Many of us have been rescued from unfamiliar¹ territory by directions from a Global Positioning System (GPS) navigator（导航器）. GPS satellites send signals to a receiver in your GPS navigator, which calculates your position based on the location of the satellites and your distance from them. The distance is determined² by how long it took the signals from various satellites to reach your receiver. The system works well, and millions rely on it every day, but what tells the GPS satellites where they are in the first place?

"For GPS to work, the orbital position（轨道位置）, or ephemeris（位置推算历）, of the satellites has to be known very precisely³," said Dr. Chopo Ma of NASA's Goddard Space Flight Center in Greenbelt, Md. "In order to know where the satellites are, you have to know the orientation⁴（方向） of the Earth very precisely."

This is not as obvious as simply looking at the Earth – space is not conveniently marked with lines to determine our planet's position. Even worse, "everything is always moving," says Ma. Earth wobbles as it rotates due to the gravitational pull (tides) from the moon and the sun. Even apparently⁵ minor⁶ things like shifts in air and ocean currents and motions in Earth's molten core（熔火之核） all influence our planet's orientation.

Just as you can use landmarks⁷ to find your place in a strange city, astronomers⁸ use landmarks in space to position the Earth. Stars seem the obvious candidate, and they were used throughout history to navigate⁹ on Earth. "However, for the extremely precise measurements needed for things like GPS, stars won't work, because they are moving too," says Ma.

What is needed are objects so remote that their motion is not detectable¹⁰. Only a couple classes of objects fit the bill, because they also need to be bright enough to be seen over incredible distances. Things like quasars（类星体）, which are typically brighter than a billion suns, can be used. Many scientists believe these objects are powered by giant black holes feeding on nearby gas. Gas trapped in the black hole's powerful gravity is compressed and heated to millions of degrees, giving off intense light and/or radio energy.

Most quasars lurk¹¹ in the outer reaches of the cosmos¹², over a billion light years away, and are therefore distant enough to appear stationary¹³ to us. For comparison, a light year, the distance light travels in a year, is almost six trillion miles. Our entire galaxy¹⁴, consisting of hundreds of billions of stars, is about 100,000 light years across.

A collection of remote quasars, whose positions in the sky are precisely known, forms a map of celestial¹⁵ landmarks in which to orient the Earth. The first such map, called the International Celestial Reference Frame (ICRF), was completed in 1995. It was made over four years using painstaking¹⁶（辛苦的，小心的） analysis of observations on the positions of about 600 objects.

Ma led a three-year effort to update and improve the precision of the ICRF map by scientists affiliated¹⁷ with（与……结合） the International Very Long Baseline Interferometry Service for Geodesy and Astrometry (IVS) and the International Astronomical¹⁸ Union (IAU). Called ICRF2, it uses observations of approximately 3,000 quasars. It was officially recognized as the fundamental reference system for astronomy by the IAU in August, 2009.

Making such a map is not easy. Despite the brilliance¹⁹ of quasars, their extreme distance makes them too faint to be located accurately²⁰ with a conventional telescope that uses optical light (the light that we can see). Instead, a special network of radio telescopes is used, called a Very Long Baseline Interferometer (VLBI).

The larger the telescope, the better its ability to see fine detail, called spatial²¹ resolution（空间分辨率）. A VLBI network coordinates²² its observations to get the resolving power of a telescope as large as the network. VLBI networks have spanned continents and even entire hemispheres of the globe, giving the resolving power of a telescope thousands of miles in diameter. For ICRF2, the analysis of the VLBI observations reduced uncertainties²³ in position to angles as small as 40 microarcseconds, about the thickness of a 0.7 millimeter mechanical pencil lead in Los Angeles when viewed from Washington. This minimum uncertainty²⁴ is about five times better than the ICRF, according to Ma.

These networks are arranged on a yearly basis as individual radio telescope stations commit time to make coordinated²⁵ observations. Managing all these coordinated observations is a major effort by the IVS, according to Ma.

Additionally, the exquisite²⁶（精致的，细腻的） precision of VLBI networks makes them sensitive to many kinds of disturbances²⁷, called noise. Differences in atmospheric²⁸ pressure and humidity（湿度，湿气） caused by weather systems, flexing²⁹ of the Earth's crust due to tides, and shifting of antenna³⁰（触角，天线） locations from plate tectonics（板块结构学） and earthquakes all affect VLBI measurements. "A significant challenge was modeling all these disturbances in computers to take them into account and reduce the noise, or uncertainty, in our position observations," said Ma.

Another major source of noise is related to changes in the structure of the quasars themselves, which can be seen because of the extraordinary resolution of the VLBI networks, according to Ma.

The ICRF maps are not only useful for navigation on Earth; they also help us find our way in space -- the ICRF grid³¹ and some of the objects themselves are used to assist spacecraft navigation for interplanetary missions（星际任务）, according to Ma.

Despite its usefulness for things like GPS, the primary application for the ICRF maps is astronomy. Researchers use the ICRF maps as driving directions for telescopes. Objects are referenced with coordinates derived³² from the ICRF so that astronomers know where to find them in the sky.