The structural properties of classical bulges and discs from z ̃ 2

Bibcode
2019MNRAS.489.4135D
DOI
10.1093/mnras/stz2421
Dimauro, Paola; Huertas-Company, Marc; Daddi, Emanuele; Pérez-González, Pablo G.; Bernardi, Mariangela; Caro, Fernando; Cattaneo, Andrea; Häußler, Boris; Kuchner, Ulrike; Shankar, Francesco; Barro, Guillermo; Buitrago, Fernando; Faber, Sandra M.; Kocevski, Dale D.; Koekemoer, Anton M.; Koo, David C.; Mei, Simona; Peletier, Reynier; Primack, Joel; Rodriguez-Puebla, Aldo; Salvato, Mara; Tuccillo, Diego
Bibliographical reference

Monthly Notices of the Royal Astronomical Society

Advertised on:
11
2019
Journal
Monthly Notices of the Royal Astronomical Society
Number of authors
22
IAC number of authors
1
Citations
14
Refereed citations
14
Description
We study the rest-frame optical mass-size relation of bulges and discs from z ̃ 2 to z ̃ 0 for a complete sample of massive galaxies in the CANDELS fields using two-component Sérsic models. Discs and star-forming galaxies follow similar mass-size relations. The mass-size relation of bulges is less steep than the one of quiescent galaxies (best-fitting slope of 0.7 for quiescent galaxies against 0.4 for bulges). We find little dependence of the structural properties of massive bulges and discs with the global morphology of galaxies (disc versus bulge dominated) and the star formation activity (star-forming versus quiescent). This result suggests similar bulge formation mechanisms for most massive galaxies and also that the formation of the bulge component does not significantly affect the disc structure. Our results pose a challenge to current cosmological models that predict distinct structural properties for stellar bulges arising from mergers and disc instabilities.
Related projects
Group members
Traces of Galaxy Formation: Stellar populations, Dynamics and Morphology

We are a large, diverse, and very active research group aiming to provide a comprehensive picture for the formation of galaxies in the Universe. Rooted in detailed stellar population analysis, we are constantly exploring and developing new tools and ideas to understand how galaxies came to be what we now observe.

Ignacio
Martín Navarro
In progress
Type
Refereed
Galaxies

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