Bibcode
Sánchez Almeida, J.
Referencia bibliográfica
Monthly Notices of the Royal Astronomical Society
Advertised on:
4
2020
Número de citas
18
Número de citas referidas
17
Descripción
The scatter in the galaxy size versus stellar mass (M⋆) relation gets largely reduced when, rather than the half-mass radius Re, the size at a fixed surface density is used. Here, we address why this happens. We show how a reduction is to be expected because any two galaxies with the same M⋆ have at least one radius with identical surface density, where the galaxies have identical size. However, the reason why the scatter is reduced to the observed level is not trivial, and we pin it down to the galaxy surface density profiles approximately following Sersic profiles with their Re and Sersic index (n) anticorrelated (i.e. given M⋆, n increases when Re decreases). Our analytical results describe very well the behaviour of the observed galaxies as portrayed in the NASA Sloan Atlas (NSA), which contains more than half a million local objects with 7 < log (M⋆/M☉) < 11.5. The comparison with NSA galaxies also allows us to find the optimal values for the mass surface density ( $2.4_{-0.9}^{+1.3}\, M_\odot \, {\rm pc}^{-2}$ ) and surface brightness (r band $24.7\pm 0.5\, {\rm mag\, arcsec^{-2}}$ ) that minimize the scatter, although the actual values depend somehow on the subset of NSA galaxies used for optimization. The physical reason for the existence of optimal values is unknown but, as Trujillo, Chamba & Knapen (2020) point out, they are close to the gas surface density threshold to form stars and thus may trace the physical end of a galaxy. Our NSA-based size-mass relation agrees with theirs on the slope as well as on the magnitude of the scatter. As a by-product of the narrowness of the size-mass relation (only 0.06 dex), we propose to use the size of a galaxy to measure its stellar mass. In terms of observing time, it is not more demanding than the usual photometric techniques and may present practical advantages in particular cases.
Proyectos relacionados
![Imagen compuesta combinando filtros de la galaxia enana CGCG-007, pobre en metales, obtenida con HST / WFC3. Los cúmulos de estrellas supermasivos son extremadamente brillantes en el UV, y está claro que algunos de ellos han fotoionizado y erosionado las nebulosas donde han nacido. Datos del programa GO-15114 (PI Sánchez-Janssen) Imagen del Proyecto](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/project/imagen-cmt.png?itok=W3PG8rhc)
Grupo de Estudios de Formación Estelar GEFE
El proyecto interno GEFE está enmarcado en el proyecto coordinado, ESTALLIDOS, financiado por el plan nacional desde el año 2001. El ultimo proyecto aprobado es ESTALLIDOS 6.0 (AYA2016- 79724-C4-2-P). En el proyecto GEFE trabajamos en base al caso científico del proyecto ESTALLIDOS 6.0. Los estallidos de formación estelar (Starbursts o SB) son
Casiana
Muñoz Tuñón