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Hierarchical models of high-redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations

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Hierarchical models of high-redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations. / Tonini, Chiara; Maraston, Claudia; Thomas, Daniel; Devriendt, J.; Silk, J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 403, No. 4, 2010, p. 1749-1758.

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Tonini, Chiara ; Maraston, Claudia ; Thomas, Daniel ; Devriendt, J. ; Silk, J. / Hierarchical models of high-redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations. In: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 403, No. 4. pp. 1749-1758.

Bibtex

@article{1ada1fa9c40d4c6f8505eff77052bfea,
title = "Hierarchical models of high-redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations",
abstract = "In a recent paper, we presented the first semi-analytic model of galaxy formation in which the thermally pulsing asymptotic giant branch (TP-AGB) phase of stellar evolution has been fully implemented. Here, we address the comparison with observations, and show how the TP-AGB recipe affects the performance of the model in reproducing the colours and near-infrared luminosities of high-redshift galaxies. We find that the semi-analytic model with the TP-AGB better matches the colour–magnitude and colour–colour relations at z∼ 2, both for nearly passive and for star-forming galaxies. The model with TP-AGB produces star-forming galaxies with red V−K colours, thus revising the unique interpretation of high-redshift red objects as ‘red and dead’. We also show that without the TP-AGB the semi-analytic model fails at reproducing the observed colours, a situation that cannot be corrected by dust reddening. We also explore the effect of nebular emission on the predicted colour–magnitude relation of star-forming galaxies, to conclude that it does not play a significant role in reddening their colours, at least in the range of star-formation rates covered by the model. Finally, the rest-frame K-band luminosity function at z∼ 2.5 is more luminous by almost 1 mag. This indicates that the active galactic nuclei feedback recipe that is adopted to regulate the high-mass end of the luminosity function should be sophisticated to take the effect of the stellar populations into account at high redshifts.",
author = "Chiara Tonini and Claudia Maraston and Daniel Thomas and J. Devriendt and J. Silk",
year = "2010",
doi = "10.1111/j.1365-2966.2009.16231.x",
language = "English",
volume = "403",
pages = "1749--1758",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Hierarchical models of high-redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations

AU - Tonini, Chiara

AU - Maraston, Claudia

AU - Thomas, Daniel

AU - Devriendt, J.

AU - Silk, J.

PY - 2010

Y1 - 2010

N2 - In a recent paper, we presented the first semi-analytic model of galaxy formation in which the thermally pulsing asymptotic giant branch (TP-AGB) phase of stellar evolution has been fully implemented. Here, we address the comparison with observations, and show how the TP-AGB recipe affects the performance of the model in reproducing the colours and near-infrared luminosities of high-redshift galaxies. We find that the semi-analytic model with the TP-AGB better matches the colour–magnitude and colour–colour relations at z∼ 2, both for nearly passive and for star-forming galaxies. The model with TP-AGB produces star-forming galaxies with red V−K colours, thus revising the unique interpretation of high-redshift red objects as ‘red and dead’. We also show that without the TP-AGB the semi-analytic model fails at reproducing the observed colours, a situation that cannot be corrected by dust reddening. We also explore the effect of nebular emission on the predicted colour–magnitude relation of star-forming galaxies, to conclude that it does not play a significant role in reddening their colours, at least in the range of star-formation rates covered by the model. Finally, the rest-frame K-band luminosity function at z∼ 2.5 is more luminous by almost 1 mag. This indicates that the active galactic nuclei feedback recipe that is adopted to regulate the high-mass end of the luminosity function should be sophisticated to take the effect of the stellar populations into account at high redshifts.

AB - In a recent paper, we presented the first semi-analytic model of galaxy formation in which the thermally pulsing asymptotic giant branch (TP-AGB) phase of stellar evolution has been fully implemented. Here, we address the comparison with observations, and show how the TP-AGB recipe affects the performance of the model in reproducing the colours and near-infrared luminosities of high-redshift galaxies. We find that the semi-analytic model with the TP-AGB better matches the colour–magnitude and colour–colour relations at z∼ 2, both for nearly passive and for star-forming galaxies. The model with TP-AGB produces star-forming galaxies with red V−K colours, thus revising the unique interpretation of high-redshift red objects as ‘red and dead’. We also show that without the TP-AGB the semi-analytic model fails at reproducing the observed colours, a situation that cannot be corrected by dust reddening. We also explore the effect of nebular emission on the predicted colour–magnitude relation of star-forming galaxies, to conclude that it does not play a significant role in reddening their colours, at least in the range of star-formation rates covered by the model. Finally, the rest-frame K-band luminosity function at z∼ 2.5 is more luminous by almost 1 mag. This indicates that the active galactic nuclei feedback recipe that is adopted to regulate the high-mass end of the luminosity function should be sophisticated to take the effect of the stellar populations into account at high redshifts.

U2 - 10.1111/j.1365-2966.2009.16231.x

DO - 10.1111/j.1365-2966.2009.16231.x

M3 - Article

VL - 403

SP - 1749

EP - 1758

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 4

ER -

ID: 70072