Left, right and the third Way

New Labour claims to have discovered a third way between Old Left and New Right, with policy implications that break with established debates and policy alternatives. But what does the third way actually mean in terms of values and its approach to policy? We argue in this article that Labour's third way does not transcend Old Left and New Right. Left and Right remain important markers for contemporary policy and politics but the third way does combine them in significant new ways. Between Old Left and New Right, we argue, there is not just space for one third way but for many, with varying values and policy positions. Le New Labour se vante d'avoir trouv une `troisime voie' entre la gauche et la droite traditionnelle, avec les consquences qui s'en suivent concernant les politiques rompant avec les dbats et les choix habituels. Mais que veut dire `la troisime voie' en termes de valeurs et d'approche politique? Dans l'article, nous partons du principe que la troisime voie du New Labour ne dpasse pas les concepts de la gauche traditionnelle et de la nouvelle droite. Gauche et droite restent d'importants marqueurs dans la politique et les politiques contemporaines, mais la troisime voie en fait de nouvelles combinaisons signifiantes. Nous pensons que, entre la gauche traditionnelle et la nouvelle droite, il n'y a pas qu'une seule possibilit de troisime voie, mais plusieurs, avec des valeurs et des prises de position varies. El Nuevo Partido Laborista afirma haber descubierto una tercera ruta entre la `antigua Izquierda' y la `nueva Derecha', con implicaciones en el programa poltico que rompen con los debates establecidos y con las polticas alternativas. Pero Qu es lo que realmente significa esta ruta en cuanto a sus valores y enfoque poltico? En este artculo discutimos que la tercera ruta del Partido Laborista, no supera en trminos polticos ni la `antigua Izquierda' ni la `nueva Derecha'. La Izquierda y la Derecha permanecen como marcadores importantes en el programa poltico contemporaneo, aunque la tercera ruta combina ambos partidos de diferente manera. Entre la `antigua Izquierda' y la `nueva Derecha', razonamos que no hay solamente lugar para una tercera ruta sino para muchas con diferentes valores y posiciones polticas

Beyond equality and liberty: New Labour's liberal conservatism

Post-Thatcherism is Tony Blair's way of saying: No Turning Back. But where is New Labour heading? Party modernisers have committed Labour to a politics which combines the free market and the strong community. The search for a dynamic market economy has pushed old ideas of equality to one side. Fears about social fragmentation have given rise to new ideas of community. But these pose awkward questions for New Labour's commitment to individual liberty. In this paper we shall suggest that the free market and the strong community in New Labour politics amounts to a radical shift to liberal conservatism

From Old Labour to New Labour: a comment on Rubinstein

In a critique of our book New Labour, David Rubinstein has argued that we exaggerate the degree of difference between Old and New Labour and underplay the similarities. In this article we agree with many of the continuities that Rubinstein outlines. However, we argue that he himself gives plenty of evidence in favour of our thesis that change has been marked in many policy areas. We argue that we give a good account of the wider social factors that he says accounts for such change. In this article we offer a restatement of the view that New Labour offers a `post-Thatcherite politics. New Labour breaks both with post-war social democracy and with Thatcherism

Equations of state and stability of MgSiO3_3 perovskite and post-perovskite phases from quantum Monte Carlo simulations

We have performed quantum Monte Carlo (QMC) simulations and density functional theory (DFT) calculations to study the equations of state of MgSiO$_3$ perovskite (Pv) and post-perovskite (PPv), up to the pressure and temperature conditions of the base of Earth's lower mantle. The ground state energies were derived using QMC and the temperature dependent Helmholtz free energies were calculated within the quasi-harmonic approximation and density functional perturbation theory. The equations of state for both phases of MgSiO$_3$ agree well with experiments, and better than those from generalized gradient approximation (GGA) calculations. The Pv-PPv phase boundary calculated from our QMC equations of states is also consistent with experiments, and better than previous LDA calculations. We discuss the implications for double crossing of the Pv-PPv boundary in the Earth

Galactic googly : the rotation-metallicity bias in the inner stellar halo of the Milky Way

The first and second moments of stellar velocities encode important information about the formation history of the Galactic halo. However, due to the lack of tangential motion and inaccurate distances of the halo stars, the velocity moments in the Galactic halo have largely remained ‘known unknowns’. Fortunately, our off-centric position within the Galaxy allows us to estimate these moments in the galactocentric frame using the observed radial velocities of the stars alone. We use these velocities coupled with the hierarchical Bayesian scheme, which allows easy marginalization over the missing data (the proper motion, and uncertainty-free distance and line-of-sight velocity), to measure the velocity dispersions, orbital anisotropy (β) and streaming motion (vrot) of the halo main-sequence turn-off (MSTO) and K-giant (KG) stars in the inner stellar halo (r ≲ 15 kpc). We study the metallicity bias in kinematics of the halo stars and observe that the comparatively metal-rich ([Fe/H] > −1.4) and the metal-poor ([Fe/H] ≤ −1.4) MSTO samples show a clear systematic difference in vrot ∼ 20-40 km s−1, depending on how restrictive the spatial cuts to cull the disc contamination are. The bias is also detected in KG samples but with less certainty. Both MSTO and KG populations suggest that the inner stellar halo of the Galaxy is radially biased i.e. σr > σθ or σϕ and β ≃ 0.5. The apparent metallicity contrariety in the rotation velocity among the halo sub-populations supports the co-existence of multiple populations in the galactic halo that may have formed through distinct formation scenarios, i.e. in situ versus accretion.Publisher PDFPeer reviewe

Australian bat lyssavirus infection in two horses

In May 2013, the first cases of Australian bat lyssavirus infections in domestic animals were identified in Australia. Two horses (filly-H1 and gelding-H2) were infected with the Yellow-bellied sheathtail bat (YBST) variant of Australian bat lyssavirus (ABLV). The horses presented with neurological signs, pyrexia and progressing ataxia. Intra-cytoplasmic inclusion bodies (Negri bodies) were detected in some Purkinje neurons in haematoxylin and eosin (H&E) stained sections from the brain of one of the two infected horses (H2) by histological examination. A morphological diagnosis of sub-acute moderate non-suppurative, predominantly angiocentric, meningo-encephalomyelitis of viral aetiology was made. The presumptive diagnosis of ABLV infection was confirmed by the positive testing of the affected brain tissue from (H2) in a range of laboratory tests including fluorescent antibody test (FAT) and real-time PCR targeting the nucleocapsid (N) gene. Retrospective testing of the oral swab from (H1) in the real-time PCR also returned a positive result. The FAT and immunohistochemistry (IHC) revealed an abundance of ABLV antigen throughout the examined brain sections. ABLV was isolated from the brain (H2) and oral swab/saliva (H1) in the neuroblastoma cell line (MNA). Alignment of the genome sequence revealed a 97.7% identity with the YBST ABLV strain

Measurements of extragalactic background light from the far UV to the far IR from deep ground- and space-based galaxy counts

Funding: Australian Research Council via Discovery Project DP130103505 (SPD).We combine wide and deep galaxy number-count data from the Galaxy And Mass Assembly, COSMOS/G10, Hubble Space Telescope (HST) Early Release Science, HST UVUDF, and various near-, mid-, and far-IR data sets from ESO, Spitzer, and Herschel. The combined data range from the far UV (0.15 μm) to far-IR (500 μm), and in all cases the contribution to the integrated galaxy light (IGL) of successively fainter galaxies converges. Using a simple spline fit, we derive the IGL and the extrapolated IGL in all bands. We argue that undetected low-surface-brightness galaxies and intracluster/group light are modest, and that our extrapolated-IGL measurements are an accurate representation of the extragalactic background light (EBL). Our data agree with most earlier IGL estimates and with direct measurements in the far IR, but disagree strongly with direct estimates in the optical. Close agreement between our results and recent very high-energy experiments (H.E.S.S. and MAGIC) suggests that there may be an additional foreground affecting the direct estimates. The most likely culprit could be the adopted model of zodiacal light. Finally we use a modified version of the two-component model to integrate the EBL and obtain measurements of the cosmic optical background (COB) and cosmic infrared background of 24+4-4 nW m−2sr−1 and 26+5-5 nW m−2sr−1 respectively (48%:52%). Over the next decade, upcoming space missions such as Euclid and the Wide Field Infrared Space Telescope will have the capacity to reduce the COB error to <1%, at which point comparisons to the very high-energy data could have the potential to provide a direct detection and measurement of the reionization field.Publisher PDFPeer reviewe

Measurements of extragalactic background light from the far uv to the far ir from deep ground- and space-based galaxy counts

We combine wide and deep galaxy number-count data from the Galaxy And Mass Assembly, COSMOS/G10, Hubble Space Telescope (HST) Early Release Science, HST UVUDF, and various near-, mid-, and far-IR data sets from ESO, Spitzer, and Herschel. The combined data range from the far UV (0.15 μm) to far-IR (500 μm), and in all cases the contribution to the integrated galaxy light (IGL) of successively fainter galaxies converges. Using a simple spline fit, we derive the IGL and the extrapolated IGL in all bands. We argue that undetected low-surface-brightness galaxies and intracluster/group light are modest, and that our extrapolated-IGL measurements are an accurate representation of the extragalactic background light (EBL). Our data agree with most earlier IGL estimates and with direct measurements in the far IR, but disagree strongly with direct estimates in the optical. Close agreement between our results and recent very high-energy experiments (H.E.S.S. and MAGIC) suggests that there may be an additional foreground affecting the direct estimates. The most likely culprit could be the adopted model of zodiacal light. Finally we use a modified version of the two-component model to integrate the EBL and obtain measurements of the cosmic optical background (COB) and cosmic infrared background of ${24}_{-4}^{+4}$ nW m−2 sr−1 and ${26}_{-5}^{+5}$ nW m−2 sr−1 respectively (48%:52%). Over the next decade, upcoming space missions such as Euclid and the Wide Field Infrared Space Telescope will have the capacity to reduce the COB error to <1%, at which point comparisons to the very high-energy data could have the potential to provide a direct detection and measurement of the reionization field

WALLABY Early Science - I. The NGC 7162 Galaxy Group

We present Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) early science results from the Australian Square Kilometre Array Pathfinder (ASKAP) observations of the NGC 7162 galaxy group. We use archival HIPASS and Australia Telescope Compact Array (ATCA) observations of this group to validate the new ASKAP data and the data reduction pipeline ASKAPsoft. We detect six galaxies in the neutral hydrogen (HI) 21-cm line, expanding the NGC 7162 group membership from four to seven galaxies. Two of the new detections are also the first HI detections of the dwarf galaxies, AM 2159-434 and GALEXASC J220338.65-431128.7, for which we have measured velocities of $cz=2558$ and $cz=2727$ km s$^{-1}$, respectively. We confirm that there is extended HI emission around NGC 7162 possibly due to past interactions in the group as indicated by the $40^{\circ}$ offset between the kinematic and morphological major axes for NGC 7162A, and its HI richness. Taking advantage of the increased resolution (factor of $\sim1.5$) of the ASKAP data over archival ATCA observations, we fit a tilted ring model and use envelope tracing to determine the galaxies' rotation curves. Using these we estimate the dynamical masses and find, as expected, high dark matter fractions of $f_{\mathrm{DM}}\sim0.81-0.95$ for all group members. The ASKAP data are publicly available.Comment: 20 pages, 11 figures, accepted for publication in MNRA

Galaxy and mass assembly (GAMA): the inferred mass–metallicity relation from z = 0 to 3.5 via forensic SED fitting

We analyse the metallicity histories of ∼4500 galaxies from the GAMA survey at z \u3c 0.06 modelled by the SED-fitting code PROSPECT using an evolving metallicity implementation. These metallicity histories, in combination with the associated star formation histories, allow us to analyse the inferred gas-phase mass–metallicity relation. Furthermore, we extract the mass– metallicity relation at a sequence of epochs in cosmic history, to track the evolving mass–metallicity relation with time. Through comparison with observations of gas-phase metallicity over a large range of redshifts, we show that, remarkably, our forensic SED analysis has produced an evolving mass–metallicity relationship that is consistent with observations at all epochs. We additionally analyse the three-dimensional mass–metallicity–SFR space, showing that galaxies occupy a clearly defined plane. This plane is shown to be subtly evolving, displaying an increased tilt with time caused by general enrichment, and also the slowing down of star formation with cosmic time. This evolution is most apparent at lookback times greater than 7 Gyr. The trends in metallicity recovered in this work highlight that the evolving metallicity implementation used within the SED-fitting code PROSPECT produces reasonable metallicity results over the history of a galaxy. This is expected to provide a significant improvement to the accuracy of the SED-fitting outputs