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To examine health-related self-efficacy for individuals following acquired brain or spinal cord injury prior to enrollment in a weight-loss intervention and associations with demographics, injury characteristics, and additional physiologic variables. Cross-sectional analysis of baseline data for community-dwelling adults following stroke (CVA), traumatic brain injury (TBI), or spinal cord injury (SCI) across three disability-adapted weight-loss interventions. Overall results suggest a significant difference between injury type and self-efficacy as measured by the Self Rated Abilities for Health Practices (SRAHP) scale. On average, individuals with SCI had the lowest overall perceived self-efficacy of the three groups (11.2-unit difference; (CI: −17.4, −5.0), followed by those with TBI (9.5-unit difference; (CI: −16.7, −2.4). There were also differences between groups in age, number of household members, time since injury, sex, race, marital status, physiological measures, and employment status. Results suggest that individuals with different disabilities following neurological injuries have different baseline perceptions in their ability to eat a healthy diet and exercise regularly. Health interventions should be tailored for these groups based on disability-specific barriers and should include components to enhance health-related self-efficacy to address weight management among these populations. Evidence suggests that health-related self-efficacy may differ following different injury types and level of disability may impact one's ability to maintain health-related behaviors Results suggest that individuals with a spinal cord injury may have different baseline perceptions of self-efficacy related to their ability to eat a healthy diet and exercise regularly compared to those with a traumatic brain injury or stroke. Health interventions should be tailored to encompass disability-specific barriers which may impact an individual's health-related self-efficacy. [ABSTRACT FROM AUTHOR]

We present a revised measurement of the extragalactic background light (EBL) at radio frequencies based on a near complete compendium of radio source counts. We present the radio-EBL at 150 MHz, 325 MHz, 610 MHz, 1.4 GHz, 3 GHz, 5 GHz, and 8.4 GHz. In all cases the contribution to the radio-EBL, per decade of flux, exhibits a two-humped distribution well matched to the active galactic nucleus (AGN) and star-forming galaxy (SFG) populations, and with each population contributing roughly equal energy. Only at 3 GHz are the source count contributions to the EBL fully convergent, and hence we report empirical lower limits to the radio-EBL in the remaining bands. Adopting predictions from the SHARK semi-analytic model for the form of the SFG population, we can fit the fainter source counts providing measurements of the total contribution to the radio-EBL for the SFG and the AGN populations separately. This constitutes an empirically constrained model-dependent measurement for the SFG contribution, but a fully empirical measurement of the AGN contribution. Using the ProSpect spectral energy distribution code we can model the ultraviolet-optical-infrared-mm-radio SFG EBL at all frequencies from the cosmic star-formation history and the adoption of a Chabrier initial mass function. However, significant discrepancy remains (5 ×) between our source-count estimates of the radio-EBL and the direct measurements reported from the Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission-2 (ARCADE-2) experiment. We can rule out a significant missing discrete source radio population and suggest that the cause of the high ARCADE-2 radio-EBL values may need to be sought either in the foreground subtraction or as a yet unknown diffuse component in the radio sky. [ABSTRACT FROM AUTHOR]

We construct the halo mass function (HMF) from the GAMA (Galaxy And Mass Assembly) galaxy group catalogue over the mass range of 1012.7–1015.5 M⊙, and find good agreement with the expectation from Lambda cold dark matter. In comparison to previous studies, this result extends the mass range over which the HMF has now been measured over by an order of magnitude. We combine the GAMA data release (DR) 4 HMF with similar data from the Sloan Digital Sky Survey (SDSS) DR12 and REFLEX II (ROSAT -ESO Flux Limited X-ray Galaxy Cluster Survey) surveys, and fit a four-parameter Murray–Robotham–Power function, valid at |$\tilde{z} \approx 0.1$|⁠ , yielding a density normalization of log10 (ϕ* Mpc |$^{3})= -3.96^{+0.55}_{-0.82}$|⁠ , a high mass turnover of log10 (M * M |$_{\odot }^{-1})=14.13^{+0.43}_{-0.40}$|⁠ , a low-mass power-law slope of |$\alpha =-1.68^{+0.21}_{-0.24}$|⁠ , and a high-mass softening parameter of |$\beta =0.63^{+0.25}_{-0.11}$|⁠. If we fold in the constraint on ΩM from the Planck 2018 cosmology, we are able to reduce these uncertainties further, but this relies on the assumption that the power-law trend can be extrapolated from 1012.7 M⊙ to zero mass. Throughout, we highlight the effort needed to improve on our HMF measurement: improved halo mass estimates that do not rely on calibration to simulations; reduced halo mass uncertainties needed to mitigate the strong Eddington bias that arises from the steepness of the HMF low-mass slope; and deeper wider area spectroscopic surveys. To our halo mass limit of 1012.7 M⊙, we are directly resolving ('seeing') 41 ± 5 per cent of the total mass density, i.e. ΩM,>12.7 = 0.128 ± 0.016, opening the door for the direct construction of three-dimensional dark matter mass maps at Mpc resolution. [ABSTRACT FROM AUTHOR]

In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to r KiDS = 19.65 mag), and is well-suited for the study of galaxy mergers, galaxy groups, and the low redshift (z  < 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX , ESO KiDS, ESO VIKING, WISE , and Herschel Space Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z  < 0.08, photometric redshift estimates for all 18 million objects to r KiDS ∼ 25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M |$_{\odot } \, h_{70}^{-2}$| and we find a total stellar mass density of ρ * = (2.97 ± 0.04) × 108 M |$_{\odot } \, h_{70}$|  Mpc−3 or |$\Omega _*=(2.17 \pm 0.03) \times 10^{-3} \, h_{70}^{-1}$|⁠. We conclude that at z  < 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population. [ABSTRACT FROM AUTHOR]

To examine the usability of an Apple Watch-based, two-way Personalized Mobile Trainer (PMT) in community-based exercise programs for individuals with chronic traumatic brain injury (cTBI). This is a prospective pilot study. Twenty participants with cTBI aged 46–73 were enrolled in a 3-month individualized exercise program. After one in-person training session on PMT and exercise program, participants were prescribed either aerobic exercise training (AET) or stretching and toning (SAT) performed at home. The PMT was used to remotely deliver updated exercise prescription, track exercise progress, and communicate with the participants. The primary outcome was compliance with the exercise programs. All the participants completed the assigned exercise program with an average compliance of 76%. Nineteen (95%) participants were able to use the PMT properly during exercise sessions. After 3 months of training, the AET trended toward maintaining exercise endurance when compared with the SAT group (0.3% vs −4%, p = 0.14) with a medium effect size of 0.43. Using the PMT system to support and track exercise in community-based exercise programs is feasible. The PMT may promote compliance with the training program but testing its effectiveness with larger trials is warranted. [ABSTRACT FROM AUTHOR]

The Galaxy And Mass Assembly Survey (GAMA) covers five fields with highly complete spectroscopic coverage (>95 per cent) to intermediate depths (r < 19.8 or i < 19.0 mag), and collectively spans 250 deg2 of equatorial or southern sky. Four of the GAMA fields (G09, G12, G15, and G23) reside in the European Southern Observatory (ESO) VST KiDS and ESO VISTA VIKING survey footprints, which combined with our GALEX, WISE , and Herschel data provide deep uniform imaging in the |$FUV/NUV/u/g/r/i/Z/Y/J/H/K_s/W1/W2/W3/W4/P100/P160/S250/S350/S500$| bands. Following the release of KiDS DR4, we describe the process by which we ingest the KiDS data into GAMA (replacing the SDSS data previously used for G09, G12, and G15), and redefine our core optical and near-infrared (NIR) catalogues to provide a complete and homogeneous data set. The source extraction and analysis is based on the new ProFound image analysis package, providing matched-segment photometry across all bands. The data are classified into stars, galaxies, artefacts, and ambiguous objects, and objects are linked to the GAMA spectroscopic target catalogue. Additionally, a new technique is employed utilizing ProFound to extract photometry in the unresolved MIR–FIR regime. The catalogues including the full FUV–FIR photometry are described and will be fully available as part of GAMA DR4. They are intended for both standalone science, selection for targeted follow-up with 4MOST, as well as an accompaniment to the upcoming and ongoing radio arrays now studying the GAMA 23h field. [ABSTRACT FROM AUTHOR]

Background: To prepare patients with traumatic brain injury (TBI) for discharge from inpatient rehabilitation, physical therapists may incorporate dual-task gait activities. Reliability of common dual-task measures for people with TBI in inpatient rehabilitation is undetermined. Our purpose was to assess inter-rater and intra-rater reliability and clinical feasibility of dual-task measures [Walking While Talking Test (WWTT), Modified Walking and Remembering Task (mWART), Timed Up and Go-cognitive (TUG-COG)] in inpatient rehabilitation for patients with TBI. Methods: A total of 22 individuals with TBI completing the dual-task measures (WWTT, Walking and Remembering Task (WART), and TUG-COG) in inpatient rehabilitation were rated concurrently by two physical therapists in a single testing session. Sessions were video recorded and rated by the same raters viewing the video 7–10 days later. Raters completed a survey assessing feasibility of conducting the dual-task measures in patients with TBI in inpatient rehabilitation. Data were analyzed by calculating ICC(2,1) for inter-rater reliability and ICC(3,1) for intra-rater reliability. Results: All dual-task measures (WWTT, mWART, TUG-COG) had excellent inter-rater and intra-rater reliability. Raters considered dual-task measures feasible for patients with TBI during inpatient rehabilitation. Conclusions: The WWTT, mWART, and TUG-COG have excellent reliability and appear clinically feasible for incorporation into clinical practice in inpatient rehabilitation following TBI. [ABSTRACT FROM AUTHOR]

Galaxies and their dark matter haloes are part of a complex network of mass structures, collectively called the cosmic web. Using the tidal tensor prescription these structures can be classified into four cosmic environments: voids, sheets, filaments and knots. As the cosmicweb may influence the formation and evolution of dark matter haloes and the galaxies they host, we aim to study the effect of these cosmic environments on the average mass of galactic haloes. To this end we measure the galaxy–galaxy lensing profile of 91 195 galaxies, within 0.039 < z < 0.263, from the spectroscopic Galaxy And Mass Assembly survey, using ∼100 deg2 of overlapping data from the Kilo-Degree Survey. In each of the four cosmic environments we model the contributions from group centrals, satellites and neighbouring groups to the stacked galaxy–galaxy lensing profiles. After correcting the lens samples for differences in the stellar mass distribution, we find no dependence of the average halo mass of central galaxies on their cosmic environment. We do find a significant increase in the average contribution of neighbouring groups to the lensing profile in increasingly dense cosmic environments. We show, however, that the observed effect can be entirely attributed to the galaxy density at much smaller scales (within 4 h−1 Mpc), which is correlated with the density of the cosmic environments. Within our current uncertainties we find no direct dependence of galaxy halo mass on their cosmic environment. [ABSTRACT FROM AUTHOR]

In this paper, we demonstrate a new method for fitting galaxy profiles which makes use of the full multiwavelength data provided by modern large optical–near-infrared imaging surveys. We present a new version of galapagos, which utilizes a recently developed multiwavelength version of galfit, and enables the automated measurement of wavelength-dependent Sérsic profile parameters for very large samples of galaxies. Our new technique is extensively tested to assess the reliability of both pieces of software, galfit and galapagos on both real ugrizY JHK imaging data from the Galaxy And Mass Assembly survey and simulated data made to the same specifications. We find that fitting galaxy light profiles with multiwavelength data increases the stability and accuracy of the measured parameters, and hence produces more complete and meaningful multiwavelength photometry than has been available previously. The improvement is particularly significant for magnitudes in low-S/N bands and for structural parameters like half-light radius re and Sérsic index n for which a prior is used by constraining these parameters to a polynomial as a function of wavelength. This allows the fitting routines to push the magnitude of galaxies for which sensible values can be derived to fainter limits. The technique utilizes a smooth transition of galaxy parameters with wavelength, creating more physically meaningful transitions than single-band fitting and allows accurate interpolation between passbands, perfect for derivation of rest-frame values. [ABSTRACT FROM AUTHOR]

We combine data from the Millennium Galaxy Catalogue, Sloan Digital Sky Survey and UKIRT Infrared Deep Sky Survey Large Area Survey to produce ugrizYJHK luminosity functions and densities from within a common, low-redshift volume ( for systems) with 100 per cent spectroscopic completeness. In the optical the fitted Schechter functions are comparable in shape to those previously reported values but with higher normalizations (typically 0, 30, 20, 15, 5 per cent higher values in , respectively, over those reported by the SDSS team). We attribute these to differences in the redshift ranges probed, incompleteness and adopted normalization methods. In the near-IR (NIR) we find significantly different Schechter function parameters (mainly in the values) to those previously reported and attribute this to the improvement in the quality of the imaging data over previous studies. This is the first homogeneous measurement of the extragalactic luminosity density which fully samples both the optical and NIR regimes. Unlike previous compilations that have noted a discontinuity between the optical and NIR regimes our homogeneous data set shows a smooth cosmic spectral energy distribution (CSED). After correcting for dust attenuation we compare our CSED to the expected values based on recent constraints on the cosmic star formation history and the initial mass function. [ABSTRACT FROM AUTHOR]

Supermassive black hole (SMBH) mass estimates are derived for 1743 galaxies from the Millennium Galaxy Catalogue (MGC) using the recently revised empirical relation between SMBH mass and the luminosity of the host spheroid. The MGC spheroid luminosities are based on bulge plus exponential-disc decompositions. The majority of black hole masses reside between and an upper limit of . Using previously determined space-density weights, we derive the SMBH mass function which we fit with a Schechter-like function. Integrating the black hole mass function over gives an SMBH mass density of ( for early-type galaxies and ( for late-type galaxies. The errors are estimated from Monte Carlo simulations which include the uncertainties in the relation, the luminosity of the host spheroid and the intrinsic scatter of the relation. Assuming SMBHs form via baryonic accretion, we find that ( per cent of the Universe's baryons are currently locked up in SMBHs. This result is consistent with our previous estimate based on the (Sérsic index) relation. [ABSTRACT FROM AUTHOR]

Simon P Driver, Peder Norberg, Ivan K Baldry, Steven P Bamford, Andrew M Hopkins, Jochen Liske, Jon Loveday, John A Peacock and the GAMA Survey Team (Galaxy and Mass Assembly) review progress on the latest large galaxy redshift survey now underway on the 3.9 m Anglo-Australian Telescope. [ABSTRACT FROM AUTHOR]

We provide a new estimate of the local supermassive black hole mass function using (i) the empirical relation between supermassive black hole mass and the Sérsic index of the host spheroidal stellar system and (ii) the measured (spheroid) Sérsic indices drawn from 10k galaxies in the Millennium Galaxy Catalogue. The observational simplicity of our approach, and the direct measurements of the black hole predictor quantity, i.e. the Sérsic index, for both elliptical galaxies and the bulges of disc galaxies makes it straightforward to estimate accurate black hole masses in early- and late-type galaxies alike. We have parametrized the supermassive black hole mass function with a Schechter function and find, at the low-mass end, a logarithmic slope (1 +α) of ∼0.7 for the full galaxy sample and ∼1.0 for the early-type galaxy sample. Considering spheroidal stellar systems brighter than , and integrating down to black hole masses of , we find that the local mass density of supermassive black holes in early-type galaxies , and in late-type galaxies . The uncertainties are derived from Monte Carlo simulations which include uncertainties in the relation, the catalogue of Sérsic indices, the galaxy weights and Malmquist bias. The combined, cosmological, supermassive black hole mass density is thus . That is, using a new and independent method, we conclude that per cent of the Universe's baryons are presently locked up in supermassive black holes at the centres of galaxies. [ABSTRACT FROM AUTHOR]

We present a detailed investigation into the recent star formation histories of 5697 luminous red galaxies (LRGs) based on the Hδ (4101 Å), and [O ii] (3727 Å) lines and the D4000 index. LRGs are luminous galaxies which have been selected to have photometric properties consistent with an old, passively evolving stellar population. For this study, we utilize LRGs from the recently completed 2dF-SDSS LRG and QSO Survey (2SLAQ). Equivalent widths of the Hδ and [O ii] lines are measured and used to define three spectral types, those with only strong Hδ absorption (k+a), those with strong [O ii] in emission (em) and those with both (em+a). All other LRGs are considered to have passive star formation histories. The vast majority of LRGs are found to be passive (∼80 per cent); however, significant numbers of k+a (2.7 per cent), em+a (1.2 per cent) and em LRGs (8.6 per cent) are identified. An investigation into the redshift dependence of the fractions is also performed. A sample of SDSS MAIN galaxies with colours and luminosities consistent with the 2SLAQ LRGs is selected to provide a low-redshift comparison. While the em and em+a fractions are consistent with the low-redshift SDSS sample, the fraction of k+a LRGs is found to increase significantly with redshift. This result is interpreted as an indication of an increasing amount of recent star formation activity in LRGs with redshift. By considering the expected lifetime of the k+a phase, the number of LRGs which will undergo a k+a phase can be estimated. A crude comparison of this estimate with the predictions from semi-analytic models of galaxy formation shows that the predicted level of k+a and em+a activities is not sufficient to reconcile the predicted mass growth for massive early types in a hierarchical merging scenario. [ABSTRACT FROM AUTHOR]

We present a spectroscopic survey of almost 15 000 candidate intermediate-redshift luminous red galaxies (LRGs) brighter than , observed with 2dF on the Anglo-Australian Telescope. The targets were selected photometrically from the Sloan Digital Sky Survey (SDSS) and lie along two narrow equatorial strips covering 180 deg2. Reliable redshifts were obtained for 92 per cent of the targets and the selection is very efficient: over 90 per cent have . More than 80 per cent of the red galaxies have pure absorption-line spectra consistent with a passively evolving old stellar population. The redshift, photometric and spatial distributions of the LRGs are described. The 2SLAQ data will be released publicly from mid-2006, providing a powerful resource for observational cosmology and the study of galaxy evolution. [ABSTRACT FROM AUTHOR]

We present an analysis of the relative bias between early- and late-type galaxies in the Two-degree Field Galaxy Redshift Survey (2dFGRS)– as defined by theη parameter of Madgwick et al., which quantifies the spectral type of galaxies in the survey. We calculate counts in cells for flux-limited samples of early- and late-type galaxies, using approximately cubical cells with sides ranging from 7 to. We measure the variance of the counts in cells using the method of Efstathiou et al., which we find requires a correction for a finite volume effect equivalent to the integral constraint bias of the autocorrelation function. Using a maximum-likelihood technique we fit lognormal models to the one-point density distribution, and develop methods of dealing with biases in the recovered variances resulting from this technique. We then examine the joint density distribution function,, and directly fit deterministic bias models to the joint counts in cells. We measure a linear relative bias of≈1.3, which does not vary significantly withℓ. A deterministic linear bias model is, however, a poor approximation to the data, especially on small scaleswhere deterministic linear bias is excluded at high significance. A power-law bias model with indexis a significantly better fit to the data on all scales, although linear bias becomes consistent with the data for. [ABSTRACT FROM AUTHOR]

It is well known that the clustering of galaxies depends on galaxy type. Suchrelative biascomplicates the inference of cosmological parameters from galaxy redshift surveys, and is a challenge to theories of galaxy formation and evolution. In this paper we perform a joint counts-in-cells analysis on galaxies in the 2dF Galaxy Redshift Survey, classified by both colour and spectral type,η, as early- or late-type galaxies. We fit three different models of relative bias to the joint probability distribution of the cell counts, assuming Poisson sampling of the galaxy density field. We investigate the non-linearity and stochasticity of the relative bias, with cubic cells of side. Exact linear bias is ruled out with high significance on all scales. Power-law bias gives a better fit, but likelihood ratios prefer a bivariate lognormal distribution, with a non-zero‘stochasticity’, i.e. scatter that may result from physical effects on galaxy formation other than those from the local density field. Using this model, we measure a correlation coefficient in log-density space (rLN) of 0.958 for cells of length, increasing to 0.970 by. This corresponds to a stochasticityofand, respectively. For smaller cells, the Poisson-sampled lognormal distribution presents an increasingly poor fit to the data, especially with regard to the fraction of completely empty cells. We compare these trends with the predictions of semi-analytic galaxy formation models: these match the data well in terms of the overall level of stochasticity, variation with scale and the fraction of empty cells. [ABSTRACT FROM AUTHOR]

Focuses on two-point correlation functions in redshift space for galaxies of different spectral types in the galaxy redshift survey. Estimate of the linear redshift space distortion parameter; Tendency of the relative bias to a constant; Consistency of the result with similar degrees of redshift space distortions.

We use more than 110 500 galaxies from the 2dF Galaxy Redshift Survey (2dFGRS) to estimate the b[sub J]-band galaxy luminosity function at redshift z = 0, taking account of evolution, the distribution of magnitude measurement errors and small corrections for incompleteness in the galaxy catalogue. Throughout the interval -16.5 > Mb[sub J] - 5 log[sub 10] h >-22, the luminosity function is accurately described by a Schechter function with M[sup *][sub b][sub J] - 5 log[sub 10] h = -19.66 ± 0.07, α = -1.21 ± 0.03 and Φ[sup *] = (1.61 ± 0.08) × 10[sup -2] h³ Mpc[sup -3], giving an integrated luminosity density of ρ[sub L] = (1.82 ± 0.17) × 10[sup 8] h L[sub ...] Mpc[sup -3] (assuming an Ω[sub 0] = 0.3, Λ[sub 0] = 0.7 cosmology). The quoted errors have contributions from the accuracy of the photometric zero-point, from large-scale structure in the galaxy distribution and, importantly, from the uncertainty in the appropriate evolutionary corrections. Our luminosity function is in excellent agreement with, but has much smaller statistical errors than, an estimate from the Sloan Digital Sky Survey (SDSS) data when the SDSS data are accurately translated to the b[sub J] band and the luminosity functions are normalized in the same way. We use the luminosity function, along with maps describing the redshift completeness of the current 2dFGRS catalogue, and its weak dependence on apparent magnitude, to define a complete description of the 2dFGRS selection function. Details and tests of the calibration of the 2dFGRS photometric parent catalogue are also presented. [ABSTRACT FROM AUTHOR]

We compare the amplitudes of fluctuations probed by the 2dF Galaxy Redshift Survey (2dFGRS) and by the latest measurements of the cosmic microwave background (CMB) anisotropies. By combining the 2dFGRS and CMB data, we find the linear-theory rms mass fluctuations in 8 h[sup -1] Mpc spheres to be σ[sub 8m]=0.73±0.05 (after marginalization over the matter density parameter Ω[sub m] and three other free parameters). This normalization is lower than the COBE normalization and previous estimates from cluster abundance, but it is in agreement with some revised cluster abundance determinations. We also estimate the scale-independent bias parameter of present-epoch L[sub s]=1.9L∗ APM-selected galaxies to be b(L[sub s],z=0)=1.10±0.08 on comoving scales of 0.02

The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250 000 galaxies. This paper describes the survey design, the spectroscopic observations, the redshift measurements and the survey data base. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2° diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than . The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning around the SGP, and the other in the northern Galactic hemisphere spanning along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 deg[sup 2] and has a median depth of . Adaptive tiling is used to give a highly uniform sampling rate of 93 per cent over the whole survey region. Redshifts are measured from spectra covering at a two-pixel resolution of 9.0 Å and a median S/N of 13 pixel[sup -1]. All redshift identifications are visually checked and assigned a quality parameter Q in the range redshifts are 98.4 per cent reliable and have an rms uncertainty of 85 km s[sup -1]. The overall redshift completeness for redshifts is 91.8 per cent, but this varies with magnitude from 99 per cent for the brightest galaxies to 90 per cent for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. [ABSTRACT FROM AUTHOR]

We combine the Two Micron All Sky Survey (2MASS) Extended Source Catalogue and the 2dF Galaxy Redshift Survey to produce an infrared selected galaxy catalogue with 17 173 measured redshifts. We use this extensive data set to estimate the galaxy luminosity functions in the J- and K[sub S]-bands. The luminosity functions are fairly well fitted by Schechter functions with parameters M[sub J][sup *]-5 log h=-22.36±0.02, α[sub J]=-0.93±0.04, Φ[sub J][sup *]=0.0104±0.0016 h[sup 3] Mpc[sup -3] in the J-band and M[sub K[sub S]][sup *]-5 log h=-23.44±0.03, α[sub K[sub S]]=-0.96±0.05, Φ[sub K[sub S]][sup *]=0.0108±0.0016 h[sup 3] Mpc[sup -3] in the K[sub S]-band (2MASS Kron magnitudes). These parameters are derived assuming a cosmological model with Ω[sub 0]=0.3 and Λ[sub 0]=0.7. With data sets of this size, systematic rather than random errors are the dominant source of uncertainty in the determination of the luminosity function. We carry out a careful investigation of possible systematic effects in our data. The surface brightness distribution of the sample shows no evidence that significant numbers of low surface brightness or compact galaxies are missed by the survey. We estimate the present-day distributions of b[sub J]-K[sub S] and J-K[sub S] colours as a function of the absolute magnitude and use models of the galaxy stellar populations, constrained by the observed optical and infrared colours, to infer the galaxy stellar mass function. Integrated over all galaxy masses, this yields a total mass fraction in stars (in units of the critical mass density) of Ω[sub stars]h =(1.6±0.24)×10[sup -3] for a Kennicutt initial mass function (IMF) and Ω[sub stars]h =(2.9±0.43)×10[sup -3] for a Salpeter IMF. These values are consistent with those inferred from observational estimates of the total star formation history of the Universe provided that dust extinction corrections are modest. [ABSTRACT FROM AUTHOR]