The SAMI Galaxy Survey: instrument specification and target selection

Bryant, Julia J.; Owers, Matt S.; Robotham, Aaron S. G.; Croom, S. M.; Driver, Simon P.; Drinkwater, Michael J.; Lorente, Nuria P. F.; Cortese, Luca; Scott, Nicholas; Colless, Matthew; Schaefer, Adam L.; Taylor, Edward N.; Konstantopoulos, I. S.; Allen, J. T.; Baldry, I. K.; Barnes, Luke A.; Bauer, A.; Bland-Hawthorn, Joss; Bloom, J. V.; Brooks, Alyson; Brough, Sarah; Cecil, Gerald; Couch, Warrick J.; Croton, Darren J.; Davies, Roger L.; Ellis, S. C.; Fogarty, L. M. R.; Foster, Caroline; Glazebrook, Karl; Goodwin, Michael; Green, Andrew W.; Gunawardhana, Madusha; Hampton, Elise; Ho, I-Ting; Hopkins, A. M.; Kewley, Lisa J.; Lawrence, Jon; Leon-Saval, Sergio G.; Leslie, S. K.; McElroy, Rebecca; Lewis, Geraint F.; Liske, J.; López-Sánchez, Á. R.; Mahajan, Smriti; Medling, Anne M.; Metcalfe, N.; Meyer, M.; Mould, Jeremy; Obreschkow, Danail; O'Toole, S. J.; Pracy, Michael; Richards, Samuel N.; Shanks, T.; Sharp, Robert; Sweet, Sarah M.; Thomas, Amberyn; Tonini, Chiara; Walcher, C. J.

doi:10.1093/mnras/stu2635

Cited by 463 publications

(406 citation statements)

References 95 publications

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“…To ensure homogeneity for our sample, we do not include the cluster galaxies in this study. The target selection for the SAMI survey is discussed in detail by Bryant et al (2015).…”

Section: Target Selectionmentioning

confidence: 99%

“…In this paper we investigate the radial distribution of star formation in galaxies observed as part of the Sydney-AAO Multi-object Integral Field Spectrograph (SAMI) Galaxy Survey (Croom et al 2012;Allen et al 2015;Bryant et al 2015;Sharp et al 2015). The application of spatiallyresolved spectroscopy to this problem represents an important step towards a better understanding of the quenching processes in galaxies.…”

Section: Introductionmentioning

confidence: 99%

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The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially-resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M * ; 10 8.1 -10 10.95 M ) and in 5 th nearest neighbour local environment density (Σ 5 ; 10 −1.3 -10 2.1 Mpc −2 ). We show that star formation rate gradients in galaxies are steeper in dense (log 10 (Σ 5 /Mpc 2 ) > 0.5) environments by 0.58 ± 0.29 dex r e −1 in galaxies with stellar masses in the range 10 10 < M * /M < 10 11 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density the star-formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scaleradius ratio (r 50,Hα /r 50,cont ), which compares the extent of ongoing star formation to previous star formation. With this metric we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ∼ 5 ± 4% in low-density environments (log 10 (Σ 5 /Mpc 2 ) < 0.0) to 30 ± 15% in the highest density environments (log 10 (Σ 5 /Mpc 2 ) > 1.0). These lines of evidence strongly suggest that with increasing local environment density the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

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“…To ensure homogeneity for our sample, we do not include the cluster galaxies in this study. The target selection for the SAMI survey is discussed in detail by Bryant et al (2015).…”

Section: Target Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

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“…MaNGA comprises two main samples, where the goal is to reach either 1.5r e (∼70% of the targets) or 2.5r e (∼20%), and it hardly samples the outer regions for most of the galaxies (Ibarra-Mendel et al 2016). Finally, SAMI, with the smallest FoV of all IFU surveys (16 /D) covers around ∼1r e of the galaxies (Bryant et al 2015).…”

Section: Introductionmentioning

confidence: 98%

CALIFA, the Calar Alto Legacy Integral Field Area survey

Sanchez

García-Benito

Zibetti

et al. 2016

A&A

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This paper describes the third public data release (DR3) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. Science-grade quality data for 667 galaxies are made public, including the 200 galaxies of the second public data release (DR2). Data were obtained with the integralfield spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto Observatory. Three different spectral setups are available: i) a low-resolution V500 setup covering the wavelength range 3745-7500 Å (4240-7140 Å unvignetted) with a spectral resolution of 6.0 Å (FWHM) for 646 galaxies, ii) a medium-resolution V1200 setup covering the wavelength range 3650-4840 Å (3650-4620 Å unvignetted) with a spectral resolution of 2.3 Å (FWHM) for 484 galaxies, and iii) the combination of the cubes from both setups (called COMBO) with a spectral resolution of 6.0 Å and a wavelength range between 3700-7500 Å (3700-7140 Å unvignetted) for 446 galaxies. The Main Sample, selected and observed according to the CALIFA survey strategy covers a redshift range between 0.005 and 0.03, spans the color-magnitude diagram and probes a wide range of stellar masses, ionization conditions, and morphological types. The Extension Sample covers several types of galaxies that are rare in the overall galaxy population and are therefore not numerous or absent in the CALIFA Main Sample. All the cubes in the data release were processed using the latest pipeline, which includes improved versions of the calibration frames and an even further improved image reconstruction quality. In total, the third data release contains 1576 datacubes, including ∼1.5 million independent spectra.

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“…Both utilize multiple fiber bundles to target multiple galaxies at the same time, enabling much more efficient observing. One of them is the SAMI Galaxy survey Bryant et al 2015) using the fiber-fed SAMI instrument (Croom et al 2012) on the 3.5 m Anglo-Australian Telescope at Siding Spring Observatory. SAMI will eventually target 3400 galaxies and has already produced results on many topics, including the kinematic morphology-density relation , outflows and extraplanar gas (Ho et al , 2016, dynamical scaling relations (Cortese et al 2014), dynamical mass-to-light ratio (M/L) of disk galaxies (Cecil et al 2016), and aperture corrections for SFRs .…”

Section: Introductionmentioning

confidence: 99%

SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY

et al. 2016

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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 for 10,000nearby galaxies at a spectral resolution of R∼2000 from 3622 to 10354 Å. 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 The Astronomical Journal, 152:197 (32pp) 1 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 (R e ) while maximizing spatial resolution. About two-thirds of the sample is covered out to 1.5R e (Primary sample), and one-thirdof the sample is covered to 2.5R e (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 ∼70 per 1.4 Å pixel for spectra stacked between 1R e and 1.5R e . 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.

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The SAMI Galaxy Survey: instrument specification and target selection

Cited by 463 publications

References 95 publications

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

CALIFA, the Calar Alto Legacy Integral Field Area survey

SDSS-IV MaNGA IFS GALAXY SURVEY—SURVEY DESIGN, EXECUTION, AND INITIAL DATA QUALITY

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