On the interplay between star formation and feedback in galaxy formation simulations
(2015) In Astrophysical Journal 804(1).- Abstract
We investigate the star formation-feedback cycle in cosmological galaxy formation simulations, focusing on the progenitors of Milky Way (MW)-sized galaxies. We find that in order to reproduce key properties of the MW progenitors, such as semi-empirically derived star formation histories (SFHs) and the shape of rotation curves, our implementation of star formation and stellar feedback requires (1) a combination of local early momentum feedback via radiation pressure and stellar winds, and subsequent efficient supernovae feedback, and (2) an efficacy of feedback that results in the self-regulation of the global star formation rate on kiloparsec scales. We show that such feedback-driven self-regulation is achieved globally for a local star... (More)
We investigate the star formation-feedback cycle in cosmological galaxy formation simulations, focusing on the progenitors of Milky Way (MW)-sized galaxies. We find that in order to reproduce key properties of the MW progenitors, such as semi-empirically derived star formation histories (SFHs) and the shape of rotation curves, our implementation of star formation and stellar feedback requires (1) a combination of local early momentum feedback via radiation pressure and stellar winds, and subsequent efficient supernovae feedback, and (2) an efficacy of feedback that results in the self-regulation of the global star formation rate on kiloparsec scales. We show that such feedback-driven self-regulation is achieved globally for a local star formation efficiency per free fall time of . Although this value is larger that the value usually inferred from the Kennicutt-Schmidt (KS) relation, we show that it is consistent with direct observational estimates of in molecular clouds. Moreover, we show that simulations with local efficiency of reproduce the global observed KS relation. Such simulations also reproduce the cosmic SFH of the MW-sized galaxies and satisfy a number of other observational constraints. Conversely, we find that simulations that a priori assume an inefficient mode of star formation, instead of achieving it via stellar feedback regulation, fail to produce sufficiently vigorous outflows and do not reproduce observations. This illustrates the importance of understanding the complex interplay between star formation and feedback, and the detailed processes that contribute to the feedback-regulated formation of galaxies.
(Less)
- author
- Agertz, Oscar LU and Kravtsov, Andrey V.
- publishing date
- 2015-05-01
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- galaxies: evolution, galaxies: formation, galaxies: high-redshift, galaxies: star formation, galaxies: stellar content, methods: numerical
- in
- Astrophysical Journal
- volume
- 804
- issue
- 1
- article number
- 18
- publisher
- American Astronomical Society
- external identifiers
-
- scopus:84936775885
- ISSN
- 0004-637X
- DOI
- 10.1088/0004-637X/804/1/18
- language
- English
- LU publication?
- no
- id
- e4277769-f956-41f5-bc90-c1c6bd948f44
- date added to LUP
- 2016-08-16 22:57:58
- date last changed
- 2022-03-01 03:05:41
@article{e4277769-f956-41f5-bc90-c1c6bd948f44,
abstract = {{<p>We investigate the star formation-feedback cycle in cosmological galaxy formation simulations, focusing on the progenitors of Milky Way (MW)-sized galaxies. We find that in order to reproduce key properties of the MW progenitors, such as semi-empirically derived star formation histories (SFHs) and the shape of rotation curves, our implementation of star formation and stellar feedback requires (1) a combination of local early momentum feedback via radiation pressure and stellar winds, and subsequent efficient supernovae feedback, and (2) an efficacy of feedback that results in the self-regulation of the global star formation rate on kiloparsec scales. We show that such feedback-driven self-regulation is achieved globally for a local star formation efficiency per free fall time of . Although this value is larger that the value usually inferred from the Kennicutt-Schmidt (KS) relation, we show that it is consistent with direct observational estimates of in molecular clouds. Moreover, we show that simulations with local efficiency of reproduce the global observed KS relation. Such simulations also reproduce the cosmic SFH of the MW-sized galaxies and satisfy a number of other observational constraints. Conversely, we find that simulations that a priori assume an inefficient mode of star formation, instead of achieving it via stellar feedback regulation, fail to produce sufficiently vigorous outflows and do not reproduce observations. This illustrates the importance of understanding the complex interplay between star formation and feedback, and the detailed processes that contribute to the feedback-regulated formation of galaxies.</p>}},
author = {{Agertz, Oscar and Kravtsov, Andrey V.}},
issn = {{0004-637X}},
keywords = {{galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: star formation; galaxies: stellar content; methods: numerical}},
language = {{eng}},
month = {{05}},
number = {{1}},
publisher = {{American Astronomical Society}},
series = {{Astrophysical Journal}},
title = {{On the interplay between star formation and feedback in galaxy formation simulations}},
url = {{http://dx.doi.org/10.1088/0004-637X/804/1/18}},
doi = {{10.1088/0004-637X/804/1/18}},
volume = {{804}},
year = {{2015}},
}