An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies

Algera, H. S. B.; Smail, Ian; Dudzevičiūtė, U.; Swinbank, A. M.; Stach, S. M.; Hodge, J. A.; Thomson, A. P.; Almaini, O.; Arumugam, V.; Blain, A. W.; Calistro-Rivera, G.; Chapman, Scott; Chen, Chian-Chou; Cunha, Elisabete da; Farrah, D.; Leslie, S. K.; Scott, Douglas; Vlugt, D. van der; Wardlow, J. L.; Werf, P. van der

doi:10.3847/1538-4357/abb77b

Cited by 29 publications

(51 citation statements)

References 127 publications

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“…Accounting for the frequency difference through scaling with α=−0.70, our S-band observations are a factor ∼13 deeper than these lower-frequency data, and hence the 1.4 GHz observations are mostly useful for the brightest sources detected at 3 and 10 GHz. Additionally, a sevenpointing mosaic at 34 GHz (rms∼1.4 μJy beam −1 , area ∼10 arcmin 2 ) exists as part of the COLDz project (Pavesi et al 2018;Riechers et al 2019;Algera et al 2020). The COSMOS-XS 10 GHz data is directly centered on this mosaic, allowing for a detailed analysis of the long-wavelength spectrum of faint radio sources with up to four frequencies.…”

Section: Radio Datamentioning

confidence: 99%

“…However, galaxies that host an AGN may have their radio emission dominated instead by the active nucleus, and will therefore be offset from the FIRC. To quantify this, we define the correlation parameter q TIR as the logarithmic ratio of a galaxy's total-IR luminosity L TIR , measured between (restframe) 8-1000 μm, and its monochromatic radio luminosity at rest-frame 1.4 GHz, L 1.4GHz (following e.g., Bell 2003;Thomson et al 2014;Magnelli et al 2015;Delhaize et al 2017;Calistro Rivera et al 2017;Algera et al 2020…”

Section: Radio-excess Agnsmentioning

confidence: 99%

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A Multiwavelength Analysis of the Faint Radio Sky (COSMOS-XS): the Nature of the Ultra-faint Radio Population

Algera

Vlugt

Hodge

et al. 2020

ApJ

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Ultra-deep radio surveys are an invaluable probe of dust-obscured star formation, but require a clear understanding of the relative contribution from radio active galactic nuclei (AGNs) to be used to their fullest potential. We study the composition of the μJy radio population detected in the Karl G. Jansky Very Large Array COSMOS-XS survey based on a sample of 1540 sources detected at 3 GHz over an area of ∼350 arcmin 2 . This ultra-deep survey consists of a single pointing in the well-studied COSMOS field at both 3 and 10 GHz and reaches rms sensitivities of 0.53 and 0.41 μJy beam −1 , respectively. We find multiwavelength counterparts for 97% of radio sources, based on a combination of near-UV/optical to sub-millimeter data, and through a stacking analysis at optical/near-IR wavelengths we further show that the sources lacking such counterparts are likely to be high-redshift in nature (typical z∼4−5). Utilizing the multiwavelength data over COSMOS, we identify AGNs through a variety of diagnostics and find these to make up 23.2±1.3% of our sample, with the remainder constituting uncontaminated star-forming galaxies. However, more than half of the AGNs exhibit radio emission consistent with originating from star formation, with only 8.8±0.8% of radio sources showing a clear excess in radio luminosity. At flux densities of ∼30 μJy at 3 GHz, the fraction of star formation-powered sources reaches ∼90%, and this fraction is consistent with unity at even lower flux densities. Overall, our findings imply that ultra-deep radio surveys such as COSMOS-XS constitute a highly effective means of obtaining clean samples of star formation-powered radio sources.

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Section: Radio Datamentioning

confidence: 99%

Section: Radio-excess Agnsmentioning

confidence: 99%

A Multiwavelength Analysis of the Faint Radio Sky (COSMOS-XS): the Nature of the Ultra-faint Radio Population

Algera

Vlugt

Hodge

et al. 2020

ApJ

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“…For example, the total flux density and, hence, the size of moderately resolved sources can differ between radio maps with different spatial resolutions (Murphy et al 2017;Bondi et al 2018). 13 We note that adopting a redshift-dependent IR-radio correlation (e.g., Delhaize et al 2017;Algera et al 2020) does not affect the sense (or significance) of the trends reported in this work.…”

Section: Estimating the Radio Size Of Galaxiesmentioning

confidence: 78%

“…One dust-unbiased, but indirect, probe of star formation can be obtained by mapping the predominantly nonthermal radio continuum emission of galaxies at centimeter wavelengths (e.g., Condon 1992;Bell 2003;Garn et al 2009;Murphy et al 2011). This star formation rate (SFR) indicator has been calibrated using the tight, yet empirical, far-infrared (far-IR)radio correlation (Helou et al 1985;Yun et al 2001;Murphy et al 2006aMurphy et al , 2006bMurphy et al , 2012bMurphy 2009;Sargent et al 2010;Magnelli et al 2015;Delhaize et al 2017;Gim et al 2019;Algera et al 2020). The physical interpretation of this relation is that far-IR emission arises from the absorption and reradiation of UV and optical photons that heat dust grains surrounding massive star-forming regions.…”

Section: Introductionmentioning

confidence: 99%

The VLA Frontier Field Survey: A Comparison of the Radio and UV/Optical Size of 0.3 ≲ z ≲ 3 Star-forming Galaxies

Jiménez-Andrade

Murphy

Heywood

et al. 2021

ApJ

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To investigate the growth history of galaxies, we measure the rest-frame radio, ultraviolet (UV), and optical sizes of 98 radio-selected, star-forming galaxies (SFGs) distributed over 0.3  z  3 with a median stellar mass of. We compare the size of galaxy stellar disks, traced by rest-frame optical emission, relative to the overall extent of star formation activity that is traced by radio continuum emission. Galaxies in our sample are identified in three Hubble Frontier Fields: MACS J0416.1−2403, MACS J0717.5+3745, and MACS J1149.5 +2223. Radio continuum sizes are derived from 3 and 6 GHz radio images (0 6 resolution, ≈0.9 μJy beam −1 noise level) from the Karl G. Jansky Very Large Array. Rest-frame UV and optical sizes are derived using observations from the Hubble Space Telescope and the Advanced Camera for Surveys and Wide Field Camera 3 instruments. We find no clear dependence between the 3 GHz radio size and stellar mass of SFGs, which contrasts with the positive correlation between the UV/optical size and stellar mass of galaxies. Focusing on SFGs with, we find that the radio/UV/optical emission tends to be more compact in galaxies with high star formation rates (100 M e yr −1 ), suggesting that a central, compact starburst (and/or an active galactic nucleus) resides in the most luminous galaxies of our sample. We also find that the physical radio/UV/optical size of radio-selected SFGs with log(M å /M e ) > 10 increases by a factor of 1.5-2 from z ≈ 3 to z ≈ 0.3, yet the radio emission remains two to three times more compact than that from the UV/optical. These findings indicate that these massive, radio-selected SFGs at 0.3  z  3 tend to harbor centrally enhanced star formation activity relative to their outer disks.

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“…This exists in star-forming galaxies because radio emission is intimately correlated with the FIR due to their mutual origin in active high-mass star-forming regions. This correlation is found to hold at high redshifts (Yun et al 2001;Garrett 2002;Sargent et al 2010; Thomson et al 2014;Pannella et al 2015;Magnelli et al 2015;Delhaize et al 2017;Algera et al 2020a), thus any AGN activity can be identified by deviations from this correlation. Here the AGN produces the excess radio emission (e.g., Donley et al 2005;Del Moro et al 2013).…”

Section: Introductionmentioning

confidence: 90%

Nowhere to hide: Radio-faint AGN in the GOODS-N field

Radcliffe

Barthel

Thomson

et al. 2021

A&A

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Context. Obtaining a census of active galactic nuclei (AGN) activity across cosmic time is critical to our understanding of galaxy evolution and formation. Many AGN classification techniques are compromised by dust obscuration. However, very long baseline interferometry (VLBI) can be used to identify high brightness temperature compact radio emission (> 105 K) in distant galaxies that can only be reliably attributed to AGN activity. Aims. We present the second in a series of papers dealing with the compact radio population in the GOODS-N field. This paper reviews the various multi-wavelength data and AGN classification techniques in the context of a VLBI-detected sample and use these to investigate the nature of the AGN as well as their host galaxies. Methods. Multi-wavelength data from radio to X-ray were compiled for the GOODS-N AGN sample, and fourteen widely used multi-wavelength AGN classification schemes were tested. We discuss and compare the various biases that affect multi-wavelength and VLBI selection. We use the physical interpretation to imply the nature of VLBI-selected AGN and their hosts. Results. Firstly, we find that no single identification technique can identify all VLBI objects as AGN. Infrared colour–colour selection is most notably incomplete. However, the usage of multiple classification schemes can identify all VLBI-selected AGN, independently verifying similar approaches used in other deep field surveys. In the era of large area surveys with instruments such as the SKA and ngVLA, multi-wavelength coverage, which relies heavily upon observations from space, is often unavailable. Therefore, VLBI remains an integral component in detecting AGN of the jetted efficient and inefficient accretion types. Secondly, a substantial fraction (46%) of the VLBI AGN have no X-ray counterpart, which is most likely due to lack of sensitivity in the X-ray band. Thirdly, a high fraction of the VLBI AGN reside in low or intermediate redshift dust-poor early-type galaxies. These most likely exhibit inefficient accretion. Fourthly, A significant fraction of the VLBI AGN reside in symbiotic dusty starburst – AGN systems. Finally, in the appendix, we present an extensive compilation of the multi-wavelength properties of all the VLBI AGN in GOODS-N.

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An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies

Cited by 29 publications

References 127 publications

A Multiwavelength Analysis of the Faint Radio Sky (COSMOS-XS): the Nature of the Ultra-faint Radio Population

A Multiwavelength Analysis of the Faint Radio Sky (COSMOS-XS): the Nature of the Ultra-faint Radio Population

The VLA Frontier Field Survey: A Comparison of the Radio and UV/Optical Size of 0.3 ≲ z ≲ 3 Star-forming Galaxies

Nowhere to hide: Radio-faint AGN in the GOODS-N field

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