The ATESP radio survey

Prandoni, I.; Gregorini, L.; Parma, P.; Ruiter, H. R. de; Vettolani, G.; Wieringa, M.; Ekers, R. D.

doi:10.1051/0004-6361:20000142

Cited by 97 publications

(142 citation statements)

References 11 publications

(11 reference statements)

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“…The FIRST catalog is severely incomplete at faint flux densities. From Prandoni et al (2001) we estimate a completeness of ≈ 50% for S ≤ 1.25 mJy and of ≈ 75% for 1.25 mJy ≤ S ≤ 1.5 mJy. This flux-density-dependent incompleteness is in addition to that discussed above.…”

Section: Sample Completenessmentioning

confidence: 85%

Decline of the Space Density of Quasars betweenz= 2 andz= 4

Vigotti

Carballo

Benn

et al. 2003

ApJ

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We define a new complete sample of 13 optically-luminous radio quasars (M AB (1450Å)< −26.m 9 and log P 1.4GHz (W Hz −1 ) > 25.7) with redshift 3.8 < z < 4.5, obtained by crosscorrelating the FIRST radio survey and the APM catalogue of POSS-I. We measure the space density to be (1.0 ± 0.3) Gpc −3 , a factor 1.9±0.7 smaller than the space density of similar quasars at z ≈ 2 (FBQS). Using a new measurement of the radio-loud fraction of quasars we find that at z = 4 the total space density of quasars with M AB (1450Å)< −26. m 9 is (7.4 ±2.6) Gpc −3 . This is a factor 1.8 ± 0.8 less than the space density at z ≈ 2, found by the 2dF quasar survey. This z = 2 / z = 4 ratio, consistent with that of the radio-loud quasars, is significantly different from the ratio ∼ 10 found for samples including lower-luminosity quasars. This suggests that the decline of the space density beyond z ≈ 2 is slower for optically-luminous quasars than for less-luminous ones.

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Section: Sample Completenessmentioning

confidence: 85%

Decline of the Space Density of Quasars betweenz= 2 andz= 4

Vigotti

Carballo

Benn

et al. 2003

ApJ

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“…The resolution bias correction factor is then simply integral size distribution is commonly used to determine resolution bias (e.g. Prandoni et al 2001) so we include it in our source count derivation, but we note it is derived from a brighter sample than our work (S1.4GHz > 0.4 mJy). The Muxlow et al (2005) sample goes to sub-100-µJy levels, but it comes from high resolution MERLIN and VLA imaging which may miss low surface brightness galaxies.…”

Section: Source Size and Resolution Biasmentioning

confidence: 99%

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

Huynh¹,

Bell²,

Hopkins³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a new image of the 5.5 GHz radio emission from the extended Chandra Deep Field South. Deep radio observations at 5.5 GHz were obtained in 2010 and presented in the first data release. A further 76 hours of integration has since been obtained, nearly doubling the integration time. This paper presents a new analysis of all the data. The new image reaches 8.6 µJy rms, an improvement of about 40% in sensitivity. We present a new catalogue of 5.5 GHz sources, identifying 212 source components, roughly 50% more than were detected in the first data release. Source counts derived from this sample are consistent with those reported in the literature for S 5.5GHz > 0.1 mJy but significantly lower than published values in the lowest flux density bins (S 5.5GHz < 0.1 mJy), where we have more detected sources and improved statistical reliability. The 5.5 GHz radio sources were matched to 1.4 GHz sources in the literature and we find a mean spectral index of −0.35 ± 0.10 for S 5.5GHz > 0.5 mJy, consistent with the flattening of the spectral index observed in 5 GHz sub-mJy samples. The median spectral index of the whole sample is α med = −0.58, indicating that these observations may be starting to probe the star forming population. However, even at the faintest levels (0.05 < S 5.5GHz < 0.1 mJy), 39% of the 5.5 GHz sources have flat or inverted radio spectra. Four flux density measurements from our data, across the full 4.5 to 6.5 GHz bandwidth, are combined with those from literature and we find 10% of sources (S 5.5GHz 0.1 mJy) show significant curvature in their radio spectral energy distribution spanning 1.4 to 9 GHz.

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“…From extragalactic source counts at 1.4 GHz in total intensity (Prandoni et al 2001), the expected source contribution is c …”

Section: Fit Of the Aps After Source Subtractionmentioning

confidence: 99%

The impact of Galactic synchrotron emission on CMB anisotropy measurements

Porta¹,

Burigana

Reich³

et al. 2007

A&A

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Context. Galactic foreground emission fluctuations are a limiting factor for precise cosmic microwave background (CMB) anisotropy measurements. Aims. We intend to improve current estimates of the influence of Galactic synchrotron emission on the analysis of CMB anisotropies. Methods. We perform an angular power spectrum analysis (APS) of all-sky total intensity maps at 408 MHz and 1420 MHz, which are dominated by synchrotron emission out of the Galactic plane. We subtract the brighter sources from the maps, which turns out to be essential for the results obtained. We study the APS as a function of Galactic latitude by considering various cuts and as a function of sky position by dividing the sky into patches of ∼15• × 15 • in size. Results. The APS of the Galactic radio diffuse synchrotron emission is best fitted by a power law, C ∼ k α , with α ∈ [−3.0, −2.6], where the lower values of α typically correspond to the higher latitudes. Nevertheless, the analysis of the patches reveals that strong local variations exist. A good correlation is found between the APS normalized amplitude, k 100 = k×100 α , at 408 MHz and 1420 MHz. The mean APS for ∈ [20, 40] is used to determine the mean spectral index between 408 MHz and 1420 MHz, β (0.408−1.4) GHz ∈ [−3.2, −2.9] (C (ν) ∝ ν −2β ), which is then adopted to extrapolate the synchrotron APS results to the microwave range. Conclusions. We use the 408 MHz and 1420 MHz APS results to predict the Galactic synchrotron emission fluctuations at frequencies above 20 GHz. A simple extrapolation to 23 GHz of the synchrotron emission APS found at these radio frequencies does not explain all the power in the WMAP synchrotron component even at middle/high Galactic latitudes. This suggests a significant microwave contribution (of about 50% of the signal) by other components such as free-free or spinning dust emission. The comparison between the extrapolated synchrotron APS and the CMB APS shows that a mask excluding the regions with |b gal | < ∼ 5• would reduce the foreground fluctuations to about half of the cosmological ones at 70 GHz even at the lowest multipoles. The main implications of our analysis for the cosmological exploitation of microwave temperature anisotropy maps are discussed.

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The ATESP radio survey

Cited by 97 publications

References 11 publications

Decline of the Space Density of Quasars betweenz= 2 andz= 4

Decline of the Space Density of Quasars betweenz= 2 andz= 4

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

The impact of Galactic synchrotron emission on CMB anisotropy measurements

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