Evolution in the bias of faint radio sources to z ∼ 2.2

Lindsay, Sam; Jarvis, M. J.; McAlpine, K.

doi:10.1093/mnras/stu453

Cited by 27 publications

(51 citation statements)

References 62 publications

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“…Therefore we are likely tracing higher mass haloes with higher clustering amplitudes. The work by Lindsay et al (2014) is more similar to ours over the majority of angular scales, again with our two-point correlation function exhibiting an excess at small angles. For their work, Lindsay et al (2014) used sources from FIRST (Becker et al 1995, Helfand et al 2015, which have a flux density limit of 1 mJy at 1.4 GHz (∼ 5 mJy at 144 MHz) and so we expect our results to be similar to this.…”

Section: Clustering In the Xmm-lss Fieldsupporting

confidence: 84%

“…This quantifies the excess probability of the clustering of galaxies at certain angular scales compared to a random distribution of galaxies in the same field (see e.g. Peebles Princeton University Press, 1980, Blake & Wall 2002, Lindsay et al 2014. To construct the random catalogue of galaxies, we considered the varying rms across the image as in Hale et al (2018).…”

Section: Clustering In the Xmm-lss Fieldmentioning

confidence: 99%

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LOFAR observations of the XMM-LSS field

Hale

Williams

Jarvis

et al. 2019

A&A

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We present observations of the XMM Large-Scale Structure (XMM-LSS) field observed with the LOw Frequency ARray (LOFAR) at 120-168 MHz. Centred at a J2000 declination of −4.5 • , this is a challenging field to observe with LOFAR because of its low elevation with respect to the array. The low elevation of this field reduces the effective collecting area of the telescope, thereby reducing sensitivity. This low elevation also causes the primary beam to be elongated in the north-south direction, which can introduce side lobes in the synthesised beam in this direction. However the XMM-LSS field is a key field to study because of the wealth of ancillary information, encompassing most of the electromagnetic spectrum. The field was observed for a total of 12 hours from three four-hour LOFAR tracks using the Dutch array. The final image presented encompasses ∼ 27 deg 2 , which is the region of the observations with a >50% primary beam response. Once combined, the observations reach a central rms of 280 µJy beam −1 at 144 MHz and have an angular resolution of 7.5 × 8.5 . We present our catalogue of detected sources and investigate how our observations compare to previous radio observations. This includes investigating the flux scale calibration of these observations compared to previous measurements, the implied spectral indices of the sources, the observed source counts and corrections to obtain the true source counts, and finally the clustering of the observed radio sources.

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Section: Clustering In the Xmm-lss Fieldsupporting

confidence: 84%

Section: Clustering In the Xmm-lss Fieldmentioning

confidence: 99%

LOFAR observations of the XMM-LSS field

Hale

Williams

Jarvis

et al. 2019

A&A

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“…Repetition of this process allows the variance of the ω(θ) values to be estimated. Lindsay et al (2014) found Poisson errors were a factor of 1.5 to 2 smaller than those estimated with bootstrap. In this paper we use 100 bootstrap resamplings to estimate the uncertainty at the 16th and 84th percentiles of the resampling.…”

Section: Estimating ω(θ) Numericallymentioning

confidence: 62%

“…If the redshift is known precisely for each galaxy then this is unambiguous. In Lindsay et al (2014), for each redshift bin, the sum of the pdfs that have their peak in that bin is used e.g. there is some contribution from outside the bin.…”

Section: Projecting From 3d and Choice Of N (Z)mentioning

confidence: 99%

The galaxy–halo connection in the VIDEO survey at 0.5 <z< 1.7

Hatfield

Lindsay

Jarvis

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a series of results from a clustering analysis of the first data release of the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey. VIDEO is the only survey currently capable of probing the bulk of stellar mass in galaxies at redshifts corresponding to the peak of star formation on degree scales. Galaxy clustering is measured with the two-point correlation function, which is calculated using a non parametric kernel based density estimator. We use our measurements to investigate the connection between the galaxies and the host dark matter halo using a halo occupation distribution methodology, deriving bias, satellite fractions, and typical host halo masses for stellar masses between 10 9.35 M and 10 10.85 M , at redshifts 0.5 < z < 1.7. Our results show typical halo mass increasing with stellar mass (with moderate scatter) and bias increasing with stellar mass and redshift consistent with previous studies. We find the satellite fraction increased towards low redshifts, from ∼ 5% at z ∼ 1.5, to ∼ 20% at z ∼ 0.6. We combine our results to derive the stellar mass to halo mass ratio for both satellites and centrals over a range of halo masses and find the peak corresponding to the halo mass with maximum star formation efficiency to be ∼ 2×10 12 M , finding no evidence for evolution.

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“…In their angular correlation analysis of the NVSS Overzier et al (2003) while the brighter, potentially FR II, sources had a scalelength r 0RR ∼ 14 h −1 Mpc. On the other hand clustering analyses of radio surveys matched to optical galaxies have found no luminosity dependence in the large-scale halo-halo regime (Donoso et al 2010;Fine et al 2011;Lindsay et al 2014b). Note that since the Overzier et al (2003) had no redshift information a considerable series of assumptions about the radio population were required to derive their result, on the other hand both Donoso et al (2010) and Fine et al (2011) Given the few constraints on r 0RR we initially make the simplest empirical assumption.…”

Section: The Clustering Strength Of Quasars and Radio Sourcesmentioning

confidence: 99%

Counting quasar–radio source pairs to derive the millijansky radio luminosity function and clustering strength toz = 3.5

Fine¹,

Shanks²,

Johnston³

et al. 2015

Mon. Not. R. Astron. Soc.

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We apply a cross-correlation technique to infer the S > 3mJy radio luminosity function (RLF) from the NRAO VLA sky survey (NVSS) to z ∼ 3.5. We measure Σ the over density of radio sources around spectroscopically confirmed quasars. Σ is related to the space density of radio sources at the distance of the quasars and the clustering strength between the two samples, hence knowledge of one constrains the other. Under simple assumptions we find Φ ∝ (1 + z) 3.7±0.7 out to z ∼ 2. Above this redshift the evolution slows and we constrain the evolution exponent to < 1.01 (2σ). This behaviour is almost identical to that found by previous authors for the bright end of the RLF potentially indicating that we are looking at the same population. This suggests that the NVSS is dominated by a single population; most likely radio sources associated with high-excitation cold-mode accretion. Inversely, by adopting a previously modelled RLF we can constrain the clustering of high-redshift radio sources and find a clustering strength consistent with r 0 = 15.0 ± 2.5 Mpc up to z ∼ 3.5. This is inconsistent with quasars at low redshift and some measurements of the clustering of bright FRII sources. This behaviour is more consistent with the clustering of lower luminosity radio galaxies in the local universe. Our results indicate that the highexcitation systems dominating our sample are hosted in the most massive galaxies at all redshifts sampled.

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Evolution in the bias of faint radio sources to z ∼ 2.2

Cited by 27 publications

References 62 publications

LOFAR observations of the XMM-LSS field

LOFAR observations of the XMM-LSS field

The galaxy–halo connection in the VIDEO survey at 0.5 <z< 1.7

Counting quasar–radio source pairs to derive the millijansky radio luminosity function and clustering strength toz = 3.5

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