Galaxy And Mass Assembly (GAMA): assimilation of KiDS into the GAMA database

Bellstedt, Sabine; Driver, Simon P.; Robotham, Aaron S. G.; Davies, Luke J. M.; Bogue, Cameron R J; Cook, Robin H. W.; Hashemizadeh, Abdolhosein; Koushan, Soheil; Taylor, Edward N.; Thorne, Jessica E.; Turner, Ryan J.; Wright, Angus H.

doi:10.1093/mnras/staa1466

Cited by 75 publications

(132 citation statements)

References 71 publications

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“…The GAMA 23 photometry catalogue (Bellstedt et al 2020) contains measured properties and classifications of each object catalogued by the ProFound j (Robotham et al 2018) source finding routine, which uses a stacked r + Z image to perform initial source finding. Approximately 48 000 objects have spectroscopic redshifts provided by the Anglo-Australian Telescope (AAT), and the survey is ∼95% spectroscopically complete up to an i band magnitude of 19.5 (Liske et al 2015).…”

Section: Gama 23 Photometry Cataloguementioning

confidence: 99%

Remnant radio galaxies discovered in a multi-frequency survey

Quici

Hurley‐Walker

Seymour

et al. 2021

Publ. Astron. Soc. Aust.

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The remnant phase of a radio galaxy begins when the jets launched from an active galactic nucleus are switched off. To study the fraction of radio galaxies in a remnant phase, we take advantage of a $8.31$ deg $^2$ subregion of the GAMA 23 field which comprises of surveys covering the frequency range 0.1–9 GHz. We present a sample of 104 radio galaxies compiled from observations conducted by the Murchison Widefield Array (216 MHz), the Australia Square Kilometer Array Pathfinder (887 MHz), and the Australia Telescope Compact Array (5.5 GHz). We adopt an ‘absent radio core’ criterion to identify 10 radio galaxies showing no evidence for an active nucleus. We classify these as new candidate remnant radio galaxies. Seven of these objects still display compact emitting regions within the lobes at 5.5 GHz; at this frequency the emission is short-lived, implying a recent jet switch off. On the other hand, only three show evidence of aged lobe plasma by the presence of an ultra-steep-spectrum ( $\alpha<-1.2$ ) and a diffuse, low surface brightness radio morphology. The predominant fraction of young remnants is consistent with a rapid fading during the remnant phase. Within our sample of radio galaxies, our observations constrain the remnant fraction to $4\%\lesssim f_{\mathrm{rem}} \lesssim 10\%$ ; the lower limit comes from the limiting case in which all remnant candidates with hotspots are simply active radio galaxies with faint, undetected radio cores. Finally, we model the synchrotron spectrum arising from a hotspot to show they can persist for 5–10 Myr at 5.5 GHz after the jets switch of—radio emission arising from such hotspots can therefore be expected in an appreciable fraction of genuine remnants.

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Section: Gama 23 Photometry Cataloguementioning

confidence: 99%

Remnant radio galaxies discovered in a multi-frequency survey

Quici

Hurley‐Walker

Seymour

et al. 2021

Publ. Astron. Soc. Aust.

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“…While the merits and failings of these approaches can be argued -through numerous tests we have found that the P F approach is far less likely to go catastrophically wrong and produces more robust photometric measurements. For full details on P F and numerous tests, we refer the reader to the code description paper and four recent applications to the DEVILS input catalogue (Davies et al 2018), GAMA photometry (Bellstedt et al 2020), the VISTA VIKING datasets (Koushan et al 2021) and evolution of the high redshift stellar mass function (Adams et al 2020).…”

Section: The Need For a New Cosmos (D10) Photometric Cataloguementioning

confidence: 99%

“…With just these data products in hand, an extensive array of measurements can be made, such as stellar masses (Kauffmann et al 2003;Baldry et al 2010;Taylor et al 2015), star-formation rates (Brinchmann et al 2004;Davies et al 2016b) and star-formation histories (𝑒.𝑔. Kauffmann et al 2003;Bellstedt et al 2020, Thorne at al 2021, metallicities (.𝑒.𝑔. Tremonti et al 2004;Bellstedt et al 2021, Thorne et al in prep.…”

Section: Introductionmentioning

confidence: 99%

“…Importantly for direct comparisons to 𝑧 ∼ 0, this photometry must be derived using an almost identical method to that used in GAMA. Recently, Bellstedt et al (2020), produced new multi-wavelength photometric measurements for the GAMA sample using the P -F (Robotham et al 2018) source detection and photometry code. In this work we apply the same process (albeit with small changes where appropriate) to the deep photometric data available in the DEVILS regions.…”

Section: Introductionmentioning

confidence: 99%

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Deep Extragalactic VIsible Legacy Survey (DEVILS): consistent multiwavelength photometry for the DEVILS regions (COSMOS, XMMLSS, and ECDFS)

Davies

Thorne

Robotham

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The Deep Extragalactic VIsible Legacy Survey (DEVILS) is an ongoing high-completeness, deep spectroscopic survey of ∼60 000 galaxies to Y < 21.2 mag, over ∼6 deg2 in three well-studied deep extragalactic fields: D10 (COSMOS), D02 (XMM-LSS) and D03 (ECDFS). Numerous DEVILS projects all require consistent, uniformly-derived and state-of-the-art photometric data with which to measure galaxy properties. Existing photometric catalogues in these regions either use varied photometric measurement techniques for different facilities/wavelengths leading to inconsistencies, older imaging data and/or rely on source detection and photometry techniques with known problems. Here we use the ProFound image analysis package and state-of-the-art imaging datasets (including Subaru-HSC, VST-VOICE, VISTA-VIDEO and UltraVISTA-DR4) to derive matched-source photometry in 22 bands from the FUV to 500 μm. This photometry is found to be consistent, or better, in colour-analysis to previous approaches using fixed-size apertures (which are specifically tuned to derive colours), but produces superior total source photometry, essential for the derivation of stellar masses, star-formation rates, star-formation histories, etc. Our photometric catalogue is described in detail and, after internal DEVILS team projects, will be publicly released for use by the broader scientific community.

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“…Then the PROFOUND R package (Robotham et al 2018) is used to detect objects in the white-light image above a threshold of 3 × RMS sky and produce a preliminary segmentation map. Similarly to Bellstedt et al (2020), this segmentation map is then manually adjusted to join mistakenly split segments or remove visibly spurious detections. PROFOUND is used once more to finalise photometric properties using the r and i-band images, these include r e (approximate elliptical semi-major axis containing half the flux), photometric position angle (PA phot ), axis ratio and apparent magnitudes, for every object detected in the field.…”

Section: Source Detectionmentioning

confidence: 99%

The MAGPI survey: Science goals, design, observing strategy, early results and theoretical framework

Foster

Mendel

Lagos

et al. 2021

Publ. Astron. Soc. Aust.

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We present an overview of the Middle Ages Galaxy Properties with Integral Field Spectroscopy (MAGPI) survey, a Large Program on the European Southern Observatory Very Large Telescope. MAGPI is designed to study the physical drivers of galaxy transformation at a lookback time of 3–4 Gyr, during which the dynamical, morphological, and chemical properties of galaxies are predicted to evolve significantly. The survey uses new medium-deep adaptive optics aided Multi-Unit Spectroscopic Explorer (MUSE) observations of fields selected from the Galaxy and Mass Assembly (GAMA) survey, providing a wealth of publicly available ancillary multi-wavelength data. With these data, MAGPI will map the kinematic and chemical properties of stars and ionised gas for a sample of 60 massive ( ${>}7 \times 10^{10} {\mathrm{M}}_\odot$ ) central galaxies at $0.25 < z <0.35$ in a representative range of environments (isolated, groups and clusters). The spatial resolution delivered by MUSE with Ground Layer Adaptive Optics ( $0.6-0.8$ arcsec FWHM) will facilitate a direct comparison with Integral Field Spectroscopy surveys of the nearby Universe, such as SAMI and MaNGA, and at higher redshifts using adaptive optics, for example, SINS. In addition to the primary (central) galaxy sample, MAGPI will deliver resolved and unresolved spectra for as many as 150 satellite galaxies at $0.25 < z <0.35$ , as well as hundreds of emission-line sources at $z < 6$ . This paper outlines the science goals, survey design, and observing strategy of MAGPI. We also present a first look at the MAGPI data, and the theoretical framework to which MAGPI data will be compared using the current generation of cosmological hydrodynamical simulations including EAGLE, Magneticum, HORIZON-AGN, and Illustris-TNG. Our results show that cosmological hydrodynamical simulations make discrepant predictions in the spatially resolved properties of galaxies at $z\approx 0.3$ . MAGPI observations will place new constraints and allow for tangible improvements in galaxy formation theory.

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Galaxy And Mass Assembly (GAMA): assimilation of KiDS into the GAMA database

Cited by 75 publications

References 71 publications

Remnant radio galaxies discovered in a multi-frequency survey

Remnant radio galaxies discovered in a multi-frequency survey

Deep Extragalactic VIsible Legacy Survey (DEVILS): consistent multiwavelength photometry for the DEVILS regions (COSMOS, XMMLSS, and ECDFS)

The MAGPI survey: Science goals, design, observing strategy, early results and theoretical framework

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