GAMA: towards a physical understanding of galaxy formation

Driver, Simon P.; Norberg, Peder; Baldry, I. K.; Bamford, Steven P.; Hopkins, A. M.; Liske, J.; Loveday, Jon; Peacock, J. A.; Hill, D. T.; Kelvin, Lee S.; Robotham, Aaron S. G.; Cross, N. J. G.; Parkinson, H; Prescott, M.; Conselice, C.; Dunne, L.; Brough, Sarah; Jones, Heath; Sharp, Robert; Kampen, E. van; Oliver, Seb; Roseboom, I. G.; Bland-Hawthorn, Joss; Croom, S. M.; Ellis, S. C.; Cameron, Ewan; Cole, Shaun; Frenk, Carlos S.; Couch, Warrick J.; Graham, Alister W.; Proctor, Rob; Propris, Roberto De; Doyle, Issi F.; Edmondson, E. M.; Thomas, R. C.; Eales, Steve; Jarvis, Matt J.; Kuijken, Konrad; Lahav, O.; Madore, Barry F.; Seibert, Mark; Meyer, M.; Staveley‐Smith, L.; Phillipps, Steven; Popescu, Cristina; Sansom, A. E.; Sutherland, William J.; Tuffs, R.; Warren, Steven J.

doi:10.1111/j.1468-4004.2009.50512.x

Cited by 431 publications

(369 citation statements)

References 29 publications

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“…Of these 2267 counterparts, 876 have spectroscopic redshifts (spec-zs) acquired either by the SDSS, the Galaxy And Mass Assembly survey (Driver et al 2009), the 2dF redshift survey (Colless et al 2001) or the 6dF redshift survey (Jones et al 2009). For the remaining counterparts, photometric redshifts (photo-zs) were estimated by applying the ANNz neural network code (Collister & Lahav 2004) (UKIDSS; Lawrence et al 2007).…”

Section: Datamentioning

confidence: 99%

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Dye

Dunne

Eales

et al. 2010

A&A

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We have determined the luminosity function of 250 μm-selected galaxies detected in the ∼14 deg 2 science demonstration region of the Herschel-ATLAS project out to a redshift of z = 0.5. Our findings very clearly show that the luminosity function evolves steadily out to this redshift. By selecting a sub-group of sources within a fixed luminosity interval where incompleteness effects are minimal, we have measured a smooth increase in the comoving 250 μm luminosity density out to z = 0.2 where it is 3.6 +1.4 −0.9 times higher than the local value.

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Section: Datamentioning

confidence: 99%

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Dye

Dunne

Eales

et al. 2010

A&A

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“…), respectively. The source catalogues are supplemented with cross-identification information from the GAMA survey (Driver et al 2009) and SDSS DR-7 (Abazajian et al 2009) as described in Smith et al (in prep.). For the sources for which spectroscopic redshifts from GAMA or SDSS are not available, we use photometric redshifts generated using the ANNz neural network code (Collister & Lahav 2004), trained with photometry from SDSS and UKIDSS LAS (Lawrence et al 2007), and spectra from the GAMA spectroscopic survey (Driver et al 2009), DEEP2 (Davis et al 2007), zCOSMOS (Lilly et al 2007), and the 2SLAQ-LRG (Cannon et al 2006) survey.…”

Section: Colour-colour Diagramsmentioning

confidence: 99%

“…and 160 μm data from PACS, and 250, 350, and 500 μm data from SPIRE. The H-ATLAS fields include 1 field close to the northern Galactic pole (150 deg 2 ), 3 fields (each 36 deg 2 ) coinciding with the GAMA redshift survey fields (Driver et al 2009), and 2 fields (total area of 250 deg 2 ) near the southern Galactic pole.…”

Section: Introductionmentioning

confidence: 99%

Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours

Amblard¹,

Cooray²,

Serra³

et al. 2010

A&A

111

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We present colour-colour diagrams of detected sources in the Herschel-ATLAS science demonstration field from 100 to 500 μm using both PACS and SPIRE. We fit isothermal modified black bodies to the spectral energy distribution (SED) to extract the dust temperature of sources with counterparts in Galaxy And Mass Assembly (GAMA) or SDSS surveys with either a spectroscopic or a photometric redshift. For a subsample of 330 sources detected in at least three FIR bands with a significance greater than 3σ, we find an average dust temperature of (28 ± 8) K. For sources with no known redshift, we populate the colour-colour diagram with a large number of SEDs generated with a broad range of dust temperatures and emissivity parameters, and compare to colours of observed sources to establish the redshift distribution of this sample. For another subsample of 1686 sources with fluxes above 35 mJy at 350 μm and detected at 250 and 500 μm with a significance greater than 3σ, we find an average redshift of 2.2 ± 0.6.

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“…In the past decade it has been demonstrated that a panchromatic, X-ray to radio, observational approach is key to develop a consensus on galaxy formation and evolution (e.g., Dickinson et al 2003;Scoville et al 2007;Driver et al 2009Driver et al , 2011Koekemoer et al 2011;Grogin et al 2011). In this context, the radio regime offers an indispensable window toward star formation and supermassive black hole properties of galaxies as radio A&A 602, A1 (2017) continuum emission i) provides a dust-unbiased star formation tracer at high angular resolution (e.g., Condon 1992;Haarsma et al 2000;Seymour et al 2008;Smolčić et al 2009b;Karim et al 2011); and ii) directly probes those active galactic nuclei (AGN) that are hosted by the most massive quiescent galaxies and deemed crucial for massive galaxy formation (e.g., Croton et al 2006;Bower et al 2006;Best et al 2006;Evans et al 2006;Hardcastle et al 2007;Smolčić et al 2009aSmolčić et al , 2015Smolčić 2009;Smolčić & Riechers 2011).…”

Section: Introductionmentioning

confidence: 99%

The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

Smolčić

Novak

Bondì

et al. 2017

A&A

307

365

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We present the VLA-COSMOS 3 GHz Large Project based on 384 h of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the two square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 µJy beam −1 over the two square degrees at an angular resolution of 0.75 . To fully account for the spectral shape and resolution variations across the broad (2 GHz) band, we image all data with a multiscale, multifrequency synthesis algorithm. We present a catalog of 10 830 radio sources down to 5σ, out of which 67 are combined from multiple components. Comparing the positions of our 3 GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, we estimate that the astrometry is accurate to 0.01 at the bright end (signal-to-noise ratio, S /N 3 GHz > 20). Survival analysis on our data combined with the VLA-COSMOS 1.4 GHz Joint Project catalog yields an expected median radio spectral index of α = −0.7. We compute completeness corrections via Monte Carlo simulations to derive the corrected 3 GHz source counts. Our counts are in agreement with previously derived 3 GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3 GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75 ) angular resolution to date, bridging the gap between last-generation and next-generation surveys.

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GAMA: towards a physical understanding of galaxy formation

Cited by 431 publications

References 29 publications

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Herschel-ATLAS: Evolution of the 250 µm luminosity function out to z=0.5

Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours

The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

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