The CALIFA view on stellar angular momentum across the Hubble sequence

• Autores: Falcón Barroso, J.; Van De Ven, G.; Lyubenova, M.; Mendez Abreu, J.; Aguerri, J.A.L.; García Lorenzo, B.; Bekeraité, S.; Sánchez, S.F.; Husemann, B.; García Benito, R.; González Delgado, R.M.; Mast, Damian; Walcher, C.J.; Zibetti, S.; Zhu, L.; Barrera Ballesteros, J.K.; Galbany, L.; Sánchez Blázquez, P.; Singh, R.; Van Den Bosch, R.C.E.; Wild, V.; Bland Hawthorn, J.; Cid Fernandes, R.; De Lorenzo Cáceres, A.; Gallazzi, A.; Marino, Ricardo Alberto; Márquez, I.; Peletier, R.F.; Pérez, E.; Pérez, I.; Roth, M.M.; Rosales Ortega, F.F.; Ruiz Lara, T.; Wisotzki, L.; Ziegler, B.
• Año de publicación: 2019
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: CD; ELLIPTICAL AND LENTICULAR; GALAXIES; GALAXIES; GALAXIES: EVOLUTION; GALAXIES: FORMATION; GALAXIES: SPIRAL; GALAXIES: STRUCTURE; KINEMATICS AND DYNAMICS
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

We present the apparent stellar angular momentum over the optical extent of 300 galaxies across the Hubble sequence using integral-field spectroscopic (IFS) data from the CALIFA survey. Adopting the same λR parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies are almost all fast rotators, as expected. Given the extent of our data, we provide relations for λR measured in different apertures (e.g. fractions of the effective radius: 0.5 Re, Re, 2 Re), including conversions to long-slit 1D apertures. Our sample displays a wide range of λRe values, consistent with previous IFS studies. The fastest rotators are dominated by relatively massive and highly star-forming Sb galaxies, which preferentially reside in the main star-forming sequence. These galaxies reach λRe values of ∼0.85, and they are the largest galaxies at a given mass, while also displaying some of the strongest stellar population gradients. Compared to the population of S0 galaxies, our findings suggest that fading may not be the dominant mechanism transforming spirals into lenticulars. Interestingly, we find that λRe decreases for late-type Sc and Sd spiral galaxies, with values that occasionally set them in the slow-rotator regime. While for some of them this can be explained by their irregular morphologies and/or face-on configurations, others are edge-on systems with no signs of significant dust obscuration. The latter are typically at the low-mass end, but this does not explain their location in the classical (V/σ, ε) and (λRe, ε) diagrams. Our initial investigations, based on dynamical models, suggest that these are dynamically hot disks, probably influenced by the observed important fraction of dark matter within Re.
Fil: Falcón Barroso, J.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Van De Ven, G.. Vienna University of Technology; Austria
Fil: Lyubenova, M.. European Southern Observatory ; Alemania
Fil: Mendez Abreu, J.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Aguerri, J.A.L.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: García Lorenzo, B.. Instituto Astrofisico de Canarias; España. Universidad de La Laguna; España
Fil: Bekeraité, S.. Leibniz Institut für Astrophysik Potsdam; Alemania
Fil: Sánchez, S.F.. Universidad Nacional Autónoma de México; México
Fil: Husemann, B.. Max Planck Institut Fur Astronomie; Alemania
Fil: García Benito, R.. Instituto de Astrofísica de Andalucía; España
Fil: González Delgado, R.M.. Instituto de Astrofísica de Andalucía; España
Fil: Mast, Damian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Walcher, C.J.. Leibniz Institut für Astrophysik Potsdam; Alemania
Fil: Zibetti, S.. Osservatorio Astrofisico Di Arcetri; Italia
Fil: Zhu, L.. Chinese Academy of Sciences; República de China
Fil: Barrera Ballesteros, J.K.. Universidad Nacional Autónoma de México; México
Fil: Galbany, L.. University of Pittsburgh; Estados Unidos
Fil: Sánchez Blázquez, P.. Universidad Autónoma de Madrid; España
Fil: Singh, R.. Max-Planck-Institut für Astronomie; Alemania
Fil: Van Den Bosch, R.C.E.. Max-Planck-Institut für Astronomie; Alemania
Fil: Wild, V.. University of St. Andrews; Reino Unido
Fil: Bland Hawthorn, J.. Centre of Excellence for All-sky Astrophysics in 3D; Australia. University of Sydney; Australia
Fil: Cid Fernandes, R.. Universidade Federal de Santa Catarina; Brasil
Fil: De Lorenzo Cáceres, A.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
Fil: Gallazzi, A.. Osservatorio Astrofisico di Arcetri; Italia
Fil: Marino, Ricardo Alberto. Zürich Institute for Astronomy; Suiza
Fil: Márquez, I.. Instituto de Astrofísica de Andalucía ; España
Fil: Peletier, R.F.. University of Groningen; Países Bajos
Fil: Pérez, E.. Instituto de Astrofísica de Andalucía ; España
Fil: Pérez, I.. Universidad de Granada. Facultad de Ciencias. Departamento de Electromagnetismo y Física de la Materia. Instituto "Carlos I" de Física Teórica y Computacional; España
Fil: Roth, M.M.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Rosales Ortega, F.F.. Instituto Nacional de Astrofísica, Óptica y Electrónica; México
Fil: Ruiz Lara, T.. Instituto de Astrofísica de Canarias; España. Universidad de La Laguna; España
Fil: Wisotzki, L.. Leibniz-Institut für Astrophysik Potsdam; Alemania
Fil: Ziegler, B.. Vienna University of Technology; Austria