Determinants of Poverty Profiles in Ogun State

Abstract: This research focuses on the Analysis of Determinants of Poverty Profiles in Ogun State using a case study of Abeokuta North Local Government. The broad objective of the study is to examine the determinants of poverty in Ogun State the case of Abeokuta North Local Government area of Ogun State. The specific objectives are to: describe the socio-economic characteristics of the respondents; determine the factors influencing poverty profile in the study area and proffer recommendations based on research findings on how to improve the welfare of the people and Ogun state in general. The study adopted descriptive statistics and Regression Analysis to achieve the stated objectives. The study revealed that majority of the respondents are males, still in their active and single. Majority of the respondents are within the age range 21-30 years with the maximum household size of 3-4, majority of the respondents stay in bedroom that are owned by them, majority are fairly educated and spend ≤₦5,000 on feeding, cloth, water bill, transportation, Nepa bill and school fees per term. The result also shows that majority opined that poverty in Ogun State will be decreasing in the next 10 years and the government is rated averagely when it comes to the amelioration of poverty. Also, the analysis shows that educational level and household size have positive relationship with the household expenditure model and both are significant at (5%) while age and marital status of the respondents have no significant difference in profile model. (proxied by household expenditure). This research therefore concluded that educational level and household size of the respondents have significant roles to play in the poverty profile in the study area. This research recommends that the government should: Create more job opportunities for people that are willing and able to work, improve the standard of educational with the introduction of vocational skills and also create an enabling environment (social amenities, infrastructure, etc.) that will enhance more investment to the state

Search for three-jet resonances in pp collisions at √s=7 TeV

This is a Pre-Print version of the Article - Copyright @ 2011 APSA model-independent search for three-jet hadronic resonance production in pp collisions at a center-of-mass energy of 7 TeV has been conducted by the CMS Collaboration at the LHC, using a data sample corresponding to an integrated luminosity of 35 inverse picobarns. Events with high jet multiplicity and a large scalar sum of jet transverse momenta are analyzed. The number of expected standard model background events is found to be in good agreement with the observed events. Limits are set on a model describing the production of R-parity-violating supersymmetric gluino pairs, and gluino masses in the range of 200 to 280 GeV/c^2 are excluded at a 95% confidence level for the first time.This work is supported by the FMSR (Austria); FNRS and FWO (Belgium); CNPq, CAPES, FAPERJ, and FAPESP (Brazil); MES (Bulgaria); CERN; CAS, MoST, and NSFC (China); COLCIENCIAS (Colombia); MSES (Croatia); RPF (Cyprus); Academy of Sciences and NICPB (Estonia); Academy of Finland, ME, and HIP (Finland); CEA and CNRS/IN2P3 (France); BMBF, DFG, and HGF (Germany); GSRT (Greece); OTKA and NKTH (Hungary); DAE and DST (India); IPM (Iran); SFI (Ireland); INFN (Italy); NRF andWCU (Korea); LAS (Lithuania); CINVESTAV, CONACYT, SEP, and UASLP-FAI (Mexico); PAEC (Pakistan); SCSR (Poland); FCT (Portugal); JINR (Armenia, Belarus, Georgia, Ukraine, Uzbekistan); MST and MAE (Russia); MSTD (Serbia); MICINN and CPAN (Spain); Swiss Funding Agencies (Switzerland); NSC (Taipei); TUBITAK and TAEK (Turkey); STFC (United Kingdom); DOE and NSF (USA)

Orbital eccentricity as a probe of thick disc formation scenarios

We study the orbital properties of stars in four (published) simulations of thick disks formed by: i) accretion from disrupted satellites, ii) heating of a pre-existing thin disk by a minor merger, iii) radial migration and iv) gas rich mergers. We find that the distribution of orbital eccentricities are predicted to be different for each model: a prominent peak at low eccentricity is expected for the heating, migration and gas-rich merging scenarios, while the eccentricity distribution is broader and shifted towards higher values for the accretion model. These differences can be traced back to whether the bulk of the stars in each case is formed 'in-situ' or is 'accreted', and are robust to the peculiarities of each model. A simple test based on the eccentricity distribution of nearby thick disk stars may thus help elucidate the dominant formation mechanism of the Galactic thick disk.Comment: 5 pages, 3 figures, accepted to MNRAS Letters. Typo correcte