SDSS IV MaNGA - sSFR profiles and the slow quenching of discs in green valley galaxies

被引:141
作者
Belfiore, Francesco [1 ,2 ,3 ]
Maiolino, Roberto [2 ,3 ]
Bundy, Kevin [1 ]
Masters, Karen [4 ]
Bershady, Matthew [5 ]
Oyarzun, Grecco A. [1 ]
Lin, Lihwai [6 ]
Cano-Diaz, Mariana [7 ]
Wake, David [8 ,9 ]
Spindler, Ashley [9 ]
Thomas, Daniel [4 ]
Brownstein, Joel R. [10 ]
Drory, Niv [11 ]
Yan, Renbin [12 ]
机构
[1] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 USA
[2] Univ Cambridge, Cavendish Astrophys, Cambridge CB3 0HE, England
[3] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HE, England
[4] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England
[5] Univ Wisconsin, Dept Astron, 475 Charter St, Madison, WI 53706 USA
[6] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan
[7] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, DF, Mexico
[8] Univ N Carolina, Dept Phys, One Univ Hts, Asheville, NC 28804 USA
[9] Open Univ, Walton Hall, Milton Keynes MK7 6AA, Bucks, England
[10] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA
[11] Univ Texas Austin, McDonald Observ, 2515 Speedway Stop C1402, Austin, TX 78712 USA
[12] Univ Kentucky, Dept Phys & Astron, 505 Rose St, Lexington, KY 40506 USA
基金
美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会;
关键词
galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM; DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; COLOR-MAGNITUDE DIAGRAM; ACTIVE GALACTIC NUCLEI; INTEGRAL FIELD SPECTROSCOPY; LOCAL UNIVERSE; HOST GALAXIES; FORMATION HISTORIES; PHYSICAL-PROPERTIES; SPIRAL GALAXIES;
D O I
10.1093/mnras/sty768
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We study radial profiles in H alpha equivalent width and specific star formation rate (sSFR) derived from spatially resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-M-star diagram. Even within the star-forming 'main sequence', the measured sSFR decreases with stellar mass, in both an integrated and spatially resolved sense. Flat sSFR radial profiles are observed for log(M-star/M-circle dot) < 10.5, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of log(M-star/M-circle dot) > 10.0 are classified spectroscopically as central low-ionization emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star-forming galaxies with the same M-star and Sigma(1 kpc) (the mass surface density within 1 kpc), we show that a high Sigma(1 kpc) is not a sufficient condition for determining central quiescence.
引用
收藏
页码:3014 / 3029
页数:16
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