With the updated sensitivity of terrestrial gravitational-wave (GW) detectors in their fourth observing run, we expect a high rate of detection of binary black hole mergers. With this comes the hope that we will detect rarer classes of merger events. Compact binaries formed dynamically in dense stellar environments are likely to be detected with a residual eccentricity as they enter the sensitivity band of ground-based GW detectors. In this paper, we present a time-domain inspiral-merger-ringdowm (IMR) waveform model ESIGMAHM constructed within a framework we named ESIGMA for coalescing binaries of spinning black holes on moderately eccentric orbits [Phys. Rev. D 97, 024031 (2018).]. We now include the effect of black hole spins on the dynamics of eccentric binaries, as well as model sub-dominant waveform harmonics emitted by them. The inspiral evolution is described by a consistent combination of latest results from postNewtonian theory, self-force, and black hole perturbation theory. We assume that these moderately eccentric binaries radiate away most of their orbital eccentricity before merger, and seamlessly connect the eccentric inspiral with a numerical relativity based surrogate waveform model NRSur7dq4 for mergers of spinning binaries on quasicircular orbits. We present two variants of ESIGMAHM: the inspiral-only version is named InspiralESIGMAHM, while the full IMR one is termed IMRESIGMAHM; or InspiralESIGMA and IMRESIGMA when only dominant modes are used. We validate ESIGMAHM against eccentric numerical relativity simulations, and also against contemporary effective-one-body and phenomenological models in the quasicircular limit. We find that ESIGMAHM achieves match values greater than 99% for quasicircular spin-aligned binaries with mass ratios up to 8, and above 97% for nonspinning and spinning eccentric systems with small or positively aligned spins. Using IMRESIGMA, we quantify the impact of orbital eccentricity on GW signals, showing that next-generation detectors can detect eccentric sources up to 10% louder than quasicircular ones. We also show that current templated LIGO-Virgo-KAGRA searches will lose more than 10% of optimal SNR for about 20% of all eccentric sources by using only quasicircular waveform templates. The same will result in a 25% loss in detection rate for eccentric sources with mass ratios m1/m2 >= 4. Our results highlight the need for including eccentricity and higher-order modes in GW source models and searches for asymmetric eccentric BBH signals.

Major constraints in exploiting full genetic potential of the crops for achieving higher yield is the supply of adequate nutrients. The application of chemical fertilizer to fulfil the nutrient requirement of crops is advocated since the introduction of green revolution in India. However, during the period 1960-69, the response to NPK fertilization was about 12 kg of food grains per kg of nutrient. It declined to 10 kg during 1980-89 and to 9 kg during 1990-99, and the declining trend in continuing. Further, high cost of chemical fertilizer, widening gap between supply and demand and low purchasing power of small and marginal farmer contributing adversely to our Agricultural production process. The situation is further complicated during the last couple of decades due to proven negative International Journal of Current Microbiology and Applied Sciences ISSN: 2319-7706 Special Issue-10 pp. 408-423 Journal homepage: http://www.ijcmas.com

ISSN: 2319-7706 Special Issue-10 pp. 392-407 Journal homepage: http://www.ijcmas.com Under present investigation 48 PGPR isolates were isolated from different rhizotic zones of maize based intercropping system by using different media from twelve different site of Bihar including diara belt. PGPR isolates are coded for Azospirillum spp. as AZS1 to AZS12, Azotobacter spp. as AZT1 to AZT12, Pseudomonas spp. as PSD1 to PSD`12 and P-solubilizing bacteria spp. as PSB1 to PSB12. These isolates were screened on the basis of seed germination, production of IAA, P-solubilization activity, antifungal activity, and nitrogenase activity for the formulation of microbial consortium. Under pot condition plant height, leaf area index, number of leaves plant -1 , fresh and dry weight of shoot and root, total biomass production, root volume, percentage root colonization by mycorrhiza in pot soil and microbial population of Pseudomonas spp. PSD6 was maximum in treatment T14 (NPK + PSD6 + AZS6 + AZT4) while microbial population of Azotobacter spp. AZT4, P-solubilization bacteria PSB4 and MPN of Azospirillum spp. AZS6 were maximum in treatment T13 (NPK + PSB4 + AZS6 + AZT4). Keeping in view of experimental findings, PGPRs of diara belt are extremely diversified and perform well in stress condition. They are also competitive in nature and efficient in nitrogen fixing, P-solubilization and producing plant growth hormones. After 60 days, growth period in maize plant N (0.78%), P (0.35%) and K (0.65%) content were significantly superior over UIC(T1) and maximum in treatment T13 (NPK + PSB4 + AZS6 + AZT4). Similarly N and K uptake by whole plant was found significantly influenced by co-inoculation of selected strains of PGPR and was maximum in treatment T14 (NPK + PSD6 + AZS6 + AZT4) which was probably due to higher biomass production. While P-uptake was found maximum in treatment T13 (NPK + PSB4 + AZS6 + AZT4). Microbial consortium improves crop growth and increase biomass production. Hence, it may be concluded that PGPRs (PSD6 + AZS6 + AZT4) form best microbial consortium in all respect than that of others which is very significant not only in growth parameters but also in maintaining soil health for sustainable crop production. K e y w o r d s PGPR, Rhizobacteria, Intercropping, Pseudomonas,

The discovery of the gravitational-wave (GW) source GW150914 with the Advanced LIGO detectors provides the first observational evidence for the existence of binary black hole (BH) systems that inspiral and merge within the age of the universe. Such BH mergers have been predicted in two main types of formation models, involving isolated binaries in galactic fields or dynamical interactions in young and old dense stellar environments. The measured masses robustly demonstrate that relatively “heavy” BHs ( 25  M) can form in nature. This discovery implies relatively weak massive-star winds and thus the formation of GW150914 in an environment with a metallicity lower than about 1/2 of the solar value. The rate of binary-BH (BBH) mergers inferred from the observation of GW150914 is consistent with the higher end of rate predictions ( 1  Gpc yr) from both types of formation models. The low measured redshift (z 0.1  ) of GW150914 and the low inferred metallicity of the stellar progenitor imply either BBH formation in a low-mass galaxy in the local universe and a prompt merger, or formation at high redshift with a time delay between formation and merger of several Gyr. This discovery motivates further studies of binary-BH formation astrophysics. It also has implications for future detections and studies by Advanced LIGO and Advanced Virgo, and GW detectors in space.

Human population in developing countries (Africa, Asia and the Americas) is increasing rapidly (Allen, 1983). Jasiorowski (1975) stated that world demand for animal protein is growing continuously. The main reason for the present low per capita consumption of animal protein is the low livestock productivity rather than the low livestock numbers (Jasiorowski, 1975; FAO, 1994). Among animal protein goat rearing for its meat is an important sector of the agro-economy in India and in Indian sub-continents. Low capital investments and higher economic returns have been the unique features of small and marginal goat production systems (Devendra, 2013). Goat meat has provided health promoting constituents to health conscious consumers and thus contribution of goats is increasing to the rising demand of animal products. The productivity of small ruminants in most tropical countries is generally low, mainly due to poor quality and inadequacy of available feeds. Protein is the most expensive feed ingredient in animal ration and there was always shortage in its supply particularly in developing countries. This shortage is very critical in both human and animal nutrition (Yagoub and Talha, 2009). Moreover, conventional feed ingredients International Journal of Current Microbiology and Applied Sciences ISSN: 2319-7706 Special Issue-7 pp. 2895-2900 Journal homepage: http://www.ijcmas.com

This is the eighth post-O2 release of PyCBC for analysis of data taken during Advanced LIGO's second observing run and Advanced Virgo's first observing run. This release is identical to the 1.9.3, except that it contains https://github.com/ligo-cbc/pycbc/commit/2557bb573c1b46fb926fbfa1345545dd15ef72ea that fixes the bad setup.py file in v1.9.3. This release has been tested against LALSuite with the hash: 8cbd1b7187ce3ed9a825d6ed11cc432f3cfde9a5 This provides functionality to provide a windowing function to apply to data segments before PSD estimation. Details of the changes since the 1.9.2 release are at https://github.com/ligo-cbc/pycbc/compare/v1.9.2..v1.9.4 A Docker container for this release is available from the pycbc/pycbc-el7 repository on Docker Hub and can be downloaded using the command: docker pull pycbc/pycbc-el7:v1.9.4 On a machine with CVMFS installed, a pre-built virtual environment is available for Red Hat 7 compatible operating systems by running the command: source /cvmfs/oasis.opensciencegrid.org/ligo/sw/pycbc/x86_64_rhel_7/virtualenv/pycbc-v1.9.4/bin/activate and for Debian 8 compatible operating systems by running the command: source /cvmfs/oasis.opensciencegrid.org/ligo/sw/pycbc/x86_64_deb_8/virtualenv/pycbc-v1.9.4/bin/activate A bundled pycbc_inspiral executable for use on the Open Science Grid is available at /cvmfs/oasis.opensciencegrid.org/ligo/sw/pycbc/x86_64_rhel_6/bundle/v1.9.4/pycbc_inspiral

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We report here the non-detection of gravitational waves from the merger of binary–neutron star systems and neutron star–black hole systems during the first observing run of the Advanced Laser Interferometer Gravitationalwave Observatory (LIGO). In particular, we searched for gravitational-wave signals from binary–neutron star systems with component masses Î  M 1, 3 [ ] and component dimensionless spins <0.05. We also searched for neutron star–black hole systems with the same neutron star parameters, black hole mass Î  M 2, 99 [ ] , and no restriction on the black hole spin magnitude. We assess the sensitivity of the two LIGO detectors to these systems and find that they could have detected the merger of binary–neutron star systems with component mass distributions of 1.35±0.13Me at a volume-weighted average distance of ∼70Mpc, and for neutron star–black hole systems with neutron star masses of 1.4Me and black hole masses of at least 5Me, a volume-weighted average distance of at least ∼110Mpc. From this we constrain with 90% confidence the merger rate to be less than 12,600Gpcyr for binary–neutron star systems and less than 3600Gpcyr for neutron star–black hole systems. We discuss the astrophysical implications of these results, which we find to be in conflict with only the most optimistic predictions. However, we find that if no detection of neutron star–binary mergers is made in the next two Advanced LIGO and Advanced Virgo observing runs we would place significant constraints on the merger rates. Finally, assuming a rate of + 10 7 20 Gpc yr, short gamma-ray bursts beamed toward the Earth, and assuming that all short gamma-ray bursts have binary–neutron star (neutron star–black hole) progenitors, we can use our 90% confidence rate upper limits to constrain the beaming angle of the gamma-ray burst to be greater than  + 2 .3 1.1 1.7 (  + 4 .3 1.9 ).

1 Department of Veterinary Physiology and Biochemistry, C.V.Sc. and A.H., N.D. University of Agriculture and Technology, Kumarganj, Faizabad, U.P., India 2 Department of Veterinary Physiology, R.V.C., B.A.U., Ranchi, India 3 Department of Chemistry, L.N.M.U., Darbhanga, India 4 Department of Agronomy (A.H.), B.A.U., Sabour, Bhagalpur, India 5 Department of Veterinary Pathology, C.V.Sc. and A.H., N.D. University of Agriculture and Technology, Kumarganj, Faizabad, U.P., India 6 Department of Veterinary Anatomy and Histology, C.V.Sc. and A.H., N.D. University of Agriculture and Technology, Kumarganj, Faizabad, U.P., India *Corresponding author

We present the results of the first search for gravitational wave bursts associated with high energy neutrinos. Together, these messengers could reveal new, hidden sources that are not observed by conventional photon astronomy, particularly at high energy. Our search uses neutrinos detected by the underwater neutrino telescope ANTARES in its 5 line configuration during the period January September 2007, which coincided with the fifth and first science runs of LIGO and Virgo, respectively. The LIGO-Virgo data were analysed for candidate gravitational-wave signals coincident in time and direction with the neutrino events. No significant coincident events were observed. We place limits on the density of joint high energy neutrino gravitational wave emission events in the local universe, and compare them with densities of merger and core-collapse events. Subject headings: gravitational waves — high energy neutrinos 1 Institut d’Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC) Universitat Politècnica de València. C/ Paranimf 1 , 46730 Gandia, Spain. 2 CPPM, Aix-Marseille Université, CNRS/IN2P3, Marseille, France 3 GRPHE Institut universitaire de technologie de Colmar, 34 rue du Grillenbreit BP 50568 68008 Colmar, France 4 Technical University of Catalonia, Laboratory of Applied Bioacoustics, Rambla Exposició, 08800 Vilanova i la Geltrú, Barcelona, Spain 5 INFN Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy 6 Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany 7 Direction des Sciences de la Matière Institut de recherche sur les lois fondamentales de l’Univers Service d’Electronique des Détecteurs et d’Informatique, CEA Saclay, 91191 Gif-surYvette Cedex, France 8 Nikhef, Science Park, Amsterdam, The Netherlands 9 APC, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris, France 10 LAM Laboratoire d’Astrophysique de Marseille, Pôle de l’Étoile Site de Château-Gombert, rue Frédéric Joliot-Curie 38, 13388 Marseille Cedex 13, France 11 INFN Sezione di Bologna, Viale C. Berti-Pichat 6/2, 40127 Bologna, Italy 12 Dipartimento di Fisica dell’Università, Viale Berti Pichat 6/2, 40127 Bologna, Italy 13 IFIC Instituto de F́ısica Corpuscular, Edificios Investigación de Paterna, CSIC Universitat de València, Apdo. de Correos 22085, 46071 Valencia, Spain 14 INFN -Sezione di Roma, P.le Aldo Moro 2, 00185 Roma, Italy 15 Dipartimento di Fisica dell’Università La Sapienza, P.le Aldo Moro 2, 00185 Roma, Italy 16 Clermont Université, Université Blaise Pascal, CNRS/IN2P3, Laboratoire de Physique Corpusculaire, BP 10448, 63000 Clermont-Ferrand, France 17 Géoazur Université de Nice Sophia-Antipolis, CNRS/INSU, IRD, Observatoire de la Côte d’Azur and Université Pierre et Marie Curie, BP 48, 06235 Villefranche-surmer, France 18 INFN Sezione di Bari, Via E. Orabona 4, 70126 Bari, Italy 19 INFN Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, 95123 Catania, Italy 20 MIO, Mediterranean Institute of Oceanography, AixMarseille University, 13288, Marseille, Cedex 9, France; Université du Sud Toulon-Var, 83957, La Garde Cedex, France CNRS-INSU/IRD UM 110 21 Univ Paris-Sud , 91405 Orsay Cedex, France 22 Kernfysisch Versneller Instituut (KVI), University of Groningen, Zernikelaan 25, 9747 AA Groningen, The Netherlands 23 Direction des Sciences de la Matière Institut de recherche sur les lois fondamentales de l’Univers Service de Physique des Particules, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France 24 INFN Sezione di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy 25 Dipartimento di Fisica dell’Università di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy 26 University Mohammed I, Laboratory of Physics of Matter and Radiations, B.P.717, Oujda 6000, Morocco 27 Royal Netherlands Institute for Sea Research (NIOZ), Landsdiep 4,1797 SZ ’t Horntje (Texel), The Netherlands 28 Dr. Remeis-Sternwarte and ECAP, Universität ErlangenNürnberg, Sternwartstr. 7, 96049 Bamberg, Germany 29 Universiteit Utrecht, Faculteit Betawetenschappen, Princetonplein 5, 3584 CC Utrecht, The Netherlands 30 Universiteit van Amsterdam, Instituut voor Hoge-Energie Fysica, Science Park 105, 1098 XG Amsterdam, The Netherlands 31 Moscow State University, Skobeltsyn Institute of Nuclear Physics, Leninskie gory, 119991 Moscow, Russia 32 INFN Sezione di Catania, Viale Andrea Doria 6, 95125 Catania, Italy 33 Dipartimento di Fisica ed Astronomia dell’Università, Viale Andrea Doria 6, 95125 Catania, Italy 34 Département de Physique Nucléaire et Corpusculaire, Université de Genève, 1211, Geneva, Switzerland 35 Institute for Space Sciences, R-77125 Bucharest, Măgurele, Romania 36 IPHC-Institut Pluridisciplinaire Hubert Curien Université de Strasbourg et CNRS/IN2P3 23 rue du Loess, BP 28, 67037 Strasbourg Cedex 2, France 37 ITEP Institute for Theoretical and Experimental Physics, B. Cheremushkinskaya 25, 117218 Moscow, Russia 38 Dipartimento di Fisica dell’Università, Via Dodecaneso 33, 16146 Genova, Italy 39 Also at University of Leiden, the Netherlands 40 On leave of absence at the Humboldt-Universität zu Berlin 41 Also at Accademia Navale di Livorno, Livorno, Italy 42 LIGO California Institute of Technology, Pasadena, CA 91125, USA 43 California State University Fullerton, Fullerton CA 92831 USA 44 SUPA, University of Glasgow, Glasgow, G12 8QQ, United Kingdom 45 Laboratoire d’Annecy-le-Vieux de Physique des Particules 4 The ANTARES Collaboration, the LIGO Scientific Collaboration and the Virgo Collaboration (LAPP), Université de Savoie, CNRS/IN2P3, F-74941 AnnecyLe-Vieux, France 46 INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy 47 Università di Napoli ’Federico II’, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy 48 Università di Salerno, I-84084 Fisciano (Salerno), Italy 49 LIGO Livingston Observatory, Livingston, LA 70754, USA 50 Cardiff University, Cardiff, CF24 3AA, United Kingdom 51 University of Sannio at Benevento, I-82100 Benevento, Italy and INFN (Sezione di Napoli), Italy 52 Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany 53 Leibniz Universität Hannover, D-30167 Hannover, Germany 54 VU University Amsterdam, De Boelelaan 1081, 1081 HV Amsterdam, the Netherlands 55 National Astronomical Observatory of Japan, Tokyo 181-8588, Japan 56 University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA 57 Università di Siena, I-53100 Siena, Italy 58 University of Florida, Gainesville, FL 32611, USA 59 LIGO Hanford Observatory, Richland, WA 99352, USA 60 University of Birmingham, Birmingham, B15 2TT, United Kingdom 61 Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Golm, Germany 62 Montana State University, Bozeman, MT 59717, USA 63 European Gravitational Observatory (EGO), I-56021 Cascina (PI), Italy 64 Syracuse University, Syracuse, NY 13244, USA 65 LIGO Massachusetts Institute of Technology, Cambridge, MA 02139, USA 66 Columbia University, New York, NY 10027, USA 67 Stanford University, Stanford, CA 94305, USA 68 IM-PAN 00-956 Warsaw, Poland 69 Astronomical Observatory Warsaw University 00-478 Warsaw, Poland 70 CAMK-PAN 00-716 Warsaw, Poland 71 Bia lystok University 15-424 Bia lystok, Poland 72 NCBJ 05-400 Świerk-Otwock, Poland 73 Institute of Astronomy 65-265 Zielona Góra, Poland 74 The University of Texas at Brownsville, Brownsville, TX 78520, USA 75 San Jose State University, San Jose, CA 95192, USA 76 Moscow State University, Moscow, 119992, Russia 77 LAL, Université Paris-Sud, IN2P3/CNRS, F-91898 Orsay, France 78 ESPCI, CNRS, F-75005 Paris, France 79 NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA 80 University of Western Australia, Crawley, WA 6009, Australia 81 The Pennsylvania State University, University Park, PA 16802, USA 82 Université Nice-Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, F-06304 Nice, France 83 Institut de Physique de Rennes, CNRS, Université de Rennes 1, 35042 Rennes, France 84 Laboratoire des Matériaux Avancés (LMA), IN2P3/CNRS, F-69622 Villeurbanne, Lyon, France 85 Washington State University, Pullman, WA 99164, USA 86 INFN, Sezione di Perugia, I-06123 Perugia, Italy 87 Università di Perugia, I-06123 Perugia, Italy 88 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Italy 89 Università degli Studi di Urbino ’Carlo Bo’, I-61029 Urbino, Italy 90 University of Oregon, Eugene, OR 97403, USA 91 Laboratoire Kastler Brossel, ENS, CNRS, UPMC, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France 92 University of Maryland, College Park, MD 20742 USA 93 Universitat de les Illes Balears, E-07122 Palma de Mallorca, Spain 94 University of Massachusetts Amherst, Amherst, MA 01003, USA 95 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H8, Canada 96 Tsinghua University, Beijing 100084 China 97 University of Michigan, Ann Arbor, MI 48109, USA 98 Louisiana State University, Baton Rouge, LA 70803, USA 99 The University of Mississippi, University, MS 38677, USA 100 Charles Sturt University, Wagga Wagga, NSW 2678, Australia 101 Caltech-CaRT, Pasadena, CA 91125, USA 102 Pusan National University, Busan 609-735, Korea 103 Australian National University, Canberra, ACT 0200, Australia 104 Carleton College, Northfield, MN 55057, USA 105 The University of Melbourne, Parkville, VIC 3010, Australia 106 INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy 107 Università di Roma Tor Vergata, I-00133 Roma, Italy 108 Università dell’Aquila, I-67100 L’Aquila, Italy 109 Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, SP, Brazil 110 The University of Sheffield, Sheffield S10 2TN, United Kingdom 111 Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29-33, Hungary 112 Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India 113 University of Minnesota, M

Lacustrine deep‐water turbidite plays are potential areas for future exploration and exploitation in NW‐SE trending 200 km long and 25 km wide Barmer Basin located in Northwest India. Sediment gravity flow deposits in the form of turbidite sand and heterolith enclosed within a background of lacustrine muds ‐ in the Palaeocene Barmer Hill Formation of the Vijaya & Vandana (V&V) Field, in the basin, provide an excellent opportunity to study the factors controlling the reservoir properties and consequent hydrocarbon accumulations in these reservoirs. In the V&V core area the entire sedimentary column is divided into seven packages, inferred to be deposited as sediment gravity flows in a mud dominated slope channel environment, downslope from a fan delta system. The top 3 packages ‐ the subject of the present study ‐ are composed of slope channel system, which at the seismic scale has an overall linear shape and oriented in ENE‐WSW direction with lateral extent variations controlled by changes in sediment input and basin slope/topography. The associated smaller scale elements – resolved from 261 m of core data from key wells – can be divided into four broad lithofacies: sandstone, heteroliths, mudstone, and porcellanite. Sandstone lithofacies – the principal reservoir in the V&V Field ‐ is quartz to sub‐litharenite in composition and is characterized by a wide variation in grain size, matrix content and cement type. Most of the sandstones cored in the study area are silty to highly silty which explains their low reservoir quality, with relative abundances of coarse to fine being guided by the distance of transport and associated subenvironments. It is, however, the burial diagenesis (involving clay mineral authigenesis and cementation, under the influence of evolving pore water at elevated pressure and temperature) that exerted primary control on reservoir quality in terms of porosity and permeability. Based on the results of thin section photomicrographs and mercury porosimetry data, three distinct sand sub classes have been identified, reflecting variation in pore throat size tight sandstone (~0.01‐0.1 mD), moderately tight sandstone (~0.1‐10 mD), and sandstone with cement dissolution (~10‐200 mD) (Figure 1). This classification can be correlated to the interplay of pore reduction and pore enhancement which is controlled by cementation clay authigenesis and grain dissolution respectively. Low pressure and low temperature ‘Early’ diagenesis commenced with grain re‐organization and mechanical compaction followed by dissolution of unstable grains. This is followed by precipitation of framboidal pyrite (due to consumption of organic matter by sulphate‐reducing bacteria) and replacement of unstable volcanic fragments by chlorite. A period of methanogenesis ensures precipitation of intergranular, siderite crystals by reaction with available ferrous iron in the system. Increased alkalinity and consequent carbonate cementation is attributed to anaerobic or less commonly aerobic degradation of oil by deeply infiltrating meteoric water during the hyperpycnal flow (Morad et al., 2002, Mansurbeg, 2017, Mansurbeg et al., 2006), the fluid mechanism believed to be responsible for the deposition of V&V sands. All these processes lead to degradation of reservoir characteristics by porosity destruction. Siderite is the most widespread cement and occurs most commonly as anhedral finely crystalline siderite partially replacing the detrital clay matrix and locally forming micronodules (Figure 2). Onset of high pressure and high temperature ‘Late’ diagenesis is marked by grain dissolution (mainly Kfeldspar grains and volcanic rock fragments) enhancing the reservoir properties. Pore fluids were acidic at the start of later diagenesis with the onset of the main phase of postcompactional grain dissolution and subsequent blocky kaolinite and quartz overgrowth development. Liberated silica and alumina ions helped in crystallization of kaolinite. Quartz overgrowths are seen to have precipitated after the main period of burial-related diagenesis from excess silica generated from unstable grain dissolution. Resulting alkaline pore water deposited ferroan calcite and ferroan dolomite. Finally minor pyrite associated with replacement gets precipitated as pore water becomes acidic at the end of diagenesis (Figure 2). This study helps in understanding the variation in reservoir quality which is mainly controlled by the relative abundance of detrital clay content (matrix) and their diagenetic derivatives (cement). This is critical in explaining the well test results and in selection of key candidate wells for an early development wherein the flow rate potential will be principally predicted through free available pore spaces.

Dark matter is among the most important and long standing open problems in modern physics. Contrary to our understanding, it is observed that the orbital velocity of a star in a galaxy increases with distance away from the center. It means there is more mass in the galaxy than the luminous mass. Dark matter is postulated by Jan Oort in 1932 to account for this effect. There are also observations that the distant galaxies are moving faster as time proceeds. There is constant energy density of the space which does not dilute with the expansion and is referred as Dark Energy. On the basis of all the observations and model calculations the composition of the universe is understood to be only ~4 % visible matter, ~70% dark energy and ~26 % dark matter. Various dark matter candidates have been proposed by several models in the support of the presence of dark matter but till date dark matter candidate is not yet discovered. The Weakly Interacting Massive Particles (WIMPS) are the most accepted candidates for dark matter. We used Germanium ionization detectors, which can be capable of observing rare weakly interacting particles by discriminating them from all known type of background particles and radiations including low energy neutrons. The goal is also to achieve very low detection threshold to observe dark matter candidate WIMP such as neutralinos. A large array of this type of detector will have discovery potential for the Dark Matter and can also be used to measure properties of neutrino from reactors or from the supernova. The detector has simple detection principle requiring limited electronics and also portable. It can also be used for the detection of neutrinoless double beta decay searches. Germanium ionization detectors are novel techniques offering kg-scale radiation sensors with sub-keV sensitivities. Germanium ionization detectors have been used for the studies of neutrino interactions and properties as well as to search for light WIMP Dark Matter. However, anomalous surface behavior, which needs to be characterized and understood. Crucial to this study, is the understanding of the selection procedures for the bulk and surface events differentiation in the sub-keV range of energy. In this report we will describe the detector characterization methods and results which are used to identify the bulk and surface events in the analysis techniques. In addition, the atomic effects due to neutrino electromagnetic properties were derived, and constraints were placed with reactor neutrino data, are summarized.

The Vijaya and Vandana (V&V) fields, located in the central part of Barmer basin, were discovered in 2005 by Cairn. The oil bearing Barmer Hill Formation consists of two types of reservoir packages– sandstones/heteroliths deposited as lacustrine hyperpicnites and porcellanites with alternations of diatomite and mudstone layers. Sandstone lithofacies is the main reservoir rock, but with permeability vastly impaired by cementation. The porosity of these sandstones ranges 10-20% and show permeability variation of 0.01-200mD. Numerous pay zones of 5-10 meters are dispersed over gross rock thickness of about 500m. Conventional testing of individual pay zones in initial wells produced oil at subcommercial rates.