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Cosmic Origins Newsletter, September 2016, Vol. 5, No. 2
National Aeronautics and Space Administration Cosmic Origins Newsletter September 2016 Volume 5 Number 2 Summer 2016 Cosmic Origins Program Inside this Issue Update Summer 2016 Cosmic Origins Program Update ............................1 Mansoor Ahmed, COR Program Manager Hubble Reveals Stellar Fireworks in ‘Skyrocket’ Galaxy ................2 Message from the Astrophysics Division Director .........................2 Susan Neff, COR Program Chief Scientist Light Echoes Give Clues to Protoplanetary Disk ............................3 Far-IR Surveyor Study Status .............................................................5 Welcome to the September 2016 Cosmic Origins (COR) newslet- LUVOIR Study Status .........................................................................5 ter. In this issue, we provide updates on several activities relevant to Strategic Astrophysics Technology (SAT) Selections the COR Program objectives. Some of these activities are not under for ROSES-2015 ...................................................................................6 the direct purview of the program, but are relevant to COR goals, Technology Solicitations to Enable Astrophysics Discoveries ......6 therefore we try to keep you informed about their progress. Cosmic Origins Suborbital Program: Balloon Program – BETTII ................................................................7 In January 2016, Paul Hertz (Director, NASA Astrophysics) News from SOFIA ...............................................................................8 presented his -
Searches for Dark Matter Self-Annihilation Signals from Dwarf Spheroidal Galaxies and the Fornax Galaxy Cluster with Imaging Air Cherenkov Telescopes
Searches for dark matter self-annihilation signals from dwarf spheroidal galaxies and the Fornax galaxy cluster with imaging air Cherenkov telescopes Dissertation zur Erlangung des Doktorgrades des Fachbereichs Physik der Universität Hamburg vorgelegt von Björn Helmut Bastian Opitz aus Warburg Hamburg 2014 Gutachter der Dissertation: Prof. Dr. Dieter Horns JProf. Dr. Christian Sander Gutachter der Disputation: Prof. Dr. Dieter Horns Prof. Dr. Jan Conrad Datum der Disputation: 17. Juni 2014 Vorsitzender des Prüfungsausschusses: Dr. Georg Steinbrück Vorsitzende des Promotionsausschusses: Prof. Dr. Daniela Pfannkuche Leiter des Fachbereichs Physik: Prof. Dr. Peter Hauschildt Dekan der MIN-Fakultät: Prof. Dr. Heinrich Graener Abstract Many astronomical observations indicate that dark matter pervades the universe and dominates the formation and dynamics of cosmic structures. Weakly inter- acting massive particles (WIMPs) with masses in the GeV to TeV range form a popular class of dark matter candidates. WIMP self-annihilation may lead to the production of γ-rays in the very high energy regime above 100 GeV, which is observable with imaging air Cherenkov telescopes (IACTs). For this thesis, observations of dwarf spheroidal galaxies (dSph) and the For- nax galaxy cluster with the Cherenkov telescope systems H.E.S.S., MAGIC and VERITAS were used to search for γ-ray signals of dark matter annihilations. The work consists of two parts: First, a likelihood-based statistical technique was intro- duced to combine published results of dSph observations with the different IACTs. The technique also accounts for uncertainties on the “J factors”, which quantify the dark matter content of the dwarf galaxies. Secondly, H.E.S.S. -
Highlights and Discoveries from the Chandra X-Ray Observatory1
Highlights and Discoveries from the Chandra X-ray Observatory1 H Tananbaum1, M C Weisskopf2, W Tucker1, B Wilkes1 and P Edmonds1 1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138. 2 NASA/Marshall Space Flight Center, ZP12, 320 Sparkman Drive, Huntsville, AL 35805. Abstract. Within 40 years of the detection of the first extrasolar X-ray source in 1962, NASA’s Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond X-ray images with 100-200 eV energy resolution for energies in the range 0.08<E<10 keV, locating X-ray sources to high precision, detecting extremely faint sources, and obtaining high resolution spectra of selected cosmic phenomena. The extended Chandra mission provides a long observing baseline with stable and well-calibrated instruments, enabling temporal studies over time-scales from milliseconds to years. In this report we present a selection of highlights that illustrate how observations using Chandra, sometimes alone, but often in conjunction with other telescopes, have deepened, and in some instances revolutionized, our understanding of topics as diverse as protoplanetary nebulae; massive stars; supernova explosions; pulsar wind nebulae; the superfluid interior of neutron stars; accretion flows around black holes; the growth of supermassive black holes and their role in the regulation of star formation and growth of galaxies; impacts of collisions, mergers, and feedback on growth and evolution of groups and clusters of galaxies; and properties of dark matter and dark energy. -
Stats2010 E Final.Pdf
Imprint Publisher: Max-Planck-Institut für extraterrestrische Physik Editors and Layout: W. Collmar und J. Zanker-Smith Personnel 1 PERSONNEL 2010 Directors Min. Dir. J. Meyer, Section Head, Federal Ministry of Prof. Dr. R. Bender, Optical and Interpretative Astronomy, Economics and Technology also Professorship for Astronomy/Astrophysics at the Prof. Dr. E. Rohkamm, Thyssen Krupp AG, Düsseldorf Ludwig-Maximilians-University Munich Prof. Dr. R. Genzel, Infrared- and Submillimeter- Scientifi c Advisory Board Astronomy, also Prof. of Physics, University of California, Prof. Dr. R. Davies, Oxford University (UK) Berkeley (USA) (Managing Director) Prof. Dr. R. Ellis, CALTECH (USA) Prof. Dr. Kirpal Nandra, High-Energy Astrophysics Dr. N. Gehrels, NASA/GSFC (USA) Prof. Dr. G. Morfi ll, Theory, Non-linear Dynamics, Complex Prof. Dr. F. Harrison, CALTECH (USA) Plasmas Prof. Dr. O. Havnes, University of Tromsø (Norway) Prof. Dr. G. Haerendel (emeritus) Prof. Dr. P. Léna, Université Paris VII (France) Prof. Dr. R. Lüst (emeritus) Prof. Dr. R. McCray, University of Colorado (USA), Prof. Dr. K. Pinkau (emeritus) Chair of Board Prof. Dr. J. Trümper (emeritus) Prof. Dr. M. Salvati, Osservatorio Astrofi sico di Arcetri (Italy) Junior Research Groups and Minerva Fellows Dr. N.M. Förster Schreiber Humboldt Awardee Dr. S. Khochfar Prof. Dr. P. Henry, University of Hawaii (USA) Prof. Dr. H. Netzer, Tel Aviv University (Israel) MPG Fellow Prof. Dr. V. Tsytovich, Russian Academy of Sciences, Prof. Dr. A. Burkert (LMU) Moscow (Russia) Manager’s Assistant Prof. S. Veilleux, University of Maryland (USA) Dr. H. Scheingraber A. v. Humboldt Fellows Scientifi c Secretary Prof. Dr. D. Jaffe, University of Texas (USA) Dr. -
The Evolving Launch Vehicle Market Supply and the Effect on Future NASA Missions
Presented at the 2007 ISPA/SCEA Joint Annual International Conference and Workshop - www.iceaaonline.com The Evolving Launch Vehicle Market Supply and the Effect on Future NASA Missions Presented at the 2007 ISPA/SCEA Joint International Conference & Workshop June 12-15, New Orleans, LA Bob Bitten, Debra Emmons, Claude Freaner 1 Presented at the 2007 ISPA/SCEA Joint Annual International Conference and Workshop - www.iceaaonline.com Abstract • The upcoming retirement of the Delta II family of launch vehicles leaves a performance gap between small expendable launch vehicles, such as the Pegasus and Taurus, and large vehicles, such as the Delta IV and Atlas V families • This performance gap may lead to a variety of progressions including – large satellites that utilize the full capability of the larger launch vehicles, – medium size satellites that would require dual manifesting on the larger vehicles or – smaller satellites missions that would require a large number of smaller launch vehicles • This paper offers some comparative costs of co-manifesting single- instrument missions on a Delta IV/Atlas V, versus placing several instruments on a larger bus and using a Delta IV/Atlas V, as well as considering smaller, single instrument missions launched on a Minotaur or Taurus • This paper presents the results of a parametric study investigating the cost- effectiveness of different alternatives and their effect on future NASA missions that fall into the Small Explorer (SMEX), Medium Explorer (MIDEX), Earth System Science Pathfinder (ESSP), Discovery, -
Spherex: New NASA MIDEX All-Sky 1-5 Um Spectral Survey
SPHEREx: New NASA MIDEX All-Sky 1-5 um Spectral Survey Designed to Explore ▪ The Origin of the Universe ▪ The Origin and History of Galaxies ▪ The Origin of Water in Planetary Systems ▪ PI Jamie Bock, CalTech The First All-Sky Near-IR Spectral Survey A Rich Legacy Archive for the Astronomy Community with 100s of Millions of Stars and Galaxies Low-Risk Implementation ▪ 2022 NASA MIDEX Launch ▪ Single Observing Mode ▪ Large Design Margins Co-I Carey Lisse, SES/SRE ▪ No Moving Optics NASA SBAG Jun 25, 2019 Copyright 2017 California Institute of Technology. U.S. Government sponsorship acknowledged. New MIDEX SPHEREx (2022-2025): All-Sky 0.8 – 5.0 µm Spectral Legacy Archives Medium- High- Accuracy Accuracy Detected Spectra Spectra Clusters > 1 billion > 100 million 10 million 25,000 All-Sky surveys demonstrate high Galaxies scientiFic returns with a lasting Main data legacy used across astronomy Sequence Brown Spectra Dust-forming Dwarfs Cataclysms For example: > 100 million 10,000 > 400 > 1,000 COBE J IRAS J Stars GALEX Asteroid WMAP & Comet Galactic Quasars Quasars z >7 Spectra Line Maps Planck > 1.5 million 1 – 300? > 100,000 PAH, HI, H2 WISE J Other More than 400,000 total citations! SPHEREx Data Products & Tools: A spectrum (0.8 to 5 micron) for every 6″ pixel on the sky Planned Data Releases Survey Data Date (Launch +) Associated Products Survey 1 1 – 8 mo S1 spectral images Survey 2 8 – 14 mo S1/2 spectral images Early release catalog Survey 3 14 – 20 mo S1/2/3 spectral images Survey 4 20 – 26 mo S1/2/3/4 spectral images Final Release -
Meeting Program
A A S MEETING PROGRAM 211TH MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY WITH THE HIGH ENERGY ASTROPHYSICS DIVISION (HEAD) AND THE HISTORICAL ASTRONOMY DIVISION (HAD) 7-11 JANUARY 2008 AUSTIN, TX All scientific session will be held at the: Austin Convention Center COUNCIL .......................... 2 500 East Cesar Chavez St. Austin, TX 78701 EXHIBITS ........................... 4 FURTHER IN GRATITUDE INFORMATION ............... 6 AAS Paper Sorters SCHEDULE ....................... 7 Rachel Akeson, David Bartlett, Elizabeth Barton, SUNDAY ........................17 Joan Centrella, Jun Cui, Susana Deustua, Tapasi Ghosh, Jennifer Grier, Joe Hahn, Hugh Harris, MONDAY .......................21 Chryssa Kouveliotou, John Martin, Kevin Marvel, Kristen Menou, Brian Patten, Robert Quimby, Chris Springob, Joe Tenn, Dirk Terrell, Dave TUESDAY .......................25 Thompson, Liese van Zee, and Amy Winebarger WEDNESDAY ................77 We would like to thank the THURSDAY ................. 143 following sponsors: FRIDAY ......................... 203 Elsevier Northrop Grumman SATURDAY .................. 241 Lockheed Martin The TABASGO Foundation AUTHOR INDEX ........ 242 AAS COUNCIL J. Craig Wheeler Univ. of Texas President (6/2006-6/2008) John P. Huchra Harvard-Smithsonian, President-Elect CfA (6/2007-6/2008) Paul Vanden Bout NRAO Vice-President (6/2005-6/2008) Robert W. O’Connell Univ. of Virginia Vice-President (6/2006-6/2009) Lee W. Hartman Univ. of Michigan Vice-President (6/2007-6/2010) John Graham CIW Secretary (6/2004-6/2010) OFFICERS Hervey (Peter) STScI Treasurer Stockman (6/2005-6/2008) Timothy F. Slater Univ. of Arizona Education Officer (6/2006-6/2009) Mike A’Hearn Univ. of Maryland Pub. Board Chair (6/2005-6/2008) Kevin Marvel AAS Executive Officer (6/2006-Present) Gary J. Ferland Univ. of Kentucky (6/2007-6/2008) Suzanne Hawley Univ. -
The Future of X-Rayastronomy
The Future of X-rayAstronomy Keith Arnaud [email protected] High Energy Astrophysics Science Archive Research Center University of Maryland College Park and NASA’s Goddard Space Flight Center Themes Politics Efficient high resolution spectroscopy Mirrors Polarimetry Other missions Interferometry Themes Politics Efficient high resolution spectroscopy Mirrors Polarimetry Other missions Interferometry How do we get a new X-ray astronomy experiment? A group of scientists and engineers makes a proposal to a national (or international) space agency. This will include a science case and a description of the technology to be used (which should generally be in a mature state). In principal you can make an unsolicited proposal but in practice space agencies have proposal rounds in the same way that individual missions have observing proposal rounds. NASA : Small Explorer (SMEX) and Medium Explorer (MIDEX): every ~2 years alternating Small and Medium, three selected for study for one year from which one is selected for launch. RXTE, GALEX, NuSTAR, Swift, IXPE Arcus, a high resolution X-ray spectroscopy mission was a finalist in the latest MIDEX round but was not selected. Missions of Opportunity (MO): every ~2 years includes balloon programs, ISS instruments and contributions to foreign missions. Suzaku, Hitomi, NICER, XRISM Large missions such as HST, Chandra, JWST are not selected by such proposals but are decided as national priorities through the Astronomy Decadal process. Every ten years a survey is run by the National Academy of Sciences to decide on priorities for both land-based and space-based astronomy. 1960: HST; 1970: VLA; 1980: VLBA; 1990: Chandra and SIRTF; 2000: JWST and ALMA; 2010 WFIRST and LSST. -
Modified Newtonian Dynamics, an Introductory Review
Modified Newtonian Dynamics, an Introductory Review Riccardo Scarpa European Southern Observatory, Chile E-mail [email protected] Abstract. By the time, in 1937, the Swiss astronomer Zwicky measured the velocity dispersion of the Coma cluster of galaxies, astronomers somehow got acquainted with the idea that the universe is filled by some kind of dark matter. After almost a century of investigations, we have learned two things about dark matter, (i) it has to be non-baryonic -- that is, made of something new that interact with normal matter only by gravitation-- and, (ii) that its effects are observed in -8 -2 stellar systems when and only when their internal acceleration of gravity falls below a fix value a0=1.2×10 cm s . Being completely decoupled dark and normal matter can mix in any ratio to form the objects we see in the universe, and indeed observations show the relative content of dark matter to vary dramatically from object to object. This is in open contrast with point (ii). In fact, there is no reason why normal and dark matter should conspire to mix in just the right way for the mass discrepancy to appear always below a fixed acceleration. This systematic, more than anything else, tells us we might be facing a failure of the law of gravity in the weak field limit rather then the effects of dark matter. Thus, in an attempt to avoid the need for dark matter many modifications of the law of gravity have been proposed in the past decades. The most successful – and the only one that survived observational tests -- is the Modified Newtonian Dynamics. -
ROSAT All-Sky Survey
ROSAT All-Sky Survey S. R. Kulkarni July 22, 2020{July 27, 2020 The Russian-German mission, Spektr-R¨ongtenGamma (SRG) is on the verge of revolution- izing X-ray astronomy. One of the instruments, eROSITA, will be undertaking an imaging survey of the X-ray sky. Each six-month the entire sky will be covered to a sensitivity which is ten times better than the previous such survey (ROSAT). After eight semesters SRG will undertake pointed observations. I provide a condensed history so that a young student can appreciate the importance of SRG/eROSITA. The first all sky survey was undertaken by the Uhuru (aka SAS-1; 1970) satellite. This was followed up by HEAO-1 (aka HEAO-A; 1977) surveys. These surveys detected 339 and 843 sources in the 2{10 keV band. For those interested in arcana, 1 Uhuru count/s is 1:7 × 10−11 erg cm−2 s−1 in the 2{6 keV band. The next major mission was HEAO-2 (aka Einstein; launched in 1978). This was a game changer since, unlike the past missions which used essentially collimators or shadow cam- eras, the centerpiece of Einstein was a true imaging telescope. Furthermore the mission carried an amazing complement of imagers and spectrometers in the focal plane. The mission coincided with my graduate school (1978-1983). R¨ontgensatellit (ROSAT) was a German mission to undertake an X-ray imaging survey of the entire sky { the first such survey. Launched in 1990 it lasted for eight years. It carried two Positional Sensitive Proportional Counter (PSPC; 0.1{2.4 keV), a High Resolution Imager (HRI) and the Wide Field Camera (WFC; 60{300 A).˚ The PSPC, with a field-of- view of 2 degrees, was the primary work horse for the X-ray sky survey and was > 100 more sensitive than the pioneering Uhuru and HEAO-A1 surveys. -
Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected]
Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 7-2017 Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky [email protected] Follow this and additional works at: http://scholarworks.rit.edu/theses Recommended Citation Lipnicky, Andrew, "Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far" (2017). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by the Thesis/Dissertation Collections at RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. R I T · · Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Andrew Lipnicky A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology © A. Lipnicky July, 2017 Rochester Institute of Technology Ph.D. Dissertation Galactic Building Blocks: Searching for Dwarf Galaxies Near and Far Author: Advisor: Andrew Lipnicky Dr. Sukanya Chakrabarti A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Approved by Dr.AndrewRobinson Date Director, Astrophysical Sciences and Technology Certificate of Approval Astrophysical Sciences and Technology R I T College of Science · · Rochester, NY, USA The Ph.D. Dissertation of Andrew Lipnicky has been approved by the undersigned members of the dissertation committee as satisfactory for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology. -
Disk Galaxy Rotation Curves and Dark Matter Distribution
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Disk galaxy rotation curves and dark matter distribution by Dilip G. Banhatti School of Physics, Madurai-Kamaraj University, Madurai 625021, India [Based on a pedagogic / didactic seminar given by DGB at the Graduate College “High Energy & Particle Astrophysics” at Karlsruhe in Germany on Friday the 20 th January 2006] Abstract . After explaining the motivation for this article, we briefly recapitulate the methods used to determine the rotation curves of our Galaxy and other spiral galaxies in their outer parts, and the results of applying these methods. We then present the essential Newtonian theory of (disk) galaxy rotation curves. The next two sections present two numerical simulation schemes and brief results. Finally, attempts to apply Einsteinian general relativity to the dynamics are described. The article ends with a summary and prospects for further work in this area. Recent observations and models of the very inner central parts of galaxian rotation curves are omitted, as also attempts to apply modified Newtonian dynamics to the outer parts. Motivation . Extensive radio observations determined the detailed rotation curve of our Milky Way Galaxy as well as other (spiral) disk galaxies to be flat much beyond their extent as seen in the optical band. Assuming a balance between the gravitational and centrifugal forces within Newtonian mechanics, the orbital speed V is expected to fall with the galactocentric distance r as V 2 = GM/r beyond the physical extent of the galaxy of mass M, G being the gravitational constant.