Dye sensitization of polymer/fullerene solar cells incorporating bulky phthalocyanines

The light-harvesting efficiency of P3HT:PCBM solar cells can be improved by incorporating near-IR dye molecules such as silicon phthalocyanine derivatives with bulky axial groups (SiPc). In order to study the size effect of the axial groups on the dye sensitization in P3HT:PCBM solar cells, we synthesized five SiPc derivatives with different axial groups: SiPc[OSi(C_{n}H_{2n+1})_{3}]_{2} (SiPcn, n = 2, 3, 4, 6) and SiPc[OSi(iBu)_{2}C_{18}H_{37}]_{2} (SiPcB18). The power conversion efficiency (PCE) increased in the order of n = 2–4, reached the maximum at around n = 4 and 6, and then decreased for SiPcB18 with the longest axial groups. As a result, the PCE was improved to 4.2%, which is larger by 10% than that of P3HT:PCBM control cells without dye molecules. We therefore conclude that the butyl or hexyl chain in the axial ligand is the most appropriate for the dye sensitization in P3HT:PCBM solar cells

The ASTRO-F Mission : Large Area Infrared Survey

ASTRO-F is the first Japanese satellite mission dedicated for large area surveys in the infrared. The 69cm aperture telescope and scientific instruments are cooled to 6K by liquid Helium and mechanical coolers. During the expected mission life of more than 500 days, ASTRO-F will make the most advanced all-sky survey in the mid- to far-infrared since the Infrared astronomical Satellite (IRAS). The survey will be made in 6 wavebands and will include the first all sky survey at >100-160(mu)m. Deep imaging and spectroscopic surveys with pointed observations will also be carried out in 13 wavelength bands from 2-160(mu)m. ASTRO-F should detect more than a half million galaxies tracing the large-scale structure of the Universe out to redshifts of unity, detecting rare, exotic extraordinarily luminous objects at high redshift, numerous brown dwarfs, Vega-like stars, protostars, and will reveal the large-scale structure of nearby galactic star forming regions. ASTRO-F is a perfect complement to Spitzer Space Telescope in respect of its wide sky and wavelength coverage. Approximately 30 percent of pointed observations will be allocated to an open-time opportunity. Updated pre-flight ensitivities as well as the observation plan including the large-area surveys are described.Comment: accepted for publication in Advances in Space Research, 15 pages, 7 Postscript figures, uses elsart.cl

A 5 kDa protein (SCS23) from the 30 S subunit of the spinach chloroplast ribosome

AbstractThe proteins of the 30 S ribosomal subunits from spinach chloroplasts were investigated using a radical-free and highly reducing (RFHR) method of two-dimensional polyacrylamide gel electrophoresis (PAGE). Twenty-three proteins were resolved on the gel down to the smallest protein of 5 kDa. The N-terminal amino acid sequence of the 5 kDa protein showed no homology with that of any other protein stored in databases, and the copy numbers were estimated to be 0.88±0.16 and 0.72±0.04 in the 30 S subunits and the 70 S ribosomes, respectively. The results suggest that the 5 kDa protein, which we have called SCS23, may be an essential ribosomal protein specific to spinach chloroplasts

North Ecliptic Pole Wide Field Survey of AKARI: Survey Strategy and Data Characteristics

We present the survey strategy and the data characteristics of the North Ecliptic Pole (NEP) Wide Survey of AKARI. The survey was carried out for about one year starting from May 2006 with 9 passbands from 2.5 to 24 micron and the areal coverage of about 5.8 sq. degrees centered on NEP. The survey depth reaches to 21.8 AB magnitude near infrared (NIR) bands, and ~ 18.6 AB maggnitude at the mid infrared (MIR) bands such as 15 and 18 micron. The total number of sources detected in this survey is about 104,000, with more sources in NIR than in the MIR. We have cross matched infrared sources with optically identified sources in CFHT imaging survey which covered about 2 sq. degrees within NEP-Wide survey region in order to characterize the nature of infrared sources. The majority of the mid infrared sources at 15 and 18 micron band are found to be star forming disk galaxies, with smaller fraction of early type galaxies and AGNs. We found that a large fraction (60~80 %) of bright sources in 9 and 11 micron stars while stellar fraction decreases toward fainter sources. We present the histograms of the sources at mid infrared bands at 9, 11, 15 and 18 micron. The number of sources per magnitude thus varies as m^0.6 for longer wavelength sources while shorter wavelength sources show steeper variation with m, where m is the AB magnitude.Comment: 18 pages, 11 figures, to appear in PASJ, Vol. 61, No. 2. April 25, 2009 issu