Environmental Policy and Firm Selection in the Open Economy

In this paper, we analyse the effects of a unilateral change in an emissions tax in a model of international trade with heterogeneous firms. We find a positive effect of tighter environmental policy on average productivity in the reforming country through reallocation of labour towards exporting firms. Domestic aggregate emissions fall, due to both a scale and a technique effect, but we show that the reduction in emissions following the tax increase is smaller than in autarky. Moreover, general equilibrium effects through changes in the foreign wage rate lead to a reduction in foreign emissions and, hence, to negative emissions leakage in case of transboundary pollution

Trade and the Environment: The Role of Firm Heterogeneity

This paper derives a new effect of trade liberalisation on the quality of the environment. We show that in the presence of heterogeneous firms the aggregate volume of emissions is influenced not only by the long-established scale effect, but also by a reallocation effect resulting from an increase in the relative size of more productive firms. We show how the relative importance of these effects, and hence the overall effect of trade liberalisation on the environment, is affected by the emission-intensity at the firm level: Aggregate emissions decrease when trade is liberalised if and only if firm-specific emission intensity decreases strongly with increasing firm productivity

Physical Properties and Baryonic Content of Low-Redshift Intergalactic Ly-alpha and O VI Absorption Systems: The PG1116+215 Sight Line

We present HST and FUSE observations of the intergalactic absorption toward PG1116+215 in the 900-3000 A spectral region. We detect 25 Ly-alpha absorbers at rest-frame equivalent widths W_r > 30 mA, yielding (dN/dz)_Ly-alpha = 154+/-18 over an unblocked redshift path of 0.162. Two additional weak Ly-alpha absorbers with W_r ~ 15-20 mA are also present. Eight of the Ly-alpha absorbers have large line widths (b > 40 km/sec). The detection of narrow OVI in the broad Ly-alpha absorber at z=0.06244 supports the idea that the Ly-alpha profile is thermally broadened in gas with T > 10^5 K. We find dN/dz ~ 50 for broad Ly-alpha absorbers with W_r > 30 mA and b > 40 km/sec. If the broad Ly-alpha lines are dominated by thermal broadening in hot gas, the amount of baryonic material in these absorbers is enormous, perhaps as much as half the baryonic mass in the low-redshift universe. We detect OVI absorption in several of the Ly-alpha clouds along the sight line. Two detections at z=0.13847 and z=0.16548 are confirmed by the presence of other ions at these redshifts, while the detections at z=0.04125, 0.05895, 0.05928, and 0.06244 are based upon the Ly-alpha and OVI detections alone. The information available for 13 low-redshift OVI absorbers with W_r > 50 mA along 5 sight lines yields (dN/dz)_OVI ~ 14 and Omega_b(OVI) > 0.0027/h_75, assuming a metallicity of 0.1 solar and an OVI ionization fraction < 0.2. The properties and prevalence of low-redshift OVI absorbers suggest that they too may be a substantial baryon repository, perhaps containing as much mass as stars and gas inside galaxies. The redshifts of the OVI absorbers are highly correlated with the redshifts of galaxies along the sight line, though few of the absorbers lie closer than 600/h_75 kpc to any single galaxy. [abbreviated]Comment: 99 pages, 30 figures, aastex format, ApJS in pres

FUSE and STIS Observations of the Warm-Hot Intergalactic Medium towards PG1259+593

We use FUSE and STIS spectra to study intergalactic absorption towards the quasar PG1259+593 (z=0.478). We identify 135 intergalactic absorption lines with equivalent widths >10mA, tracing 78 absorption components in 72 Ly alpha/beta absorption-line systems. We concentrate on the distribution and physical properties of the WHIM as sampled by OVI and intrinsically broad Ly alpha lines. The number of intervening OVI absorbers for equivalent widths W>24 mA is 3-6 over an unobscured redshift path of dz=0.368. This implies a number density of OVI systems, dN/dz, of ~8-16 along this sight line. This range is consistent with estimates from other sight lines, supporting the idea that intervening intergalactic OVI absorbers contain an substantial fraction of the baryonic mass in the low-redshift Universe. We identify a number of broad Ly alpha absorbers with large Doppler parameters (b~40-200 km/s) and low column densities (N(HI)<10^14 cm^-2). For pure thermal broadening, these widths correspond to temperatures of ~1x10^5 to 3x10^6 K. While these broad absorbers could be caused by blends of multiple, unresolved lines, continuum undulations, or by kinematic flows and Hubble broadening, we consider the possibility that some of these features are single-component, thermally broadened Ly alpha lines. These systems could represent WHIM absorbers that are too weak, too metal-poor, and/or too hot to be detected in OVI. If so, their widths and their frequency in the PG1259+593 spectrum imply that these absorbers trace an even larger fraction of the baryons in the low-redshift Universe than the OVI absorbing systems (abridged version).Comment: 71 pages, 25 figures; accepted for publication in ApJ

Phosphocholine-Modified Lipooligosaccharides of Haemophilus influenzae Inhibit ATP-Induced IL-1beta Release by Pulmonary Epithelial Cells

Phosphocholine-modified bacterial cell wall components are virulence factors enabling immune evasion and permanent colonization of the mammalian host, by mechanisms that are poorly understood. Recently, we demonstrated that free phosphocholine (PC) and PC-modified lipooligosaccharides (PC-LOS) from Haemophilus influenzae, an opportunistic pathogen of the upper and lower airways, function as unconventional nicotinic agonists and efficiently inhibit the ATP-induced release of monocytic IL-1beta. We hypothesize that H. influenzae PC-LOS exert similar effects on pulmonary epithelial cells and on the complex lung tissue. The human lung carcinoma-derived epithelial cell lines A549 and Calu-3 were primed with lipopolysaccharide from Escherichia coli followed by stimulation with ATP in the presence or absence of PC or PC-LOS or LOS devoid of PC. The involvement of nicotinic acetylcholine receptors was tested using specific antagonists. We demonstrate that PC and PC-LOS efficiently inhibit ATP-mediated IL-1beta release by A549 and Calu-3 cells via nicotinic acetylcholine receptors containing subunits alpha7, alpha9, and/or alpha10. Primed precision-cut lung slices behaved similarly. We conclude that H. influenzae hijacked an endogenous anti-inflammatory cholinergic control mechanism of the lung to evade innate immune responses of the host. These findings may pave the way towards a host-centered antibiotic treatment of chronic airway infections with H. influenzae

The Diversity of High- and Intermediate-Velocity Clouds: Complex C versus IV Arch

We present Far Ultraviolet Spectroscopic Explorer (FUSE) and Space Telescope Imaging Spectrograph (STIS) observations of interstellar ultraviolet absorption lines in the Galactic high-velocity cloud Complex C and the Intermediate Velocity Arch (IV Arch) in direction of the quasar PG 1259+593 (l=120,b=+58 deg). Absorption lines from CII, NI, NII, OI, AlII, SiII, PII, SII, ArI, FeII, and FeIII are used to study the atomic abundances in these two halo clouds at V_LSR=-130 km/s (Complex C) and V_LSR=-55 km/s (IV Arch). The OI/HI ratio provides the best measure of the overall metallicity in the diffuse interstellar medium, because ionization effects do not alter the ratio, and oxygen is at most only lightly depleted from the gas into dust grains. For Complex C, we find an oxygen abundance of 0.093 (+0.125, -0.047) solar, consistent with the idea that Complex C represents the infall of low metallicity gas onto the Milky Way. In contrast, the oxygen abundance in the IV Arch is 0.98 (+1.21,-0.46) solar, which indicates a Galactic origin. We report the detection of an intermediate- velocity absorption component at +60 km/s that is not seen in HI 21cm emission. The clouds along the PG 1259+593 sight line have a variety of properties, proving that multiple processes are responsible for the creation and circulation of intermediate- and high-velocity gas in the Milky Way halo.Comment: 12 pages, 3 tables, 3 figures; accepted for publication in Ap