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Q: Best practice for naming unit and integration test methods? I've recently inherited an application that is written by different people at different times and looking for guidance on how to standardize.

A: I just write what it's for. It's not like you're going to have to type the names in anywhere else, so having a testWibbleDoesNotThrowAnExceptionIfPassedAFrobulator isn't a problem. Anything which is a test begins with 'test', obviously.

A: There is no standard as such, different people/places will have different schemes. The important thing is you stick to a standard.
Personally I'm a fan of the following - example code in C#, but very close to Java, same rules apply:
[Test]
public void person_should_say_hello()
{
     // Arrange
     var person = new Person();
     // Act
     string result = person.SayHello();
     // Assert
     Assert(..., "The person did not say hello correctly!");
}

Explicit
The test name should give the name of the class under test. In this example, the class being tested is Person. The test name should also have the name of the method that is being tested. This way, if the test was to fail, you'll at least know where to look to solve it. I'd also recommend following the AAA - Arrange, Act, Assert rule, it will ensures your tests are easy to read and follow.
Friendly fail messages
When it comes to asserting a result/state, its useful to include an optional message. This makes it easier when a test fails, especially when run as part of a build process or via an external tool.
Underscores
The final (though optional) stance I follow is using underscores for tests names. While I'm no fan of underscores in production code, their use in test names is useful as test names are often much longer. Quickly glancing at a test name that uses underscores proves to be much more readable, though this is subjective and the source of much debate with regards unit testing practices.
Integration Tests
The same standards apply to integration tests, the only difference being the location of such tests should be separate from unit tests. In the example code above, the test class would be called PersonTests and located in a file called PersonTests.cs. The integration tests would be named in a similar manner - PersonIntegrationTests, located in PersonIntegrationTests.cs. The same project can be used for these tests, but ensure they are located in separate directories.

A: It's instructive to look at BDD (behavioural driven development) and this blog post in particular.
BDD is essentially focusing on components and what they should do. Consequently it impacts directly on how you name/structure your tests, and the code they use to set up conditions and validate. BDD allows not only the developers to read/write the tests, but non-technical members of the team (business analysts etc.) can contribute by specifying the tests and validating them.

A: Assuming NUnit:
[Test]
public void ObjectUnderTest_StateChanged_Consequence()
{
    Assert.That(tra_la_la);
}

[Test]
public void ObjectUnderTest_Behaviour_Consequence()
{
    Assert.That(tra_la_la);
}

for example:
[Test]
public void WifeIsTired_TakeWifeToDinner_WifeIsGrateful()
{
    Assert.That(tra_la_la);
}

[Test]
public void WifeIsTired_MentionNewGirlfriend_WifeGetsHalf()
{
    Assert.That(tra_la_la);
}

A: I ran across two good suggestions. Links here:  http://slott-softwarearchitect.blogspot.com/2009/10/unit-test-naming.html
http://weblogs.asp.net/rosherove/archive/2005/04/03/TestNamingStandards.aspx
http://openmrs.org/wiki/Unit_Testing_with_@should

A: In that situation I'd probably find the naming convention that was used the most and refactor the rest of the code to use that.  If the one that was used the most is truly horrid, I'd still look to the existing code and try to find one that I could live with.  Consistency is more important than arbitrary conventions.

A: I use a FunctionTestCondition construct. If I have two methods, Get and Set I would maybe create the following test methods:

*

*GetTest being a positive test (everything is ok).

*GetTestInvalidIndex to test an invalid index being passed to the method.

*GetTestNotInitialized to test when the data is not inited before use.

*SetTest

*SetTestInvalidIndex

*SetTestTooLargeValue

*SetTestTooLongString

A: Group your tests by setup, make a test class around this setup and name is with suffix Test or IntegrationTest. Using a test framework like JUnit or TestNG you can name your test methods as you want. I would name the method as what it tests, a sentence in camel case, not test prefix. The frameworks use a @Test annotation to mark a method as test.


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Fermi LAT Search for Photon Lines from 30 to 200 GeV
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A. A. Abdo Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA National Research Council Research Associate, National Academy of Sciences, Washington, DC 20001, USA M. Ackermann W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA M. Ajello W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA W. B. Atwood Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA L. Baldini Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy J. Ballet Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France G. Barbiellini Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy D. Bastieri Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy K. Bechtol W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA R. Bellazzini Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy B. Berenji W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA E. D. Bloom W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA E. Bonamente Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy A. W. Borgland W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA A. Bouvier W. W. 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Çelik NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA A. Chekhtman Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA George Mason University, Fairfax, VA 22030, USA J. Chiang W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA S. Ciprini Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy R. Claus W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA J. Cohen-Tanugi Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France J. Conrad Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation C. D. Dermer Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA A. de Angelis Dipartimento di Fisica, Università di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy F. de Palma Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy S. W. Digel W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA E. do Couto e Silva W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA P. S. Drell W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA A. Drlica-Wagner W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA R. Dubois W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA D. Dumora Université de Bordeaux, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France CNRS/IN2P3, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France Y. Edmonds W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA R. Essig W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA C. Farnier Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France C. Favuzzi Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy S. J. Fegan Laboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, France W. B. Focke W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA P. Fortin Laboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, France M. Frailis Dipartimento di Fisica, Università di Udine and Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, Gruppo Collegato di Udine, I-33100 Udine, Italy Y. Fukazawa Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan S. Funk W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA P. Fusco Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy F. Gargano Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy D. Gasparrini Agenzia Spaziale Italiana (ASI) Science Data Center, I-00044 Frascati (Roma), Italy N. Gehrels NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA Department of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USA S. Germani Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy N. Giglietto Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy F. Giordano Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy T. Glanzman W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA G. Godfrey W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA I. A. Grenier Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France J. E. Grove Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA L. Guillemot Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany S. Guiriec Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, AL 35899, USA M. Gustafsson Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy D. Hadasch Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona, Spain A. K. Harding NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA D. Horan Laboratoire Leprince-Ringuet, École polytechnique, CNRS/IN2P3, Palaiseau, France R. E. Hughes Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA M. S. Jackson The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden Department of Physics, Royal Institute of Technology (KTH), AlbaNova, SE-106 91 Stockholm, Sweden G. Jóhannesson W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA A. S. Johnson W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA R. P. Johnson Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA W. N. Johnson Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA T. Kamae W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA H. Katagiri Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan J. Kataoka Waseda University, 1-104 Totsukamachi, Shinjuku-ku, Tokyo, 169-8050, Japan N. Kawai Department of Physics, Tokyo Institute of Technology, Meguro City, Tokyo 152-8551, Japan Cosmic Radiation Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351-0198, Japan M. Kerr Department of Physics, University of Washington, Seattle, WA 98195-1560, USA J. Knödlseder Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, BP 44346, F-30128 Toulouse Cedex 4, France M. Kuss Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy J. Lande W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA L. Latronico Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy M. Llena Garde Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden F. Longo Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy F. Loparco Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy B. Lott Université de Bordeaux, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France CNRS/IN2P3, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France M. N. Lovellette Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA P. Lubrano Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy A. Makeev Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA George Mason University, Fairfax, VA 22030, USA M. N. Mazziotta Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy J. E. McEnery NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Department of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USA C. Meurer Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden P. F. Michelson W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA W. Mitthumsiri W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA T. Mizuno Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan A. A. Moiseev Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Department of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USA C. Monte Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy M. E. Monzani W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA A. Morselli Istituto Nazionale di Fisica Nucleare, Sezione di Roma "Tor Vergata", I-00133 Roma, Italy I. V. Moskalenko W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA S. Murgia W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA P. L. Nolan W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA J. P. Norris Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA E. Nuss Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France T. Ohsugi Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan N. Omodei Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy E. Orlando Max-Planck Institut für extraterrestrische Physik, 85748 Garching, Germany J. F. Ormes Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA M. Ozaki Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan D. Paneque W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA J. H. Panetta W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA D. Parent Université de Bordeaux, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France CNRS/IN2P3, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France V. Pelassa Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France M. Pepe Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy Dipartimento di Fisica, Università degli Studi di Perugia, I-06123 Perugia, Italy M. Pesce-Rollins Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy F. Piron Laboratoire de Physique Théorique et Astroparticules, Université Montpellier 2, CNRS/IN2P3, Montpellier, France S. Rainò Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy R. Rando Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy M. Razzano Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy A. Reimer Institut für Astro- und Teilchenphysik and Institut für Theoretische Physik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA O. Reimer Institut für Astro- und Teilchenphysik and Institut für Theoretische Physik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA T. Reposeur Université de Bordeaux, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France CNRS/IN2P3, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France J. Ripken Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden S. Ritz Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA A. Y. Rodriguez Institut de Ciencies de l'Espai (IEEC-CSIC), Campus UAB, 08193 Barcelona, Spain M. Roth Department of Physics, University of Washington, Seattle, WA 98195-1560, USA H. F.-W. Sadrozinski Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA A. Sander Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA P. M. Saz Parkinson Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA J. D. Scargle Space Sciences Division, NASA Ames Research Center, Moffett Field, CA 94035-1000, USA T. L. Schalk Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA A. Sellerholm Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden C. Sgrò Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy E. J. Siskind NYCB Real-Time Computing Inc., Lattingtown, NY 11560-1025, USA D. A. Smith Université de Bordeaux, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France CNRS/IN2P3, Centre d'Études Nucléaires Bordeaux Gradignan, UMR 5797, Gradignan, 33175, France P. D. Smith Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA G. Spandre Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy P. Spinelli Dipartimento di Fisica "M. Merlin" dell'Università e del Politecnico di Bari, I-70126 Bari, Italy Istituto Nazionale di Fisica Nucleare, Sezione di Bari, 70126 Bari, Italy J.-L. Starck Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France M. S. Strickman Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA D. J. Suson Department of Chemistry and Physics, Purdue University Calumet, Hammond, IN 46323-2094, USA H. Tajima W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA H. Takahashi Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan T. Tanaka W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA J. B. Thayer W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA J. G. Thayer W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA L. Tibaldo Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy Dipartimento di Fisica "G. Galilei", Università di Padova, I-35131 Padova, Italy Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d'Astrophysique, CEA Saclay, 91191 Gif sur Yvette, France D. F. Torres Institució Catalana de Recerca i Estudis Avançats (ICREA), Barcelona, Spain Institut de Ciencies de l'Espai (IEEC-CSIC), Campus UAB, 08193 Barcelona, Spain Y. Uchiyama W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA T. L. Usher W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA V. Vasileiou Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA N. Vilchez Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, BP 44346, F-30128 Toulouse Cedex 4, France V. Vitale Istituto Nazionale di Fisica Nucleare, Sezione di Roma "Tor Vergata", I-00133 Roma, Italy Dipartimento di Fisica, Università di Roma "Tor Vergata", I-00133 Roma, Italy A. P. Waite W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA P. Wang W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA B. L. Winer Department of Physics, Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA K. S. Wood Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA T. Ylinen Department of Physics, Royal Institute of Technology (KTH), AlbaNova, SE-106 91 Stockholm, Sweden School of Pure and Applied Natural Sciences, University of Kalmar, SE-391 82 Kalmar, Sweden The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden M. Ziegler Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA
Dark matter (DM) particle annihilation or decay can produce monochromatic γ-rays readily distinguishable from astrophysical sources. γ-ray line limits from 30 GeV to 200 GeV obtained from 11 months of Fermi Large Area Space Telescope data from 20-300 GeV are presented using a selection based on requirements for a γ-ray line analysis, and integrated over most of the sky. We obtain γ-ray line flux upper limits in the range 0.6−4.5×10−9cm−2s−1, and give corresponding DM annihilation cross-section and decay lifetime limits. Theoretical implications are briefly discussed.
95.35.+d, 95.85.Pw, 98.70.Vc
††preprint:
Introduction: Annihilation or decay of dark matter (DM) particles can give rise to Standard Model particles, including γ-rays. The predicted γ-ray flux is usually weak compared to astrophysical sources, and striking experimental signatures are valuable in recognizing a signal. A distinctive signal would be the detection of a narrow γ-ray line Srednicki et al. (1986); Rudaz (1986); Bergström and Snellman (1988); Rudaz and Stecker (1991); Jungman et al. (1996); Bergström and Ullio (1997a); Bergström et al. (2008) originating from dark matter particles annihilating or decaying into γX, where X can be another photon, a Z-boson, a Higgs-boson, or a non-Standard Model particle. A γ-ray line search using data from EGRET in the energy range 1−10 GeV has been presented in Pullen et al. (2007) . We present here for the first time results from 11 months of Fermi Large Area Telescope (LAT) data in the energy range 20-300 GeV and obtain limits for 30-200 GeV.
DM particles of mass mχ annihilating into γX produce monochromatic γ-rays of energy Eγ=mχ(1−m2X4m2χ), where mX is the mass of X. For decays χ→γX, the equation gives the photon energy after the substitution mχ→mχ/2. Since dark matter is strongly constrained to be electrically neutral, it has no direct coupling to photons. The process χ(χ)→γX thus occurs only at higher orders, and with a branching fraction that is typically only 10−4−10−1 compared to the total annihilation or decay rate. However, a strong line feature, or a strong line-like feature such as a sharp cut-off at a particular energy, can be expected in models with supersymmetry Bergström and Ullio (1997b); Bern et al. (1997); Ullio and Bergstrom (1998); Bergström et al. (2005); Bringmann et al. (2008a) , an extended Higgs sector Gustafsson et al. (2007) , from final state radiation Beacom et al. (2005); Bergstrom et al. (2005); Birkedal et al. (2005) , from gravitino decay Ibarra and Tran (2008) , or in scenarios with non-thermal WIMP production Kane et al. (2009) .
LAT Data Selection and Analysis: The LAT is a pair-conversion telescope that combines silicon-strip/tungsten trackers and hodoscopic CsI(Tl) calorimeters into a 4x4 array of 16 identical modules. The tracker is covered by a segmented anti-coincidence detector (ACD). Including the tracker, the LAT presents 10 radiation lengths for normal incidence. The depth, segmentation, and wide field of view of the LAT enable its high-energy reach. Separation of the very large charged cosmic-ray background from γ-rays is achieved via the combination of the data acquisition trigger, on-board event software filter system, and extensive ground processing of the data. Details of the LAT, and the data analysis are given in Atwood et al. (2009) . An account of how the LAT is calibrated on orbit is presented in Abdo et al. (2009a) . The LAT nominally operates in a scanning mode that covers the whole sky every two orbits (∼3 hours). The analysis described here uses data taken in this scanning mode from Aug 7, 2008, to July 21, 2009, corresponding to an average exposure of 3.3×1010 cm2s.
Events are selected for this analysis only if they pass additional cuts to the Pass6V3 diffuse class cuts, i.e., the cleanest photon sample in the currently public Fermi data release Atwood et al. (2009); pub . These additional cuts are: a) a small average charge deposited in the tracker planes (veto against heavy ions); b) a transverse shower size in the calorimeter within a size range expected for electromagnetic showers (veto against hadronic showers and minimum ionizing particles). Cuts a) and b) dramatically reduce the charged particle background at the loss of some effective area, yielding a γ-ray efficiency >90% relative to that of Pass6V3 diffuse class. These cuts remove charged particle backgrounds that would worsen our upper limits, and that can even yield structures that might be interpreted as γ-ray lines. These cuts are a subset of those used in the LAT Measurements of the Isotropic Diffuse Gamma-Ray Emission Abdo et al. (2009b) .
In addition, we use only one of the three energy measurement methods from the LAT standard analysis. The method used is the LAT profile method Atwood et al. (2009) , in order to not introduce energy dependent artifacts that arise from switching between methods over the energy range discussed here. In the profile method, the energy is obtained from a fit to the longitudinal shower profile while considering the transverse profile. The exclusive use of the profile energy method led to no additional reduction in efficiency. The instrument response functions (IRFs) are recalculated for this data selection and for the use of the profile method.
The resulting energy resolution averaged over the LAT acceptance is 11% FWHM for 20-100 GeV, increasing to 13% FWHM for 150-200 GeV. The photon angular resolution is less than 0.1∘ over the energy range of interest (68% containment). The absolute calibration and energy resolution of the LAT was determined by comparing with e− beam test data, taken at CERN in a secondary e− beam with energies up to 300 GeV using a special calibration unit made up of flight spare towers and ACD tiles (not the LAT itself) Abdo et al. (2009c) . The energy resolution measured in the beam tests is in agreement with the predictions from the Monte Carlo simulator based on GEANT4 that was used to define the IRFs (GLEAM Atwood et al. (2009) ). Also, the systematic error on the absolute energy of the LAT was determined to be −10+5% for 20-300 GeV.
The systematic uncertainties for the exposure over this energy range are ±20% based on the extrapolation of studies comparing the efficiencies of analysis cuts for data and simulation of observations of Vela Abdo et al. (2008) . The Vela studies cut off at 10 GeV, and measurements of the systematic errors above 10 GeV will be made when sufficient statistics are available from high-energy sources. Thus, the exposure systematic errors above 10 GeV that we quote for this study have not been fully validated. We believe that any reasonably projected uncertainty would not have a significant impact on the interpretation of the limits presented here.
In our search for lines we use a region of interest (ROI) that covers most of the sky: an all-sky ROI with the Galactic plane removed (i.e., |b|>10∘ as the Galactic plane is very bright in photons from gas interactions) plus a 20∘×20∘ square centered on the Galactic center (GC) and aligned on the (ℓ,b) grid of the Galactic coordinate system (Galactic coordinates in degrees are used in this paper). Though increasing the photon flux limits averaged over the reported energy range by less than 10%, including the GC gives significantly better theoretical line limits. For the highly point source rich region within 1∘ of the GC, no point source removal was done as this would have removed the GC. For the remaining part of the ROI, point sources obtained from the year-1 catalog under development by the LAT team Abdo et al. (2009d) were masked from the analysis using a circle of radius 0.2∘ centered on the measured point source position (conservative, considering the angular resolution above 20 GeV). This last cut removes about 0.4% of the solid angle and about 5% of the total photons.
In searching for deviations from a locally-determined background, we use a sliding energy window with the window size adjusted to reflect the energy resolution. This results in limits for 30<Eγ<200 GeV using data in the range 20<Eγ<300 GeV. The response of the LAT to a line feature in energy were determined from full detector simulations (GLEAM Atwood et al. (2009) ). Fig. 1 shows a binned representation of the fit and a close-up of the LAT line response function at 40 GeV. This fit also shows the largest line "signal" that was obtained in the reported energy region. We use an unbinned likelihood method, with the likelihood function L(¯E|f,Γ)=ntot∏i=0f⋅S(Ei)+(1−f)⋅B(Ei,Γ). Here, Ei denotes the measured energy of the ith photon. The parameters f and Γ are free and represent the signal fraction and the index of the power-law function,B(Ei,Γ), used to model the background. We require f≥0 in the fit. The function S(Ei) models the signal shape, i.e., the LAT response for a line feature in energy averaged over the acceptance of the LAT. The confidence intervals are determined using the profile likelihood method (MINOS within MINUIT) MIN , which provides two sided confidence intervals. The properties of this statistical method (coverage and power) have been thoroughly tested. At 100 GeV, for example, the coverage is close to nominal for a range of true signal fractions from 0 to 50%, and the power reaches 100% for signal fractions of about 10%. The method overcovers slightly due to the physical constraint on the signal fraction, f.
Figure 1: A binned representation of a typical fit (done unbinned), here centered at 40 GeV, used to extract the flux upper limits presented in the tables. The fitting process is described in the text. In the main part of the figure, the lower (upper) dotted line is the signal (background) from the fit and the red(or black) line is the total fit. This fit also shows the largest line "signal" that was obtained in the reported energy region. The inset shows a blow-up of the signal, which is the line energy response function, S(E), used in this fit, and is typical of line shapes for 20-300 GeV.
Eγ
95%CLUL
⟨σv⟩γγ [γZ] (10−27 cm3s−1)
τγγ [γZ] (1028 s)
(GeV)
(10−9 cm−2s−1)
NFW
Einasto
30 3.5 0.3 [2.6] 0.2 [1.9] 0.5 [4.5] 17.6 [4.2] 17.8 [4.2] 17.5 [4.2]
60 3.1 1.1 [4.2] 0.8 [3.0] 1.8 [7.3] 9.8 [3.5] 10.0 [3.5] 9.7 [3.5]
80 0.9 0.5 [1.7] 0.4 [1.2] 0.9 [2.9] 26.0 [10.4] 26.4 [10.5] 25.8 [10.3]
90 2.6 2.0 [6.0] 1.5 [4.3] 3.5 [10.3] 7.7 [3.2] 7.8 [3.2] 7.6 [3.1]
100 1.4 1.4 [3.8] 1.0 [2.8] 2.4 [6.6] 12.6 [5.4] 12.8 [5.4] 12.5 [5.3]
130 1.8 3.0 [7.3] 2.1 [5.3] 5.1 [12.6] 7.6 [3.4] 7.8 [3.5] 7.6 [3.4]
160 1.1 2.7 [6.3] 2.0 [4.5] 4.7 [10.9] 10.2 [4.8] 10.4 [4.8] 10.1 [4.7]
Table 1: Flux, annihilation cross-section upper limits, and decay lifetime lower limits: γ-ray energies measured and corresponding 95% c.l. upper limits (CLUL) on fluxes, for |b|>10∘ plus a 20∘×20∘ square around the Galactic center. For each energy and flux limit, ⟨σv⟩γγ and ⟨σv⟩γZ upper limits, and τγγ and τγZ lower limits are given for three Galactic dark matter distributions (see text). The systematic error in the absolute energy of the LAT discussed in the text propagates to a −20%+10% systematic error on ⟨σv⟩γγ, while for the decay lower limits the systematic error in the absolute energy of the LAT discussed in the text propagates to a +10%−5% systematic error on τγγ.
Results & Discussion: Table 1 shows flux limits as a function of photon energy that can be translated into bounds on the annihilation cross-section or decay lifetime assuming a specific halo dark matter density profile, ρ(→r). The monochromatic gamma-ray flux from dark matter annihilating into γX with a cross-section ⟨σv⟩ is Φ=Nγ8π⟨σv⟩m2χL, where Nγ=2 for X=γ and Nγ=1 otherwise. Here,
L=∫db∫dℓ∫dscosbρ2(→r), (1)
where the integral is over the ROI, r=(s2+R2⊙−2sR⊙cosℓcosb)1/2, and R⊙≃8.5 kpc is the distance from the sun to the GC Ghez et al. (2008) . For decays, the flux is given by substituting in the equation for Φ, ⟨σv⟩/2m2χ→1/τmχ, where τ is the DM lifetime, and ρ2→ρ in Eq. (1) for L.
We consider three theoretically-motivated halo profiles: the NFW profile, ρNFW(r)=ρs/[(r/rs)(1+r/rs)2] with rs=20 kpc Navarro et al. (1997) , the Einasto profile, ρEinasto(r)=ρsexp{−(2/α)[(r/rs)α−1]} with rs=20 kpc and α=0.17 Einasto (1965); Navarro et al. (2008) , and the very shallow isothermal profile ρisothermal(r)=ρs/(1+(r/rs)2) with rs=5 kpc Bahcall and Soneira (1980) . We determine ρs using ρ(R⊙)=0.4 GeV cm−3 Catena and Ullio (2009) . Taking the mass of the Milky-Way halo to be ∼1.2×1012M⊙ (see e.g. Wilkinson and Evans (1999); Xue et al. (2008) ), we determine maximum values for r of ∼150 kpc for the Einasto and NFW profiles, and ∼100 kpc for the isothermal profile.
Table 1 shows the cross-section and lifetime limits for the above profiles. We verified that there is only a minor dependence of the flux upper limits when changing the lower bound of |b| in the range 8∘<|b|<15∘, leaving the GC region fixed. The cross-section limits are sensitive to the halo profile. For the ROI used here, DM annihilation has a value of L (Eq. (1)) for the Einasto profile that is 40% larger than for the NFW profile, while for DM decays the L values are almost the same. This sensitivity is greater for cuspier profiles than those discussed here. For example the Moore density profile Moore et al. (1998) gives a factor of ∼6 stronger limits than the Einasto profile, using lower bounds on ℓ and b for the Moore profile integration that correspond to a distance of 10−3 pc from the Galactic center.
The limits on ⟨σv⟩γγ (⟨σv⟩γZ) shown in Table 1 are about one or more orders of magnitude weaker than the cross-sections expected for a typical thermal WIMP. However, there are several models in the literature that predict larger cross-sections and are constrained by these results. A WIMP produced non-thermally may have a much larger annihilation cross-section than a thermally produced WIMP and still produce the required DM relic density. An example is the "Wino LSP" model Kane et al. (2009) that explains the recent positron measurement by PAMELA Adriani et al. (2008) , and predicts ⟨σv⟩γZ≃1.4×10−26 cm3 s−1 at Eγ∼170 GeV. Our results disfavor this model by about a factor of ∼2−5, depending on the dark matter halo profile (see Table 1). Other models that are partially constrained include Mambrini (2009) , while models that are only constrained assuming a much cuspier profile include Bertone et al. (2009); Bringmann et al. (2008b) .
Dark matter decays into γX are ruled out for lifetimes below ∼1029s, a limit that is largely independent of the dark matter halo profile. This constrains, for example, a subset of the lifetime range of interest for gravitinos decaying into mono-energetic photons Ibarra and Tran (2008) .
Acknowledgements: We thank Louis Lyons for very useful discussions. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Études Spatiales in France.
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redpajama_set_name: RedPajamaCommonCrawl


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Here is a link to a video showing, once again, that it is the Federal government and its agents who are engaged in terrorist acts and violence, and that there is absolutely nothing that they can't get away with. As if we need any more evidence of that anyway. Where are the national media when it comes to showing the Feds burning these peoples' homes down and their livestock alive? Where are PETA? Meanwhile, the Feds are sending Oregon ranchers to prison for back burning (controlled burning) to save their houses and grazing fields, under anti-terrorism acts. This is what has spurred the occupation (people camping) of so called "federal" land in Oregon by Americans protesting the continuous unjust actions and use of force by the State. If only we had more of that. Much more of that! But alas our masses are too conditioned and manipulated to see their own proverbial noses in front of their face.
As the laughable charges against the Oregonian ranchers and the above video demonstrates, the real terrorists are, as always, in the federal government which operates with impunity whilst claiming absolute sovereignty and authority over everyone else. Their subjects. Who seemingly refuse to collectively wake up. What's more, incited by propaganda fueled, Leftist media outlets operating on behalf of the State, they viciously attack and calumniate those who do wake up and make a stand, as violent terrorists. But what individuals and groups that take a stand against oppressive governments aren't vilified and smeared by the State, State media and supportive individuals who have been collectively brainwashed?
The type of individuals who can't help but to bring up asinine racial double-standards here rather than focusing on actual government malice and abuse. For instance, they claim that if those peacefully occupying "government" land by camping there, were Black, that they would be called thugs and terrorists and even worse, dead. Of course this is a direct result of abating any attempt at critical thinking utilizing scientific principles such as properly observing, analyzing, comparing and contrasting beyond conditioned, knee-jerk, collective racial-judgement.
First off, in all of the recent racially charged riots Mainstream media has done its best to absolve the local Black communities and participants of responsibility while casting them as peaceful protestors, demonstrators and victims of social injustice who were being overshadowed by "outsiders" and "anarchist" whom the MSM ridiculously positioned as the sole parties responsible for the violence and mayhem.
Secondly, the reason that Black rioters, not legitimate Black protestors, are called thugs by many Americans of all stripes and some independent journalists when they riot; loot; burn peoples' businesses, homes and cities down while seeking retributive racial-justice whereby people are targeted, ambushed and violently attacked for the color of their skin; is because that is not just thuggery but insanity. It is insane to attack and murder people because of the color of their skin like in the LA Riots, for example, or the Atlanta Race Riots of 1906 where Whites were targeting Blacks, and like we saw with the racial violence that came with the recent rash of racial riots. Collectively blaming individuals based on group characteristics such as skin color and attacking them, is never sane because collective racial-judgement is just an illogical form of primitivism.
Furthermore, unlike the false predictions stemming from the anti-reality sentiments of indoctrinated Leftists, Black armed protestors march in the streets with no problems whatsoever when they do so peacefully. As this video demonstrates. Also, unarmed White protestors get shot. Just look at Kent State where the National Guard started mowing down White students, for a famous example. White strikers have met similar fate. United Mine Workers were massacred by the State for its overseers in the Ludlow massacre in Colorado. Anyone who stands in the way of industry, the State and the powerful men with control over its levers is dispensable, and quickly dispensed with. It isn't about race it is about the Powers That Be squashing dissent that threatens their power, whenever and wherever necessary, by any means necessary. As history can attest to, they won't hesitate to put any of us down when it serves their interests. They silently carry out genocides against all racial groups daily. It is just that most are not informed about them and are too busy working harder for less, and soaking up the latest bit of distractive B.S. to become informed about.
Now contrast racially charged riots predicated on racial rage fomented by the MSM, their manufactured narratives and the ruling elite in order to manipulate people into political action against their own interests; with actual peaceful protests consisting largely of White people who are being branded by a brainwashed public and mainstream outlets as Domestic Rightwing Terrorists. People who have committed zero violence and property damage. People who are thirty miles from the nearest town and who are a threat to absolutely no one but those who assail them first with force. Now for a question for those making claims of racial double-standards regarding these apples and oranges scenarios. What if the Feds were circling Black ranchers with fires burning down their homes and torching their livestock? How differently would those hate filled anti-White zealots feel about those ranchers' protests then? Would they be calling them terrorists? No way! And why? Because they have been indoctrinated with the dogmas of their social Marxist theology that calls for them to collectively judge the victim statuses and the grievances of individuals and groups, not based on merit, but rather on skin color and other superficial group characteristics, alone.
According to their "academic" indoctrination, government, media, and MTV Millennial shows, Whites are victimizing oppressors and non-Whites are oppressed victims. Without exceptions. All Whites are inherently "privileged" irrespective of their individual circumstances and experiences, and are thus not permitted any grievances no matter what, and anyone claiming otherwise should be laughed at and scorned. Conversely, all grievances of non-Whites are real and can never be denied because to do so would further victimize the minority groups. Reality doesn't matter here. Only race does. It is the thing upon which an individual's legal status, protections and entitlements are conferred. And this is what dictates whether or not an individual or a group are "terrorists" or "protestors". Not their actions. It matters not if one group peacefully assembles in the isolation of the woods posing no threat to anyone or anything. And it matters not if another group is looting and burning down cities while committing violent acts against people out of racial rage and animosity. All that matters is where you fall on the melanin-based oppression index. Aside from that we are not supposed to analyze, compare and contrast. Just accept the new dogmas as being self-evident truth and process and proceed accordingly.
Therefore, if these protestors with real grievances were Black, those dogmatically committed to collective racial-judgment would be charging the federal government with racism and terrorism against a protected minority group under the new social hierarchy, where Minority Privilege is the law of the land. Not dismissing their grievances based on race and calling for them to be massacred by the government after branding them as terrorists. And I have a feeling that mainstream media would be having a field day with the injustices as everyone was spun into a racial frenzy. There would be more Black riots across the country prompting President Obama and the DOJ to initiate federal civil rights investigations as they bent over backwards and called for national dialogue, meaning that Whites must admit guilt, repudiate their White "privilege" and accept responsibility for all that ails non-Whites. All as cities were burning and targeted Whites were suffering brutality due to the actions of the State and those who have been conditioned and manipulated to act against an "oppressive" racial group rather than the State which actually oppresses them.
These organized movements and riots, I mean "protests" sowing more racial tension and division, would be orchestrated by social justice groups funded with tens of millions of dollars by George Soros as racial chaos ensued, and the government would likely be caving in ways we will never see with these largely White protestors. And the ire and civil rights investigations would be warranted. Just not the blame that would be shifted from the State to White people, or the violence taken out on the innocent as a result.
Make no mistake, despite what Leftist media outlets would have you believe, these rural White ranchers and protestors are not "Thugs" and "Terrorists" like the urban terrorists that proliferate the inner-cities, burning them down and terrorizing the good, hardworking families in their own communities who are shot up in their own homes, and on their own streets and playgrounds every single day across the country at rates that far exceed all police shootings by many factors. That is real terrorism by the way. But more importantly, we must understand in no uncertain terms, that It is the federal government if – more likely when – they use force, that will be the terrorists. Murdering innocent, peaceful people whom they will have forced to defend themselves. This is true no matter what color they are. Just as it is true that people who burn down peoples' businesses and assault people who have nothing to do with their grievances are actually thugs, not protestors, no matter what color they are or how loud Leftists claim the contrary while crying racism when someone points out the obvious.
But racially dividing us is the point. Its a good trick you see. The country is intentionally kept divided between White and non-White, Left vs Right and everything else that can bring about desired division so that we are placed in boxes. Boxes from which we are constantly undermining each other's protests when we should be united in standing against the expansion of unchecked tyranny and the police state that is a growing threat to all of us. One that profiles us all and treats us all with suspicion and as subjects with no rights or privacy. Just revocable "privileges".
Native Americans should be standing there with these men against federal oppressors. I mean who knows of federal oppression like they do? So should Blacks whose communities have been left to rot in tombs while the federal government commits economic terrorism against them and the rest of us, as our jobs are taken, our wages and savings eroded through the manipulation of fiat currency and the labor and job supply that affects the economic balance of power as it is increasingly, with rapidity, shifted into the hands of the ruling elite. Further widening income disparities and eliminating economic opportunity for those at the bottom as they are pushed into greater government dependency. We are all collectively having our standard of living reduced as our wealth, resources and livelihood are stolen – in ways that, unfortunately, most do not realize or have the capacity to diagnose – by an occupational government ran by shadow overseers.
We have been being plundered increasingly each and every day over a period of generations, by a criminal, occupational government that has subverted our individual, state and national sovereignty. Eradicating our rights and subjugating us in our own land while people are too busy being misdirected by the contrived racial narratives, and other false narratives propagated through the media. Too busy with gladiatorial type entertainment (sports, reality tv etc.), which is a sure sign of a dying empire in which the people become numb and induced into a lethargic trance and slumber. We must wake up and rise together or fall together under the yoke of those working towards what they always have – the enslavement of humanity.
No political party is looking out for us. We are all chattel of the State living under martial rule and the expansion of Emergency and War powers enshrined in hundreds of federal codes. Most are just to under-informed, misdirected and conditioned over a protracted period spanning from birth to ever realize it. Both political parties represent the corporate government duopoly. Your government is Monsanto, Syngenta, Dow chemical, the banking cartels, Exon Mobile, Bayer, Pfizer, Merck and the rest of the transnational corporate bodies and foundations run and controlled by the ruling elite who pay for your politician's campaigns. Who blackmail and extort them with every nasty thing they can use against them that has been collected under the NSA spying apparatus, should they dare to betray their benefactors for their constituents or a growing conscious. This was exposed by the Church Committee in the 70s, and in many times and in many ways since. And it has only gotten worse with the advancement of technology.
The FTAs like the TPP, TPIP and NAFTA etc., which are pushed through with bipartisan support knowing full well the devastation such treasonous acts will have against the American people, are not for the benefit of Americans but for their rulers. As is everything else they push together behind the grand theater that plays out in the media, providing cover and the illusion of choice. When they poison us and our children through the oligarchical food system, our water supplies, our land, our air and through forced medical interventions where we are forced to comply or lose our children or face jail time – that is not to benefit us. Nor is it for the claimed "greater good", or the children that they use as props and shields. It is all a part of a strategy that benefits them. Our rulers who were once obfuscated by the shadows of secrecy but now sit in plain sight, yet unobserved by the masses.
We are being lied to and propagandized daily. Used and manipulated daily. Severely abused daily. Laughed at daily. As all is being taken from under our feet clear as day, by our users and abusers. A few powerful people who sit atop the hierarchy. We have no choice in political matters where it matters. Not in Food. Education. Medium of exchange. Medicine. National borders. Our privacy. Or the expanding global; social, economic and political system under which we are being reduced to our lowest common denominator as working units of labor. Just like honey bees being smoked into complacency and docility while their masters steal the fruits of their labor.
We are being tricked! Bamboozled! And all while grinning with self-righteous superiority and anger directed at the wrong people and places, due to the ease with which they are able to control us with simple triggers as we are inundated with their propaganda. Manipulated into political action to serve their interests. Including attacking those that stand against them. You would think Divide and Rule was too old too be effective yet here we are being divided, herded and lorded over by those that are using the age old, but highly effective strategy. We must eventually wake up once and for all or else we are doomed to a world in which the only progress is to be made by those that mean humanity the most harm. We only have ourselves to blame, for the darkest acts of inhumanity enacted by our rulers could not be made without our unwavering collective-submission to their authority. All they do they do because we allow them to do it. A heavy cross to bear.


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Anthemius Engineers was founded in 2016 by a team of Civil and Structural Engineers with over 25 years of experience in the field of buildings and infrastructure. Our team's extent experience in both engineering and construction industries, our deep knowledge of the behaviour of all structural materials (from prestressed concrete to glass) and the academic credentials of all our engineers, guarantee the quality of our work. We stay committed to liaising with clients, contractors and other engineering disciplines in pursue of a safe, cost efficient and constructable solution.
• Prestressed Concrete and Composite Bridges
• Reinforced Concrete and Steel Buildings
• Monumental Masonry Structures
• Aluminium and Glass Façade
• Scheduling
• Site Supervision
• Quantity Surveying
• Cutting-Edge FEA Software
• Up to date with Ιnternational Codes
and Regulations (EN, DIN-FB, ASCE)
• Publications in scientific journals
Here's a gallery of some selected projects from partners' portfolio.
Stavros Niarchos Foundation Cultural Center in Athens, Greece
Highway Α2 (E90), Bridge at Agios Nikolaos, Ioannina, Greece
Highway Α29, Overpass at Kastoria, Greece
Highway A2 (E90), Bridge at Eirini River, Evros, Greece
A.U.Th. Research Dissemination Center in Thessaloniki, Greece
Highway Α29, Overpass at Maniaki, Kastoria, Greece
Highway A24, Overpass at Agios Dimitrios, Kassandria, Greece
Royal Theatre in Thessaloniki, Greece
Sakis Kompselidis
Fotios Kandylas
Dr. Thomas Salonikios
Dr. Olympia Taskari
George Palaskas
Despina Sachinidou
Kostas Tsolis
Sakis Kompselidis obtained his Civil Engineering Diploma from Aristotle University of Thessaloniki. His thesis focused on steel structures. Sakis has over 25 years of experience in the field of structural engineering. His portfolio covers a broad range of industrial building design and construction supervision. He has also designed numerous prestressed concrete and composite bridges. Sakis is consulting engineer in special issues on steel and composite structures.
Fotios Kandylas obtained his Civil Engineering Diploma from Aristotle University of Thessaloniki. His thesis focused on nonlinear analysis of reinforced concrete structures. Fotios is the head of bridge engineering in our team, having over 20 years of experience in the design of prestressed concrete structures. During his career as an engineer, he has designed over 150 prestressed concrete bridges. He has also worked as a consulting engineer in special reinforced concrete and prestressed concrete structures.
Thomas Salonikios obtained his Civil Engineering Diploma and Ph.D. in experimental methods in earthquake engineering from Aristotle University of Thessaloniki. His Ph.D. thesis focused on reinforced concrete walls under cyclic loading. Thomas is the head of building design department in our team. The last 25 years he has designed numerous reinforced concrete buildings, special structures and steel and masonry structures. He is familiar with experimental testing of structural elements, in situ examination of existing structures and measurement of their eigenproperties by the use of local accelerometer networks. He is also reviewer in several international scientific journals.
Olympia Taskari obtained her Civil Engineering Diploma, MSc in Earthquake Engineering and Ph.D. in computational bridge engineering from Aristotle University of Thessaloniki. Her Ph.D. thesis focused on seismic assessment of prestressed concrete bridges. She joined the Mid-America Earthquake Center group (MAE) in University of Illinois at Urbana-Champaign for one year as a visiting research scholar. During her staying in US, she studied hybrid simulation techniques in bridges using sophisticated FEA software. Later, as a postdoctoral researcher in the National Technical University of Athens, she investigated the seismic response of bridges on liquefiable soil profiles. She is also reviewer in several international scientific journals. Olympia's strong theoretical background adds a lot to our bridge engineering department.
George Palaskas obtained his Civil Engineering Diploma and MSc in Earthquake Engineering from Aristotle University of Thessaloniki. His MSc thesis focused on nonlinear analysis of reinforced concrete bridge piers on deformable soil profiles. As a structural engineer, he has designed structures of all known materials (from reinforced concrete to glass and aluminium) located both in Europe and overseas. In the construction industry, his experience ranges from construction management to technical office management. George is the connection between engineering and construction.
Despina Sachinidou obtained her Civil Engineering Diploma in structural engineering and MSc in environmental engineering from Aristotle University of Thessaloniki. Her thesis focused on the reinforced concrete structures design. Despina is familiar with sophisticated FEA and CAD software and is our team specialist in bridge detailing design. By undertaking a great number of demanding projects over the last decade, Despina has all the hands-on experience needed to ensure our team commitment to excellence.
Kostas Tsolis obtained his Civil Engineering Diploma from National Technical University of Athens. His thesis focused on highway infrastructure. He has more than 25 years of experience in the design of reinforced concrete buildings and complex structures. Kostas has been involved in site supervision of numerous projects and he is consulting engineer in special issues on reinforced concrete structures.
Feel free to contact us for any information you need.
2B Eantos street, 551 33
T: +30 2310 41 41 33
F: +30 2310 44 48 44
anthemius@anthemius.gr
© Anthemius Engineers 2017. All Rights Reserved.


Designed to work with the popular and free FMS flight simulator, this new software interface cable plugs into any Hitec, JR or DIN plug Futaba transmitter with a trainer cord plug. Featuring a USB plug for easy installation into your PC, it is also compatible with most joystick operating flying simulator. Requires transmitter with 1/8" mini plug or DIN trainer cord socket and a PC with a free USB port. Compatible with Windows 98, ME, 2000, and XP.
The freeware FMS flight simulator has become very popular because it is free, and because many manufacturers are directly supporting it with their transmitters. Many modelers are making their own model files for use with FMS so there is a wide variety of models available for free on the internet.
FMS Home Page - the latest software and information is available from this site.


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idw |
Kill Shakespeare Volume 1
by Rob McMonigal July 02, 2011
Written by Conor McCreery and Anthony Del Col
Illustrated by Andy Belanger
Almost from the early days of recorded literature, it's been cool to write about the same characters others used before you. The Greek tragedians took Homer's historical creations and made them into epic dramas. Chaucer took some of the same characters and re-used them. Then Shakespeare turned around and did it to Chaucer, amongst many, many others.
We see this today, with everyone from Sherlock Holmes to Doyle himself getting either re-imagined to fight zombies or used as a focal character to tell stories not unlike those written by a famous author themselves.
When done badly, it's hackery at its worst, because using someone else's toys to tell a crappy story is even worse than creating your own characters and telling a crappy story. When done well, however, it's a thing of beauty that the original writer would most likely appreciate, were he or she around to see it.
That's definitely the case for Kill Shakespeare, a story that weaves various elements of the bard's plays into a shared universe where treachery abounds and even comedic figures and romantic leads are pressed into a desperate fight to keep the worst of Shakespeare's characters from taking over the world. It's an amazingly simple concept--what if Shakespeare's characters all lived at the same time and were vaguely aware of their creator?--that plays out so very well in the hands of McCreery, Del Col, and Belanger.
Kill Shakespeare is the story of Hamlet, who instead of staying in Denmark opts to leave for England after all. He's shipwrecked and lands into the clutches of Richard III (the design for Richard is awesome, by the way), who promises that he can do the unthinkable--bring King Hamlet back from the grave. The offer, however, is a life for a life--kill Shakespeare, and Hamlet lives again.
We know Richard won't do anything of the kind, especially since he's allied with MacBeth and Iago, but in true Shakespearean fashion, Hamlet is manipulated into doing Richard's bidding, though he is far from the only one. Before we know it, Hamlet meets characters from other tragedies, who have a very different story to tell. But can one believe the words of the braggart Falstaff? Buffeted by dreams and wild accusations on every side, Hamlet seems to be out of the oven and into the frying pan. What will he do?
As the book closes on this first act, it's really hard to know, and that's part of what makes it so good. There are multiple levels of scheming going on, and just about every character has a personal agenda that doesn't quite mesh with those of their allies. I really love the way Kill Shakespeare brings home the idea that the protagonists in the bard's plays, no matter what the classification, are clearly flawed people. Hamlet may want to do the right thing, but he's a killer with severe mental issues, who can't really figure out what the right thing is. Are Juliet and Othello really after justice, or are their quests suicidal? Is Richard III really as bad as he appears to be, or is he trying to make his Kingdom a better place? (Okay, so maybe that last one isn't so hard to figure out!)
There are a lot of intricacies to the story that I'd be spoiling if I talked too much about them. Suffice it to say that each character is true to their Shakespearean original, right down to how they act with other characters. The setting may have changed, but the quest for power or revenge or pleasure, three key elements to Shakespeare's plays, are still very much in force. The fact that McCreery and Del Col can keep the story feeling original while echoing arguably the greatest writer (or team of writers) who ever lived is a testament to their writing powers.
If you ever read Shakespeare, you know his plays were generally quite dark and full of death. Kill Shakespeare definitely follows this pattern, with a heavy body count that includes ripping out body parts, decimating villages, and even a nice nod to Edgar Allan Poe. There are plenty of creepy elements, all drawn perfectly by Andy Bellenger, who manages to evoke Mike Mignola without trying to copy him. His backgrounds are extremely detailed, and I love when he is drawing Hamlet's fever-dreams or the scenes with witchcraft. Bellanger also uses heavy facial inks to good effect, which are offset by the eye-popping color choices of Ian Herring.
I rarely comment on a book's coloring, but Herring makes Bellanger's art sing. Unlike other colorists who might have muddied the book with browns, grays, an other colors that are supposed to invoke menace and add weight to the proceedings, Herring is not afraid to be almost garish in his choices, and I love the results. Blood is bright red! Good! Who cares if that's not realistic, it looks awesome! Just about all of the color choices are vivid, and I wish more creators would try that. This is colored more like a webcomic than a comic book, and I mean that as a compliment.
Kill Shakespeare is one of the best books I've read where a new author is playing with someone else's toys. This is on a par with Moore's first League book, which I think set the standard for these kinds of adaptations. I can't wait to read the second half of the series when it comes out in book form in October. Don't delay on reading this one, however: It gets my strongest possible recommendation and is definitely one of my favorite books I've read so far in 2011.


One of our more challenging projects and one that we are quite proud of. The lower landscape is comprised of a series of radiuses formed from Corten Steel intersecting a number of large stones while the overall garden mixes specimen plant material, water features, sculptural elements and unique material choices.
Part of a larger project this feature seamlessly fuses together both water and fire.
AguaFina is pleased to announce the introduction of our 2010 product catalog, now available for both immediate viewing and downloading at http://www.aguafina.com/Store.asp The catalog features many of the distinctive garden decor pieces in our collection including AguaFina's signature fountains, Japanese lanterns, basins, sculptural elements and one of a kind pieces.


Containing dangerous, toxic spills in a Portable Spill Mat is much more desirable than trying to clean spilled liquids up off the ground.
You have the benefit of catching the spilled liquid in the sump, and can easily recover the spilled liquid again for re-use. Portable Spill Mats are so versatile and easy to use. They are uniquely designed to fold up to a compact size for easy storage in tight of difficult locations. Manufactured from UV Stable PVC or XR5 Evaloy Heavy Grade hydrocarbon secondary containment material.


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Home/MLB Draft/Diamond Digest's Final Mock Draft
Diamond Digest's Final Mock Draft
Tyler Jennings June 3, 2019
Bobby Witt Jr. (Photo courtesy of Baseball Factory/Under Armour All American Games)
It is officially draft day!
As we get ready to watch how the draft unfolds tonight, we figured it would be nice to give it one last go with a mock draft before the draft begins. There is considerable change in this one, as we have expanded our mock to include 41 picks and some players with considerable "helium" have jumped into the rankings. With that being said, here are some notes to take in before we reveal our final mock draft:
The Baltimore Orioles have mentioned the possibility of not taking Adley Rutschman at first overall, but many believe it is just noise. Teams haven't been very vocal about who they are taking in recent years, but this is just a rumor. There's still a very good chance that Adley goes to Baltimore.
There has been some rumblings about C.J. Abrams sliding past the sixth overall pick. Much like Adley, we doubt that this will occur, but there's always a possibility this happens.
You may notice that the back end of this mock will be significantly different than the previous two. That's mainly because of guys whose stock has risen considerably in recent weeks.
Lastly, let's talk about Jack Leiter. The NJ prep star has a very, very strong commitment to Vanderbilt. Any team that takes him after the first round will have to give him an overslot deal, meaning they will give underslot deals to others. It'll be interesting how this plays into the draft tonight.
Without further ado, here is our final MLB Draft mock! Me and Mick will also be live streaming on YouTube with coverage of the draft, be sure to watch and feel free to ask questions!
Tyler Jennings
Hi, I'm Tyler, one of the many writers here at Diamond Digest. A Red Sox fan at heart, I live in Raleigh, NC and currently work full-time, although I plan on a return to college in 2019. I have previously been featured on MLB Daily Dish, Hardball Scoop, and Baseball Essential. I am pursuing a career in Sports Journalism, as well as an internship at Baseball America. Outside of that, I ran Cross Country in High School and College and live with a stutter. I plan to bring unbiased baseball coverage to DD, with a primary focus on the MLB Draft, as well as general MLB news.
Scouting Report: Garrett Crochet
Padres Day Two Draft Review
Athletics Day Two Draft Review
About Tyler Jennings


It's that time of year again – Halloween season! I love Autumn for a number of reasons; the changing colour of the leaves, the excuse to finally wear boots and jumpers, and the baking. Summer's great while it lasts, but you can always rely UK to pull off a good Autumn, not just with the weather but with the baking options too. I'm such a huge fan of themed baking and Halloween has become one of my favourite of them all – I mean when else are bugs, brains and blood stained baked goods appropriate to serve?
So with that I wanted to share with you all some little Halloween creatures I've been baking this weekend. As an Arachnophobic I must say these were a little creepy to bake but my goodness they are delicious.
I'm not going to claim these cuties as my own as I found them on pinterest and followed the link to the Mommysmusings.com but I have made a few adjustments. I have developed a milk allergy so these are milk free, and the recipe below will be in UK Conversions as opposed to U.S. which some of you followers may find useful.
I hope to be able to share some more Halloween recipes soon so do keep your eyes open for more.
Place the soy butter, peanut butter, caster sugar, brown sugar, egg, vanilla and soy milk into a large bowl and beat until well combined.
In another bowl mix together the flour, baking powder and salt, then gradually fold the dry mixture to the wet mixture until blended into a dough.
Pour caster sugar out onto a plate and leave to one side. Form the mixture into 1″ balls and roll them around in the sugar before placing a couple of inches apart, onto a lined baking sheet.
Bake for 10-12 minutes until golden then place on a wire rack and immediately gently press a Reese's buttercup on top of each biscuit.
The heat from the biscuits will gently melt the chocolate on the buttercup allowing you to then stick down two eyes onto it.
Place the chocolate chips into a small microwavable bowl and blast in the microwave for 30 seconds at a time until fully melted then transfer the chocolate to a small piping bag.
Cut the end of the piping bag and pipe the legs either side of the Reeses buttercup (you'll need 8 legs unlike my photo where there are only 6 – eyerolling emoji) Lets say mine are a new breed of 6 legged spider.
Previous Post The Unicorn Cookbook is coming!


I cant thank Complete Cricket enough for all they have done for me. Not only making my journey to England as smooth as possible and looking after me once I arrived. They have gone over and above for me and I cannot recommend them enough.


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Communications Security Establishment with University of New Brunswick Uses AWS to Drive Innovative Cybersecurity Research
The Communications Security Establishment (CSE) is one of the Government of Canada's key security and intelligence organizations. As part of its mandate to protect the government's electronic information and communications networks, CSE explores new and innovative solutions to combat new cyberattack methods by researching cybersecurity data.
Using AWS, we scaled to hundreds of virtual servers at the click of a button, and we could do a year's worth of compute in one day. We could not have done that without the AWS Cloud."
Dr. Arash Habibi Lashkari
Assistant Professor, Canadian Institute for Cybersecurity at the University of New Brunswick
When CSE recently embarked on a new research initiative to find updated test data, it saw serious limitations in current datasets. "We found there wasn't a lot of great data out there," says Mike Davie, a cybersecurity engineer at CSE. "Much of it was sensitive and not suitable for public research, and it was outdated, so it didn't take into account modern attack methods."
To address these issues, CSE reached out to the Canadian Institute for Cybersecurity at the University of New Brunswick (UNB), which had recently conducted promising cybersecurity research around modern attack methods, including brute force, botnet, and denial of service. Both CSE and UNB, though, lacked the compute capacity to simulate cyberattacks on a large scale. "We needed hundreds of virtual machines and computers to simulate a medium-sized enterprise being attacked, but neither organization had that capacity internally," Davie says. "We also wanted to do this research cost-effectively, which meant avoiding the procurement of a bunch of servers for a two-week project."
Creating Realistic Datasets on AWS
To overcome its scalability and cost roadblocks, CSE chose to create a research simulation project on the Amazon Web Services (AWS) Cloud. "We explored different technologies, but we liked AWS the best because of the scalability and on-demand cost benefits it provided," says Davie. "The infrastructure-as-a-service model was a perfect fit for how we wanted to do our research."
To get the project up and running quickly, CSE and UNB received $80,000 in project funding from the AWS Cloud Credits for Research Program, a program that has helped global researchers expedite their research with the power of the cloud. "That was a major help in starting the research, because both CSE and UNB have research budgetary constraints," says Davie. Once the project started, the CSE and UNB used more than 100 virtual servers running on Amazon Elastic Compute Cloud (Amazon EC2) instances to support a test network simulating a company with five departments and 500 employees using PCs. Researchers from CSE and UNB developed 13 attack scenarios and executed them for 10 days, capturing network traffic and machine logs and, ultimately, generating a new cybersecurity dataset. The research results were made available through an open data portal hosted on AWS. "Being able to host our open data portal on AWS was important because we want the data to be available for other researchers to use," says Davie.
Scaling to Simulate Cyberattacks on 500 PCs
By hosting the cybersecurity test and datasets on AWS, CSE and UNB were able to quickly deploy hundreds of servers. "When I conducted research several years ago, I only had 25 servers," says Dr. Arash Habibi Lashkari, assistant professor at UNB. "Using AWS, we scaled to hundreds of virtual servers at the click of a button, and we could do a year's worth of compute in one day. We could not have done that without the AWS Cloud."
Using AWS to support the datasets, CSE was able to predict and control its costs. "We didn't have to buy a bunch of hardware for a 10-day project and then continue to pay for it when the project was finished," says Davie. "AWS gives us a predictable cost model, so we knew upfront exactly how much it would cost."
Advancing the Cybersecurity Fight
By completing its research on AWS, CSE and UNB met the government's requirement of providing realistic datasets to support the development and testing of new and advanced cybersecurity solutions. "With the research we conducted on AWS, we were able to detect specific attacks such as DDoS, infiltration, and web attacks faster and more accurately than before," Lashkari says. "We were able to extract approximately 80 network traffic features, some in a matter of seconds. We couldn't have accomplished this without doing it on the AWS Cloud."
As a result of the project, CSE and UNB have made new cybersecurity data publicly available for other researchers to support additional research in the field. "More than 800 universities and cybersecurity researchers around the world have already cited our datasets in their research," says Lashkari. CSE can now better support its mission of sharing new research with cybersecurity technology companies. "This supports our goal of using better technology to advance research in the field," says Davie. "By providing better research data, we can help fight cyberattacks across Canada and throughout the world and help networks be more secure."
About Communications Security Establishment
The Communications Security Establishment (CSE) is the Government of Canada's national cryptologic agency. It is responsible for foreign signals intelligence and protecting the government's electronic information and communication networks.
Quickly scales to simulate 13 cyberattacks on 500 PCs
Reduces operational costs
Advances cybersecurity research around the globe
Secure and resizable compute capacity in the cloud. Launch applications when needed without upfront commitments.


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Commission Aims to Create Roadmap for US Role in Global Health Security
Home » News » Emerging Infectious Disease » Commission Aims to Create Roadmap for US Role in Global Health Security
Emerging Infectious Disease, Legislation, News
A commission including global health and national security leaders, and members of Congress has released a set of recommendations it believes can serve as a blueprint for improved U.S. action on global health security.
"We began the Commission's work with a simple, powerful proposition: health security is national security, in a world that is increasingly dangerous and interdependent," Dr. Julie L. Gerberding, the co-chair of the Center for Strategic and International Studies Commission on Strengthening America's Health Security, said in her written testimony for a Senate Committee on Armed Services Subcommittee hearing Wednesday.
"We need to adjust our thinking to account for this fundamental new reality. We need new approaches to operate effectively, on-the-ground, in difficult, insecure places," she said in the testimony. "The Commission also arrived at a stark, companion conclusion: U.S. health security policy is caught in a cycle of crisis and complacency, which leaves Americans very vulnerable."
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