November 2013 One of the SKA's Founding Scientists Moves Closer To
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Annual Report 2013 E.Indd
2013 ANNUAL REPORT NATIONAL RADIO ASTRONOMY OBSERVATORY 1 NRAO SCIENCE NRAO SCIENCE NRAO SCIENCE NRAO SCIENCE NRAO SCIENCE NRAO SCIENCE NRAO SCIENCE 493 EMPLOYEES 40 PRESS RELEASES 462 REFEREED SCIENCE PUBLICATIONS NRAO OPERATIONS $56.5 M 2,100+ ALMA OPERATIONS SCIENTIFIC USERS $31.7 M ALMA CONSTRUCTION $11.9 M EVLA CONSTRUCTION A SUITE OF FOUR WORLDCLASS $0.7 M ASTRONOMICAL OBSERVATORIES EXTERNAL GRANTS $3.8 M NRAO FACTS & FIGURES $ 2 Contents DIRECTOR’S REPORT. 5 NRAO IN BRIEF . 6 SCIENCE HIGHLIGHTS . 8 ALMA CONSTRUCTION. 26 OPERATIONS & DEVELOPMENT . 30 SCIENCE SUPPORT & RESEARCH . 58 TECHNOLOGY . 74 EDUCATION & PUBLIC OUTREACH. 80 MANAGEMENT TEAM & ORGANIZATION. 84 PERFORMANCE METRICS . 90 APPENDICES A. PUBLICATIONS . 94 B. EVENTS & MILESTONES . 118 C. ADVISORY COMMITTEES . .120 D. FINANCIAL SUMMARY . .124 E. MEDIA RELEASES . .126 F. ACRONYMS . .136 COVER: The National Radio Astronomy Observatory Karl G. Jansky Very Large Array, located near Socorro, New Mexico, is a radio telescope of unprecedented sensitivity, frequency coverage, and imaging capability that was created by extensively modernizing the original Very Large Array that was dedicated in 1980. This major upgrade was completed on schedule and within budget in December 2012, and the Jansky Very Large Array entered full science operations in January 2013. The upgrade project was funded by the US National Science Foundation, with additional contributions from the National Research Council in Canada, and the Consejo Nacional de Ciencia y Tecnologia in Mexico. Credit: NRAO/AUI/NSF. LEFT: An international partnership between North America, Europe, East Asia, and the Republic of Chile, the Atacama Large Millimeter/submillimeter Array (ALMA) is the largest and highest priority project for the National Radio Astronomy Observatory, its parent organization, Associated Universities, Inc., and the National Science Foundation – Division of Astronomical Sciences. -
Arxiv:1402.1456V1 [Astro-Ph.CO] 6 Feb 2014 2.4.1 Intrinsic Variation in Seds
Dusty Star-Forming Galaxies at High Redshift Caitlin M. Casey1;2, Desika Narayanan3, Asantha Cooray1 1Department of Physics and Astronomy, University of California, Irvine, CA 92697 2Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Dr, Honolulu, HI 96822 3Department of Physics and Astronomy, Haverford College, 370 Lancaster Avenue, Haverford, PA 19041 Abstract Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest 13 of these galaxies have infrared luminosities in excess of 10 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wave- lengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both space- based and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the best- understood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. -
Dusty Star Forming Galaxies at High Redshift
Dusty Star Forming Galaxies at High Redshift Caitlin M. Casey1;2, Desika Narayanan3, Asantha Cooray1 1Department of Physics and Astronomy, University of California, Irvine, CA 92697 2Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Dr, Honolulu, HI 96822 3Department of Physics and Astronomy, Haverford College, 370 Lancaster Avenue, Haverford, PA 19041 Abstract Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest 13 of these galaxies have infrared luminosities in excess of 10 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both space-based and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the best-understood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. -
Newsletter Submillimeter Array Newsletter Number 16 | July 2013
SMA Newsletter Submillimeter Array Newsletter Number 16 | July 2013 CONTENTS FROM THE DIRECTOR 1 From the Director Dear SMA Newsletter readers, SCIENCE HIGHLIGHTS: The SMA recently reached another scientific milestone with more than five hundred scientific 2 Submillimeter Galaxy papers published in refereed journals, and combined citations in excess of ten thousand. Since Merger Leading to the inauguration of the SMA in 2004, the publication rate has risen steadily. A significant con- Massive Elliptical Galaxy tributing factor has been the improvement in sensitivity resulting from lower-noise receivers Formation at z=2.3 coupled with a two-fold increase in processed bandwidth. 4 The Galactic Center Cloud For the past two years, the receiver group has been working towards developing even wider G0.253+0.016: A Dense Cloud With Low Star bandwidth receivers at 230 and 345 GHz. Wide-band receivers at 230 GHz are available on Formation Potential all eight of the SMA antennas, four of which have also been equipped with wide-band 345 GHz receivers. During the coming months we expect to complete installation of the remain- 7 Detection of Rotational Lines ing receivers at 345 GHz. In addition, the SMA correlator group has been developing a sec- of TiO and TiO2 in VY CMa ond-generation spectrometer, which, when used in parallel with the existing SMA correlator, TECHNICAL HIGHLIGHTS: will enable another doubling of the processed bandwidth. While the second-generation spec- bk Digital Back End (DBE): trometer is still under development at the Cambridge labs, initial on-sky tests at reduced ca- SMA Phase Agile Antenna pacity are encouraging.