Skip to content
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies
Monthly Notices of the Royal Astronomical Society, Volume 477, No. 3, Year 2018
Notification
URL copied to clipboard!
Description
We study radial profiles in Ha equivalent width and specific star formation rate (sSFR) derived from spatially resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-M* diagram. Even within the star-forming 'main sequence', the measured sSFR decreases with stellar mass, in both an integrated and spatially resolved sense. Flat sSFR radial profiles are observed for log(M*/M⊙) < 10.5, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of log(M*/M⊙) > 10.0 are classified spectroscopically as central low-ionization emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star-forming galaxies with the sameM* and Σ1 kpc (the mass surface density within 1 kpc), we show that a high Σ1 kpc is not a sufficient condition for determining central quiescence. © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
Authors & Co-Authors
Belfiore, Francesco M.C.
United States, Santa Cruz
University of California, Santa Cruz
United Kingdom, Cambridge
University of Cambridge
Maiolino, Roberto
United Kingdom, Cambridge
University of Cambridge
Bundy, Kevin A.
United States, Santa Cruz
University of California, Santa Cruz
Masters, Karen L.
United Kingdom, Portsmouth
University of Portsmouth
Bershady, Matthew A.
United States, Madison
University of Wisconsin-madison
Oyarzun, Grecco A.
United States, Santa Cruz
University of California, Santa Cruz
Lin, Lihwai
Taiwan, Nankang
Academia Sinica Taiwan
Cano-Díaz, Mariana
Mexico, Mexico
Universidad Nacional Autónoma de México
Wake, David A.
United States, Asheville
The University of North Carolina at Asheville
United Kingdom, Milton Keynes
The Open University
Thomas, Daniel B.
United Kingdom, Portsmouth
University of Portsmouth
Brownstein, Joel R.
United States, Salt Lake City
The University of Utah
Drory, Niv
United States, Austin
The University of Texas at Austin
Yan, Renbin
United States, Lexington
University of Kentucky
Statistics
Citations: 105
Authors: 13
Affiliations: 11
Identifiers
Doi:
10.1093/mnras/sty768
ISSN:
00358711
Research Areas
Environmental