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PurposeMalignant pleural mesothelioma (MPM) has a high symptom burden and poor survival. Evidence from other cancer types suggests some benefit in health-related quality of life (HRQoL) with early specialist palliative care (SPC) integrated with oncological services, but the certainty of evidence is low.MethodsWe performed a multicentre, randomised, parallel group controlled trial comparing early referral to SPC versus standard care across 19 hospital sites in the UK and one large site in Western Australia. Participants had newly diagnosed MPM; main carers were additionally recruited. Intervention: review by SPC within 3 weeks of allocation and every 4 weeks throughout the study. HRQoL was assessed at baseline and every 4 weeks with the European Organization for Research and Treatment of Cancer (EORTC) Quality of Life Questionnaire Core 30. Primary outcome: change in EORTC C30 Global Health Status 12 weeks after randomisation.ResultsBetween April 2014 and October 2016, 174 participants were randomised. There was no significant between group difference in HRQoL score at 12 weeks (mean difference 1.8 (95% CI −4.9 to 8.5; p=0.59)). HRQoL did not differ at 24 weeks (mean difference −2.0 (95% CI −8.6 to 4.6; p=0.54)). There was no difference in depression/anxiety scores at 12 weeks or 24 weeks. In carers, there was no difference in HRQoL or mood at 12 weeks or 24 weeks, although there was a consistent preference for care, favouring the intervention arm.ConclusionThere is no role for routine referral to SPC soon after diagnosis of MPM for patients who are cared for in centres with good access to SPC when required.Trial registration numberISRCTN18955704.

Obscured quasars hidden in deep X-ray surveys can be recovered by looking at mid-infrared wavelengths, where dust re-radiates the absorbed radiation. Here we present a sample of obscured quasars in the redshift range 1 < z < 4 based on data from the UKIDSS Ultra-Deep Survey (UDS), the deepest near-IR survey over ~ 1 sq. deg. to date. Candidates that are primarily selected by their 24 μm emission are probed by decomposing their spectral energy distribution (SED) to disentangle the emission from the AGN and its host galaxy. We show preliminary results on their host galaxy properties as well as their clustering, showing that obscured quasars are found in galaxies located in the green valley, residing in dark matter haloes not different from normal galaxies at those redshifts.

We use the UKIDSS Ultra-Deep Survey, the deepest degree-scale near-infrared survey to date, to investigate the clustering of star-forming and passive galaxies to z ~ 3.5. Our new measurements include the first determination of the clustering for passive galaxies at z > 2, which we achieve using a cross-correlation technique. We find that passive galaxies are the most strongly clustered, typically hosted by massive dark matter halos with Mhalo > 1013 M⊙ irrespective of redshift or stellar mass. Our findings are consistent with models in which a critical halo mass determines the transition from star-forming to passive galaxies.

We investigate the resolved star formation properties of a sample of 45 massive galaxies (M* > 1011 M⊙) within a redshift range of 1.5 ⩽ z ⩽ 3 detected in the GOODS NICMOS Survey (Conselice et al. 2011), a HST H160-band imaging program. We derive the star formation rate as a function of radius using rest frame UV data from deep z850 ACS imaging. The star formation present at high redshift is then extrapolated to z = 0, and we examine the stellar mass produced in individual regions within each galaxy. We also construct new stellar mass profiles of the in situ stellar mass at high redshift from Sérsic fits to rest-frame optical, H160-band, data. We combine the two stellar mass profiles to produce an evolved stellar mass profile. We then fit a new Sérsic profile to the evolved profile, from which we examine what effect the resulting stellar mass distribution added via star formation has on the structure and size of each individual galaxy.

Galaxy assembly is an unsolved problem, with ΛCDM theoretical models unable to easily account for among other things, the abundances of massive galaxies, and the observed merger history. We show here how the problem of galaxy formation can be addressed in an empirical way without recourse to models. We discuss how galaxy assembly occurs at 1.5 < z < 3 examining the role of major and minor mergers, and gas accretion from the intergalactic medium in forming massive galaxies with log M* > 11 found within the GOODS NICMOS Survey (GNS). We find that major mergers, minor mergers and gas accretion are roughly equally important in the galaxy formation process during this epoch, with 64% of the mass assembled through merging and 36% through accreted gas which is later converted to stars, while 58% of all new star formation during this epoch arises from gas accretion. We also discuss how the total gas accretion rate is measured as Ṁ = 90±40 M⊙ yr−1 at this epoch, a value close to those found in some hydrodynamical simulations.

Civil wars and internal conflicts pose the greatest threat to international peace and security in the twenty-first century. Nowhere is this problem more acute than in East Asia and the Pacific, which has far more of its share of such conflicts. Unraveling Internal Conflicts in East Asia and the Pacific: Incidence, Consequences, and Resolution, edited by Jacob Bercovitch and Karl DeRouen, Jr., is a book of originally commissioned essays on civil wars which provide a compelling area of inquiry. Many of the Asia-Pacific region's wars are very long (such as in Myanmar), some tend to recur (also in Myanmar); some involve religion (Philippines, Thailand), and some (Aceh, Bougainville, East Timor) of the longest have ended in the last few years. In short, the region presents a variety of interesting dynamics that merit close attention in one volume. The aim of Unraveling Internal Conflicts in East Asia and the Pacific is to provide an original look at these civil wars. The unique feature of the book is that it brings a variety of perspectives together into one volume. Bercovitch and DeRouen, Jr., do this in four sections: The first, titled \"Security and Internal Conflicts in the Region,\" is an overview of conflict and conflict management in the region. Section Two is called \"Features of Conflict in the Region.\" Here the authors cover conflict contours, including intractability, conflict resolution, recurrence, and Islam. Section Three, \"External Involvement in Regional Conflicts,\" focuses on third party intervention in regional conflicts. The individual chapters cover mediation, peacekeeping, and other forms of third party involvement. The final section ties the chapters together. Unraveling Internal Conflicts in East Asia and the Pacific: Incidence, Consequences, and Resolution, edited by Jacob Bercovitch and Karl DeRouen, Jr., provides a fresh and comprehensive look at conflict in the part of the world where internal conflict is most prevalent.

The evolution of the number density of galaxies in the universe, and thus also the total number of galaxies, is a fundamental question with implications for a host of astrophysical problems including galaxy evolution and cosmology. However there has never been a detailed study of this important measurement, nor a clear path to answer it. To address this we use observed galaxy stellar mass functions up to \\(z\\sim8\\) to determine how the number densities of galaxies changes as a function of time and mass limit. We show that the increase in the total number density of galaxies (\\(\\phi_{\\rm T}\\)), more massive than M\\(_{*} = 10^{6}\\) M_0, decreases as \\(\\phi_{\\rm T} \\sim t^{-1}\\), where \\(t\\) is the age of the universe. We further show that this evolution turns-over and rather increases with time at higher mass lower limits of M\\(_{*}>10^{7}\\) M_0. By using the M\\(_{*}=10^{6}\\) M_0 lower limit we further show that the total number of galaxies in the universe up to \\(z = 8\\) is \\(2.0^{+0.7}_{-0.6} \\times 10^{12}\\) (two trillion), almost a factor of ten higher than would be seen in an all sky survey at Hubble Ultra-Deep Field depth. We discuss the implications for these results for galaxy evolution, as well as compare our results with the latest models of galaxy formation. These results also reveal that the cosmic background light in the optical and near-infrared likely arise from these unobserved faint galaxies. We also show how these results solve the question of why the sky at night is dark, otherwise known as Olbers' paradox.

We present a new, robust measurement of the evolving rest-frame UV galaxy luminosity function (LF) over the key redshift range z = 2 - 4. Our results are based on the high dynamic range provided by combining the HUDF, CANDELS/GOODS-South, and UltraVISTA/COSMOS surveys. We utilise the unparalleled multi-frequency photometry available in this survey `wedding cake' to compile complete galaxy samples at z ~ 2,3,4 via photometric redshifts (calibrated against the latest spectroscopy) rather than colour-colour selection, and to determine accurate rest-frame UV absolute magnitudes from SED fitting. Our new determinations of the UV LF extend from M_{1500} ~ -22 down to M_{1500} = -14.5, -15.5 and -16 at z ~ 2, 3 and 4 respectively (thus reaching ~ 3 - 4 magnitudes fainter than previous blank-field studies at z ~ 2 - 3). At z ~ 2 - 3 we find a much shallower faint-end slope (alpha = -1.32 +- 0.03) than the steeper values (alpha ~ -1.7) reported by Reddy & Steidel (2009) or by Alavi et al. (2014), and show that this new measurement is robust. By z ~ 4 the faint-end slope has steepened slightly, to alpha = -1.43 +- 0.04, and we show that these measurements are consistent with the overall evolutionary trend from z = 0 to z = 8. Finally, we find that while characteristic number density (phi*) drops from z ~ 2 to z ~ 4, characteristic luminosity (M*) brightens by ~ 1 mag over this redshift range. This, combined with the new flatter faint-end slopes, has the consequence that UV luminosity density (and hence unobscured star-formation density) peaks at z ~ 2.5 - 3, when the Universe was ~ 2.5 Gyr old.

Due to significant galaxy contamination and impurity in stellar mass selected samples (up to 95% from z=0-3), we examine the star formation history, quenching time-scales, and structural evolution of galaxies using a constant number density selection with data from the UKIDSS Ultra-Deep Survey field. Using this methodology we investigate the evolution of galaxies at a variety of number densities from \\(z=0-3\\). We find that samples chosen at number densities ranging from \\(3\\times10^{-4}\\) to 10\\(^{-5}\\) galaxies Mpc\\(^{-3}\\) (corresponding to \\(z\\sim0.5\\) stellar masses of M\\(_{*}= 10^{10.95-11.6}\\) M\\(_{0}\\)) have a star forming blue fraction of \\(\\sim50\\)\\% at \\(z\\sim2.5\\), which evolves to a nearly \\(100\\)\\% quenched red and dead population by \\(z\\sim 1\\). We also see evidence for number density downsizing, such that the galaxies selected at the lowest densities (highest masses) become a homogeneous red population before those at higher number densities. Examining the evolution of the colours for these systems furthermore shows that the formation redshift of galaxies selected at these number densities is \\(z_{\\rm form}>3\\). The structural evolution through size and Sersic index fits reveal that while there remains evolution in terms of galaxies becoming larger and more concentrated in stellar mass at lower redshifts, the magnitude of the change is significantly smaller than for a mass selected sample. We also find that changes in size and structure continues at \\(z < 1\\), and is coupled strongly to passivity evolution. We conclude that galaxy structure is driving the quenching of galaxies, such that galaxies become concentrated before they become passive.

We present a new method for tracing the evolution of BCGs from \\(z\\sim 2\\) to \\(z\\sim 0\\). We conclude on the basis of semi-analytical models that the best method to select BCG progenitors at \\(z\\sim 2\\) is a hybrid environmental density and stellar mass ranking approach. Ultimately we are able to retrieve 45\\% of BCG progenitors. We apply this method on the CANDELS UDS data to construct a progenitor sample at high redshift. We furthermore populate the comparisons in local universe by using SDSS data with statistically likely contamination to ensure a fair comparison between high and low redshifts. Using these samples we demonstrate that the BCG sizes have grown by a factor of \\(\\sim 3.2\\) since \\(z\\sim 2\\), and BCG progenitors are mainly late-type galaxies, exhibiting less concentrated profiles than their early-type local counterparts. We find that BCG progenitors have more disturbed morphologies. In contrast, local BCGs have much smoother profiles. Moreover, we find that the stellar masses of BCGs have grown by a factor of \\(\\sim 2.5\\) since \\(z\\sim 2\\), and the SFR of BCG progenitors has a median value of 13.5 \\(M_\\odot\\)yr\\(^{-1}\\), much higher than their quiescent local descendants. We demonstrate that over \\(z=1-2\\) star formation and merging contribute equally to BCG mass growth. However, merging plays a dominant role in BCG assembly at \\(z \\lesssim 1\\). We also find that BCG progenitors at high-\\(z\\) are not significantly different from other galaxies of similar mass at the same epoch. This suggests that the processes which differentiate BCGs from normal massive elliptical galaxies must occur at \\(z \\lesssim 2\\).