Crystal structure and second harmonic generation in Bi₂TeO₅: An X-N study from synchrotron and neutron diffraction data

Ló,pez, C.A.,Bâ,ati, E.,Fern&aacute,ndez-Dí,az, M.T.,Saouma, F.O.,Jang, J.I.,Alonso, J.A. Academic Press 2019 Journal of solid state chemistry Vol.276 No.-

<P><B>Abstract</B></P> <P>Bi<SUB>2</SUB>TeO<SUB>5</SUB> has been obtained in polycrystalline form via solid state reaction and structurally characterized from both synchrotron and neutron powder diffraction data, enabling the precise determination of the atomic positions. The crystal structure is defined in the acentric <I>Amb</I>2 space group, containing three crystallographically unequivalent Bi atoms. The position of the stereochemically active electron lone pairs of both Bi<SUP>3+</SUP> and Te<SUP>4+</SUP> ions is inferred to be opposite to the strongly covalent BiO and TeO chemical bonds; the global electron polarization arises from the non-compensated Bi<SUP>3+</SUP> lone electron pairs. Additionally, from difference Fourier maps between synchrotron and neutron diffraction data (X-N technique) it was possible to observe experimental evidence of the lone electron pair for Bi<SUP>3+</SUP>. Nonlinear optical measurements display highly active second harmonic generation response, comparable to that of reference AgGaSe<SUB>2</SUB>.</P> <P><B>Highlights</B></P> <P> <UL> <LI> The crystal structure is defined in the non-centrosymmetric <I>Amb</I>2 space group. </LI> <LI> Fourier maps between synchrotron and neutron diffraction data (X-N technique). </LI> <LI> Experimental evidence of Bi<SUP>3+</SUP>lone electron pair from X-N study. </LI> <LI> Nonlinear optical measurements display highly active SHG response. </LI> </UL> </P> <P><B>Graphical abstract</B></P> <P>[DISPLAY OMISSION]</P>

THE UNAM-KIAS CATALOG OF ISOLATED GALAXIES

Hern&aacute,ndez-Toledo, H. M.,V&aacute,zquez-Mata, J. A.,Martí,nez-V&aacute,zquez, L. A.,Choi, Yun-Young,Park, Changbom American Institute of Physics 2010 The Astronomical journal Vol.139 No.6

<P>A new catalog of isolated galaxies from the Sloan Digital Sky Survey Data Release 5 (SDSS DR5) is presented. A total of 1520 isolated galaxies were found in 1.4 sr of sky. The selection criteria in this UNAM-KIAS catalog are a variation on the criteria developed by Karachentseva, including full redshift information. Through an image processing pipeline that takes advantage of the high-resolution (~0<img entity='farcs' SRC='http://ej.iop.org/icons/Entities/farcs.gif' ALT='farcs' ALIGN='BOTTOM' />4 pixel<SUP>–1</SUP>) and high dynamic range of the SDSS images, a uniform g-band morphological classification for all these galaxies is presented. We identify 80% (Sa-Sm) spirals (50% later than Sbc types) on one hand, and a scarce population of early-type E (6.5%) and S0 (8%) galaxies amounting to 14.5% on the other hand. This magnitude-limited catalog is ~80% complete at 16.5, 15.6, 15.2, 14.6, and 14.4 mag in the ugriz bands, respectively. Some representative physical properties including SDSS magnitudes and color distributions, color-color diagrams, absolute magnitude-color, and concentration-color diagrams as a function of morphological type are presented. The UNAM-KIAS Morphological Atlas is also released along with this paper. For each galaxy of a type later than Sa, a mosaic is presented that includes (1) a g-band logarithmic image, (2) a g-band filtered-enhanced image where a Gaussian kernel of various sizes was applied, and (3) a red giant branch color image from the SDSS database. For E/S0/Sa galaxies, in addition to the images in (1), (2), and (3), plots of r-band surface brightness and geometric profiles (ellipticity ε, position angle PA, and A<SUB>4</SUB>/B<SUB>4</SUB> coefficients of the Fourier series expansions of deviations of a pure ellipse) are provided. The size of the sample, the redshift completeness, the availability of high-quality multicolor photometric data and detailed morphological and spectroscopic information make the UNAM-KIAS catalog of isolated galaxies a suitable sample to address important issues such as (1) comparative studies of environmental effects, (2) constraining the currently competing scenarios of galaxy formation and evolution, (3) the nature and evolution of elliptical and spiral galaxies in the field, (4) the spectral properties of a statistically significant number of isolated galaxies and their evolution as a function of redshift, and (5) the fraction of active galactic nuclei in isolated environments, among other important topics. The optimization and estimation of new structural parameters as well as important information to complement existing ones in other wavelengths is being carried out.</P>

C₆₀ dimers connected through pleiadene bridges: fullerenes talking to each other

Sastre-Santos, &Aacute,ngela,Parejo, Concepció,n,Martí,n-Gomis, Luis,Ohkubo, Kei,Fern&aacute,ndez-Lá,zaro, Fernando,Fukuzumi, Shunichi Royal Society of Chemistry 2011 Journal of materials chemistry Vol.21 No.5

<P>New C<SUB>60</SUB> dimers 1, 2 and 3 that differ in the distance between the two balls, connected through pleiadene bridges have been synthesized. Different synthetic strategies have been used to prepare C<SUB>60</SUB> dimers 1–3. A diastereoisomeric mixture was obtained for C<SUB>60</SUB> dimer 1, which was separated by column chromatography and characterized by NMR. By CV measurements, no interaction between the two balls was found in the ground state in any type of C<SUB>60</SUB> dimer. By reduction with dimeric benzylnicotinamide [(BNA)<SUB>2</SUB>], a two electron reductant, the interaction between both C<SUB>60</SUB> units has been analyzed using electron paramagnetic resonance (EPR). For C<SUB>60</SUB> dimer 3, upon addition of 1 equivalent (BNA)<SUB>2</SUB> no electronic interaction in the C<SUB>60</SUB>˙<SUP>−</SUP>–C<SUB>60</SUB>˙<SUP>−</SUP> was observed due to the long distance between the C<SUB>60</SUB> balls (20 Å). However, for C<SUB>60</SUB> dimer 1, where the distance between radicals is shorter, 10 Å, the electronic interaction in the di(radical anion), C<SUB>60</SUB>˙<SUP>−</SUP>–C<SUB>60</SUB>˙<SUP>−</SUP> in the presence of 1 equivalent of (BNA)<SUB>2</SUB> was observed by EPR, corresponding to a triplet biradical.</P> <P>Graphic Abstract</P><P>Addition of 1 equivalent of (BNA)<SUB>2</SUB> to dimer 1 yields the C<SUB>60</SUB>˙<SUP>−</SUP>–C<SUB>60</SUB>˙<SUP>−</SUP> triplet biradical where electronic interaction is observed. <IMG SRC='http://pubs.rsc.org/services/images/RSCpubs.ePlatform.Service.FreeContent.ImageService.svc/ImageService/image/GA?id=c0jm02635b'> </P>

Global Overview of the Transnational Alliance for Regenerative Therapies in Cardiovascular Syndromes (TACTICS) Recommendations

Fern&aacute,ndez-Avilé,s, Francisco,Sanz-Ruiz, Ricardo,Climent, Andreu M.,Badimon, Lina,Bolli, Roberto,Charron, Dominique,Fuster, Valentin,Janssens, Stefan,Kastrup, Jens,Kim, Hyo-Soo,Lü,sche American Heart Foundation 2018 Circulation research Vol.122 No.2

KINEMATICS OF THE ENVELOPE AND TWO BIPOLAR JETS IN THE CLASS 0 PROTOSTELLAR SYSTEM L1157

Kwon, Woojin,Fern&aacute,ndez-Ló,pez, Manuel,Stephens, Ian W.,Looney, Leslie W. IOP Publishing 2015 The Astrophysical journal Vol.814 No.1

<P>A massive envelope and a strong bipolar outflow are the two main structures characterizing the youngest protostellar systems. In order to understand the physical properties of a bipolar outflow and the relationship with those of the envelope, we obtained a mosaic map covering the whole bipolar outflow of the youngest protostellar system L1157 with about 5 '' angular resolution in CO J = 2-1 using the Combined Array for Research in Millimeter-wave Astronomy. By utilizing these observations of the whole bipolar outflow, we estimate its physical properties and show that they are consistent with multiple jets. We also constrain a preferred precession direction. In addition, we observed the central envelope structure with 2' resolution in the lambda = 1.3 and 3 mm continua and various molecular lines: (CO)-O-17, (CO)-O-18, (13)CO3 CS, CN, N2H+, CH3OH, H2O, SO, and SO2. All of the CO isotopes and CS, CN, and N2H+ have been detected and imaged. We marginally detected the features that can be interpreted as a rotating inner envelope in (CO)-O-17 and (CO)-O-18 and as an infalling outer envelope in N2H+. We also estimated the envelope and central protostellar masses and found that the dust-opacity spectral index changes with radius.</P>

CARMA LARGE AREA STAR FORMATION SURVEY: DENSE GAS IN THE YOUNG L1451 REGION OF PERSEUS

Storm, Shaye,Mundy, Lee G.,Lee, Katherine I.,Fern&aacute,ndez-Ló,pez, Manuel,Looney, Leslie W.,Teuben, Peter,Arce, Hé,ctor G.,Rosolowsky, Erik W.,Meisner, Aaron M.,Isella, Andrea,Kauffmann American Astronomical Society 2016 The Astrophysical journal Vol.830 No.2

<P>We present a 3 mm spectral line and continuum survey of L1451 in the Perseus Molecular Cloud. These observations are from the CARMA Large Area Star Formation Survey (CLASSy), which also imaged Barnard. 1, NGC 1333, Serpens Main, and Serpens South. L1451 is the survey region with the lowest level of star formation activity-it contains no confirmed protostars. HCO+, HCN, and N2H+ (J = 1 -> 0). are all detected throughout the region, with HCO+ being the most spatially widespread, and molecular emission seen toward 90% of the area above N(H-2) column densities of 1.9 x 10(21) cm(-2). HCO+ has the broadest velocity dispersion, near 0.3 km s(-1) on average, compared with similar to 0.15 km s(-1) for the other molecules, thus representing a range of subsonic to supersonic gas motions. Our non-binary dendrogram analysis reveals that the dense gas traced by each molecule has a similar hierarchical structure, and that gas surrounding the candidate first hydrostatic core (FHSC), L1451-mm, and other previously detected single-dish continuum clumps has similar hierarchical structure; this suggests that different subregions of L1451 are fragmenting on the pathway to forming young stars. We determined that the three-dimensional morphology of the largest detectable dense-gas structures was relatively ellipsoidal compared with other CLASSy regions, which appeared more flattened at the largest scales. A virial analysis shows that the most centrally condensed dust structures are likely unstable against collapse. Additionally, we identify a new spherical, centrally condensed N2H+ feature that could be a new FHSC candidate. The overall results suggest that L1451 is a young region starting to form its generation of stars within turbulent, hierarchical structures.</P>

ALMA Observations of Polarized 872 <i>μ</i>m Dust Emission from the Protostellar Systems VLA 1623 and L1527

Harris, Robert J.,Cox, Erin G.,Looney, Leslie W.,Li, Zhi-Yun,Yang, Haifeng,Fern&aacute,ndez-Ló,pez, Manuel,Kwon, Woojin,Sadavoy, Sarah,Segura-Cox, Dominique,Stephens, Ian,Tobin, John American Astronomical Society 2018 The Astrophysical journal Vol.861 No.2

<P>We present high-sensitivity (sigma(I) similar to 0.2-0.5 mJy, sigma(QU) similar to 0.05 mJy), high-resolution (similar to 0.'' 12-0.'' 2) observations of polarized 872 mu m dust emission from the young multiple system VLA 1623 in rho Ophiuchus and the protostar L1527 in Taurus. We detect the circumstellar material of VLA 1623A, the extended Keplerian disk surrounding VLA 1623A that we call VLA 1623CBdisk, VLA 1623B, VLA 1623W, and L1527 strongly in the polarized emission, at the similar to 1%-3% level. We spatially resolve VLA 1623A into two sources, VLA 1623Aa and VLA 1623Ab, separated by similar to 30 au and located within a cavity of radius similar to 50 au within the circumbinary Keplerian disk, as well as the edge-on disk of VLA 1623W. The polarization angle of the emission is uniform across each protostellar source and nearly coincides with each disk's minor axis. The offsets between the minor axis position angle and the polarization angle are not uniformly distributed at the P less than or similar to 2 x 10(-4) level. The circumbinary disk surrounding VLA 1623Aab is azimuthally symmetrically polarized. Each compact source's emission is partially optically thick (tau greater than or similar to 1) at 872 mu m, complicating interpretations of polarization involving aligned grains. We find evidence against alignment by radiative flux in each source, particularly in the edge-on VLA 1623W and L1527. We detect astrometric offsets between the polarized emission and the total intensity in VLA 1623Aa, VLA 1623Ab, and VLA 1623B, as predicted if self-scattering in the optically thick limit operates. We conclude that self-scattering is likely responsible for disk-scale polarization at 872 mu m in these systems.</P>

Common non-synonymous SNPs associated with breast cancer susceptibility: findings from the Breast Cancer Association Consortium

Milne, Roger L.,Burwinkel, Barbara,Michailidou, Kyriaki,Arias-Perez, Jose-Ignacio,Zamora, M. Pilar,Mené,ndez-Rodrí,guez, Primitiva,Hardisson, David,Mendiola, Marta,Gonz&aacute,lez-Neira, A IRL Press 2014 Human molecular genetics Vol.23 No.22

<P>Candidate variant association studies have been largely unsuccessful in identifying common breast cancer susceptibility variants, although most studies have been underpowered to detect associations of a realistic magnitude. We assessed 41 common non-synonymous single-nucleotide polymorphisms (nsSNPs) for which evidence of association with breast cancer risk had been previously reported. Case-control data were combined from 38 studies of white European women (46 450 cases and 42 600 controls) and analyzed using unconditional logistic regression. Strong evidence of association was observed for three nsSNPs: <I>ATXN7-</I>K264R at 3p21 [rs1053338, per allele OR = 1.07, 95% confidence interval (CI) = 1.04–1.10, <I>P</I> = 2.9 × 10<SUP>−6</SUP>], <I>AKAP9-</I>M463I at 7q21 (rs6964587, OR = 1.05, 95% CI = 1.03–1.07, <I>P</I> = 1.7 × 10<SUP>−6</SUP>) and <I>NEK10-</I>L513S at 3p24 (rs10510592, OR = 1.10, 95% CI = 1.07–1.12, <I>P</I> = 5.1 × 10<SUP>−17</SUP>). The first two associations reached genome-wide statistical significance in a combined analysis of available data, including independent data from nine genome-wide association studies (GWASs): for <I>ATXN7-</I>K264R, OR = 1.07 (95% CI = 1.05–1.10, <I>P</I> = 1.0 × 10<SUP>−8</SUP>); for <I>AKAP9-</I>M463I, OR = 1.05 (95% CI = 1.04–1.07, <I>P</I> = 2.0 × 10<SUP>−10</SUP>). Further analysis of other common variants in these two regions suggested that intronic SNPs nearby are more strongly associated with disease risk. We have thus identified a novel susceptibility locus at 3p21, and confirmed previous suggestive evidence that rs6964587 at 7q21 is associated with risk. The third locus, rs10510592, is located in an established breast cancer susceptibility region; the association was substantially attenuated after adjustment for the known GWAS hit. Thus, each of the associated nsSNPs is likely to be a marker for another, non-coding, variant causally related to breast cancer risk. Further fine-mapping and functional studies are required to identify the underlying risk-modifying variants and the genes through which they act.</P>

Similar worldwide patterns in the sex pheromone signal and response in the oriental fruit moth, <i>Grapholita molesta</i> (Lepidoptera: Tortricidae)

Knight, A.L.,Barros-Parada, W.,Bosch, D.,Escudero-Colomar, L.A.,Fuentes-Contreras, E.,Hern&aacute,ndez-S&aacute,nchez, J.,Yung, C.,Kim, Y.,Kovanci, O.B.,Levi, A.,Lo, P.,Molinari, F.,Valls, J.,Gemeno, Cambridge University Press 2015 Bulletin of entomological research Vol.105 No.1

<B>Abstract</B><P>The response of <I>Grapholita molesta</I> (Busck) males to three-component sex pheromone blends containing a 100% ratio of the major sex pheromone component, (<I>Z</I>)-8-dodecenyl acetate and a 10% ratio of (<I>Z</I>)-8-dodecenol, but with varying ratios of (<I>E</I>)-8-dodecenyl acetate (0.4, 5.4, 10.4, 30.4, and 100.1% <I>E</I>-blends) was tested with populations in eight stone and pome fruit orchards in Europe, Asia, and North and South America. Traps baited with the 5.4% <I>E</I>-blend caught significantly more males than traps with any other blend with all populations. Significantly more males were caught in traps baited with the 10.4% <I>E</I>-blend than in traps with the remaining blends, except with the 0.4% <I>E-</I>blend in Turkey. Significant differences in male moth catches occurred between the other blends with the 0.4>30.4% <I>E-</I>blend, and the 30.4>100.1% <I>E-</I>blend. Male moth catches with the 100.1% <I>E</I>-blend only differed from the hexane control in Chile. No apparent differences were noted to these blends in populations collected from pome or stone fruits. Flight tunnel assays to synthetic blends with a subset of populations were similar to the field results, but the breadth of the most attractive <I>E-</I>blends was wider. Flight tunnel assays also demonstrated a high level of male-female cross-attraction among field-collected populations. Female gland extracts from field-collected populations did not show any significant variation in their three-component blends. The only exceptions in these assays were that long-term laboratory populations were less responsive and attractive, and produced different blend ratios of the two minor components than recently collected field populations.</P>

The pulsating hot subdwarf Balloon 090100001: results of the 2005 multisite campaign

Baran, A.,Oreiro, R.,Pigulski, A.,Hern&aacute,ndez, F. Pé,rez,Ulla, A.,Reed, M. D.,Rodrí,guez-Ló,pez, C.,Moskalik, P.,Kim, S.-L.,Chen, W.-P.,Crowe, R.,Siwak, M.,Armendarez, L.,Binder Blackwell Publishing Ltd 2009 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.392 No.3

<P>ABSTRACT</P><P>We present the results of a multisite photometric campaign on the pulsating B-type hot subdwarf star Balloon 090100001 (Bal09). The star is one of the two known hybrid hot subdwarfs with both long- and short-period oscillations, theoretically attributed to <I>g</I> and <I>p</I> modes. The campaign involved eight telescopes with three obtaining <I>UBVR</I> data, four <I>B</I>-band data and one Strömgren <I>uvby</I> photometry. The campaign covered 48 nights, providing a temporal resolution of 0.36 μHz with a detection threshold of about 0.2 mmag in <I>B</I>-filter data.</P><P>Bal09 has the richest pulsation spectrum of any known pulsating subdwarf B star, and our analysis detected 114 frequencies including 97 independent and 17 combination ones. Most of the 24 <I>g</I>-mode frequencies are between 0.1 and 0.4 mHz. Of the remaining 73, presumably <I>p</I> modes, 72 group into four distinct regions near 2.8, 3.8, 4.7 and 5.5 mHz. The density of frequencies requires that some modes must have degrees ℓ larger than 2. The modes in the 2.8 mHz region have the largest amplitudes. The strongest mode (<I>f</I><SUB>1</SUB>) is most likely radial, while the remaining ones in this region form two nearly symmetric multiplets: a triplet and quintuplet, attributed to rotationally split ℓ= 1 and 2 modes, respectively. We find clear increases of splitting in both multiplets between the 2004 and 2005 observing campaigns, amounting to ∼15 per cent on average. The observed splittings imply that the rotational rate in Bal09 depends on stellar latitude and is the fastest on the equator. We also speculate on the possible reasons for the changes of splitting. The only plausible explanation we find is torsional oscillation. This hypothesis, however, needs to be verified in the future by detailed modelling. In this context, it is very important to monitor the splittings on a longer time-scale as their behaviour may help to explain this interesting phenomenon.</P><P>The amplitudes of almost all terms detected in both 2004 and 2005 were found to vary. This is evident even during one season; for example, amplitudes of modes <I>f</I><SUB>8</SUB> and <I>f</I><SUB>C</SUB> were found to change by a factor of 2–3 within about 50 d during 2005.</P><P>We use a small grid of models to constrain the main mode (<I>f</I><SUB>1</SUB>), which most likely represents the radial fundamental pulsation. The groups of <I>p</I>-mode frequencies appear to lie in the vicinity of the consecutive radial overtones, up to the third one. Despite the large number of <I>g</I>-mode frequencies observed, we failed to identify them, most likely because of the disruption of asymptotic behaviour by mode trapping. The observed frequencies were not, however, fully exploited in terms of seismic analysis which should be done in the future with a larger grid of reliable evolutionary models of hot subdwarfs.</P>