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P-MaNGA : gradients in recent star formation histories as diagnostics for galaxy growth and death

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1502.07040v1_li_2015.pdf (1.443Mb)
Date
11/05/2015
Author
Li, Cheng
Wang, Enci
Lin, Lin
Bershady, Matthew A.
Bundy, Kevin
Tremonti, Christy A.
Xiao, Ting
Yan, Renbin
Bizyaev, Dmitry
Blanton, Michael
Cales, Sabrina
Cherinka, Brian
Cheung, Edmond
Drory, Niv
Emsellem, Eric
Fu, Hai
Gelfand, Joseph
Law, David R.
Lin, Lihwai
MacDonald, Nick
Maraston, Claudia
Masters, Karen L.
Merrifield, Michael R.
Pan, Kaike
Sanchez, S. F.
Schneider, Donald P.
Thomas, Daniel
Wake, David
Wang, Lixin
Weijmans, Anne-Marie
Wilkinson, David
Yoachim, Peter
Zhang, Kai
Zheng, Tiantian
Keywords
Astrophysics - Astrophysics of Galaxies
Astrophysics - Cosmology and Nongalactic Astrophysics
Galaxies: evolution
Galaxies: formation
Galaxies: general
Galaxies: stellar content
Methods: observational
Surveys
QB Astronomy
QC Physics
3rd-DAS
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Abstract
We present an analysis of the data produced by the MaNGA prototype run (P-MaNGA), aiming to test how the radial gradients in recent star formation histories, as indicated by the 4000AA-break (D4000), Hdelta absorption (EW(Hd_A)) and Halpha emission (EW(Ha)) indices, can be useful for understanding disk growth and star formation cessation in local galaxies. We classify 12 galaxies observed on two P-MaNGA plates as either centrally quiescent (CQ) or centrally star-forming (CSF), according to whether D4000 measured in the central spaxel of each datacube exceeds 1.6. For each galaxy we generate both 2D maps and radial profiles of D4000, EW(Hd_A) and EW(Ha). We find that CSF galaxies generally show very weak or no radial variation in these diagnostics. In contrast, CQ galaxies present significant radial gradients, in the sense that D4000 decreases, while both EW(Hd_A) and EW(Ha) increase from the galactic center outward. The outer regions of the galaxies show greater scatter on diagrams relating the three parameters than their central parts. In particular, the clear separation between centrally-measured quiescent and star-forming galaxies in these diagnostic planes is largely filled in by the outer parts of galaxies whose global colors place them in the green valley, supporting the idea that the green valley represents a transition between blue-cloud and red-sequence phases, at least in our small sample. These results are consistent with a picture in which the cessation of star formation propagates from the center of a galaxy outwards as it moves to the red sequence.
Citation
Li , C , Wang , E , Lin , L , Bershady , M A , Bundy , K , Tremonti , C A , Xiao , T , Yan , R , Bizyaev , D , Blanton , M , Cales , S , Cherinka , B , Cheung , E , Drory , N , Emsellem , E , Fu , H , Gelfand , J , Law , D R , Lin , L , MacDonald , N , Maraston , C , Masters , K L , Merrifield , M R , Pan , K , Sanchez , S F , Schneider , D P , Thomas , D , Wake , D , Wang , L , Weijmans , A-M , Wilkinson , D , Yoachim , P , Zhang , K & Zheng , T 2015 , ' P-MaNGA : gradients in recent star formation histories as diagnostics for galaxy growth and death ' , Astrophysical Journal , vol. 804 , no. 2 . https://doi.org/10.1088/0004-637X/804/2/125
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.1088/0004-637X/804/2/125
ISSN
0004-637X
Type
Journal article
Rights
© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://dx.doi.org/10.1088/0004-637X/804/2/125
Description
C.L. acknowledges the support of the 100 Talents Program of Chinese Academy of Sciences (CAS). This work is supported by NSFC (11173045, 11233005, 11325314, 11320101002), by the Strategic Priority Research Program "The Emergence of Cosmological Structures" of CAS (grant No. XDB09000000), and by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. We have made use of data from HyperLeda for our work. Funding for SDSS-III and SDSS-IV has been provided by the Alfred P. Sloan Foundation and Participating Institutions. Additional funding for SDSS-III comes from the National Science Foundation and the U.S. Department of Energy Office of Science.
Collections
  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2015arXiv150207040L
URI
http://hdl.handle.net/10023/6178

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