The vacuum tanks arrive at Hanford in August 1997. Credit: LIGO

Built to look for gravitational waves, the ripples in the fabric of space itself that were predicted by Einstein in 1916, the Laser Interferometer Gravitational-Wave Observatory (LIGO) is the most ambitious project ever funded by the National Science Foundation. LIGO consists of two L-shaped interferometers with four-kilometer-long arms; at their ends hang mirrors whose motions are measured to within one-thousandth the diameter of a proton. Managed jointly by Caltech and MIT, Initial LIGO became operational in 2001; the second-generation Advanced LIGO was dedicated on May 19.

Barry Barish is the Roland and Maxine Linde Professor of Physics, Emeritus. He was LIGO's principal investigator from 1994 to 1997, and director from 1997 to 2006. Stan Whitcomb (BS '73) was an assistant professor of physics at Caltech from 1980 to 1985. He returned to campus as a member of the professional staff in 1991 and has served the LIGO project in various capacities ever since. We talked with each of them about how LIGO came to be.

Q: How did LIGO get started?

BARISH: Einstein didn't think that gravitational waves could ever be detected, because gravity is such a weak force. But in the 1960s, Joseph Weber at the University of Maryland turned a metric ton of aluminum into a bar 153 centimeters long. The bar naturally rang at a frequency of about 1,000 Hertz. A collapsing supernova should produce gravitational waves in that frequency range, so if such a wave passed through the bar, the bar's resonance might amplify it enough to be measurable. It was a neat idea, and basically initiated the field experimentally. But you can only make a bar so big, and the signal you see depends on the size of the detector.

[Professor of Physics, Emeritus] Ron Drever, whom we recruited from the University of Glasgow, had started out working on bar detectors. But when we hired him, he and Rainer [Rai] Weiss at MIT were independently developing interferometer-type detectors—a concept previously suggested by others. Usually you fasten an interferometer's mirrors down tightly so they keep their alignment, but LIGO's mirrors have to be free to swing so that the gravitational waves can move them. It's very difficult to do incredibly precise things with big, heavy masses that want to move around.

WHITCOMB: Although bar detectors were by far the most sensitive technology at the time, it appeared that they would have a much harder path reaching the sensitivity they would ultimately need. Kip Thorne [BS '62, Richard P. Feynman Professor of Theoretical Physics, Emeritus] was really instrumental in getting Caltech to jump into interferometer technology and to try to bring that along.

Ron's group at Glasgow had built a 10-meter interferometer, which was all the space they had. We built a 40-meter version largely based on their designs, but trying to improve them where possible. In those days we were working with argon-ion lasers, which were the best available, but very cantankerous. Their cooling water introduced a lot of vibrational noise into the system, making it difficult to reach the sensitivity we needed. We were also developing the control systems, which in those days had to be done with analog electronics. And we had some of the first "supermirrors," which were actually military technology that we were able to get released for scientific use. The longer the interferometer's arms, the smaller the displacements it can measure, and the effective length is the cumulative distance the light travels. We bounce the light back and forth hundreds of times, essentially making the interferometer several thousand kilometers long.

By February 1998 the vacuum equipment is installed at the point of the L. The center vertical tank houses the beam splitter. At right one of the beam tubes takes off into the desert. Credit: LIGO

Q: When did the formal collaboration with MIT begin?

BARISH: Rai [Weiss] and Ron [Drever] were running their own projects at MIT and Caltech, respectively, until [R. Stanton Avery Distinguished Service Professor and Professor of Physics, Emeritus] Robbie Vogt, Caltech's provost, brought them together. They had very different ways of approaching the world, but Robbie somehow pulled what was needed out of both of them.

Robbie spearheaded the proposal that was submitted to the National Science Foundation in 1989. That two-volume, nearly 300-page document contained the underpinnings—the key ideas, technologies, and concepts that we use in LIGO today. A lot of details are different, a lot of things have been invented, but basically even the dimensions are much the same.

WHITCOMB: When I returned in 1991, LIGO had become a joint Caltech/MIT project with a single director, Robbie Vogt. Robbie had brought in a set of engineers, many borrowed or recruited from JPL, to do the designs. The late Boude Moore [BS '48 EE, MS '49 EE], our vacuum engineer, was figuring out how to make LIGO's high-vacuum systems out of low-hydrogen-outgassing stainless steel. This had never been done before. Hydrogen atoms absorbed in the metal slowly leak out over the life of the system, but our measurements are so precise that stray atoms hitting the mirrors would ruin the data. Boude was doing some relatively large-scale tests, mostly in the synchrotron building, but we also built a test cylinder 80 meters long near Caltech's football field, behind the gym.

So all of these tests were going on piecemeal at different places, and at the 40-meter interferometer we brought it all together. We were still mostly using analog electronics, but we had a new vacuum system, we redid all the suspension systems, we added several new features to the detector, and we had attained the sensitivity we were going to need for the full-sized, four-kilometer LIGO detectors.

And at the same time, in 1991, we got word that the full-scale project had been approved.

Q: How were the sites in Hanford, Washington, and Livingston, Louisiana, selected?

WHITCOMB: I cochaired the site-evaluation committee with LIGO's chief engineer, [Member of the Professional Staff] Bill Althouse. We visited most of the potential sites, evaluated them, and recommended a set of best site pairs to NSF. We had several sets of criteria. The engineering criteria included how level the site was, how stable it was against things like frost heaves, how much road would need to be built, and the overall cost of construction. We had criteria about proximity to people, and to noise sources like airports and railroads. We also had scientific criteria. For example, we wanted the two sites to be as far apart in the U.S. as you could reasonably get. We also wanted LIGO to work well with either of the two proposed European detectors—GEO [in Hanover, Germany] and Virgo [in Tuscany, Italy]. We needed to be able to triangulate a source's position on the sky, so we did not want LIGO's sites to form a line with either of them.

The 4-inch thick, 10-inch diameter mirrors at the ends of the beam tubes recycle the laser light. The polished mirrors are coated with up to 35 layers of a purple dielectric coating designed to achieve the reflectance and transmission of light for the wavelengths used by LIGO. Credit: LIGO

Q: What makes Advanced LIGO more sensitive?

BARISH: Well, it's complicated. Most very sensitive physics experiments get limited by some source of background noise, so you concentrate on that thing and figure out how to beat it down. But LIGO has three limits. We are looking for gravitational waves over a range of frequencies from 10 Hertz to 10 kilohertz. Our planet is incredibly noisy seismically, so from 10 Hertz to about 100 Hertz we have to isolate ourselves from that shaking. And at very high frequencies, we have to sample fast enough to see the signal, so we're limited by the laser's power, which determines the number of photons we can sample in a short amount of time. And in the middle frequencies, we're limited by what we call "thermal noise"—the atoms in the mirrors moving around, and so forth.

Advanced LIGO has a very much more powerful laser to take care of the high frequencies. It has much fancier isolation systems, including active feedback systems. And we have bigger test masses with better mirror coatings to minimize the thermal background. All of these improvements were in the 1989 proposal, which called for Initial LIGO to be built with proven techniques that had mostly been tested here on campus in the 40-meter prototype; followed by Advanced LIGO, to be built using techniques we would test in the 40-meter after Initial LIGO went operational. And now we're using the 40-meter lab to develop and test the next round of upgrades.

One of the dual instruments of the Laser Interferometer Gravitational-Wave Observatory sprawls across the desert near Hanford, Washington, each arm extending four kilometers and meeting at the corner of an L. The support buildings at the corner house laboratories as well as electronic and optical equipment, which will send a laser beam, split in two, back and forth down the two arms to intercept the infinitesimally small signal of a gravitational wave. Credit: LIGO

Q: How close do you think we are to a detection?

BARISH: I've always had the fond wish that we'd do it by 2016, which is the hundredth anniversary of Einstein's theory. Advanced LIGO may take three to five years to reach the designed sensitivity, but we'll be taking data along the way, so the probability of a detection will be continually increasing. Our sensitivity is designed to improve by a factor of 10 to 20, and a factor of 10 increases the detection probability by a factor of 1,000. The sensitivity tells you how far out you can see, and volume increases with the cube of the distance.

When we started this back in 1989, some people were a bit skeptical, saying maybe it's a little bit like fusion. They always say fusion is "50 years away." With LIGO the common lore is we are 10 years away from detecting gravitational waves. I would say that it's not 10 years any longer. It's probably within five.

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