IR, Visible and Radio SETI Andrew Siemion, David Anderson, Bob Bankay, Henry Chen, Jeff Cobb, Griffin Foster, Andrew Howard, Eric Korpela,

Slides:



Advertisements
Similar presentations
Arecibo 40th Anniversary Workshop--R. L. Brown The Arecibo Astrometric/Timing Array Robert L. Brown.
Advertisements

PAPER’s Sweet Sixteen: Imaging the Low Frequency Sky with a Sixteen Element Array Nicole Gugliucci for the PAPER Team* USNC/URSI National Radio Science.
Team Presentation July 22, Jodrell Bank is the original arboretum for Manchester University. Immediately after World War II, first radio telescope.
SETI Mike Poeschl Matt Boggess. What is SETI? Acronym for Search for Extra- Terrestrial Intelligence Began in 1960 at Cornell University (Frank Drake)
Multiwave, Lonely, and ET. Where do I live? The image of the IR man is from the Infrared Processing and Analysis Center at the California Institute.
Jim Cordes and Dan Werthimer And Five Milliion Volunteers in 226 countries
Introduction to Radio Astronomy Updated February 2009.
The Search for Spock The Scientific Search for Extraterrestrial Life Or Graur Student Seminar
Light and Telescopes Chapter 5. Traditional Telescopes The 4-m Mayall Telescope at Kitt Peak National Observatory (Arizona)
Transient SETI Dan Werthimer University of California, Berkeley
Light and Telescopes Chapter 5. Radio Interferometry The Very Large Array (VLA): 27 dishes are combined to simulate a large dish of 36 km in diameter.
What does do? Mini-project for CSE 260 Qian Peng 15 November 2001 Ref.
K.S. Dawson, W.L. Holzapfel, E.D. Reese University of California at Berkeley, Berkeley, CA J.E. Carlstrom, S.J. LaRoque, D. Nagai University of Chicago,
10/14/03Prof. Lynn Cominsky1 Class web site: Office: Darwin 329A and NASA E/PO (707) Best way to.
The Nature of Light In Astronomy II. The Earth’s atmosphere absorbs most of EM spectrum, including all UV, X ray, gamma ray and most infrared. We have.
Andrew Siemion SSL Colloquium April 10, 2009 Andrew Siemion SSL Colloquium April 10, 2009 Searching for Radio Ephemera: The Fly’s Eye AstroPulse Searching.
Sunny Gleason COM S 717 November 29, 2001 (Based on the article, Massively Distributed Computing for SETI.”)
Mapping Hydrogen in the Galaxy, Galactic Halo and Local Group with the Galactic Arecibo L-Band Feed Array (GALFA) The GALFA-HI Survey starting with TOGS.
Introduction of Space Technology. The James Webb Space Telescope The James Webb Space Telescope was previously known as the Next Generation Space Telescope.
Dark Skies are a Universal Resource. So Are Quiet Skies! In the same way that man-made light obscures our night sky and blinds ground-based optical telescopes,
Theories Of Existence Pranshu Sanghai IX C. The Need To Search For Aliens In the past couple of decades, the study of life on Earth has revealed the existence.
Infrared Telescopes 1.
Current Approaches to the Search for Life Dan Werthimer, UC Berkeley
Extra-terrestrial Civilizations: Interstellar Radio Communications.
SETI on the SKA Dan Werthimer University of California, Berkeley
Radio Astronomy and SETI
The Milky Way Galaxy.
Telescope Technologies
SETI Search for Extra Terrestrial Intelligence FYOS Lecture 8.
Search for Extraterrestrial Life PHY 100. How life emerged on earth  Amino acids, “building blocks of life” form via chemical reactions  With help of.
G oldstone A pple V alley R adio T elescope GAVRT IS: ★ A partnership involving NASA, the Jet Propulsion Laboratory (JPL), and The Lewis Center. ★ An.
Medium-Rare Earth. Rare Earth Right distance from star Right mass of star Stable planetary orbits Right planetary mass Jupiter-like neighbor Plate tectonics.
Imaging the sky in radio domain Andrzej Marecki Centre for Astronomy Copernicus University Toruń.
HOW DO WE SEARCH FOR LIFE IN THE UNIVERSE?. Necessary Assumptions All civilizations follow a certain set of broad universal pathways. There are civilizations.
A multiwavelength approach is needed to discover a quasars’ behaviour as a whole and uncover its structure. This means obtaining data from the long wavelength.
Jason Manley, Aaron Parsons, Don Backer, Henry Chen, Terry Filiba, David MacMahon, Peter McMahon, Arash Parsa, Andrew Siemion, Dan Werthimer, Mel Wright.
Russian 6-m Nasmyth focus platforms Problems: 17-ton mirror has thermal time constant of a few days; location based on politics. Note alt-az mount.
Rachael Ainsworth Dublin Institute for Advanced Studies YERAC 2011.
Methanol maser and 3 mm line studies of EGOs Xi Chen (ShAO) 2009 East Asia VLBI Workshop, March , Seoul Simon Ellingsen (UTAS) Zhi-Qiang Shen.
What Channel is That?.  Visible light is a form of electromagnetic radiation.  Others include:  Radio waves  Infrared waves (heat)  Ultraviolet waves.
Spectrums & Telescopes *A device that makes distant objects appear to be closer *They detect electromagnetic radiation – light or energy that can travel.
Chapter 21: Stars, Galaxies, Universe Section 1: telescopes
K-Band Focal Plane Array Project Engineering Overview Matt Morgan National Radio Astronomy Observatory 2/27/2008.
Observations of Near Infrared Extragalactic Background (NIREBL) ISAS/JAXAT. Matsumoto Dec.2-5, 2003 Japan/Italy seminar at Niigata Univ.
G Z The LIGO gravitational wave detector consists of two observatories »LIGO Hanford Observatory – 2 interferometers (4 km long arms and 2 km.
Exploring the Unknown with CASPER Instrumentation Andrew Siemion CASPER Workshop 2011.
A101 Slide Set: Shockingly Bright Pulsar Developed by the NuSTAR EPO Group at Sonoma State University 0 Topic: Pulsars, X-rays, black holes Concepts: multi-wavelength.
OSETI with MAGIC IntroductionIntroduction Radio SETIRadio SETI Optical SETIOptical SETI OSETI with MAGICOSETI with MAGIC SummarySummary July 2004.
Analysis of GALFACTS Data for the Study Of Variable Radio Sources Scott Barenfeld 1, Tapasi Ghosh 2, Chris Salter 2 1 NAIC/University of Rochester, 2 NAIC.
SCM x330 Ocean Discovery through Technology Area F GE.
By: Carlos E. Marín Pérez & Edwin C. López Ramos Mentor: Dr. Tapasi Ghosh Arecibo Observatory Gas in Luminous Infrared Galaxies.
NIR, MIR, & FIR.  Near-infrared observations have been made from ground based observatories since the 1960's  Mid and far-infrared observations can.
Space Tools Key Point (Std ): Compare the purposes of the tools and the technology that scientists use to study space.
Planning for the ATA David DeBoer OWG AOC March 13, 2006.
History of SETI Is there intelligent life out there?
Do Luminous Infrared Galaxies -LIRGs- follow Hubble’s Law? Harrison Rivera Colon and Yesenia M. Rivera Lopez; Antonio Lucchetti Voc. H.S., Arecibo, Puerto.
Telescope Technology Types of Telescopes Hubble Telescope and NASA’s Great Observatories.
Observability of YSOs with the WISE and AKARI infrared observatories Sarolta Zahorecz Eötvös University, Budapest PhD student, 3. year Thesis advisor:
Space Tools Standard Compare the purposes of the tools & the technology that scientists use to study space.
SETI Spectrometer Development for ALFA
Chapter 6 Astronomical Instruments
The Tools of the Astronomer
David P. Anderson Space Sciences Lab UC Berkeley LASER
Goal: To understand intelligent life in our universe.
DIRECT DETECTION OF GRAVITATIONAL WAVES FROM NEUTRON STARS
Tools of Space Exploration
The SERENDIP, SEVENDIP, Astropulse, and SPOCK SETI Programs
A Study of Accretion Disks Around Young Binary Star Systems
The Quest for Extraterrestrial Intelligence
Presentation transcript:

IR, Visible and Radio SETI Andrew Siemion, David Anderson, Bob Bankay, Henry Chen, Jeff Cobb, Griffin Foster, Andrew Howard, Eric Korpela, Matt Lebofsky, Aaron Parsons, Josh Von Korff, Dan Werthimer University of California, Berkeley SETISERENDIPIR ExcessJPL/SETI Spectrometer Because of disk access limitations, the spectrometer does not write out every channel of every spectrum. Instead, each channel is divided by the average of adjacent channels, and only those channels for which this ratio exceeds a user defined threshold are written to disk. The JPL/SETI Spectrometer operates on the Berkeley Emulation Engine - 2 (BEE2) FPGA based computing platform. It was installed at NASA’s 34- meter DSS-13 radio telescope in August of This spectrometer is capable of performing an astonishing 134,217,728- channel FFT every 0.67 seconds, with a total bandwidth of 200 MHz, centered at 2 GHz. NASA DSS-13, GDSCC SETI Spectrometer Spectrum Plot NAIC Arecibo Observatory Screenshot Cut-away Diagram of an Idealized Dyson Surface SERENDIP Progress: Past, Present and Future Schematic Diagram of SETI Photometer The UC Berkeley Infrared Excess Search attempts to identify excess thermal infrared radiation emitted from highly advanced civilizations by searching the IRAS and 2MASS catalogs and performing follow-up observations on likely candidates with the Serendip V, and Optical SETI databases. SERENDIP has been in operation for 28 years, beginning with SERENDIP I in 1979 and continuing most recently with SERENDIP V. ALFA Multi-Beam Receiver Launched in 1999, has engaged over 5 million people in 226 countries in the search for life on other worlds. Currently, participants in the project are generating a collective equivalent of 200 TeraFLOPs/sec. II users have performed over 1.4 x FLOPs to-date. This immense and growing computing power is being used to conduct a commensal sky survey utilizing Arecibo’s ALFA multi- beam receiver. The pulse search utilizes Berkeley's 30 inch automated telescope at Leuschner Observatory in Lafayette (15 miles east of campus) using a custom built photometer designed specifically for the optical SETI project. The Optical SETI program at UC Berkeley searches for nanosecond time scale pulses, perhaps transmitted by a powerful pulsed laser operated by a distant civilization. Began in 1997, this program was the first search of its kind. Leuschner 30 in. Telescope The initial dataset consists of 1000 stars with ages determined by Ca II absorption to be >1 gigayear to reduce the likelihood of an associated protoplanetary disk. Infrared excess for all 540 target stars (upper left) and based on stellar type. Infrared excess was determined via the K-[12] indicator. The K band is thought to be quite insensitive to stellar atmosphere fluctuations, and hence provides a stable benchmark for color excess. 33 IR excess candidates were found and subsequently searched for anomalous radio emission nanosecond-scale optical pulses. No convincing signals were found. The upcoming SERENDIP V sky survey will use the 7-beam Arecibo L-band Feed Array (ALFA) at Arecibo Observatory to carry out a high sensitivity survey of the sky visible to Arecibo. This survey will search for narrow-band signals in an ~300 MHz band surrounding 1420 MHz. The observations will be 10 times more sensitive and 100 times more comprehensive than the most sensitive existing SETI large-area surveys (SERENDIP IV and The two billion channel SERENDIP V spectrometer, to be deployed at Arecibo late 2008, will analyze signals from all seven beams simultaneously in dual polarization, effectively observing seven points on the sky simultaneously. Serendip V Specs II Specs Optical SETI Specs