The SAMI Galaxy Survey: Data Release One with emission-line physics value-added products

Creators: Green, Andrew W.; Medling, Anne M.

Abstract

We present the first major release of data from the SAMI Galaxy Survey. This data release focuses on the emission-line physics of galaxies. Data Release One includes data for 772 galaxies, about 20 per cent of the full survey. Galaxies included have the redshift range 0.004 < z < 0.092, a large mass range (7.6 < log M*/ M⊙ < 11.6), and star formation rates of ∼10^(−4) to ∼10^1M⊙ yr^(−1). For each galaxy, we include two spectral cubes and a set of spatially resolved 2D maps: single- and multi-component emission-line fits (with dust-extinction corrections for strong lines), local dust extinction, and star formation rate. Calibration of the fibre throughputs, fluxes, and differential atmospheric refraction has been improved over the Early Data Release. The data have average spatial resolution of 2.16 arcsec (full width at half-maximum) over the 15 arcsec diameter field of view and spectral (kinematic) resolution of R = 4263 (σ = 30 km s^(−1)) around H α. The relative flux calibration is better than 5 per cent, and absolute flux calibration has an rms of 10 per cent. The data are presented online through the Australian Astronomical Observatory's Data Central.

Additional Information

© 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 December 1. Received 2017 November 30; in original form 2017 May 16. Published: 11 December 2017. The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney/AAO Multi-object Integral-field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the GAMA survey, and the VST ATLAS survey. The SAMI Galaxy Survey is funded by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/. JTA acknowledges the award of a SIEF John Stocker Fellowship. MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). BG is the recipient of an Australian Research Council Future Fellowship (FT140101202). NS acknowledges support of a University of Sydney Postdoctoral Research Fellowship. SB acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). JvdS is funded under Bland-Hawthorn's ARC Laureate Fellowship (FL140100278). SMC acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). Support for AMM is provided by NASA through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. CF gratefully acknowledges funding provided by the Australian Research Council's Discovery Projects (grants DP150104329 and DP170100603). BC is the recipient of an Australian Research Council Future Fellowship (FT120100660). Author contributions.AWG and SMC oversaw DR1 and edited the paper. SMC is the survey's Principal Investigator. JBH and SMC wrote the introduction. JB oversaw the target selection and wrote those parts of the paper. NS wrote sections on the changes to the data reduction, and oversaw the data reduction with JTA and RS. ITH oversaw the emission-line fits and produced Figs 11 and 12, with BG providing additional clarifying text. AMM ran quality control on the emission-line fits, produced the higher order value-added data products, and coordinated ingestion of these to the data base. BG helped coordinate preparation of value-added products for release. MJD and LC oversaw the formatting and preparation of all data for inclusion in the online data base. JvdS prepared the survey overview diagram, Fig. 4. SMC checked the flux calibration accuracy and wrote Section 3.4.3 and prepared Fig. 7. ADT and SMC measured the accuracy of the WCS information and wrote the corresponding Section 3.4.4. RMM provided heliocentric velocity corrections. FDE and JTA created Figs 6 and 7 and contributed to the data reduction software and to the assessment of the data quality, Section 3.4. AWG, EM, LH, SO, MV, KS, and AMH built the online data base serving the data. Remaining authors contributed to overall team operations including target catalogue and observing preparation, instrument maintenance, observing at the telescope, writing data reduction and analysis software, managing various pieces of team infrastructure such as the website and data storage systems, and innumerable other tasks critical to the preparation and presentation of a large data set such as this DR1.

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