The Parkes selected regions: powerful radio galaxies and quasars at high redshifts

Downes, A. J. B.; Peacock, J. A.; Savage, A.; Carrie, D. R.

doi:10.1093/mnras/218.1.31

Cited by 215 publications

(227 citation statements)

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“…24µm-selected galaxies, optical i-band selected galaxies, etc) having a given space density. The p-value is calculated via the following as described in Downes et al (1986):…”

Section: Radio Counterpartsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…24µm-selected galaxies, optical i-band selected galaxies, etc) having a given space density. The p-value is calculated via the following as described in Downes et al (1986):…”

Section: Radio Counterpartsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…It is thus more relevant to compare our results to higher flux limit surveys. In the Parkes sample (Wall et al, 1971;Downes et al, 1986;Dunlop et al 1989), at the flux limit of S2.7GHz = 100mJy, no flat spectrum radio galaxy was found below z = 0.02, the redshift at which a 10 23 W Hz −1 source is at the Parkes flux limit. We find 5 flat spectrum ellipticals (0.75 < z < 1) in the volume contained in our 10 ′ × 10 ′ MOS field, which is 7.5 times smaller than the volume in the Parkes survey to z = 0.02.…”

Section: Radio Emission From Distant Ellipticals Compared To Nearby Onesmentioning

confidence: 99%

The Canada–France Redshift Survey – VII. Optical counterparts of microjansky radio sources

Hammer¹,

Crampton

Lilly

et al. 1995

Monthly Notices of the Royal Astronomical Society

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Deep imaging and spectroscopy have been carried out for optical counterparts of a complete sample of S>16 µJy radiosources during the course of the Canada-France Redshift Survey (CFRS). All 36 sources but two have been optically identified, and spectra have been obtained for 23 of them. The objects brighter than I AB <22.5 for which we have spectra reveal three populations dominating the µJy radio counts: z>0.7 early-type galaxies with radio emission powered by an AGN, intermediate redshift poststarburst galaxies, and lower redshift blue emission-line objects. From their radio and optical properties, it is argued that the 11 objects fainter than I AB >22.5 are mostly at z>1, and one half of them are probably early-type galaxies. We conclude that ∼40 per cent of the µJy sources are likely to be at z >1.Between one third and one half of the luminous ellipticals in this field beyond z = 0.7 show moderately powerful radio emission (P ∼ 5 10 23 W Hz −1 ) which is at least 10 times more powerful than seen in local samples, and probably reflects evolution of the activity in their nuclei. Only one classical starburst galaxy is identified in the sample; the rest of the blue emission-line objects show optical and radio activity more typical of low power AGNs than starbursts. The number of post-starbursts at µJy levels is considerably higher than the surface density of mJy starburst galaxies, suggesting the latter are the parent population of the former. While starburst galaxies are considered to be major contributors to the mJy radiosources counts, the majority of the µJy radio sources appear to be related to AGN activity rather than to normal star formation.

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“…Clearly, more sophisticated matching algorithms must be considered A significant number of techniques exist to facilitate the matching of catalogues. Techniques such as the p-statistic (Downes et al 1986) and the likelihood ratio (Sutherland & Saunders 1992) make use of the number density of background (and true counterpart) sources to 'weigh' potential counterparts within a given search radius, but cannot take into account the likelihood that several radio components may correspond to one optical component. More recently, Budavári & Szalay (2008) outlined a Bayesian method to determine the most likely match.…”

Section: Classification and Cross-identificationmentioning

confidence: 99%