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Yvette Burkhammer
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You Bet Your Head was an interactive trivia game in which animated contestants would be flattened by the MC, a hammer, for wrong answers. To answer the questions yourself, you pressed Caps Lock and chose a numbered answer.
Draw Morph let you choose from various stop motion animated figures, such as Pipecleaner Man, who performed acrobatics while walking across the screen. You could also create your own series of images to be animated.
A blast from the past, this screensaver featured a man listening to a vintage radio show while reading a paper, together with images of radio announcers and antique phones, set to the sound of old radio shows and ringing phones.
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SETI@home ("SETI at home") is a project of the Berkeley SETI Research Center to analyze radio signals with the aim of searching for signs of extraterrestrial intelligence. Until March 2020, it was run as an Internet-based public volunteer computing project that employed the BOINC software platform. It is hosted by the Space Sciences Laboratory at the University of California, Berkeley, and is one of many activities undertaken as part of the worldwide SETI effort.
SETI@home software was released to the public on May 17, 1999,[5][6][7][8] making it the third large-scale use of volunteer computing over the Internet for research purposes, after Great Internet Mersenne Prime Search (GIMPS) was launched in 1996 and distributed.net in 1997. Along with MilkyWay@home and Einstein@home, it is the third major computing project of this type that has the investigation of phenomena in interstellar space as its primary purpose.
In March 2020, the project stopped sending out new work to SETI@home users, bringing the crowdsourced computing aspect of the project to a stop.[9] At the time, the team intended to shift focus onto the analysis and interpretation of the 20 years' worth of accumulated data. However, the team left open the possibility of eventually resuming volunteer computing using data from other radio telescopes, such as MeerKAT and FAST.[10]
As of November 2021, the science team has analysed the data and removed noisy signals (Radio Frequency Interference) using the Nebula tool they developed and will choose the top-scoring 100 or so multiplets to be observed using the Five-hundred-meter Aperture Spherical Telescope, to which they have been granted 24 hours of observation time.[11]
The second of these goals is considered to have succeeded completely. The current BOINC environment, a development of the original SETI@home, is providing support for many computationally intensive projects in a wide range of disciplines.
The first of these goals has to date yielded no conclusive results: no evidence for ETI signals has been shown via SETI@home. However, the ongoing continuation is predicated on the assumption that the observational analysis is not "ill-posed." The remainder of this article deals specifically with the original SETI@home observations/analysis. The vast majority of the sky (over 98%) has yet to be surveyed, and each point in the sky must be surveyed many times to exclude even a subset of possibilities.
There are many variations on how an ETI signal may be affected by the interstellar medium, and by the relative motion of its origin compared to Earth. The potential "signal" is thus processed in many ways (although not testing all detection methods nor scenarios) to ensure the highest likelihood of distinguishing it from the scintillating noise already present in all directions of outer space. For instance, another planet is very likely to be moving at a speed and acceleration with respect to Earth, and that will shift the frequency, over time, of the potential "signal." Checking for this through processing is done, to an extent, in the SETI@home software.
The process is somewhat like tuning a radio to various channels, and looking at the signal strength meter. If the strength of the signal goes up, that gets attention. More technically, it involves a lot of digital signal processing, mostly discrete Fourier transforms at various chirp rates and durations.
To date, the project has not confirmed the detection of any ETI signals. However, it has identified several candidate targets (sky positions), where the spike in intensity is not easily explained as noise spots,[16] for further analysis. The most significant candidate signal to date was announced on September 1, 2004, named Radio source SHGb02+14a.
Astronomer Seth Shostak stated in 2004 that he expects to get a conclusive signal and proof of alien contact between 2020 and 2025, based on the Drake equation.[19] This implies that a prolonged effort may benefit SETI@home, despite its (present) twenty-year run without success in ETI detection.
Observational data were recorded on 2-terabyte SATA hard disk drives fed from the Arecibo Telescope in Puerto Rico, each holding about 2.5 days of observations, which were then sent to Berkeley.[20] Arecibo does not have a broadband Internet connection, so data must go by postal mail to Berkeley.[21] Once there, it is divided in both time and frequency domains work units of 107 seconds of data,[22] or approximately 0.35 megabytes (350 kilobytes or 350,000 bytes), which overlap in time but not in frequency.[20] These work units are then sent from the SETI@home server over the Internet to personal computers around the world to analyze.
The initial software platform, now referred to as "SETI@home Classic", ran from May 17, 1999, to December 15, 2005. This program was only capable of running SETI@home; it was replaced by Berkeley Open Infrastructure for Network Computing (BOINC), which also allows users to contribute to other volunteer computing projects at the same time as running SETI@home. The BOINC platform also allowed testing for more types of signals.
On May 3, 2006, new work units for a new version of SETI@home called "SETI@home Enhanced" started distribution. Since computers had the power for more computationally intensive work than when the project began, this new version was more sensitive by a factor of two concerning Gaussian signals and to some kinds of pulsed signals than the original SETI@home (BOINC) software. This new application had been optimized to the point where it would run faster on some work units than earlier versions. However, some work units (the best work units, scientifically speaking) would take significantly longer.
In addition, some distributions of the SETI@home applications were optimized for a particular type of CPU. They were referred to as "optimized executables", and had been found to run faster on systems specific for that CPU. As of 2007[update], most of these applications were optimized for Intel processors and their corresponding instruction sets.[26]
There were plans to get data from the Parkes Observatory in Australia to analyze the southern hemisphere.[29] However, as of 3 June 2018[update], these plans were not mentioned in the project's website. Other plans include a Multi-Beam Data Recorder, a Near Time Persistency Checker and Astropulse (an application that uses coherent dedispersion to search for pulsed signals).[30] Astropulse will team with the original SETI@home to detect other sources, such as rapidly rotating pulsars, exploding primordial black holes, or as-yet unknown astrophysical phenomena.[31] Beta testing of the final public release version of Astropulse was completed in July 2008, and the distribution of work units to higher spec machines capable of processing the more CPU intensive work units started in mid-July 2008.
On March 31, 2020, UC Berkeley stopped sending out new data for SETI@Home clients to process, ending the effort for the time being. The program stated they were at a point of "diminishing returns" with the volunteer processing and needed to put the effort into hibernation while they processed the results.[32]
SETI@home users quickly started to compete with one another to process the maximum number of work units. Teams were formed to combine the efforts of individual users. The competition continued and grew larger with the introduction of BOINC.
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