The SDSS-IV MaNGA sample : design, optimization, and usage considerations
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We describe the sample design for the SDSS-IV MaNGA survey and present the final properties of the main samples along with important considerations for using these samples for science. Our target selection criteria were developed while simultaneously optimizing the size distribution of the MaNGA integral field units (IFUs), the IFU allocation strategy, and the target density to produce a survey defined in terms of maximizing S/N, spatial resolution, and sample size. Our selection strategy makes use of redshift limits that only depend oni-band absolute magnitude (Mi), or, for a small subset of our sample, Mi and color (NUV-i). Such a strategy ensures that all galaxies span the same range in angular size irrespective of luminosity and are therefore covered evenly by the adopted range of IFU sizes. We define three samples: the Primary and Secondary samples are selected to have a flat number density with respect to Mi and are targeted to have spectroscopic coverage to 1.5 and 2.5 effective radii (Re),respectively. The Color-Enhanced supplement increases the number of galaxies in the low-density regions of color-magnitude space by extending the redshift limits of the Primary sample in the appropriate color bins. The samples cover the stellar mass range 5 x 108 ≤ M⋆ ≤ 3 x 1011 M⊙ /h2 and are sampled at median physical resolutions of 1.37 kpc and 2.5 kpc for the Primary and Secondary samples respectively. We provide weights that will statistically correct for our luminosity and color-dependent selection function and IFU allocation strategy, thus correcting the observed sample to a volume limited sample.
Wake , D A , Bundy , K , Diamond-Stanic , A M , Yan , R , Blanton , M R , Bershady , M A , Sánchez-Gallego , J R , Drory , N , Jones , A , Kauffmann , G , Law , D R , Li , C , MacDonald , N , Masters , K , Thomas , D , Tinker , J , Weijmans , A-M & Brownstein , J R 2017 , ' The SDSS-IV MaNGA sample : design, optimization, and usage considerations ' Astronomical Journal , vol 154 , no. 3 , 86 . DOI: https://doi.org/10.3847/1538-3881/aa7ecc
© 2017, American Astronomical Society. This work has been 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 iopscience.iop.org / https://doi.org/10.3847/1538-3881/aa7ecc
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