인문학
사회과학
자연과학
공학
의약학
농수해양학
예술체육학
복합학
DBpia AI
AI 에이전트
AI 아이디어
AI 리더
AI 뷰어
Citeasy
크롬 서지관리 다운로드
지원사업
학술연구/단체지원/교육 등 연구자 활동을 지속하도록 DBpia가 지원하고 있어요.
커뮤니티
연구자들이 자신의 연구와 전문성을 널리 알리고, 새로운 협력의 기회를 만들 수 있는 네트워킹 공간이에요.
초록·키워드
Context. Bars are ubiquitously found in disc galaxies and they are known to drive galaxy evolution through secular processes. However, the specific contribution of the bars in the suppression of star formation is still a matter of debate. Aims. Our aim is to investigate the role of bars in quenching star formation using spatially resolved UV-optical colour maps and radial colour profiles of a sample of 17 centrally quenched barred galaxies in the redshift range of 0.02–0.06. Methods. We selected the sample of centrally quenched barred galaxies based on their location in the SFR-M ⋆ plane. They are classified as passive based on the parameters from the Max Planck Institute for Astrophysics (MPA) and Johns Hopkins University (JHU) value-added catalogue (MPA – JHU VAC); however, they have also been classified as non-passive based on the parameters from the GALEX-SDSS-WISE Legacy (GSWLC) catalogue, indicating a passive inner region and recent star formation in their extended disc. We used the archival SDSS optical r-band and GALEX far- and near- ultraviolet (FUV and NUV) imaging data of these galaxies and created spatially resolved (FUV−NUV versus NUV−r) colour-colour maps to understand the nature of the UV emission from different regions of these galaxies. We also analysed their NUV−r colour radial profiles and use the NUV−r colour as a proxy for the stellar population age in the different regions of these galaxies. We also analysed a control sample of eight centrally quenched unbarred galaxies to disentangle the effect of bulge and bar in quenching star formation. Results. The centrally quenched barred galaxies display redder colours (NUV−r > 4 – 4.5 mag) in the inner regions, up to the length of the bar, indicating the age of the stellar population in these regions is older than > 1 Gyr. Most barred galaxies in our sample host pseudo-bulges and do not host an active galactic nucleus (AGN), indicating that the most probable reason for the internal quenching of these galaxies is the action of stellar bar. In comparison to their unbarred counterparts, lying in a similar regime of stellar mass and redshifts, the barred galaxies show redder colours (NUV−r > 4 mag) to a larger spatial extent. Conclusions. In their later stages of evolution, bars turn the inner regions of galaxies redder, leading to quenching, with the effect being most prominent up to the ends of the bar and creating a region dominated by older stellar population. This may occur because bars have already funneled gas to the galactic centre leaving behind no fuel for further star formation. Spatially resolved studies of a larger sample of barred galaxies at different redshifts will provide more insights to the role of bar in quenching star formation and the different evolutionary stages of quenching.
인공지능 문자 인식 모델을 통해 추출된 텍스트로, 일부 오타나 오류가 포함될 수 있으나 지속적으로 개선 중입니다.
오류를 발견하셨다면 해당 부분을 드래그한 후 ' 를 통해 신고해주세요.
오류를 발견하셨다면 해당 부분을 드래그한 후 ' 를 통해 신고해주세요.
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