Bulk scalar field in DGP braneworld cosmology

We investigated the effects of bulk scalar field in the braneworld cosmological scenario. The Friedmann equations and acceleration condition in presence of the bulk scalar field for a zero tension brane and cosmological constant are studied. In DGP model the effective Einstein equation on the brane is obtained with bulk scalar field. The rescaled bulk scalar field on the brane in the DGP model behaves as an effective four dimensional field, thus standard type cosmology is recovered. In present study of the DGP model, the late-time accelerating phase of the universe can be explained .Comment: 10 pages, to appear in JCA

A new class of two-channel biorthogonal filter banks and wavelet bases

We propose a novel framework for a new class of two-channel biorthogonal filter banks. The framework covers two useful subclasses: i) causal stable IIR filter banks. ii) linear phase FIR filter banks. There exists a very efficient structurally perfect reconstruction implementation for such a class. Filter banks of high frequency selectivity can be achieved by using the proposed framework with low complexity. The properties of such a class are discussed in detail. The design of the analysis/synthesis systems reduces to the design of a single transfer function. Very simple design methods are given both for FIR and IIR cases. Zeros of arbitrary multiplicity at aliasing frequency can be easily imposed, for the purpose of generating wavelets with regularity property. In the IIR case, two new classes of IIR maximally flat filters different from Butterworth filters are introduced. The filter coefficients are given in closed form. The wavelet bases corresponding to the biorthogonal systems are generated. the authors also provide a novel mapping of the proposed 1-D framework into 2-D. The mapping preserves the following: i) perfect reconstruction; ii) stability in the IIR case; iii) linear phase in the FIR case; iv) zeros at aliasing frequency; v) frequency characteristic of the filters

Second Backbend in the Mass A ~ 180 Region

Within the framework of selfconsistent cranked Hartree-Fock- Bogoliubov theory(one-dimensional) we predict second backbend in the yrast line of Os-182 at $I \approx 40$, which is even sharper than the first one observed experimentally at $I \approx 14$. Around such a high spin the structure becomes multi-quasiparticle type, but the main source of this strong discontinuity is a sudden large alignment of i_13/2 proton orbitals along the rotation axis followed soon by the alignment of j_15/2 neutron orbitals. This leads to drastic structural changes at such high spins. When experimentally confirmed, this will be observed for the first time in this mass region, and will be at the highest spin so far.Comment: 13 pages, 4 ps figure

Bird Responses to Habitat Change in the Karst Area of Bantimurung Bulusaraung National Park

Birds are useful bioindicators to habitat changes. This study aims to determine the responses of birds to habitat change at Maros-Pangkep karst area, Bantimurung-Bulusaraung National Park. The research was carried out in three disturbance degrees (core-zone, wilderness-zone, and the community-gardens), which represents minimal, middle, and high interference level. A modified square-line method was used to observe vegetation of bird habitat. Point count method was used to observe bird population. Data of the bird habitat vegetation was analyzed using vegetation density. The difference of vegetation composition was analyzed using Sorensen-similarity index. Data of the bird was analyzed using abundance, and indexes of Shannon-Weinner diversity, Simpson dominance, Pielou evenness, and Margalef species richness. Significant differences between the number of the individual bird were tested using one-way ANOVA, Tukey-Bonferroni test. The results showed that birds living in karst were sensitive to habitat changes. Birds responded through reducing the number of individuals and species, shifting the species of bird that has high importance value index from low tolerance species to high tolerance species. Birds also responded by shifting the feeding guild that has high important value index from frugivore to frugivore-insectivore and then to granivore, decreasing the number of bird species with large body size, reducing the number of bird species that need a special location to build nest. Considering that Maros-Pangkep Karst has vital roles, scientific values, and biodiversity richness, it is necessary to involve all stakeholders to maintain its sustainability, including the establishment of entire Maros-Pangkep Karst area as the karst-landscape area

Three-body resonances Lambda-n-n and Lambda-Lambda-n

Possible bound and resonant states of the hypernuclear systems $\Lambda nn$ and $\Lambda\Lambda n$ are sought as zeros of the corresponding three-body Jost functions calculated within the framework of the hyperspherical approach with local two-body S-wave potentials describing the $nn$, $\Lambda n$, and $\Lambda\Lambda$ interactions. Very wide near-threshold resonances are found for both three-body systems. The positions of these resonances turned out to be sensitive to the choice of the $\Lambda n$-potential. Bound $\Lambda nn$ and $\Lambda\Lambda n$ states only appear if the two-body potentials are multiplied by a factor of $\sim 1.5$.Comment: 12 pages, 5 figures. Acknowledgments are added in the new versio

The MACHO Project LMC Microlensing Results from the First Two Years and the Nature of the Galactic Dark Halo

The MACHO Project is a search for dark matter in the form of massive compact halo objects (Machos). Photometric monitoring of millions of stars in the Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), and Galactic bulge is used to search for gravitational microlensing events caused by these otherwise invisible objects. Analysis of the first 2.1 years of photometry of 8.5 million stars in the LMC reveals 8 candidate microlensing events. This is substantially more than the number expected ($\sim 1.1$) from lensing by known stellar populations. The timescales (\that) of the events range from 34 to 145 days. We estimate the total microlensing optical depth towards the LMC from events with 2 < \that < 200 days to be \tau_2^{200} = 2.9 ^{+1.4}_{-0.9} \ten{-7} based upon our 8 event sample. This exceeds the optical depth, \tau_{\rm backgnd} = 0.5 \ten{-7}, expected from known stars, and the difference is to be compared with the optical depth predicted for a ``standard" halo composed entirely of Machos: \tau_{halo} = 4.7\ten{-7}. Likelihood analysis gives a fairly model independent estimate of the halo mass in Machos within 50 kpc of 2.0^{+1.2}_{-0.7} \ten{11} \msun, about half of the ``standard halo" value. We also find a most probable Macho mass of 0.5^{+0.3}_{-0.2}\msun, although this value is strongly model dependent. Additionally, the absence of short duration events places stringent upper limits on the contribution of low-mass Machos: objects from 10^{-4} \msun to 0.03 \msun contribute \simlt 20\% of the ``standard" dark halo.Comment: Latex, 54 pages, uses aas2pp4.sty and astrobib.sty, with 24 out of 26 Postscript figures in gzipped tar file. 2 extra greyscale figures and/or full paper available from ftp://igpp.llnl.gov/pub/macho/LMC2/ Submitted to ApJ, June 199

Constraints on Intervening Stellar Populations Toward the Large Magellanic Cloud

The suggestion by Zaritsky & Lin that a vertical extension of the red clump feature in color-magnitude diagrams of the Large Magellanic Cloud (LMC) is consistent with a significant population of foreground stars to the LMC that could account for the observed microlensing optical depth has been challenged by various investigators. We respond by (1) examining each of the challenges presented and (2) presenting new photometric and spectroscopic data. We conclude that although the CMD data do not mandate the existence of a foreground population, they are entirely consistent with a foreground population associated with the LMC that contributes significantly (~ 50%) to the observed microlensing optical depth. From our new data, we conclude that <~ 40% of the VRC stars are young, massive red clump stars because (1) synthetic color-magnitude diagrams created using the star formation history derived indepdently from HST data suggest that < 50% of the VRC stars are young, massive red clump stars, (2) the angular distribution of the VRC stars is more uniform than that of the young (age < 1 Gyr) main sequence stars, and (3) the velocity dispersion of the VRC stars in the region of the LMC examined by ZL is inconsistent with the expectation for a young disk population. Each of these arguments is predicated on assumptions and the conclusions are uncertain. Therefore, an exact determination of the contribution to the microlensing optical depth by the various hypothesized foreground populations, and the subsequent conclusions regarding the existence of halo MACHOs, requires a detailed knowledge of many complex astrophysical issues, such as the IMF, star formation history, and post-main sequence stellar evolution. (abridged)Comment: Scheduled for publication in AJ in May 199

Quantitative microarray profiling of DNA-binding molecules

A high-throughput Cognate Site Identity (CSI) microarray platform interrogating all 524 800 10-base pair variable sites is correlated to quantitative DNase I footprinting data of DNA binding pyrrole-imidazole polyamides. An eight-ring hairpin polyamide programmed to target the 5 bp sequence 5'-TACGT-3' within the hypoxia response element (HRE) yielded a CSI microarray-derived sequence motif of 5'-WWACGT-3' (W = A,T). A linear beta-linked polyamide programmed to target a (GAA)_3 repeat yielded a CSI microarray-derived sequence motif of 5'-AARAARWWG-3' (R = G,A). Quantitative DNase I footprinting of selected sequences from each microarray experiment enabled quantitative prediction of K_a values across the microarray intensity spectrum