Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

Hα3 : an Hα imaging survey of HI selected galaxies from ALFALFA. VI. The role of bars in quenching star formation from z = 3 to the present epoch.

Gavazzi, G. and Consolandi, G. and Dotti, M. and Fanali, R. and Fossati, M. and Fumagalli, M. and Viscardi, E. and Savorgnan, G. and Boselli, A. and Gutiérrez, L. and Hernández Toledo, H. and Giovanelli, R. and Haynes, M. P. (2015) 'Hα3 : an Hα imaging survey of HI selected galaxies from ALFALFA. VI. The role of bars in quenching star formation from z = 3 to the present epoch.', Astronomy and astrophysics., 580 . A116.

Abstract

A growing body of evidence indicates that the star formation rate per unit stellar mass (sSFR) decreases with increasing mass in normal main-sequence star-forming galaxies. Many processes have been advocated as being responsible for this trend (also known as mass quenching), e.g., feedback from active galactic nuclei (AGNs), and the formation of classical bulges. In order to improve our insight into the mechanisms regulating the star formation in normal star-forming galaxies across cosmic epochs, we determine a refined star formation versus stellar mass relation in the local Universe. To this end we use the Hα narrow-band imaging follow-up survey (Hα3) of field galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Coma and Local superclusters. By complementing this local determination with high-redshift measurements from the literature, we reconstruct the star formation history of main-sequence galaxies as a function of stellar mass from the present epoch up to z = 3. In agreement with previous studies, our analysis shows that quenching mechanisms occur above a threshold stellar mass Mknee that evolves with redshift as ∝ (1 + z)2. Moreover, visual morphological classification of individual objects in our local sample reveals a sharp increase in the fraction of visually classified strong bars with mass, hinting that strong bars may contribute to the observed downturn in the sSFR above Mknee. We test this hypothesis using a simple but physically motivated numerical model for bar formation, finding that strong bars can rapidly quench star formation in the central few kpc of field galaxies. We conclude that strong bars contribute significantly to the red colors observed in the inner parts of massive galaxies, although additional mechanisms are likely required to quench the star formation in the outer regions of massive spiral galaxies. Intriguingly, when we extrapolate our model to higher redshifts, we successfully recover the observed redshift evolution for Mknee. Our study highlights how the formation of strong bars in massive galaxies is an important mechanism in regulating the redshift evolution of the sSFR for field main-sequence galaxies.

Item Type:Article
Keywords:Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: star formation.
Full text:(VoR) Version of Record
Download PDF
(1249Kb)
Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1051/0004-6361/201425351
Publisher statement:Reproduced with permission from Astronomy & Astrophysics, © ESO 2015
Date accepted:25 May 2015
Date deposited:20 August 2015
Date of first online publication:August 2015
Date first made open access:No date available

Save or Share this output

Export:
Export
Look up in GoogleScholar