by clusters, filaments, and walls, where most galaxies concentrate, but also under-dense regions called voids. The void regions and the galaxies within represent an ideal place for the study of galaxy formation and evolution, as they are largely unaffected by the complex physical processes that transform galaxies in high-density environments. The void galaxies may hold the key to answer current challenges to the ΛCDM paradigm as well. The CAVITY survey is a Legacy project approved by the Calar Alto Observatory to obtain spatially resolved spectroscopic information of ∼300 void galaxies in the Local Universe (0.005 < z < 0.050), covering −17.0 to −21.5 in r band absolute magnitude. It officially started in January 2021 and has been awarded 110 useful dark observing nights at the 3.5 m telescope using the PMAS spectrograph. Complementary follow-up projects, including deep optical imaging, integrated as well as resolved CO data, and integrated HI spectra, have joined the PMAS observations and naturally complete the scientific aim of characterising galaxies in cosmic voids. The extension data has been named CAVITY+. The data will be available to the whole community in different data releases, the first of which is planned for July 2024, and it will provide the community with PMAS datacubes for around 100 void galaxies through a user friendly and well documented database platform. Here, we present the survey, sample selection, data reduction, quality control schemes, science goals, and some examples of the scientific power of the CAVITY and CAVITY+ data.
AB - We have learnt in the last decades that the majority of galaxies belong to high density regions interconnected in a sponge-like fashion. This large-scale structure is characterised by clusters, filaments, and walls, where most galaxies concentrate, but also under-dense regions called voids. The void regions and the galaxies within represent an ideal place for the study of galaxy formation and evolution, as they are largely unaffected by the complex physical processes that transform galaxies in high-density environments. The void galaxies may hold the key to answer current challenges to the ΛCDM paradigm as well. The CAVITY survey is a Legacy project approved by the Calar Alto Observatory to obtain spatially resolved spectroscopic information of ∼300 void galaxies in the Local Universe (0.005 < z < 0.050), covering −17.0 to −21.5 in r band absolute magnitude. It officially started in January 2021 and has been awarded 110 useful dark observing nights at the 3.5 m telescope using the PMAS spectrograph. Complementary follow-up projects, including deep optical imaging, integrated as well as resolved CO data, and integrated HI spectra, have joined the PMAS observations and naturally complete the scientific aim of characterising galaxies in cosmic voids. The extension data has been named CAVITY+. The data will be available to the whole community in different data releases, the first of which is planned for July 2024, and it will provide the community with PMAS datacubes for around 100 void galaxies through a user friendly and well documented database platform. Here, we present the survey, sample selection, data reduction, quality control schemes, science goals, and some examples of the scientific power of the CAVITY and CAVITY+ data.
KW - Surveys
KW - Galaxies: general
KW - Galaxies: kinematics and dynamics
KW - Galaxies: photometry
KW - Galaxies: stellar content
KW - Large-scale structure of universe
UR - https://www.scopus.com/pages/publications/85197461832
U2 - 10.1051/0004-6361/202449749
DO - 10.1051/0004-6361/202449749
M3 - Article
SN - 0004-6361
VL - 689
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
M1 - A213
ER -