Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

Mancuso, C.; Lapi, A.; Prandoni, I.; Obi, Ikechukwu; González‐Nuevo, J.; Perrotta, F.; Bressan, A.; Celotti, A.; Danese, L.

doi:10.3847/1538-4357/aa745d

Cited by 104 publications

(122 citation statements)

References 190 publications

(299 reference statements)

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“…ure 7) from the Tiered Radio Extragalactic Continuum Simulation (T-RECS) byBonaldi et al (2019) who modeled the corresponding sub-populations, over the 150 MHz -20 GHz range. Our results concurs with the results of these models from literature, especially to theMancuso et al (2017) andBonaldi et al (2019) models at high luminosities. Note, however, that in the first two redshift bins the faint end of theMancuso et al (2017) models is lower than that of our SFG LF.…”

supporting

confidence: 93%

“…Our results concurs with the results of these models from literature, especially to theMancuso et al (2017) andBonaldi et al (2019) models at high luminosities. Note, however, that in the first two redshift bins the faint end of theMancuso et al (2017) models is lower than that of our SFG LF. Also, the faint end of theBonaldi et al (2019) andWilman et al (2008) models are higher than our measured SFG LF.…”

supporting

confidence: 93%

“…However, deep multi-frequency radio observations of representative samples of galaxies are needed to study the radio SED and understand the physical processes shaping it across redshifts. We also compare our results to models from the literature and find that the Mancuso et al (2017) and Wilman et al (2008) models do compare well to our data. However, there is an exception for the lowest redshift bin, where none of the models is able to reproduce the low- luminosity observations.…”

Section: Discussionsupporting

confidence: 69%

“…Mancuso et al (2016b). These models are based on two main ingredients: (i) the redshiftdependent SFR functions inferred from the latest UV/far-IR data from HST/Herschel and related statistics of strong gravitationally lensed sources, and (ii) deterministic tracks for the co-evolution of star formation and BH accretion in an individual galaxy, determined from a wealth of multiwavelength observations (see Mancuso et al (2017)). We also compare to SFG models (see open brown diamonds in Fig The breakdown of the luminosity, number density (Φ 610 (Mpc −3 dex −1 )) and the number of sources in each redshift bin is presented in Table 6.…”

Section: Rlf As a Function Of Zmentioning

confidence: 99%

“…Figure 7presents the radio luminosity functions of SFGs at ν = 610 MHz in different redshift bins (black open circles). Scaled down luminosity functions from 1.4 GHz to 610 MHz bySmolčić et al (2009a),McAlpine et al (2013) andNovak et al (2017) are shown as green pluses, orange pentagons and blue diamonds respectively in each panel.We compare with LFs derived fromWilman et al (2008) semi-empirical simulation of the SKA andMancuso et al (2017) models. TheMancuso et al (2017) models were obtained by following the model-independent approach byMancuso et al (2016a);…”

mentioning

confidence: 99%

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Cosmic evolution of star-forming galaxies to z ≃ 1.8 in the faint low-frequency radio source population

Ocran

Taylor

Vaccari

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the properties of star-forming galaxies selected at 610 MHz with the GMRT in a survey covering ∼1.86 deg 2 down to a noise of ∼7.1 µJy / beam. These were identified by combining multiple classification diagnostics: optical, X-ray, infrared and radio data. Of the 1685 SFGs from the GMRT sample, 496 have spectroscopic redshifts whereas 1189 have photometric redshifts. We find that the IRRC of star-forming galaxies, quantified by the infrared-to-1.4 GHz radio luminosity ratio q IR , decreases with increasing redshift: q IR = 2.86 ± 0.04(1 + z) −0.20±0.02 out to z ∼ 1.8. We use the V/V max statistic to quantify the evolution of the co-moving space density of the SFG sample. Averaged over luminosity our results indicate V/V max to be 0.51 ± 0.06, which is consistent with no evolution in overall space density. However we find V/V max to be a function of radio luminosity, indicating strong luminosity evolution with redshift. We explore the evolution of the SFGs radio luminosity function by separating the source into five redshift bins and comparing to theoretical model predictions. We find a strong redshift trend that can be fitted with a pure luminosity evolution of the form L 610 MHz ∝ ( 1 + z) (2.95±0.19)−(0.50±0.15)z . We calculate the cosmic SFR density since z ∼ 1.5 by integrating the parametric fits of the evolved 610 MHz luminosity function. Our sample reproduces the expected steep decline in the star formation rate density since z ∼ 1.

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supporting

confidence: 93%

supporting

confidence: 93%

Section: Discussionsupporting

confidence: 69%

Section: Rlf As a Function Of Zmentioning

confidence: 99%

mentioning

confidence: 99%

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Cosmic evolution of star-forming galaxies to z ≃ 1.8 in the faint low-frequency radio source population

Ocran

Taylor

Vaccari

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A high-resolution self-consistent whole sky foreground model

Huang

Chen

2019

Sci. China Phys. Mech. Astron.

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The neutral hydrogen 21cm line is potentially a very powerful probe of the observable universe, and a number of on-going experiments are trying to detect it at cosmological distances. However, the presence of strong foreground radiations such as the galactic synchrotron radiation, galactic free-free emission and extragalactic radio sources make it a very challenging task. For the design of 21cm experiments and analysis of their data, simulation is an essential tool, and good sky foreground model is needed. With existing data the whole sky maps are available only in low angular resolutions or for limited patches of sky, which is inadequate in the simulation of these new 21cm experiments. In this paper, we present the method of constructing a high resolution self-consistent sky model at low frequencies, which incorporates both diffuse foreground and point sources. Our diffuse map is constructed by generating physical foreground components including the galactic synchrotron emission and galactic freefree emission. The point source sample is generated using the actual data from the NRAO VLA Sky Survey (NVSS) and the Sydney University Molonglo Sky Survey (SUMSS) where they are available and complete in flux limit, and mock point sources according to statistical distributions. The entire model is made self-consistent by removing the integrated flux of the point sources from the diffuse map so that this part of radiation is not double counted. We show that with the point sources added, a significant angular power is introduced in the mock sky map, which may be important for foreground subtraction simulations. Our sky maps and point source catalogues are available to download. neutral hydrogen, 21cm line, foreground model, whole sky map, simulation PACS number(s): 95.80.+p, 95.85.Bh, 98.70.Dk, 95.75.Mn, 95.75.Pq Citation: Huang Q Z, Wu F Q & Chen X L, A high-resolution self-consistent whole sky foreground model, Sci. China-Phys. Mech. Astron. ??, 000000 (2018), doi: ? 1) https://lambda.gsfc.nasa.gov/product/foreground/haslam_408.cfm 2)

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Imaging and photometric studies of NGC 1316 (Fornax A) using Astrosat/UVIT

Vagshette¹,

Naik

Kumari

et al. 2021

J Astrophys Astron

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We present imaging and photometric studies of the radio galaxy NGC 1316 (Fornax A) using high spatial resolution near-ultraviolet (NUV) and far-ultraviolet (FUV) imaging telescopes of the first Indian multi-wavelength space observatory AstroSat. The residual maps of UV emission obtained from the subtraction of smooth models witness peculiar features within the central few kpc (1-2 kpc) region. The spatial correspondence between the radio emission maps and FUV imaging study reveal that the UV emitting sources are displaced away from the centre by the AGN outburst (radio jet). The presence of rims and clumpy structures in the outskirt of this galaxy delineate that the galaxy has acquired a large fraction of gas through merger-like events and is still in the process of settling. The estimates of the star formation rates (SFR) using FUV and NUV luminosities are found to be 0.15 M yr À1 and 0.36 M yr À1 , respectively, and provide the lower limit due to the screen effect. The estimated lower rates of SFR in this galaxy probably represent its quenching due to the AGN driven outflows emanating from the central engine of NGC 1316.

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Galaxy Evolution in the Radio Band: The Role of Star-forming Galaxies and Active Galactic Nuclei

Cited by 104 publications

References 190 publications

Cosmic evolution of star-forming galaxies to z ≃ 1.8 in the faint low-frequency radio source population

Cosmic evolution of star-forming galaxies to z ≃ 1.8 in the faint low-frequency radio source population

A high-resolution self-consistent whole sky foreground model

Imaging and photometric studies of NGC 1316 (Fornax A) using Astrosat/UVIT

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