Comoving distance

Part of a series on

Full-sky image derived from nine years' WMAP data

Early universe

Backgrounds
Inflation · Nucleosynthesis
Gravitational wave (GWB) Microwave (CMB) · Neutrino (CNB)

Expansion · Future

Components · Structure

Components
Lambda-CDM model Dark energy · Dark fluid · Dark matter
Structure
Shape of the universe Galaxy filament · Galaxy formation Large quasar group Large-scale structure Reionization · Structure formation

Experiments

Scientists

List of cosmologists

Subject history

Category
Cosmology portal
Astronomy portal

In standard cosmology, comoving distance and proper distance are two closely related distance measures used by cosmologists to define distances between objects. Proper distance roughly corresponds to where a distant object would be at a specific moment of cosmological time, which can change over time due to the expansion of the universe. Comoving distance factors out the expansion of the universe, giving a distance that does not change in time due to the expansion of space (though this may change due to other, local factors, such as the motion of a galaxy within a cluster). Comoving distance and proper distance are defined to be equal at the present time; therefore, the ratio of proper distance to comoving distance now is 1. At other times, the scale factor differs from 1. The Universe's expansion results in the proper distance changing, while the comoving distance is unchanged by this expansion because it is the proper distance divided by that scale factor.

Comoving coordinates

The evolution of the universe and its horizons in comoving distances

Although general relativity allows one to formulate the laws of physics using arbitrary coordinates, some coordinate choices are more natural or easier to work with. Comoving coordinates are an example of such a natural coordinate choice. They assign constant spatial coordinate values to observers who perceive the universe as isotropic. Such observers are called "comoving" observers because they move along with the Hubble flow.

A comoving observer is the only observer that will perceive the universe, including the cosmic microwave background radiation, to be isotropic. Non-comoving observers will see regions of the sky systematically blue-shifted or red-shifted. Thus isotropy, particularly isotropy of the cosmic microwave background radiation, defines a special local frame of reference called the comoving frame. The velocity of an observer relative to the local comoving frame is called the peculiar velocity of the observer.

Most large lumps of matter, such as galaxies, are nearly comoving, so that their peculiar velocities (owing to gravitational attraction) are low.

The comoving time coordinate is the elapsed time since the Big Bang according to a clock of a comoving observer and is a measure of cosmological time. The comoving spatial coordinates tell where an event occurs while cosmological time tells when an event occurs. Together, they form a complete coordinate system, giving both the location and time of an event.

Space in comoving coordinates is usually referred to as being "static", as most bodies on the scale of galaxies or larger are approximately comoving, and comoving bodies have static, unchanging comoving coordinates. So for a given pair of comoving galaxies, while the proper distance between them would have been smaller in the past and will become larger in the future due to the expansion of space, the comoving distance between them remains constant at all times.

The expanding Universe has an increasing scale factor which explains how constant comoving distances are reconciled with proper distances that increase with time.

Comoving distance and proper distance

Comoving distance is the distance between two points measured along a path defined at the present cosmological time. For objects moving with the Hubble flow, it is deemed to remain constant in time. The comoving distance from an observer to a distant object (e.g. galaxy) can be computed by the following formula:

\chi = \int_{t_e}^t c \; {\mbox{d} t' \over a(t')}

where a(t′) is the scale factor, t_e is the time of emission of the photons detected by the observer, t is the present time, and c is the speed of light in vacuum.

Despite being an integral over time, this does give the distance that would be measured by a hypothetical tape measure at fixed time t, i.e. the "proper distance" as defined below, divided by the scale factor a(t) at that time. For a derivation see "standard relativistic definitions" from Davis & Lineweaver 2004.^[1]

Definitions

Many textbooks use the symbol $\chi$ for the comoving distance. However, this $\chi$ must be distinguished from the coordinate distance $r$ in the commonly used comoving coordinate system for a FLRW universe where the metric takes the form

ds^{2}=-c^{2}d\tau ^{2}=-c^{2}dt^{2}+a(t)^{2}\left({\frac {dr^{2}}{1-kr^{2}}}+r^{2}\left(d\theta ^{2}+\sin ^{2}\theta d\phi ^{2}\right)\right)

In this case the comoving coordinate distance

r

is related to

\chi

by:^[2]^[3]^[4]

\chi ={\begin{cases}\sinh ^{-1}r,&{\text{if }}k=-1\ {\text{(a negatively curved ‘hyperbolic’ universe)}}\\r,&{\text{if }}k=0\ {\text{(a spatially flat universe)}}\\\sin ^{-1}r,&{\text{if }}k=1\ {\text{(a positively curved ‘spherical’ universe)}}\end{cases}}

Most textbooks and research papers define the comoving distance between comoving observers to be a fixed unchanging quantity independent of time, while calling the dynamic, changing distance between them proper distance. On this usage, comoving and proper distances are numerically equal at the current age of the universe, but will differ in the past and in the future; if the comoving distance to a galaxy is denoted $\chi$ , the proper distance $d(t)$ at an arbitrary time $t$ is simply given by $d(t)=a(t)\chi$ where $a(t)$ is the scale factor (e.g. Davis & Limeweaver 2004).^[1] The proper distance $d(t)$ between two galaxies at time t is just the distance that would be measured by rulers between them at that time.^[5]

Uses of the proper distance

The evolution of the universe and its horizons in proper distances

Cosmological time is identical to locally measured time for an observer at a fixed comoving spatial position, that is, in the local comoving frame. Proper distance is also equal to the locally measured distance in the comoving frame for nearby objects. To measure the proper distance between two distant objects, one imagines that one has many comoving observers in a straight line between the two objects, so that all of the observers are close to each other, and form a chain between the two distant objects. All of these observers must have the same cosmological time. Each observer measures their distance to the nearest observer in the chain, and the length of the chain, the sum of distances between nearby observers, is the total proper distance.^[6]

It is important to the definition of both comoving distance and proper distance in the cosmological sense (as opposed to proper length in special relativity) that all observers have the same cosmological age. For instance, if one measured the distance along a straight line or spacelike geodesic between the two points, observers situated between the two points would have different cosmological ages when the geodesic path crossed their own world lines, so in calculating the distance along this geodesic one would not be correctly measuring comoving distance or cosmological proper distance. Comoving and proper distances are not the same concept of distance as the concept of distance in special relativity. This can be seen by considering the hypothetical case of a universe empty of mass, where both sorts of distance can be measured. When the density of mass in the FLRW metric is set to zero (an empty 'Milne universe'), then the cosmological coordinate system used to write this metric becomes a non-inertial coordinate system in the Minkowski spacetime of special relativity where surfaces of constant Minkowski proper-time τ appear as hyperbolas in the Minkowski diagram from the perspective of an inertial frame of reference.^[7] In this case, for two events which are simultaneous according to the cosmological time coordinate, the value of the cosmological proper distance is not equal to the value of the proper length between these same events,^[8] which would just be the distance along a straight line between the events in a Minkowski diagram (and a straight line is a geodesic in flat Minkowski spacetime), or the coordinate distance between the events in the inertial frame where they are simultaneous.

If one divides a change in proper distance by the interval of cosmological time where the change was measured (or takes the derivative of proper distance with respect to cosmological time) and calls this a "velocity", then the resulting "velocities" of galaxies or quasars can be above the speed of light, c. This apparent superluminal expansion is not in conflict with special or general relativity, and is a consequence of the particular definitions used in cosmology. Even light itself does not have a "velocity" of c in this sense; the total velocity of any object can be expressed as the sum $v_{tot}=v_{rec}+v_{pec}$ where $v_{rec}$ is the recession velocity due to the expansion of the universe (the velocity given by Hubble's law) and $v_{pec}$ is the "peculiar velocity" measured by local observers (with $v_{rec}={\dot {a}}(t)\chi (t)$ and $v_{pec}=a(t){\dot {\chi }}(t)$ , the dots indicating a first derivative), so for light $v_{pec}$ is equal to c (-c if the light is emitted towards our position at the origin and +c if emitted away from us) but the total velocity $v_{tot}$ is generally different from c.^[1] Even in special relativity the coordinate speed of light is only guaranteed to be c in an inertial frame; in a non-inertial frame the coordinate speed may be different from c.^[9] In general relativity no coordinate system on a large region of curved spacetime is "inertial", but in the local neighborhood of any point in curved spacetime we can define a "local inertial frame" in which the local speed of light is c^[10] and in which massive objects such as stars and galaxies always have a local speed smaller than c. The cosmological definitions used to define the velocities of distant objects are coordinate-dependent - there is no general coordinate-independent definition of velocity between distant objects in general relativity.^[11] The issue of how best to describe and popularize the apparent superluminal expansion of the universe has caused a minor amount of controversy. One viewpoint is presented in Davis and Lineweaver, 2004.^[1]

Short distances vs. long distances

Within small distances and short trips, the expansion of the universe during the trip can be ignored. This is because the travel time between any two points for a non-relativistic moving particle will just be the proper distance (that is, the comoving distance measured using the scale factor of the universe at the time of the trip rather than the scale factor "now") between those points divided by the velocity of the particle. If the particle is moving at a relativistic velocity, the usual relativistic corrections for time dilation must be made.

References

1 2 3 4 T.M. Davis, C.H. Lineweaver (2004). "Expanding Confusion: Common Misconceptions of Cosmological Horizons and the Superluminal Expansion of the Universe". Publications of the Astronomical Society of Australia. 21 (1): 97–109. arXiv:astro-ph/0310808v2. Bibcode:2004PASA...21...97D. doi:10.1071/AS03040.
↑ Roos, Matts (2015). Introduction to Cosmology (4th ed.). John Wiley & Sons. p. 37. ISBN 978-1-118-92329-0. Extract of page 37 (see equation 2.39)
↑ Webb, Stephen (1999). Measuring the Universe: The Cosmological Distance Ladder (illustrated ed.). Springer Science & Business Media. p. 263. ISBN 978-1-85233-106-1. Extract of page 263
↑ Lachièze-Rey, Marc; Gunzig, Edgard (1999). The Cosmological Background Radiation (illustrated ed.). Cambridge University Press. p. 9-12. ISBN 978-0-521-57437-2. Extract of page 11
↑ see p. 4 of Distance Measures in Cosmology by David W. Hogg.
↑ Steven Weinberg, Gravitation and Cosmology (1972), p. 415
↑ See the diagram on p. 28 of Physical Foundations of Cosmology by V. F. Mukhanov, along with the accompanying discussion.
↑ E.L. Wright (2009). "Homogeneity and Isotropy". E.L. Wright. Retrieved February 2015. Check date values in: |access-date= (help)
↑ see p. 219 of Relativity and the Nature of Spacetime by Vesselin Petkov
↑ see p. 94 of An Introduction to the Science of Cosmology by Derek J. Raine, Edwin George Thomas, and E. G. Thomas
↑ J. Baez and E. Bunn (2006). "Preliminaries". University of California. Retrieved February 2015. Check date values in: |access-date= (help)

External links

This article is issued from Wikipedia - version of the 10/10/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.