The SAMI Galaxy Survey: Instrument specification and target selection

By J. Bryant, M. Owers, A. Robotham, Scott M. Croom, S. Driver, Michael Drinkwater, N. Lorente, L. Cortese, Nicholas Scott, M. Colless and 48 more. 2014

332 citations recorded by the source corpus.

The SAMI Galaxy Survey will observe 3400 galaxies with the Sydney-AAO Multi- object Integral-field spectrograph (SAMI) on the Anglo-Australian Telescope (AAT) in a 3-year survey which began in 2013. We present the throughput of the SAMI system, the science basis and specifications for the target selection, the survey observation plan and the combined properties of the selected galaxies. The survey includes four volume-limited galaxy samples based on cuts in a proxy for stellar mass, along with low-stellar-mass dwarf galaxies all selected from the Galaxy And Mass Assembly (GAMA) survey. The GAMA regions were selected because of the vast array of ancillary data available, including ultraviolet through to radio bands. These fields are on the celestial equator at 9, 12, and 14.5 hours, and cover a total of 144 square degrees (in GAMA-I). Higher density environments are also included with the addition of eight clusters. The clusters have spectroscopy from 2dFGRS and SDSS and photometry in regions covered by the Sloan Digital Sky Survey (SDSS) and/or VLT Survey Telescope/ATLAS. The aim is to cover a broad range in stellar mass and environment, and therefore the primary survey targets cover redshifts 0.004 < z < 0.095, magnitudes rpet < 19.4, stellar masses 107– 1012M⊙, and environments from isolated field galaxies through groups to clusters of _ 1015M⊙.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2c788b622b2ae61ff387a8781198cfc4b0c3c895

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Improving the full spectrum fitting method: accurate convolution with Gauss-Hermite functions (2016, methodology): “In fact, one new characteristic of both the MaNGA and SAMI survey is that they are observing large numbers of galaxies (especially spirals) with stellar velocity dispersion σ well below the instrumental dispersion σinst of the spectrographs.”
Galaxy and mass assembly (GAMA): End of survey report and data release 2 (2015, background): “In addition, GAMA provides the basis for numerous follow-up projects (in particular of group galaxies), and even serves as a stepping stone for other large, independent survey projects such as the SAMI Galaxy Survey (Allen et al. 2015; Bryant et al. 2015).”
The SDSS-IV MaNGA Sample: Design, Optimization, and Usage Considerations (2017, result): “A number of our design choices, such as an even sampling in stellar mass, roughly uniform radial coverage, and a sample size in the thousands, are similar in spirit to those of the SAMI survey (Croom et al. 2012; Bryant et al. 2015).”
THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, background): “Ongoing spatially-resolved spectroscopic surveys, such as the SDSS-IV/MaNGA IFU (Law et al. 2015) and SAMI (Bryant et al. 2015) galaxy surveys, will provide a dataset capable of unraveling the relative contributions of HII regions and diffuse ionized gas to global galaxy spectra.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “This is the time when the first generation of IFS surveys, which targeted one galaxy at a time (SAURON de Zeeuw et al. 2002, ATLAS3D Cappellari et al. 2011a, CALIFA Sánchez et al. 2012, DiskMass Bershady et al. 2010) have been completed and a new generation of multiplexed IFS surveys, which can obs”