Nowadays we use just this method to measure distances precisely, because we can measure time more accurately than length. In effect, the meter is defined to be the distance traveled by light in 0.000000003335640952 second, as measured by a cesium clock. (The reason for that particular number is that it corresponds to the historical definition of the meter - in terms of two marks on a particular platinum bar kept in Paris.) Equally, we can use a more convenient, new unit of length called a light-second. This is simply defined as the distance that light travels in one second. In the theory of relativity, we now define distance in terms of time and the speed of light, so it follows automatically that every observer will measure light to have the same speed (by definition, 1 meter per 0.000000003335640952 second). There is no need to introduce the idea of an ether, whose presence anyway cannot be detected, as the Michelson-Morley experiment showed. The theory of relativity does, however, force us to change fundamentally our ideas of space and time. We must accept that time is not completely separate from and independent of space, but is combined with it to form an object called space-time.
It is a matter of common experience that one can describe the position of a point in space by three numbers, or coordinates. For instance, one can say that a point in a room is seven feet from one wall, three feet from another, and five feet above the floor. Or one could specify that a point was at a certain latitude and longitude and a certain height above sea level. One is free to use any three suitable coordinates, although they have only a limited range of validity. One would not specify the position of the moon in terms of miles north and miles west of Piccadilly Circus and feet above sea level. Instead, one might describe it in terms of distance from the sun, distance from the plane of the orbits of the planets, and the angle between the line joining the moon to the sun and the line joining the sun to a nearby star such as Alpha Centauri.
Even these coordinates would not be of much use in describing the position of the sun in our galaxy or the position of our galaxy in the local group of galaxies. In fact, one may describe the whole universe in terms of a collection of overlapping patches. In each patch, one can use a different set of three coordinates to specify the position of a point.
Coordinate 座標
現在我們正是用這種方法來準確地測量距離，因為我們可以比測量長度更為準確地測量時間。實際上，米是被定義為光在以鉑原子鐘測量的0.000000003335640952秒內走過的距離（取這個特別的數字的原因是，因為它對應於歷史上的米的定義——按照保存在巴黎的特定鉑棒上的兩個刻度之間的距離）。同樣，我們可以用叫做光秒的更方便更新的長度單位，這就是簡單地定義為光在一秒走過的距離。現在，我們在相對論中按照時間和光速來定義距離，這樣每個觀察者都自動地測量出同樣的光速（按照定義為每0. 000000003335640952秒之1米）。沒有必要引入以太的觀念，正如麥克爾遜——莫雷實驗顯示的那樣，以太的存在是無論如何檢測不到的。然而，相對論迫使我們從根本上改變了對時間和空間的觀念。我們必須接受的觀念是：時間不能完全脫離和獨立於空間，而必須和空間結合在一起形成所謂的時空的客體。
我們通常的經驗是可以用三個數或座標去描述空間中的一點的位置。譬如，人們可以說屋子裡的一點是離開一堵牆7英尺（1英尺=0.3048米），離開另一堵牆3英尺（1英尺=0.3048米），並且比地面高5英尺（1英尺=0.3048米）。人們也可以用一定的緯度、經度和海拔來指定該點。人們可以自由地選用任何三個合適的座標，雖然它們只在有限的範圍內有效。人們不是按照在倫敦皮卡迪裡圓環以北和以西多少英里（1英里=1.609公里）以及高於海平面多少英尺（1英尺=0.3048米）來指明月亮的位置，而是用離開太陽、離開行星軌道面的距離以及月亮與太陽的連線和太陽與臨近的一個恆星——例如α-半人馬座——連線之夾角來描述之。
甚至這些座標對於描寫太陽在我們星系中的位置，或我們星系在局部星系群中的位置也沒有太多用處。事實上，人們可以用一族互相交迭的座標碎片來描寫整個宇宙。在每一碎片中，人們可用不同的三個座標的集合來指明點的位置。
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