IMF shape constraints from stellar populations and dynamics from CALIFA

In this Paper, we describe how we use stellar dynamics information to constrain the shape of the stellar initial mass function (IMF) in a sample of 27 early-type galaxies from the CALIFA survey. We obtain dynamical and stellar mass-to-light ratios, γdyn and γ*, over a homogenous aperture of 0.5 Re....

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Detalles Bibliográficos
Autores: Lyubenova, M., Martín-Navarro, I., van de Ven, G., Falcón-Barroso, J., Galbany, L., Gallazzi, A., García-Benito, R., González Delgado, R., Husemann, B., La Barbera, F., Marino, R.A., Mast, Damian, Mendez-Abreu, J., Peletier, R.F.P., Sanchez-Blázquez, P., Sánchez, S.F., Trager, S.C., van den Bosch, R.C.E., Vazdekis, A., Walcher, C.J., Zhu, L., Zibetti, S., Ziegler, B., Bland-Hawthorn, J.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2016
País:Argentina
Institución:Consejo Nacional de Investigaciones Científicas y Técnicas
Repositorio:CONICET Digital (CONICET)
Idioma:inglés
OAI Identifier:oai:ri.conicet.gov.ar:11336/63592
Acceso en línea:http://hdl.handle.net/11336/63592
Access Level:acceso abierto
Palabra clave:ELLIPTICAL AND LENTICULAR, CD
KINEMATICS AND DYNAMICS
STELLAR CONTENT
https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
Descripción
Sumario:In this Paper, we describe how we use stellar dynamics information to constrain the shape of the stellar initial mass function (IMF) in a sample of 27 early-type galaxies from the CALIFA survey. We obtain dynamical and stellar mass-to-light ratios, γdyn and γ*, over a homogenous aperture of 0.5 Re. We use the constraint γdyn ≥ γ* to test two IMF shapes within the framework of the extended MILES stellar population models. We rule out a single power-law IMF shape for 75 per cent of the galaxies in our sample. Conversely, we find that a double power-law IMF shape with a varying high-mass end slope is compatible (within 1σ) with 95 per cent of the galaxies. We also show that dynamical and stellar IMF mismatch factors give consistent results for the systematic variation of the IMF in these galaxies.

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