The SAMI Galaxy Survey : spatially resolving the main sequence of star formation

We present the ∼800 star formation rate maps for the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey based on H α emission maps, corrected for dust attenuation via the Balmer decrement, that are included in the SAMI Public Data Release 1. We mask out spaxels contaminated by...

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Bibliographic Details
Published in:Monthly Notices of the Royal Astronomical Society
Main Authors: Medling, Anne M., Cortese, Luca, Croom, Scott M., Green, Andrew W., Groves, Brent, Hampton, Elise, Ho, I-Ting, Davies, Luke J. M., Kewley, Lisa J., Moffett, Amanda J., Schaefer, Adam L., Taylor, Edward, Zafar, Tayyaba, Bekki, Kenji, Bland-Hawthorn, Joss, Bloom, Jessica V., Brough, Sarah, Bryant, Julia J., Catinella, Barbara, Cecil, Gerald, Colless, Matthew, Couch, Warrick J., Drinkwater, Michael J., Driver, Simon P., Federrath, Christoph, Foster, Caroline, Goldstein, Gregory, Goodwin, Michael, Hopkins, Andrew, Lawrence, J. S., Leslie, Sarah K., Lewis, Geraint F., Lorente, Nuria P. F., Owers, Matt S., McDermid, Richard, Richards, Samuel N., Sharp, Robert, Scott, Nicholas, Sweet, Sarah M., Taranu, Dan S., Tescari, Edoardo, Tonini, Chiara, Sande, Jesse van de, Walcher, C. Jakob, Wright, Angus
Other Authors: University of St Andrews. School of Physics and Astronomy
Format: Article in Journal/Newspaper
Language:English
Published: 2018
Subjects:
Surveys
Galaxies: evolution
Galaxies: star formation
QB Astronomy
QC Physics
DAS
QB
QC
sami
Online Access:http://hdl.handle.net/10023/12963
https://doi.org/10.1093/mnras/sty127
Description
Summary:We present the ∼800 star formation rate maps for the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey based on H α emission maps, corrected for dust attenuation via the Balmer decrement, that are included in the SAMI Public Data Release 1. We mask out spaxels contaminated by non-stellar emission using the [O iii]/H β, [N ii]/H α, [S ii]/H α, and [O i]/H α line ratios. Using these maps, we examine the global and resolved star-forming main sequences of SAMI galaxies as a function of morphology, environmental density, and stellar mass. Galaxies further below the star-forming main sequence are more likely to have flatter star formation profiles. Early-type galaxies split into two populations with similar stellar masses and central stellar mass surface densities. The main-sequence population has centrally concentrated star formation similar to late-type galaxies, while galaxies >3σ below the main sequence show significantly reduced star formation most strikingly in the nuclear regions. The split populations support a two-step quenching mechanism, wherein halo mass first cuts off the gas supply and remaining gas continues to form stars until the local stellar mass surface density can stabilize the reduced remaining fuel against further star formation. Across all morphologies, galaxies in denser environments show a decreased specific star formation rate from the outside in, supporting an environmental cause for quenching, such as ram-pressure stripping or galaxy interactions. Publisher PDF Peer reviewed

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