Axillary Surgery

Bloom, Sara A.; Manasseh, Donna‐Marie

doi:10.1016/b978-141602951-9.50057-8

Cited by 1 publication

(1 citation statement)

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“…Because star formation rates are most affected on the outskirts of the galaxy, we favor stripping as the dominant mechanism; however, we cannot rule out the possibility that these processes operate in tandem. Bloom et al (2017) found that SAMI galaxies with kinematic asymmetries have more centrally-concentrated star formation, which may simply be due to galaxy-galaxy interactions triggering enhanced central star formation (e.g. Bekki & Couch 2011;Ellison et al 2013;Moreno et al 2015) and/or stripping gas from the outskirts.…”

Section: The Radial Component Of Environmental Effectsmentioning

confidence: 99%

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

Medling

Cortese

Croom

et al. 2018

Monthly Notices of the Royal Astronomical Society

116

103

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We present the ∼800 star formation rate maps for the SAMI Galaxy Survey based on Hα 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]/Hβ, [N II]/Hα, [S II]/Hα, and [O I]/Hα 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.

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Section: The Radial Component Of Environmental Effectsmentioning

confidence: 99%