SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality
The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R ~ 2000 from 3622 − 10, 354Å. The design of the survey is dr...
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| Format: | Journal article |
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Institute of Physics
2016
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| _version_ | 1797087890871681024 |
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| author | Cappellari, M Graham, M |
| author_facet | Cappellari, M Graham, M |
| author_sort | Cappellari, M |
| collection | OXFORD |
| description | The MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R ~ 2000 from 3622 − 10, 354Å. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is ~ 73 per 1.4Å pixel for spectra stacked between 1–1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals. |
| first_indexed | 2024-03-07T02:42:04Z |
| format | Journal article |
| id | oxford-uuid:aacb68a1-e466-45a6-accf-570638b31c8c |
| institution | University of Oxford |
| last_indexed | 2024-03-07T02:42:04Z |
| publishDate | 2016 |
| publisher | Institute of Physics |
| record_format | dspace |
| spelling | oxford-uuid:aacb68a1-e466-45a6-accf-570638b31c8c2022-03-27T03:17:31ZSDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data QualityJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:aacb68a1-e466-45a6-accf-570638b31c8cSymplectic Elements at OxfordInstitute of Physics2016Cappellari, MGraham, MThe MaNGA Survey (Mapping Nearby Galaxies at Apache Point Observatory) is one of three core programs in the Sloan Digital Sky Survey IV. It is obtaining integral field spectroscopy (IFS) for 10K nearby galaxies at a spectral resolution of R ~ 2000 from 3622 − 10, 354Å. The design of the survey is driven by a set of science requirements on the precision of estimates of the following properties: star formation rate surface density, gas metallicity, stellar population age, metallicity, and abundance ratio, and their gradients; stellar and gas kinematics; and enclosed gravitational mass as a function of radius. We describe how these science requirements set the depth of the observations and dictate sample selection. The majority of targeted galaxies are selected to ensure uniform spatial coverage in units of effective radius (Re) while maximizing spatial resolution. About 2/3 of the sample is covered out to 1.5Re (Primary sample), and 1/3 of the sample is covered to 2.5Re (Secondary sample). We describe the survey execution with details that would be useful in the design of similar future surveys. We also present statistics on the achieved data quality, specifically, the point spread function, sampling uniformity, spectral resolution, sky subtraction, and flux calibration. For our Primary sample, the median r-band signal-to-noise ratio is ~ 73 per 1.4Å pixel for spectra stacked between 1–1.5 Re. Measurements of various galaxy properties from the first year data show that we are meeting or exceeding the defined requirements for the majority of our science goals. |
| spellingShingle | Cappellari, M Graham, M SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title | SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title_full | SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title_fullStr | SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title_full_unstemmed | SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title_short | SDSS-IV MaNGA IFS Galaxy Survey --- Survey Design, Execution, and Initial Data Quality |
| title_sort | sdss iv manga ifs galaxy survey survey design execution and initial data quality |
| work_keys_str_mv | AT cappellarim sdssivmangaifsgalaxysurveysurveydesignexecutionandinitialdataquality AT grahamm sdssivmangaifsgalaxysurveysurveydesignexecutionandinitialdataquality |