Citation for published item:viskeD tF nd fldryD sFuF nd hriverD FF nd u'sD FtF nd elpslnD wF nd endreD iF nd froughD F nd gluverD wFiF nd qrootesD wFF nd qunwrdhnD wFvFF nd uelvinD vFF nd vovedyD tF nd oothmD eFFqF nd ylorD iFxF nd fmfordD FF nd flndErwthornD tF nd frownD wFtFsF nd hrinkwterD wFtF nd ropkinsD eFwF nd weyerD wFtF nd xorergD F nd eokD tFeF nd egiusD xFuF nd endrewsD FuF nd fuerD eFiF nd ghingD tFrFF nd gollessD wF nd gonselieD gFtF nd groomD FwF nd hviesD vFtFwF nd he roprisD F nd hunneD vF nd irdleyD iFwF nd illisD F nd posterD gF nd prenkD gFF nd r¤ ußlerD fF nd rolwerdD fFF nd rowlettD gF nd srrD rF nd trvisD wFtF nd tonesD hFrF nd u)eD FF nd veyD gFqF nd vngeD F nd vrEv¡ opezD wFeF nd v¡ opezE¡ nhezD ¡ eFF nd wddoxD F nd wdoreD fFpF nd wxughtEoertsD F nd wo'ettD eFtF nd xiholD FgF nd ywersD wFF nd lmrD hF nd ennyD FtF nd hillippsD F nd imletD uFeF nd opesuD gFgF nd resottD wF nd rotorD F nd dlerD iFwF nd nsomD eFiF nd eiertD wF nd hrpD F nd utherlndD F nd ¡ zquezEwtD tFeF nd vn umpenD iF nd ilkinsD FwF nd illimsD F nd rightD eFrF @PHISA 9qlxy end wss essemly @qeweA X end of survey report nd dt relese PF9D wonthly noties of the oyl estronomil oietyFD RSP @PAF ppF PHVUEPIPTF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTThe Galaxy And Mass Assembly (GAMA) survey is one of the largest contemporary spectroscopic surveys of low redshift galaxies. Covering an area of ∼286 deg 2 (split among five survey regions) down to a limiting magnitude of r < 19.8 mag, we have collected spectra and reliable redshifts for 238 000 objects using the AAOmega spectrograph on the Anglo-Australian Telescope. In addition, we have assembled imaging data from a number of independent surveys in order to generate photometry spanning the wavelength range 1 nm-1 m. Here, we report on the recently completed spectroscopic survey and present a series of diagnostics to assess its final state and the quality of the redshift data. We also describe a number of survey aspects and procedures, or updates thereof, including changes to the input catalogue, redshifting and re-redshifting, and the derivation of ultraviolet, optical and near-infrared photometry. Finally, we present the second public release of GAMA data. In this release, we provide input catalogue and targeting information, spectra, redshifts, ultraviolet, optical and near-infrared photometry, single-component Sérsic fits, stellar masses, Hα-derived star formation rates, environment information, and group p...

The Galaxy And Mass Assembly (GAMA) survey furnishes a deep redshift catalog that, when combined with the Wide-field Infrared Explorer (WISE), allows us to explore for the first time the mid-infrared properties of > 110, 000 galaxies over 120 deg 2 to z ≃ 0.5. In this paper we detail the procedure for producing the matched GAMA-WISE catalog for the G12 and G15 fields, in particular characterising and measuring resolved sources; the complete catalogs for all three GAMA equatorial fields will be made available through the GAMA public releases. The wealth of multiwavelength photometry and optical spectroscopy allows us to explore empirical relations between optically determined stellar mass (derived from synthetic stellar population models) and 3.4µm and 4.6µm WISE measurements. Similarly dust-corrected Hα-derived star formation rates can be compared to 12µm and 22µm luminosities to quantify correlations that can be applied to large samples to z < 0.5. To illustrate the applications of these relations, we use the 12µm star formation prescription to investigate the behaviour of specific star formation within the GAMA-WISE sample and underscore the ability of WISE to detect star-forming systems at z ∼ 0.5. Within galaxy groups (determined by a sophisticated friends-of-friends scheme), results suggest that galaxies with a neighbor within 100 h −1 kpc have, on average, lower specific star formation rates than typical GAMA galaxies with the same stellar mass.

We use data from the Galaxy And Mass Assembly (GAMA) survey in the redshift range 0.01

We present accurate resolved WISE photometry of galaxies in the combined SINGS and KINGFISH sample. The luminosities in the W3 12µm and W4 23µm bands are calibrated to star formation rates (SFRs) derived using the total infrared luminosity, avoiding UV/optical uncertainties due to dust extinction corrections. The W3 relation has a 1-σ scatter of 0.15 dex over nearly 5 orders of magnitude in SFR and 12µm luminosity, and a range in host stellar mass from dwarf (10 7 M ) to ∼ 3×M (10 11.5 M ) galaxies. In the absence of deep silicate absorption features and powerful active galactic nuclei, we expect this to be a reliable SFR indicator chiefly due to the broad nature of the W3 band. By contrast the W4 SFR relation shows more scatter (1-σ = 0.18 dex). Both relations show reasonable agreement with radio continuum-derived SFRs and excellent accordance with so-called "hybrid" Hα + 24µm and FUV+24µm indicators. Moreover, the WISE SFR relations appear to be insensitive to the metallicity range in the sample. We also compare our results with IRAS-selected luminous infrared galaxies, showing that the WISE relations maintain concordance, but systematically deviate for the most extreme galaxies. Given the all-sky coverage of WISE and the performance of the W3 band as a SFR indicator, the L 12µm SFR relation could be of great use to studies of nearby galaxies and forthcoming large area surveys at optical and radio wavelengths.