{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:Y2PZDBBVYYHCITVSSBWEFMCLV3","short_pith_number":"pith:Y2PZDBBV","schema_version":"1.0","canonical_sha256":"c69f918435c60e244eb2906c42b04baecd928541d639547e7d19b981b401b09a","source":{"kind":"arxiv","id":"1607.08245","version":1},"attestation_state":"computed","paper":{"title":"Evidence of Bar-induced Secular Evolution in the Inner Regions of Stellar Discs in Galaxies: What Shapes Disc Galaxies?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Albert Bosma, Dimitri A. Gadotti, E. Athanassoula, Kartik Sheth, Myung Gyoon Lee, Taehyun Kim","submitted_at":"2016-07-27T20:00:08Z","abstract_excerpt":"We present evidence of bar-induced secular evolution in galactic discs using 3.6 ${\\mu m}$ images of nearby galaxies from the Spitzer Survey of Stellar Structure in Galaxies (S4G). We find that among massive galaxies ($M_{star}/M_{sun}> 10^{10}$), longer bars tend to reside in inner discs having a flatter radial profile. Such galaxies show a light deficit in the disc surrounding the bar, within the bar radius and often show a $\\Theta$-shaped morphology. We quantify this deficit and find that among all galaxies explored in this study (with $10^{9} 10^{10}$), longer bars tend to reside in inner discs having a flatter radial profile. Such galaxies show a light deficit in the disc surrounding the bar, within the bar radius and often show a $\\Theta$-shaped morphology. We quantify this deficit and find that among all galaxies explored in this study (with $10^{9}