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Shrimp Fishing in Mexico
235 Shrimp fishing in Mexico Based on the work of D. Aguilar and J. Grande-Vidal AN OVERVIEW Mexico has coastlines of 8 475 km along the Pacific and 3 294 km along the Atlantic Oceans. Shrimp fishing in Mexico takes place in the Pacific, Gulf of Mexico and Caribbean, both by artisanal and industrial fleets. A large number of small fishing vessels use many types of gear to catch shrimp. The larger offshore shrimp vessels, numbering about 2 212, trawl using either two nets (Pacific side) or four nets (Atlantic). In 2003, shrimp production in Mexico of 123 905 tonnes came from three sources: 21.26 percent from artisanal fisheries, 28.41 percent from industrial fisheries and 50.33 percent from aquaculture activities. Shrimp is the most important fishery commodity produced in Mexico in terms of value, exports and employment. Catches of Mexican Pacific shrimp appear to have reached their maximum. There is general recognition that overcapacity is a problem in the various shrimp fleets. DEVELOPMENT AND STRUCTURE Although trawling for shrimp started in the late 1920s, shrimp has been captured in inshore areas since pre-Columbian times. Magallón-Barajas (1987) describes the lagoon shrimp fishery, developed in the pre-Hispanic era by natives of the southeastern Gulf of California, which used barriers built with mangrove sticks across the channels and mouths of estuaries and lagoons. The National Fisheries Institute (INP, 2000) and Magallón-Barajas (1987) reviewed the history of shrimp fishing on the Pacific coast of Mexico. It began in 1921 at Guaymas with two United States boats. -
Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Multicolor Surface Photometry of Lenticular Galaxies
The Astronomical Journal, 129:630–646, 2005 February # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. MULTICOLOR SURFACE PHOTOMETRY OF LENTICULAR GALAXIES. I. THE DATA Sudhanshu Barway School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Y. D. Mayya Instituto Nacional de Astrofisı´ca, O´ ptica y Electro´nica, Apdo. Postal 51 y 216, Luis Enrique Erro 1, 72000 Tonantzintla, Pue., Mexico; [email protected] Ajit K. Kembhavi Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411007, India; [email protected] and S. K. Pandey1 School of Studies in Physics, Pandit Ravishankar Shukla University, Raipur 492010, India; [email protected] Receivedv 2003 Auggust 13; accepted 2004 October 20 ABSTRACT We present multicolor surface and aperture photometry in the B, V, R,andK0 bands for a sample of 34 lenticular galaxies from the Uppsala General Catalogue. From surface photometric analysis, we obtain radial profiles of surface brightness, colors, ellipticity, position angle, and the Fourier coefficients that describe the departure of isophotal shapes from a purely elliptical form; we find the presence of dust lanes, patches, and ringlike structure in several galaxies in the sample. We obtain total integrated magnitudes and colors and find that these are in good agreement with the values from the Third Reference Catalogue. Isophotal colors are correlated with each other, following the sequence expected for early-type galaxies. The color gradients in lenticular galaxies are more negative than the corresponding gradients in elliptical galaxies. There is a good correlation between BÀVand BÀR color gradients, and the mean gradients in the BÀV, BÀR,andVÀK0 colors are À0:13 Æ 0:06, À0:18 Æ 0:06, and À0:25 Æ 0:11 mag dexÀ1 in radius, respectively. -
Southern Arp - AM # Order
Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
2014 Observers Challenge List
2014 TMSP Observer's Challenge Atlas page #s # Object Object Type Common Name RA, DEC Const Mag Mag.2 Size Sep. U2000 PSA 18h31m25s 1 IC 1287 Bright Nebula Scutum 20'.0 295 67 -10°47'45" 18h31m25s SAO 161569 Double Star 5.77 9.31 12.3” -10°47'45" Near center of IC 1287 18h33m28s NGC 6649 Open Cluster 8.9m Integrated 5' -10°24'10" Can be seen in 3/4d FOV with above. Brightest star is 13.2m. Approx 50 stars visible in Binos 18h28m 2 NGC 6633 Open Cluster Ophiuchus 4.6m integrated 27' 205 65 Visible in Binos and is about the size of a full Moon, brightest star is 7.6m +06°34' 17h46m18s 2x diameter of a full Moon. Try to view this cluster with your naked eye, binos, and a small scope. 3 IC 4665 Open Cluster Ophiuchus 4.2m Integrated 60' 203 65 +05º 43' Also check out “Tweedle-dee and Tweedle-dum to the east (IC 4756 and NGC 6633) A loose open cluster with a faint concentration of stars in a rich field, contains about 15-20 stars. 19h53m27s Brightest star is 9.8m, 5 stars 9-11m, remainder about 12-13m. This is a challenge obJect to 4 Harvard 20 Open Cluster Sagitta 7.7m integrated 6' 162 64 +18°19'12" improve your observation skills. Can you locate the miniature coathanger close by at 19h 37m 27s +19d? Constellation star Corona 5 Corona Borealis 55 Trace the 7 stars making up this constellation, observe and list the colors of each star asterism Borealis 15H 32' 55” Theta Corona Borealis Double Star 4.2m 6.6m .97” 55 Theta requires about 200x +31° 21' 32” The direction our Sun travels in our galaxy. -
Observing Galaxies in Pegasus 01 October 2015 23:07
Observing galaxies in Pegasus 01 October 2015 23:07 Context As you look towards Pegasus you are looking below the galactic plane under the Orion spiral arm of our galaxy. The Perseus-Pisces supercluster wall of galaxies runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. It includes the Pegasus I group noted later this document. The constellation is well placed from mid summer to late autumn. Pegasus is a rich constellation for galaxy observing. I have observed 80 galaxies in this constellation. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 7331 MAG 9 This is the stand out galaxy of the constellation. It is similar to our milky way. Around it are a number of fainter NGC galaxies. I have seen the brightest one, NGC 7335 in my 10 inch scope with averted vision. I have seen NGC 7331 in my 25 x 100mm binoculars. NGC 7814 - Mag 10 ? Not on observed list ? This is a very lovely oval shaped galaxy. By constellation Page 1 NGC 7332 MAG 11 / NGC 7339 MAG 12 These galaxies are an isolated bound pair about 67 million light years away. NGC 7339 is the fainter of the two galaxies at the eyepiece. I have seen NGC 7332 in my 25 x 100mm binoculars. -
By Philip R. Woodside U.S. Geological Survey Open-File Report 8L This
UNITED STATES DEPARTMENT OF THE INTERIOR GEOLOGICAL SURVEY THE PETROLEUM GEOLOGY OF TRINIDAD AND TOBAGO By Philip R. Woodside U.S. Geological Survey Open-File Report 8l This report is preliminary and has not been reviewed for conformity with U.S. Geological Survey editorial standards and stratigraphic nomenclature* Any use of trade names is for descriptive purposes only and does not imply endorsment by the USGS. 1981 CONTENTS Page For ewo r d •————————•———-————————————————•————————•—•————•—— Abstract —• Introduction ——————————————————————————————————————————— 1 Structural Geology ————•—-———————•———•—•—————-———•—•——•—— 4 Introduction -——————————————————————————————————————— 4 Structural Areas of Trinidad ——————————————————————————— 5 The Northern Range ——————————•—————————————————————— 5 The Northern (Caroni) Basin —————————————————————————— 6 The Central Range ————————————————————————————————— 6 The Southern Basin (including Naparima Thrust Belt) ———————— 6 Los Bajos fault ———————————————————————————————— 7 The Southern Range ————————————————————————————————— 9 Shale Diapirs ———————————————————————————————————— 10 Stratigraphy ——————————————————————————————————————————— 11 Northern Range and Northern Basin ——————————————————————— 11 Central Range —————————————————————————————————————— 12 Southern Basin and Southern Range —————-————————————————— 14 Suimnary ————————————————————————————————————————————— 18 Oil and Gas Occurrence ———•——————————•——-——————•————-—•—•— 19 Introduction ————•—•————————————————————————-—— 19 Hydrocarbon Considerations -
Arxiv:Astro-Ph/0305472 V1 23 May 2003
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) An Hα survey aiming at the detection of extraplanar diffuse ionized gas in halos of edge–on spiral galaxies ? II. The Hα survey atlas and catalog J. Rossa ??1,2 and R.–J. Dettmar1 1 Astronomisches Institut, Ruhr–Universit¨at Bochum, D–44780 Bochum, Germany e-mail: [email protected], [email protected] 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. (present address) Received 14 February 2003 / Accepted 6 May 2003 Abstract. In this second paper on the investigation of extraplanar diffuse ionized gas in nearby edge–on spiral galaxies we present the actual results of the individual galaxies of our Hα imaging survey. A grand total of 74 galaxies have been studied, including the 9 galaxies of a recently studied sub–sample (Rossa & Dettmar 2000). 40.5% of all studied galaxies reveal extraplanar diffuse ionized gas, whereas in 59.5% of the survey galaxies no extraplanar diffuse ionized gas could be detected. The average distances of this extended emission above the galactic midplane range from 1–2 kpc, while individual filaments in a few galaxies reach distances of up to |z| ∼ 6 kpc. In several cases a pervasive layer of ionized gas was detected, similar to the Reynolds layer in our Milky Way, while other galaxies reveal only extended emission locally. The morphology of the diffuse ionized gas is discussed for each galaxy and is compared with observations of other important ISM constituents in the context of the disk–halo connection, in those cases where published results were available. -
Health and Climate Change: Country Profile 2020
TRINIDAD AND TOBAGO HEALTH & CLIMATE CHANGE COUNTRY PROFILE 2020 Small Island Developing States Initiative CONTENTS 1 EXECUTIVE SUMMARY 2 KEY RECOMMENDATIONS 3 BACKGROUND 4 CLIMATE HAZARDS RELEVANT FOR HEALTH 7 HEALTH IMPACTS OF CLIMATE CHANGE 9 HEALTH VULNERABILITY AND ADAPTIVE CAPACITY 11 HEALTH SECTOR RESPONSE: MEASURING PROGRESS Acknowledgements This document was developed in collaboration with the Ministry of Health and the Ministry of Planning and Development, who together with the World Health Organization (WHO), the Pan American Health Organization (PAHO), and the United Nations Framework Convention on Climate Change (UNFCCC) gratefully acknowledge the technical contributions of Mr Arnold Ramkaran, Dr Roshan Parasram, Mr Lawrence Jaisingh and Mr Kishan Kumarsingh. Financial support for this project was provided by the Norwegian Agency for Development Cooperation (NORAD). ii Health and Climate Change Country Profile “Many of the public health gains we have made in recent decades are at risk due to the direct and indirect impacts of climate variability and climate change.” EXECUTIVE SUMMARY Despite producing very little greenhouse gas policies, building resilience must happen in emissions that cause climate change, people parallel with the reduction of carbon emissions living in small island developing States (SIDS) by countries around the world. are on the frontline of climate change impacts. The WHO Special Initiative on Climate Change These countries face a range of acute to long- and Health in SIDS aims to provide national term risks, including extreme weather events health authorities in SIDS with the political, such as floods, droughts and cyclones, increased technical and financial support required to better average temperatures and rising sea levels. -
Education in Trinidad and Tobago
An Overview of The Educational System of Trinidad & Tobago American & Caribbean Law Initiative Fall 2008 Introduction to Trinidad and Tobago Located 7 mile off the coast of Venezuela The Republic of Trinidad and Tobago has a population of approximately 1.3 million inhabitants Majority of the population is located in Trinidad with about 50,000 inhabitants on the smaller island of Tobago Ruled by the British, Trinidad and Tobago gained independence in 1962 and declared itself a republic in 1976 The economy is largely based on the country’s abundance of natural resources, particularly Oil and Gas. Introduction to Trinidad and Tobago The country has a stable government and considers itself to be a leading political and economic power in the Caribbean. The total GDP in 2005 was approximately 14 million USD Literacy rate is 98.6- highest in the Caribbean The official language is English with French, Chinese, Spanish and the Caribbean Hindustani, a dialect of Hindi also spoken Map of Trinidad and Tobago Education System Based on British Model Education is free and compulsory for children ages 5 to 13 years of age Education System divided into 3 phases: Primary Education Secondary Education Higher Education Higher Education Higher Education is post-secondary study leading to diploma, certificates and degrees Two major higher education institutions: University of West Indies National Institute for Higher Education Primary Education Primary consists of 2 preparatory ("infant") grades and 5 "standard" grades Includes children -
Sea Level Rise and Land Use Planning in Barbados, Trinidad and Tobago, Guyana, and Pará
Water, Water Everywhere: Sea Level Rise and Land Use Planning in Barbados, Trinidad and Tobago, Guyana, and Pará Thomas E. Bassett and Gregory R. Scruggs © 2013 Lincoln Institute of Land Policy Lincoln Institute of Land Policy Working Paper The findings and conclusions of this Working Paper reflect the views of the author(s) and have not been subject to a detailed review by the staff of the Lincoln Institute of Land Policy. Contact the Lincoln Institute with questions or requests for permission to reprint this paper. [email protected] Lincoln Institute Product Code: WP13TB1 Abstract The Caribbean and northern coastal Brazil face severe impacts from climate change, particularly from sea-level rise. This paper analyses current land use and development policies in three Caribbean locations and one at the mouth of the Amazon River to determine if these policies are sufficient to protect economic, natural, and population resources based on current projections of urbanization and sea-level rise. Where policies are not deemed sufficient, the authors will address the question of how land use and infrastructure policies could be adjusted to most cost- effectively mitigate the negative impacts of climate change on the economies and urban populations. Keywords: sea-level rise, land use planning, coastal development, Barbados, Trinidad and Tobago, Guyana, Pará, Brazil About the Authors Thomas E. Bassett is a senior program associate at the American Planning Association. He works on the Energy and Climate Partnership of the Americas grant from the U.S. Department of State as well as the domestic Community Assistance Program. Thomas E. Bassett 1030 15th Street NW Suite 750W Washington, DC 20005 Phone: 202-349-1028 Email: [email protected]; [email protected] Gregory R.