The host galaxies of active galactic nuclei

Hubble Space Telescope A-band images of a sample of 10 radio galaxies (RG), 10 radio-loud quasars (RLQ) and 13 radio-quiet quasars (RQQ) at redshift z ≃ 0.2 are presented. The sources comprising the radio-loud sub-samples have been selected to be indistinguishable in the P₅Gₕ₂ ~ z plane. The two quasar sub-samples have been similarly selected to have indistinguishable distributions in the V — z plane. All three sub-samples have been analysed with two-dimensional modelling software, designed to accurately determine the host-galaxy parameters.The modelling results show all of the RG, and all of the quasars with Mᵥ < -23, to have bulge-dominated host galaxies, excluding the hypothesis that host morphology is responsible for the radio-loudness dichotomy. Furthermore, the host galaxies are found to be essentially identical to a de Vaucouleurs (ß = 0.25) law, with 30/33 objects having ß parameters in the range 0.2 < ß < 0.3. The hosts of all of the objects studied are found to be extremely luminous (L ≥ L*), with 25/33 objects having L ≥ 2L*, the hosts of the RQQs are found to be typically 0.4 magnitudes fainter than their radio-loud counterparts. The host galaxies of all three sub-samples are found to be larger than average ellipticals (= 10.5 kpc), with a trend found for the RQQ hosts to be some 20% smaller than those of the RLQs. For the first time it is demonstrated that the hosts of quasars, as well as RG, display a Kormendy relation basically identical to that of inactive ellipticals.In combination with the previous K-band modelling of this sample (Taylor et al. 1996) the first set of reliable optical-infrared colours for a significant sample of AGN host galaxies has been determined. The R - K colours of the hosts in all three xxxiii sub-samples are shown to be consistent with each other, with the close agreement of the median colour of R - K=2.5 with that expected from a ~ 14 Gyr-old stellar population implying that the host galaxies of both RGs and quasars are consistent with having formed at high redshift (z ≥ 3).The nuclear colours of the RGs are shown to be perfectly consistent with those of dust reddened RLQ nuclei. The combined luminosity, scalelength, Kormendy relation and R - K colour results for the RG and RLQ sub-samples clearly demonstrate that they are drawn from the same parent population, in strong support of the orientationbased unification scheme of Barthel (1989). The corresponding results for the full 33 object sample show that, in terms of their global structural parameters, the hosts of powerful AGN are no different to normal massive ellipticals.The host galaxy-black-hole mass correlations of Magorrian et al. (1998) and Franceschini et al. (1998) are combined with the AGN modelling results to investigate the quasar radio-loudness dichotomy. All methods of black-hole mass estimation lead to the conclusion that RLQs harbour black-holes of mass ≥ 10¹⁰M⨀. The RQQ blackhole masses estimated via the Magorrian relation are typically smaller than those of the RLQs (~ 5 x 10⁹M⨀), but show sufficient overlap to require the influence of another physical parameter, possibly black-hole spin, to explain the radio-loudness dichotomy. In contrast, the use of the Franceschini black-hole estimator predicts RQQ black-hole masses a factor of two smaller than those of the RLQs, suggesting that black-hole mass alone may be the crucial factor.The application of the modelling technique to an existing HST survey of 3CR radio galaxies at z ~ 1 shows them to have a scalelength distribution and Kormendy relation indistinguishable from their z ~ 0.2 counterparts. The implied luminosity evolution between z ~ 0.2 and z ~ 0.8 is shown to be consistent with that expected from passive evolution alone in a low density Universe, with a high galaxy formation redshift (z ≥ 3). The lack of evidence for significant merger activity in the redshift range 0.2 < z < 0.8 leads to the conclusion that the traditional passive evolution interpretation of the radio galaxy K - z relation remains acceptable

The host galaxies and black-hole:galaxy mass ratios of luminous quasars at z~4

We present and analyse the deepest, high-quality Ks-band images ever obtained of luminous quasars at z~4, in an attempt to determine the basic properties of their host galaxies less than 1 Gyr after the first recorded appearance of black holes with Mbh > 10^9 Msol. To maximise the robustness of our results we have carefully selected two SDSS quasars at z~4. These quasars are representative of the most luminous quasars known at this epoch but they also, crucially, lie within 40 arcsec of comparably-bright foreground stars (required for accurate PSF definition), and have redshifts which ensure line-free Ks-band imaging. The data were obtained in excellent seeing (<0.4-arcsec) at the ESO VLT with integration times of ~5.5 hours per source. Via carefully-controlled separation of host-galaxy and nuclear light, we estimate the luminosities and stellar masses of the host galaxies, and set constraints on their half-light radii. The quasar host galaxies have K-band luminosities similar to radio galaxies at comparable redshifts, suggesting that these quasar hosts are also among the most massive galaxies in existence at this epoch. However, the quasar hosts are a factor ~5 smaller than the host galaxies of luminous low-redshift quasars. We estimate the stellar masses of the z~4 host galaxies to lie in the range 2-10x10^11 Msol, and use the CIV emission line in the Sloan spectra to estimate the masses of their black holes. The results imply a black-hole:host-galaxy mass ratio Mbh:Mgal~0.01-0.05. This is an order of magnitude higher than typically seen in the low-redshift Universe, and is consistent with existing evidence for a systematic growth in this mass ratio with increasing redshift, at least for objects selected as powerful AGN.Comment: 10 pages, 6 figure

Deep GMOS Spectroscopy of Extremely Red Galaxies in GOODS-South: Ellipticals, Mergers and Red Spirals at 1<z<2

We have performed a deep spectroscopic survey of extremely red galaxies on the GOODS-South field, using GMOS on Gemini South. We present here spectra and redshifts for 16 ERGs at 0.87<z<2.02, to a limit K=20.2. The ERHs are a mixture of spheroidals, mergers and spirals, with one AGN. For at least 10 of these galaxies we observe [OII] emission lines. We perform an age-dating analysis by fitting the spectra and 9-band photometry of the ERGs with models of passively evolving stellar populations combined with a younger star-forming component. The best-fitting ages for the old stellar components range from 0.6 to 4.5 Gyr, with a mean 2.1 Gyr. Masses range from 3 to 20 times 10^10 solar masses. The star-forming component typically forms a few per cent of the total mass, with dust reddening averaging E(B-V)=0.35. Its timescale tends to be short for mergers (<50 Myr) and longer (200-800 Myr) for spiral ERGs.Comment: 19 pages, 9 figure

A near-infrared morphological comparison of high-redshift submm and radio galaxies: massive star-forming discs vs relaxed spheroids

We present deep, high-quality K-band images of complete subsamples of powerful radio and sub-mm galaxies at z=2. The data were obtained in the best available seeing at UKIRT and Gemini North, with integration times scaled to ensure that comparable rest-frame surface brightness levels are reached for all galaxies. We fit two-dimensional axi-symmetric galaxy models to determine galaxy morphologies at rest-frame optical wavelengths > 4000A, varying luminosity, axial ratio, half-light radius, and Sersic index. We find that, while some images show evidence of galaxy interactions, >95% of the rest-frame optical light in all galaxies is well-described by these simple models. We also find a clear difference in morphology between these two classes of galaxy; fits to the individual images and image stacks reveal that the radio galaxies are moderately large (=8.4+-1.1kpc; median r{1/2}=7.8), de Vaucouleurs spheroids ( = 4.07+-0.27; median n=3.87), while the sub-mm galaxies appear to be moderately compact (=3.4+-0.3kpc; median r{1/2}=3.1kpc) exponential discs (=1.44+-0.16; median n=1.08). We show that the z=2 radio galaxies display a well-defined Kormendy relation but that, while larger than other recently-studied high-z massive galaxy populations, they are still ~1.5 times smaller than their local counterparts. The scalelengths of the starlight in the sub-mm galaxies are comparable to those reported for the molecular gas. Their sizes are also similar to those of comparably massive quiescent galaxies at z>1.5. In terms of stellar mass surface density, the majority of the radio galaxies lie within the locus defined by local ellipticals. In contrast, while best modelled as discs, most of the sub-mm galaxies have higher stellar mass densities than local galaxies, and appear destined to evolve into present-day massive ellipticals.Comment: 24 pages, 9 figure

The cosmological evolution of quasar black-hole masses

Virial black-hole mass estimates are presented for 12698 quasars in the redshift interval 0.1<z<2.1, based on modelling of spectra from the Sloan Digital Sky Survey (SDSS) first data release. The black-hole masses of the SDSS quasars are found to lie between \simeq10^{7}\Msun and an upper limit of \simeq 3\times 10^{9}\Msun, entirely consistent with the largest black-hole masses found to date in the local Universe. The estimated Eddington ratios of the broad-line quasars (FWHM\geq 2000 kms^{-1}) show a clear upper boundary at $L_{bol}/L_{Edd}\simeq 1$, suggesting that the Eddington luminosity is still a relevant physical limit to the accretion rate of luminous broad-line quasars at $z\leq 2$. By combining the black-hole mass distribution of the SDSS quasars with the 2dF quasar luminosity function, the number density of active black holes at $z\simeq 2$ is estimated as a function of mass. In addition, we independently estimate the local black-hole mass function for early-types using the $M_{bh}-\sigma$ and $M_{bh}-L_{bulge}$ correlations. Based on the SDSS velocity dispersion function and the 2MASS $K-$band luminosity function, both estimates are found to be consistent at the high-mass end (M_{bh}\geq 10^{8}\Msun). By comparing the estimated number density of active black holes at $z\simeq 2$ with the local mass density of dormant black holes, we set lower limits on the quasar lifetimes and find that the majority of black holes with mass \geq 10^{8.5}\Msun are in place by $\simeq 2$.Comment: 15 pages, 10 figures, revised version, accepted for publication by MNRA

The host galaxies of luminous quasars

We present results of a deep HST/WFPC2 imaging study of 17 quasars at z~0.4, designed to determine the properties of their host galaxies. The sample consists of quasars with absolute magnitudes in the range -24>M_V>-28, allowing us to investigate host galaxy properties across a decade in quasar luminosity, but at a single redshift. We find that the hosts of all the RLQs, and all the RQQs with nuclear luminosities M_V<-24, are massive bulge-dominated galaxies, confirming and extending the trends deduced from our previous studies. From the best-fitting model host galaxies we have estimated spheroid and black-hole masses, and the efficiency (with respect to Eddington luminosity) with which each quasar is radiating. The largest inferred black-hole mass in our sample is \~3.10^9 M_sun, comparable to those at the centres of M87 and Cygnus A. We find no evidence for super-Eddington accretion in even the most luminous objects. We investigate the role of scatter in the black-hole:spheroid mass relation in determining the ratio of quasar to host-galaxy luminosity, by generating simulated populations of quasars lying in hosts with a Schechter mass function. Within the subsample of the highest luminosity quasars, the observed variation in nuclear-host luminosity ratio is consistent with being the result of the scatter in the black-hole:spheroid relation. Quasars with high nuclear-host ratios can be explained by sub-Eddington accretion onto black holes in the high-mass tail of the black-hole:spheroid relation. Our results imply that, owing to the Schechter cutoff, host mass should not continue to increase linearly with quasar luminosity, at the very highest luminosities. Any quasars more luminous than M_V=-27 should be found in massive elliptical hosts which at the present day would have M_V ~ -24.5.Comment: Accepted for publication in MNRAS. 18 pages; 7 figures and 17 greyscale images are reproduced here at low quality due to space limitations. High-resolution figures are available from ftp://ftp.roe.ac.uk/pub/djef/preprints/floyd2004

An optimal ALMA image of the Hubble Ultra Deep Field in the era of JWST: obscured star formation and the cosmic far-infrared background

We combine archival ALMA data targeting the Hubble Ultra Deep Field (HUDF) to produce the deepest currently attainable 1-mm maps of this key, extragalactic survey field. Combining all existing data in Band 6, our deepest map covers 4.2arcmin^2, with a beamsize of 1.49"x1.07" at an effective frequency of 243GHz (1.23mm). It reaches an rms of 4.6uJy/beam, with 1.5arcmin^2 below 9.0uJy/beam, an improvement of >5% over the best previously published map and 50% improvement in some regions. We also make a wider, but shallower map, covering 25.4arcmin^2. We detect 45 galaxies in the deep map down to 3.6sigma, including 10 more 1-mm sources than previously detected. 38 of these galaxies have a JWST ID from the JADES NIRCam imaging and the new sources are typically faint and red. A stacking analysis on the positions of ALMA-undetected JADES galaxies yields detections for z<4 and stellar masses from 10^(8.4) to 10^(10.4)Msun, extracting 10% of additional stacked signal from our map compared to previous analyses. Detected sources and stacking contribute (10.0+/-0.5)Jy/deg^2 of the cosmic infrared background (CIB) at 1.23mm. Although this is short of the (uncertain) background level of about 20Jy/deg^2, after taking into account intrinsic fluctuations in the CIB, our measurement is consistent with the background if the HUDF is a mild (~2sigma) negative fluctuation. This suggests that within the HUDF, JWST may have detected essentially all of the galaxies that contribute to the CIB. Our stacking analysis predicts that the field contains around 60 additional galaxies with 1.23mm flux densities averaging around 15uJy, and over 300 galaxies at the few uJy level. However, the contribution of these fainter more modestly-obscured objects to the background is small, and converging, as anticipated from the now well-established strong correlation between galaxy stellar mass and obscured star formation.Comment: Submitted to MNRA

Accounting for Cosmic Variance in Studies of Gravitationally-Lensed High-Redshift Galaxies in the Hubble Frontier Field Clusters

Strong gravitational lensing provides a powerful means for studying faint galaxies in the distant universe. By magnifying the apparent brightness of background sources, massive clusters enable the detection of galaxies fainter than the usual sensitivity limit for blank fields. However, this gain in effective sensitivity comes at the cost of a reduced survey volume and, in this {\it Letter}, we demonstrate there is an associated increase in the cosmic variance uncertainty. As an example, we show that the cosmic variance uncertainty of the high redshift population viewed through the Hubble Space Telescope Frontier Field cluster Abell 2744 increases from ~35% at redshift z~7 to >~65% at z~10. Previous studies of high redshift galaxies identified in the Frontier Fields have underestimated the cosmic variance uncertainty that will affect the ultimate constraints on both the faint end slope of the high-redshift luminosity function and the cosmic star formation rate density, key goals of the Frontier Field program.Comment: 5 pages, 3 figures. Version accepted by ApJ