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Adjuvant-dependent innate and adaptive immune signatures of risk of SIV<sub>mac251</sub> acquisition
Vaccari, Monica,Gordon, Shari N,Fourati, Slim,Schifanella, Luca,Liyanage, Namal P M,Cameron, Mark,Keele, Brandon F,Shen, Xiaoying,Tomaras, Georgia D,Billings, Erik,Rao, Mangala,Chung, Amy W,Dowell, Ka Nature Publishing Group 2016 Nature medicine Vol.22 No.7
<P>A recombinant vaccine containing Aventis Pasteur's canarypox vector (ALVAC)-HIV and gp120 alum. decreased the risk of HIV acquisition in the RV144 vaccine trial. The substitution, of alum with the more immunogenic MF59 adjuvant is under consideration for the next efficacy human trial. We found here that an ALVAC-simian immunodeficiency virus (SIV) and gp120 alum (ALVAC-SIV + gp120) equivalent vaccine, but not an ALVAC-SIV + gp120 MF59 vaccine, was efficacious in delaying the onset of SIVmac251 in rhesus macaques, despite the higher immunogenicity of the latter adjuvant. Vaccine efficacy was associated with alum-induced, but not with MF59-induced, envelope (Env)-dependent mucosal innate lymphoid cells (ILCs) that produce interleukin (IL)-17, as well as with mucosal IgG to the gp120 variable region 2 (V2) and the expression of 12 genes, ten of which are part of the RAS pathway. The association between RAS activation and vaccine efficacy was also observed in an independent efficacious SIV-vaccine approach. Whether RAS activation, mucosal ILCs and antibodies to V2 are also important hallmarks of HIV-vaccine efficacy in humans will require further studies.</P>
AKARI-NEP : EFFECTS OF AGN PRESENCE ON SFR ESTIMATES OF GALAXIES
L. Marchetti,A. Feltre,S. Berta,I. Baronchelli,S. Serjeant,M. Vaccari,D. Bulgarella,M.Karouzos,K. Murata,N.Oi,C. Pearson,G. Rodighiero,C. Segdwick,G. J. White 한국천문학회 2017 天文學論叢 Vol.32 No.1
How does the presence of an AGN influence the total SFR estimates of galaxies and change their distribution with respect to the \textit{Galaxy Main Sequence}?To contribute to solving this question, we study a sample of 1133 sources detected in the North Ecliptic Pole field (NEP) by AKARI and Herschel. We create a multi-wavelength dataset for these galaxies and we fit their multi-wavelength Spectral Energy Distribution (SED) using the whole spectral regime (from 0.1 to 500 $\mu$m). We perform the fit using three procedures: \texttt{LePhare} and two optimised codes for identifying AGN tracers from the SED analysis. In this work we present an overview of the comparison between the estimates of the Infrared bolometric luminosities (between 8 and 1000 $\mu$m) and the AGN fractions obtained exploiting these different procedures. In particular, by estimating the AGN contribution in four different wavelength ranges (5-40 $\mu$m, 10-20 $\mu$m, 20-40 $\mu$m and 8-1000 $\mu$m) we show how the presence of an AGN affects the PAH emission by suppressing the ratio $\frac{L_{\rm8~\mu m}}{L_{\rm4.5~\mu m}}$ as a function of the considered wavelength range.
AKARI DEEP FIELD SOUTH: SPECTROSCOPIC OBSERVATIONS OF INFRARED SOURCES
Chris Sedgwick,STEPHEN SERJEANT,CHRIS PEARSON,Shuji Matsuura,MAI SHIRAHATA,Hideo Matsuhara,Lucia Marchetti,Glenn J. White,Mattia Vaccari,Ivano Baronchelli,Giulia Rodighiero,Bunyo Hadsukade,David L. Cl 한국천문학회 2017 天文學論叢 Vol.32 No.1
We present a summary of our spectroscopic redshift catalogue of 404 sources in the {\it AKARI} Deep Field South (ADF-S). We have used the AAOmega spectrograph to target mid-infrared and far-infrared sources selected primarily from {\it AKARI} observations in this field for which we were able to obtain optical counterparts. Our sources with identified redshifts include 316 with H$\alpha$ detections at z ≤ 0.345 and 15 sources at z > 1 with MgII or Lyα emission lines. About 13% of our z ≤0.345 sources are dominated by active galactic nuclei (AGN) emission, although many show emission from both star formation and AGNs. The median Balmer decrement is 5.9. Ultra-luminous infrared galaxies (ULIRGs) were found only in the higher-redshift sources. Optical and near infrared data will be available shortly, enabling calibration of the line luminosities and spectral energy distribution (SED) fitting for these sources.