The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching
The mechanism by which galaxies stop forming stars and get rid of their interstellar medium (ISM) remains elusive. Here, we study a sample of more than two thousand elliptical galaxies in which dust emission has been detected. This is the largest sample of such galaxies ever analysed. We infer the t...
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| creator | Leśniewska, Aleksandra Michałowski, Michał Jerzy Gall, Christa Hjorth, Jens Nadolny, Jakub Ryzhov, Oleh Solar, Martin |
| description | The mechanism by which galaxies stop forming stars and get rid of their interstellar medium (ISM) remains elusive. Here, we study a sample of more than two thousand elliptical galaxies in which dust emission has been detected. This is the largest sample of such galaxies ever analysed. We infer the timescale for removal of dust in these galaxies and investigate its dependency on physical and environmental properties. We obtain a dust removal timescale in elliptical galaxies of \(\tau\) = 2.26 \(\pm\) 0.18 Gyr, corresponding to a half-life time of 1.57 \(\pm\) 0.12 Gyr. This timescale does not depend on environment, stellar mass or redshift. We observe a departure of dusty elliptical galaxies from the star formation rate vs. dust mass relation. This is caused by the star-formation rates declining faster than the dust masses and indicates that there exists an internal mechanism, which affects star formation, but leaves the ISM intact. Morphological quenching together with ionisation or outflows caused by older stellar populations (supernova type Ia or planetary nebulae) are consistent with these observations. |
| doi_str_mv | 10.48550/arxiv.2306.05774 |
| format | Article |
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We obtain a dust removal timescale in elliptical galaxies of \(\tau\) = 2.26 \(\pm\) 0.18 Gyr, corresponding to a half-life time of 1.57 \(\pm\) 0.12 Gyr. This timescale does not depend on environment, stellar mass or redshift. We observe a departure of dusty elliptical galaxies from the star formation rate vs. dust mass relation. This is caused by the star-formation rates declining faster than the dust masses and indicates that there exists an internal mechanism, which affects star formation, but leaves the ISM intact. 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| subjects | Cosmic dust Dust Dust control Elliptical galaxies Interstellar matter Morphology Physics - Astrophysics of Galaxies Planetary nebulae Quenching Red shift Star & galaxy formation Star formation rate Stellar mass Stellar populations Time |
| title | The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching |
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