An evaluation of the analytic continuation by duality technique

In Nucl. Phys. B391 (1993) 127, the value of the oblique correction parameter S for walking technicolor theories was estimated using a technique called Analytic Continuation by Duality (ACD). We apply the ACD technique to the perturbative vacuum polarization function and find that it fails to reproduce the well known result S=1/6\pi. This brings into question the reliability of the ACD technique and the ACD estimate of S.Comment: 8 pages, LaTeX, 1 postscript figure. Uses cite.sty, sprocl.sty, and epsfig.sty. Talk presented at the 1996 International Workshop on Perspectives of Strong Coupling Gauge Theories (SCGT'96), 13-16 Nov. 1996, Nagoy

Clustering of Far-Infrared Galaxies in the AKARI All-Sky Survey

We present the first measurement of the angular two-point correlation function for AKARI 90-$\mu$m point sources, detected outside of the Milky Way plane and other regions characterized by high Galactic extinction, and categorized as extragalactic sources according to our far-infrared-color based criterion (Pollo et al. 2010). This is the first measurement of the large-scale angular clustering of galaxies selected in the far-infrared after IRAS measurements. Although a full description of clustering properties of these galaxies will be obtained by more detailed studies, using either spatial correlation function, or better information about properties and at least photometric redshifts of these galaxies, the angular correlation function remains the first diagnostics to establish the clustering properties of the catalog and observed galaxy population. We find a non-zero clustering signal in both hemispheres extending up to $\sim 40$ degrees, without any significant fluctuations at larger scales. The observed correlation function is well fitted by a power law function. The notable differences between a northern and southern hemisphere are found, which can be probably attributed to the photometry problems and point out to a necessity of performing a better calibration in the data from southern hemisphere.Comment: 6 pages, 6 figures, accepted for publication in Earth, Planets, and Spac

Star formation and dust extinction properties of local galaxies from AKARI-GALEX All-Sky Surveys: First results from most secure multiband sample from FUV to FIR

The AKARI All-Sky Survey provided the first bright point source catalog detected at 90um. Starting from this catalog, we selected galaxies by matching AKARI sources with those in the IRAS PSCz. Next, we have measured total GALEX FUV and NUV flux densities. Then, we have matched this sample with SDSS and 2MASS galaxies. By this procedure, we obtained the final sample which consists of 607 galaxies. If we sort the sample with respect to 90um, their average SED shows a coherent trend: the more luminous at 90um, the redder the global SED becomes. The M_r--NUV-r color-magnitude relation of our sample does not show bimodality, and the distribution is centered on the green valley between the blue cloud and red sequence seen in optical surveys. We have established formulae to convert FIR luminosity from AKARI bands to the total infrared (IR) luminosity L_TIR. With these formulae, we calculated the star formation directly visible with FUV and hidden by dust. The luminosity related to star formation activity (L_SF) is dominated by L_TIR even if we take into account the far-infrared (FIR) emission from dust heated by old stars. At high star formation rate (SFR) (> 20 Msun yr^-1), the fraction of directly visible SFR, SFR_FUV, decreases. We also estimated the FUV attenuation A_FUV from FUV-to-total IR (TIR) luminosity ratio. We also examined the L_TIR/L_FUV-UV slope (FUV- NUV) relation. The majority of the sample has L_TIR/L_FUV ratios 5 to 10 times lower than expected from the local starburst relation, while some LIRGs and all the ULIRGs of this sample have higher L_TIR/L_FUV ratios. We found that the attenuation indicator L_TIR/L_FUV is correlated to the stellar mass of galaxies, M*, but there is no correlation with specific SFR (SSFR), SFR/M*, and dust attenuation L_TIR/L_FUV. (abridged)Comment: 13 pages, 18 figures, accepted for publication in A&

Beating the Standard Quantum Limit with Four Entangled Photons

Precision measurements are important across all fields of science. In particular, optical phase measurements can be used to measure distance, position, displacement, acceleration and optical path length. Quantum entanglement enables higher precision than would otherwise be possible. We demonstrate an optical phase measurement with an entangled four photon interference visibility greater than the threshold to beat the standard quantum limit--the limit attainable without entanglement. These results open the way for new high-precision measurement applications.Comment: 5 pages, 4 figures Author name was slightly modifie

The infrared emission of ultraviolet selected galaxies from z = 0 to z=1

We select galaxies in UV rest-frame at z=0, z~0.7 and z~1 together with a sample of LBGs at z~1, the samples are built in order to sample the same range of luminosity at any redshift. The evolution of the IR and UV luminosities with z is analysed for individual galaxies as well as in terms of luminosity functions. The L_IR/L_UV ratio is used to measure dust attenuation. This ratio does not exhibit a strong evolution with z for the bulk of our sample galaxies but some trends are found for galaxies with a strong dust attenuation and for UV luminous sources: galaxies with L_IR/L_UV>10 are more frequent at z>0 than at z=0 and the largest values of L_IR/L_UV are found for UV faint objects; conversely the most luminous galaxies of our samples (L_UV> 2 10^{10} L_sun$), detected at z=1, exhibit a lower dust attenuation than the fainter ones. L_IR/L_UV increases with the K rest-frame luminosity of the galaxies at all the redshifts considered and shows a residual anti-correlation with L_UV. The most massive and UV luminous galaxies exhibit quite large specific star formation rates. LBGs exhibit systematically lower dust attenuation than UV selected galaxies of same luminosity but similar specific star formation rates. The analysis of the UV+IR luminosity functions leads to the conclusion that up to z = 1 most of the star formation activity of UV selected galaxies is emitted in IR. Whereas we are able to retrieve all the star formation from our UV selection at z=0.7, at z = 1 we miss a large fraction of galaxies more luminous than ~ 10^{11} L_sun. The effect is found larger for Lyman Break Galaxies.Comment: 13 pages. accepted for publication (Astronomy and Astrophysics

Far-Ultraviolet and Far-Infrared Bivariate Luminosity Function of Galaxies: Complex Relation between Stellar and Dust Emission

Far-ultraviolet (FUV) and far-infrared (FIR) luminosity functions (LFs) of galaxies show a strong evolution from $z = 0$ to $z = 1$, but the FIR LF evolves much stronger than the FUV one. The FUV is dominantly radiated from newly formed short-lived OB stars, while the FIR is emitted by dust grains heated by the FUV radiation field. It is known that dust is always associated with star formation activity. Thus, both FUV and FIR are tightly related to the star formation in galaxies, but in a very complicated manner. In order to disentangle the relation between FUV and FIR emissions, we estimate the UV-IR bivariate LF (BLF) of galaxies with {\sl GALEX} and {\sl AKARI} All-Sky Survey datasets. Recently we invented a new mathematical method to construct the BLF with given marginals and prescribed correlation coefficient. This method makes use of a tool from mathematical statistics, so called "copula". The copula enables us to construct a bivariate distribution function from given marginal distributions with prescribed correlation and/or dependence structure. With this new formulation and FUV and FIR univariate LFs, we analyze various FUV and FIR data with {\sl GALEX}, {\sl Spitzer}, and {\sl AKARI} to estimate the UV-IR BLF. The obtained BLFs naturally explain the nonlinear complicated relation between FUV and FIR emission from star-forming galaxies. Though the faint-end of the BLF was not well constrained for high-$z$ samples, the estimated linear correlation coefficient $\rho$ was found to be very high, and is remarkably stable with redshifts (from 0.95 at $z = 0$ to 0.85 at $z = 1.0$). This implies the evolution of the UV-IR BLF is mainly due to the different evolution of the univariate LFs, and may not be controlled by the dependence structure.Comment: 10 pages, 7 figures, Earth, Planets and Space, in pres

Disclosure of the Producer of Style

Fashion is intriguing in that it is a kind of ritual based on the concealment of seemingly perpetual shame. The psychological mask of style remains an agent of socially precipitated narcissism. Guilt about it stokes the fire. I pour water on this fire by aiming to mediate it with a spirit of respect in the handling of appropriated fashion images. The resulting works I construct may be taken and changed in turn. This non-hierarchical exchange of recast photos allows for the possibility of upturning established codes of visual hegemony. Fashion propaganda tends to dismiss the power of certain populations. While I slip into the role of unacknowledged laborer of a psychological product, the object of envy, a carefree identity of extreme relevance, sweatshop workers in remote locations are set aside. A denial of the reality of self seems requisite. The projection of desire onto products, and ultimately onto human flesh, is contingent on the fallacy of a non-existent producer. I invoke an affirmation of the laborer, especially in regards to the woman, bearer of humans, on whom the psychic shroud is doubled down. While I repudiate the deceptive attitude of fashion, I won’t deny simultaneously seizing the joy of faulty glamour. There comes a particular satisfaction in the lifting of rejected culture, and its transformation into exquisite specimens of communication. Beauty thrives on the make-do of its bankrupt beginnings