On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36 þ5 −4 M ⊙ and 29 þ4 −4 M ⊙ ; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be < 0.7 (at 90% probability). The luminosity distance to the source is 410 −0.07 . This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.

This paper presents updated estimates of source parameters for GW150914, a binary black-hole coalescence event detected by the Laser Interferometer Gravitational-wave Observatory (LIGO) in 2015 [Abbott et al. Phys. Rev. Lett. 116, 061102 (2016).]. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] presented parameter estimation of the source using a 13-dimensional, phenomenological precessing-spin model (precessing IMRPhenom) and an 11-dimensional nonprecessing effective-onebody (EOB) model calibrated to numerical-relativity simulations, which forces spin alignment (nonprecessing EOBNR). Here, we present new results that include a 15-dimensional precessingspin waveform model (precessing EOBNR) developed within the EOB formalism. We find good agreement with the parameters estimated previously [Abbott et al. Phys. Rev. Lett. 116, 241102 (2016).], and we quote updated component masses of 35 þ5 −3 M ⊙ and 30 þ3 −4 M ⊙ (where errors correspond to 90% symmetric credible intervals). We also present slightly tighter constraints on the dimensionless spin magnitudes of the two black holes, with a primary spin estimate < 0.65 and a secondary spin estimate < 0.75 at 90% probability. Abbott et al. [Phys. Rev. Lett. 116, 241102 (2016).] estimated the systematic parameter-extraction errors due to waveform-model uncertainty by combining the posterior probability densities of precessing IMRPhenom and nonprecessing EOBNR. Here, we find that the two precessing-spin models are in closer agreement, suggesting that these systematic errors are smaller than previously quoted.

We review the progress towards developing epitaxial graphene as a material for carbon electronics. In particular, we discuss improvements in epitaxial graphene growth, interface control and the understanding of multilayer epitaxial graphene's (MEG's) electronic properties. Although graphene grown on both polar faces of SiC will be discussed, our discussions will focus on graphene grown on the C-face of SiC. The unique properties of C-face MEG have become apparent. These films behave electronically like a stack of nearly independent graphene sheets rather than a thin Bernal stacked graphite sample. The origins of multilayer graphene's electronic behaviour are its unique highly ordered stacking of non-Bernal rotated graphene planes. While these rotations do not significantly affect the inter-layer interactions, they do break the stacking symmetry of graphite. It is this broken symmetry that leads to each sheet behaving like isolated graphene planes.

The authors examined ratings of facial attractiveness, rankings of faces and reasons given by young, middle-aged, and older men and women for young, middle-aged, and older male and female face attractiveness. No support for predictions derived from similarity, interest, and cohort hypotheses was obtained. In support of the expertise hypothesis, young and middle-aged adults rated younger faces as more attractive than old faces, whereas older adults rated all aged faces equally. In support of the crone hypothesis, older female faces were rated the lowest of all faces. Theoretical implications and real-world applications are discussed.

Employing a molar excess of carbon dioxide (P c = 71.8 bar; T c = 31.1 °C), supercritical 1-butene/isobutane alkylation is performed at temperatures lower than the critical temperature of isobutane (<135 °C), resulting in virtually steady alkylate (trimethylpentanes and dimethylhexanes) production on both microporous zeolitic (H−USY) and mesoporous solid acid (sulfated zirconia) catalysts for experimental durations of up to nearly 2 days. At a space velocity of 0.25 g of 1-butene/g of catalyst/h, a feed CO2/isobutane/olefin ratio of 86:8:1, 50 °C, and 155 bar, roughly 5% alkylate yield (alkylates/C5+) and 20% butenes conversion are observed at steady state. The ability of the carbon dioxide based supercritical reaction mixtures to mitigate coking and thereby to maintain better pore accessibilities is also evident from the narrow product spectrum (confined to C8's), the lighter color of the spent catalyst samples, and relatively low surface-area and pore-volume losses (<25%) in the spent catalysts. For identical weight hourly 1-butene space-velocity and feed isobutane/olefin ratios, the alkylate formation declines continuously with time when the reaction is carried out without employing carbon dioxide. At the high temperatures (>135 °C) required for supercritical operation without carbon dioxide, cracking and coking reactions are dominant as inferred from the rather wide product spectrum and extensive surface area/pore volume losses (up to 90%) in the spent catalysts. The carbon dioxide based, fixed-bed, solid acid alkylation process shows promise as an environmentally safer alternative to conventional alkylation that employs liquid acids.