Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 498, Issue 3, Pages 4345-4355Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa2488
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: star formation
Categories
Funding
- European Southern Observatory -Government of Chile JointCommittee
- Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Innovation and Technology (MOIT)
- Debre Birhan University
- Spanish MEC [AYA2016-76682-C3-1-P]
- State Agency for Research of the Spanish MCIU through the `Center of Excellence Severo Ochoa' award [SEV-2017-0709, `CONICYT+PCI+REDES 190194, CONICYT+PCI + INSTITUTO MAX PLANCK DE ASTRONOMIA MPG190030]
- FONDECYT [1191124]
- Leverhulme Trust
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University, University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University
- Pennsylvania State University, University of Portsmouth
- Princeton University
- Spanish Participation Group, University of Tokyo, University of Utah
- Yale University - National Aeronautics and Space Administration
Ask authors/readers for more resources
We study a sample of 48 127 galaxies selected from the SDSS MPA-JHU catalogue, with log M-star/M-circle dot = 10.73-11.03 and z < 0.1. Local galaxies in this stellar mass range have been shown to have systematically shorter assembly times within their inner regions (<0.5 R-50) when compared to that of the galaxy as a whole, contrary to lower or higher mass galaxies that show consistent assembly times at all radii. Hence, we refer to these galaxies as Inside-Out Assembled Galaxy (IOAG) candidates. We find that the majority of IOAG candidates with well-detected emission lines are classified as either active galactic nucleus (AGN; 40 per cent) or composite (40 per cent) in the BPT (Baldwin, Phillips & Terlevich) diagram. We also find that the majority of our sources are located below the main sequence of star formation, and within the green valley or red sequence. Most BPT-classified star-forming IOAG candidates have spiral morphologies and are in the main sequence, whereas Seyfert 2 and composites have mostly spiral morphologies but quiescent star formation rates (SFRs). We argue that a high fraction of IOAG candidates seem to be in the process of quenching, moving from the blue cloud to the red sequence. Those classified as AGN have systematically lower SFRs than star-forming galaxies, suggesting that AGN activity may be related to this quenching. However, the spiral morphology of these galaxies remains in place, suggesting that the central star formation is suppressed before the morphological transformation occurs.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available