Subscribe to the gold package and get unlimited access to Shamra Academy
Register a new userEnvironments of z>5 quasars: searching for protoclusters at submillimetre wavelengths
98
0
0.0
(
0
)
Ask ChatGPT about the research
No Arabic abstract
The most massive haloes at high redshift are expected, according to hierarchical cosmologies, to reside in the most biased density fields. If powerful active galactic nuclei (AGN) are expected to exist anywhere in the early Universe (z>5), it is within these massive haloes. The most luminous of these AGN, powered by supermassive black holes (SMBHs) ~10^9Msun, thereby present an opportunity to test models of galaxy formation. Here, we present submillimetre (submm) continuum images of the fields of three luminous quasars at z>5, obtained at 850 and 450um using the Submm Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). N-body simulations predict that such quasars evolve to become the central dominant galaxies of massive clusters at z=0, but at z=5-6 they are actively forming stars and surrounded by a rich proto-filamentary structure of young galaxies. Our images show evidence of extended emission on a scale of ~100kpc from at least one quasar - indicative of a partially resolved merger or a colossal host galaxy. In addition, at >3sigma significance we detect 12 (5) submm galaxies (SMGs) at 850um (450um) in the surrounding fields. Number counts of these SMGs are systematically overabundant relative to blank-field submm surveys. Whilst the redshift-sensitive 850um/450um and 850um/1.4GHz flux density ratios indicate that some of these SMGs are likely foreground objects, the counts suggest that many probably lie in the same large-scale structures as the quasars.
rate research
Read More
We present submillimetre continuum observations of a sample of some of the highest redshift quasars currently known, made with the SCUBA bolometer array on the JCMT. The median redshift of the sample is 5.3. Two z>5 objects are strong (6 sigma) detections, with S(850um)>10mJy. A firm (5 sigma) detection is obtained for the z=5.7 quasar SDSS J1044-0125; and SDSS J1306+0356, at z=6.0, is detected with a signal-to-noise approx. 4. For the remainder of the sample we have obtained sensitive (sigma=1.5mJy) upper limits. Submm spectral indices measured for two of the sources are consistent with thermal reradiation from dust, rather than from synchrotron emission. Sensitive 450um upper limits imply that the dust is cool,suggesting large dust masses only 1Gyr after the Big Bang.
We report on submillimetre observations of three high redshift (z>6) quasars, made using the SCUBA camera on the JCMT. Only one of the sample was detected at 850um-- SDSS J1148+5251 (z=6.43). It was also detected (>3 sigma significance) at 450um, one of the few z>4 quasars for which this is the case. In combination with existing millimetric data, the submm detections allow us to place limits on the temperature of the submm-emitting dust, hence on the mass of dust to be synthesized under the time constraint imposed by the quasars redshift.
We use the GALFORM semi-analytical model to study high density regions traced by radio galaxies and quasars at high redshifts. We explore the impact that baryonic physics has upon the properties of galaxies in these environments. Star-forming emission-line galaxies (Ly{alpha} and H{alpha} emitters) are used to probe the environments at high redshifts. Radio galaxies are predicted to be hosted by more massive haloes than quasars, and this is imprinted on the amplitude of galaxy overdensities and cross-correlation functions. We find that Ly{alpha} radiative transfer and AGN feedback indirectly affect the clustering on small scales and also the stellar masses, star- formation rates and gas metallicities of galaxies in dense environments. We also investigate the relation between protoclusters associated with radio galaxies and quasars, and their present- day cluster descendants. The progenitors of massive clusters associated with radio galaxies and quasars allow us to determine an average protocluster size in a simple way. Overdensities within the protoclusters are found to correlate with the halo descendant masses. We present scaling relations that can be applied to observational data. By computing projection effects due to the wavelength resolution of modern spectrographs and narrow-band filters we show that the former have enough spectral resolution to map the structure of protoclusters, whereas the latter can be used to measure the clustering around radio galaxies and quasars over larger scales to determine the mass of dark matter haloes hosting them.
Submillimetre-selected galaxies (SMGs) at high redshift ($z$ $sim$ 2) are potential host galaxies of active galactic nuclei (AGN). If the local Universe is a good guide, $sim$ 50$%$ of the obscured AGN amongst the SMG population could be missed even in the deepest X-ray surveys. Radio observations are insensitive to obscuration; therefore, very long baseline interferometry (VLBI) can be used as a tool to identify AGN in obscured systems. A well-established upper limit to the brightness temperature of 10$^5$ K exists in star-forming systems, thus VLBI observations can distinguish AGN from star-forming systems via brightness temperature measurements. We present 1.6 GHz European VLBI Network (EVN) observations of four SMGs (with measured redshifts) to search for evidence of compact radio components associated with AGN cores. For two of the sources, e-MERLIN images are also presented. Out of the four SMGs observed, we detect one source, J123555.14, that has an integrated EVN flux density of 201 $pm$ 15.2 $mu$Jy, corresponding to a brightness temperature of 5.2 $pm$ 0.7 $times$ 10$^5$ K. We therefore identify that the radio emission from J123555.14 is associated with an AGN. We do not detect compact radio emission from a possible AGN in the remaining sources (J123600.10, J131225.73, and J163650.43). In the case of J131225.73, this is particularly surprising, and the data suggest that this may be an extended, jet-dominated AGN that is resolved by VLBI. Since the morphology of the faint radio source population is still largely unknown at these scales, it is possible that with a $sim$ 10 mas resolution, VLBI misses (or resolves) many radio AGN extended on kiloparsec scales.
We have carried out multicolour imaging of a complete sample of radio-loud quasars at 0.6 < z < 1.1 and find groups or clusters of galaxies in the fields of at least 8 and possibly 13 of the 21 sources. There is no evidence for an evolution in the richness of the environments of radio-loud quasars from other low-redshift studies to z >~ 0.9. The quasars associated with groups and clusters in our sample do not necessarily reside in the centre of the galaxy distribution which rarely displays a spherical geometry. Clustering is preferentially associated with small or asymmetric steep-spectrum radio sources. The quasars with the largest projected angular size are, in nearly all cases, found in non-clustered environments. Radio-based selection (including source size) of high-redshift groups and clusters can be a very efficient method of detecting rich environments at these redshifts. We find that in optical searches for galaxy overdensities above z ~ 0.6 multiple filters must be used. If the single-filter counting statistics used by groups at lower redshift are applied to our data, uncertainties are too large to make accurate quantifications of cluster richness. This means that genuine clustering of galaxies about quasars will be missed and, in ~10% of cases, putative clusters turn out to be false detections. The statistics are further diluted by the fact that galaxy overdensities are generally not centred on the quasar.
Log in to be able to interact and post comments
comments
Fetching comments
Sign in to be able to follow your search criteria
