Cosmic Star Formation History Measured at 1.4 GHz

Matthews, A. M.; Condon, J. J.; Cotton, W. D.; Mauch, T.

doi:10.3847/1538-4357/abfaf6

Cited by 28 publications

(51 citation statements)

References 45 publications

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“…We examined SFRD evaluated from constant radio to IR luminosity fraction for all redshift and found that constant 𝑞 TIR gives higher SFRD at 𝑧 > 3.5. Matthews et al (2021) introduced luminosity dependent non-linear 𝑞 parameter in order to exclude the bias caused by flux limited sample. The FIR/radio correlation is a critical quantity to draw SFRD from radio luminosity.…”

Section: Discussionmentioning

confidence: 99%

An Empirical Estimation of the Galaxy Radio Number Counts model at 3~GHz and the Effect of Gravitational Lensing

Kono¹,

Takeuchi²

2021

Preprint

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We analyzed the evolution of 3GHz luminosity function of radio selected galaxies through cosmic time, up to about 1 Gyr after Big Bang, with making use of the VLA-COSMOS 3GHz large project. We estimated the luminosity function for SFGs and AGNs in the VLA-COSMOS field respectively with two independent methods, the non-parametric 𝐶 − method for accuracy to avoid the effect of cosmic variance and parametric MCMC method assuming pure luminosity evolution. We obtained pure luminosity evolution parameter as 𝐿 * ,SFG ∝ (1 + 𝑧) (3.36±0.05)−(0.31±0.02) 𝑧 for SFG and 𝐿 * ,AGN ∝ (1 + 𝑧) (2.91 +0.18 −0.19 )−(0.99±0.08) 𝑧 for AGN. The resultant model agreed well with observed number counts down to sub-𝜇Jy level. Additionally, we compared the model with cosmic star formation rate density history with multiple observations in various wavelength and confirmed that our result is consistent with literature up to 𝑧 ∼ 3. We further analyzed the statistical effect of gravitational lensing due to the dark matter halos and found that the effect is maximized at 𝑆 3 GHz ∼ 100 𝜇Jy with about 1 % contribution for SFG and less than 0.5% for AGN for the flux range considered in this study. In order to evaluate the effect of lensing magnification on parameter estimation in the SKA observations, we performed Fisher analysis and find that while the bias is limited, there is a distinguishable effect on SFG LF evolution parameter with SKA I MID wide survey, and all-sky and wide survey for AGN LF evolution parameters.

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Section: Discussionmentioning

confidence: 99%

An Empirical Estimation of the Galaxy Radio Number Counts model at 3~GHz and the Effect of Gravitational Lensing

Kono¹,

Takeuchi²

2021

Preprint

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“…For comparison, we also plot the cosmic star formation rate density (SFRD) from Madau & Dickinson (2014), Zavala et al (2021) and the radio-derived SFRD from Matthews et al (2021) in Fig. 14.…”

Section: Comparing the Agn Luminosity Density With The Sfrdmentioning

confidence: 99%

“…We include comparisons of the luminosity density from previous results(Ranalli et al 2016;Lacy et al 2007) as shown in the upper left legend. Additionally shown on the right side y-axis (and the lower right legend) are the star formation rate densities (SFRD) fromMadau & Dickinson (2014),Zavala et al (2021), and the 1.4 GHz radio-derived SFRD fromMatthews et al (2021).…”

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confidence: 99%

Consistent analysis of the AGN LF in X-ray and MIR in the XMM-LSS field

Runburg,

Farrah,

Sajina

et al. 2021

Preprint

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The luminosity function (LF) of active galactic nuclei (AGN) probes the history of supermassive black hole assembly and growth across cosmic time. To mitigate selection biases, we present a consistent analysis of the AGN LFs derived for both X-ray and mid-infrared (MIR) selected AGN in the XMM-Large Scale Structure (XMM-LSS) field. There are 4268 AGN used to construct the MIR luminosity function (IRLF) and 3427 AGN used to construct the X-ray luminosity function (XLF), providing the largest census of the AGN population out to z = 4 in both bands with significant reduction in uncertainties. We are able for the first time to see the knee of the IRLF at z > 2 and observe a flattening of the faint-end slope as redshift increases. The bolometric luminosity density, a proxy for the cosmic black hole accretion history, computed from our LFs shows a peak at z ≈ 2.25 consistent with recent estimates of the peak in the star formation rate density (SFRD). However, at earlier epochs, the AGN luminosity density is flatter than the SFRD. If confirmed, this result suggests that the build up of black hole mass outpaces the growth of stellar mass in high mass systems at z 2.5. This is consistent with observations of redshift z ∼ 6 quasars which lie above the local M − σ relationship. The luminosity density derived from the IRLF is higher than that from the XLF at all redshifts. This is consistent with the dominant role of obscured AGN activity in the cosmic growth of supermassive black holes.

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“…Though there have been many attempts to explore its evolution, it remains still controversial (e.g., Bourne et al 2011;Mao et al 2011;Schleicher & Beck 2013;Schober et al 2016;Delvecchio et al 2021;Molnár et al 2021). In spite of such uncertainties, the potential use of the radio continuum as an SFR estimator has attracted attention (e,g., Bell 2003;Murphy et al 2011;Matthews et al 2021). Particularly, the recent development of long-wavelength facilities is a driving force to push forward such studies, gearing at the SKA (e.g., Shao et al 2018;Read et al 2018;Tisanić et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Estimation of the Star Formation Rate of Galaxies with Radio Continuum Obtained with Murchison Widefield Array

Takeuchi¹,

Yoshida²,

Cortese³

et al. 2022

Preprint

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We investigate the correlation between the integrated low-frequency and infrared (IR) emissions of star-forming galaxies extracted from the Herschel Reference Survey. By taking advantage of the GaLactic Extragalactic All-sky MWA (GLEAM) survey operated by the Murchison Widefield Array (MWA) we examine how this correlation varies at a function of frequency across the 20 GLEAM narrow bands at 72-231 [MHz]. These examinations are important for ensuring the reliability of the radio luminosity as a SFR indicator. In this study, we focus on 18 star-forming galaxies whose radio emission is detected by the GLEAM survey. These galaxies show that a single power-law is sufficient to characterise the far-infrared-to-radio correlation across the GLEAM frequency bands and up to 1.5 [GHz]. Thus, the radio continuum in this wavelength range can serve as a good dust extinction-free SFR estimator. This is particularly important for future investigation of the cosmic SFR independently from other estimators, since the radio continuum can be detected from z = 0 to high redshifts (z ∼ 5-10) in a coherent manner.

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Cosmic Star Formation History Measured at 1.4 GHz

Cited by 28 publications

References 45 publications

An Empirical Estimation of the Galaxy Radio Number Counts model at 3~GHz and the Effect of Gravitational Lensing

An Empirical Estimation of the Galaxy Radio Number Counts model at 3~GHz and the Effect of Gravitational Lensing

Consistent analysis of the AGN LF in X-ray and MIR in the XMM-LSS field

Estimation of the Star Formation Rate of Galaxies with Radio Continuum Obtained with Murchison Widefield Array

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