The VLA-VIRMOS Deep Field

Bondì, M.; Ciliegi, P.; Zamorani, G.; Gregorini, L.; Vettolani, G.; Parma, P.; Ruiter, H. de; Fèvre, O. Le; Arnaboldi, M.; Guzzo, L.; Maccagni, D.; Scaramella, R.; Adami, C.; Bardelli, S.; Bolzonella, M.; Bottini, D.; Cappi, A.; Foucaud, Sylvie; Franzetti, P.; Garilli, B.; Gwyn, Stephen; Ilbert, O.; Iovino, A.; Brun, V. Le; Marano, B.; Marinoni, C.; McCracken, H. J.; Meneux, B.; Pollo, A.; Pozzetti, L.; Radovich, M.; Ripepi, V.; Rizzo, D.; Scodeggio, M.; Tresse, L.; Zanichelli, A.; Zucca, E.

doi:10.1051/0004-6361:20030382

Cited by 148 publications

(223 citation statements)

References 24 publications

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“…The extension of a radio source increases its total flux density when compared to its peak surface brightness, however, background noise can lower the total flux density (see Bondi et al 2003). Therefore, in Fig.…”

Section: Resolved Versus Unresolved Sourcesmentioning

confidence: 99%

“…In recent decades, radio interferometers, such as the Karl G. Jansky Very Large Array (VLA), Australia Telescope Compact Array (ATCA), and Giant Meterwave Radio Telescope (GMRT), have surveyed fields of different sizes (ranging from tens of square arcminutes to thousands of square degrees), depths (microjansky to jansky), and multiwavelength coverage (e.g., Becker et al 1995;Condon et al 1998Condon et al , 2003Condon et al , 2012Ciliegi et al 1999;Georgakakis et al 1999;Bock et al 1999;Prandoni et al 2001;Hopkins et al 2003;Schinnerer et al 2004;Bondi et al 2003Bondi et al , 2007Norris et al 2005;Schinnerer et al 2007Schinnerer et al , 2010; Afonso et al 2005;Tasse et al 2007;Smolčić et al 2008Smolčić et al , 2014Owen & Morrison 2008;Miller et al 2008Miller et al , 2013Owen et al 2009;Hales et al 2014). These past surveys have shown that deep observations at high angular resolution ( 1 ) with exquisite panchromatic coverage are critical to comprehensively study the radio properties of the main galaxy populations, avoiding cosmic variance with large area coverage (e.g., Padovani et al 2009;Padovani 2011;Smolčić et al 2008Smolčić et al , 2009bSmolčić 2009;Smolčić & Riechers 2011;Seymour et al 2008;Bonzini et al 2012Bonzini et al , 2013.…”

Section: Introductionmentioning

confidence: 99%

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

Smolčić

Novak

Bondì

et al. 2017

A&A

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299

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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Section: Resolved Versus Unresolved Sourcesmentioning

confidence: 99%

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

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299

365

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“…Bondi et al 2003). We employed the aips task sad on both the mosaic image and the noise image to obtain a catalogue of candidate sources above the threshold of 4.5σ.…”

Section: Source Cataloguementioning

confidence: 99%

The eMERGE Survey – I: Very Large Array 5.5 GHz observations of the GOODS-North Field

Guidetti

Bondì

Prandoni

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present new observations of the GOODS-N field obtained at 5.5 GHz with the Karl G. Jansky Very Large Array (VLA). The central region of the field was imaged to a median r.m.s. of 3 µJy beam −1 with a resolution of 0.5 arcsec. From a 14-arcmin diameter region we extracted a sample of 94 radio sources with signal-to-noise ratio greater than 5. Near-IR identifications are available for about ∼88 percent of the radio sources. We used different multi-band diagnostics to separate active galactic nuclei (AGN), both radiatively efficient and inefficient, from star-forming galaxies. From our analysis, we find that about 80 percent of our radio-selected sample is AGNdominated, with the fraction raising to 92 percent when considering only the radio sources with redshift > 1.5. This large fraction of AGN-dominated radio sources at very low flux densities (the median flux density at 5.5 GHz is 42 µJy), where star-forming galaxies are expected to dominate, is somewhat surprising and at odds with other results. Our interpretation is that both the frequency and angular resolution of our radio observations strongly select against radio sources whose brightness distribution is diffuse on scale of several kpc. Indeed, we find that the median angular sizes of the AGN-dominated sources is around 0.2-0.3 arcsec against 0.8 arcsec for star-forming galaxies. This highlights the key role that high frequency radio observations can play in pinpointing AGN-driven radio emission at µJy levels. This work is part of the eMERGE legacy project.

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“…Radio observations of the CFHTLS-D1 field were taken at 1.4 GHz and 610 MHz from the Very Large Array (VLA, B-Array) and the Giant Metrewave Radio Telescope (GMRT), respectively, as part of the VLT-VIRMOS survey (Bondi et al 2003). Details of the observations and reduction of the VLA data are given in Ciliegi et al (2005) and those of the GMRT data are given in Bondi et al (2007).…”

Section: Other Ancillary Datamentioning

confidence: 99%

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

Lemaux

Floc’h

Fèvre

et al. 2014

A&A

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We investigate of the properties of ∼2000 Herschel/SPIRE far-infrared-selected galaxies from 0 < z < 4 in the CFHTLS-D1 field. Using a combination of extensive spectroscopy from the VVDS and ORELSE surveys, deep multiwavelength imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated spectral energy distribution fitting, Herschel-bright galaxies are compared to optically-selected galaxies at a variety of redshifts. Herschel-selected galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming "main sequence" is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities (L TIR ) are compared. Bluer optical colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger L TIR , suggesting that low-L TIR galaxies are undergoing rejuvenated starbursts while galaxies with higher L TIR are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting all types of AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts (0 < z < 4) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison (z > 0.5), the highest L TIR galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.

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The VLA-VIRMOS Deep Field

Cited by 148 publications

References 24 publications

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

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

The eMERGE Survey – I: Very Large Array 5.5 GHz observations of the GOODS-North Field

Hidden starbursts and active galactic nuclei at 0 < z < 4 from theHerschel-VVDS-CFHTLS-D1 field: Inferences on coevolution and feedback

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