Anasteroid spectral type is assigned toasteroids based on theirreflectance spectrum,color, and sometimesalbedo. These types are thought to correspond to an asteroid's surface composition. For small bodies that are notinternally differentiated, the surface and internal compositions are presumably similar, while large bodies such asCeres andVesta are known to have internal structure. Over the years, there has been a number of surveys that resulted in a set of different taxonomic systems such as theTholen,SMASS andBus–DeMeo classifications.[1]
In 1975, astronomersClark R. Chapman,David Morrison, and Ben Zellner developed a simple taxonomic system for asteroids based oncolor,albedo, andspectral shape. The three categories were labelled "C" for dark carbonaceous objects, "S" for stony (siliceous) objects, and "U" for those that did not fit into either C or S.[2] This basic division of asteroid spectra has since been expanded and clarified.[3] A number of classification schemes are currently in existence,[4] and while they strive to retain some mutual consistency, quite a few asteroids are sorted into different classes depending on the particular scheme. This is due to the use of different criteria for each approach. The two most widely used classifications are described below:
| Tholen Class | SMASSII (Bus Class) | Albedo | Spectral Features |
|---|---|---|---|
| A | A | moderate | Very steep red slope shortward of 0.75 μm; moderately deep absorption feature longward of 0.75 μm. |
| B,F | B | low | Linear, generally featureless spectra. Differences in UV absorption features and presence/absence of narrow absorption feature near 0.7 μm. |
| C,G | C, Cb, Ch, Cg, Chg | low | Linear, generally featureless spectra. Differences in UV absorption features and presence/absence of narrow absorption feature near 0.7 μm. |
| D | D | low | Relatively featureless spectrum with very steep red slope. |
| E,M,P | X, Xc, Xe, Xk | from low (P) to very high (E) | Generally featureless spectrum with reddish slope; differences in subtle absorption features and/or spectral curvature and/or peak relative reflectance. |
| Q | Q | moderate | Reddish slope shortward of 0.7 μm; deep, rounded absorption feature longward of 0.75 μm. |
| R | R | moderate | Moderate reddish slope downward of 0.7 μm; deep absorption longward of 0.75 μm. |
| S | S, Sa, Sk, Sl, Sq, Sr | moderate | Moderately steep reddish slope downward of 0.7 μm; moderate to steep absorption longward of 0.75 μm; peak of reflectance at 0.73 μm. Bus subgroups intermediate between S and A, K, L, Q, R classes. |
| T | T | low | Moderately reddish shortward of 0.75 μm; flat afterward. |
| V | V | moderate | Reddish shortward of 0.7 μm; extremely deep absorption longward of 0.75 μm. |
| — | K | moderate | Moderately steep red slope shortward of 0.75 μm; smoothly angled maximum and flat to blueish longward of 0.75 μm, with little or no curvature. |
| — | L, Ld | moderate | Very steep red slope shortward of 0.75 μm; flat longward of 0.75 μm; differences in peak level. |
| — | O | — | Peculiar trend, known so far for very few asteroids. |
TheSmall Solar System Objects Spectroscopic Survey (S3OS2or S3OS2, also known as theLazzaro classification) observed 820 asteroids, using the formerESO 1.52-metre telescope atLa Silla Observatory during 1996–2001.[1] This survey applied both the Tholen and Bus–Binzel (SMASS) taxonomy to the observed objects, many of which had previously not been classified. For the Tholen-like classification, the survey introduced a new "Caa-type", which shows a broad absorption band associated indicating an aqueous alteration of the body's surface. The Caa class corresponds to Tholen's C-type and to the SMASS' hydrated Ch-type (including some Cgh-, Cg-, and C-types), and was assigned to 106 bodies or 13% of the surveyed objects. In addition, S3OS2 uses the K-class for both classification schemes, a type which does not exist in the original Tholen taxonomy.[1]
The Bus-DeMeo classification is an asteroid taxonomic system designed byFrancesca DeMeo,Schelte Bus andStephen Slivan in 2009.[6] It is based on reflectance spectrum characteristics for 371 asteroids measured over the wavelength 0.45–2.45 micrometers. This system of 24 classes introduces a new "Sv"-type and is based upon aprincipal component analysis, in accordance with the SMASS taxonomy, which itself is based upon the Tholen classification.[6]
The most widely used taxonomy is that ofDavid J. Tholen, first proposed in 1984. This classification was developed from broad band spectra (between 0.31 μm and 1.06 μm) obtained during theEight-Color Asteroid Survey (ECAS) in the 1980s, in combination withalbedo measurements.[7] The original formulation was based on 978 asteroids. The Tholen scheme includes 14 types with the majority of asteroids falling into one of three broad categories, and several smaller types(also see§ Overview of Tholen and SMASS above). The types are, with their largest exemplars in parentheses:
The Tholen taxonomy may encompass up to four letters (e.g. "SCTU"). The classification scheme uses the letter "I" for "inconsistent" spectral data, and should not be confused with a spectral type. An example is the Themistian asteroid515 Athalia, which, at the time of classification was inconsistent, as the body's spectrum and albedo was that of a stony and carbonaceous asteroid, respectively.[8] When the underlying numerical color analysis was ambiguous, objects were assigned two or three types rather than just one (e.g. "CG" or "SCT"), whereby the sequence of types reflects the order of increasing numerical standard deviation, with the best fitting spectral type mentioned first.[8] The Tholen taxonomy also has additional notations, appended to the spectral type. The letter "U" is a qualifying flag, used for asteroids with an "unusual" spectrum, that falls far from the determined cluster center in the numerical analysis. The notation ":" (single colon) and "::" (two colons) are appended when the spectral data is "noisy" or "very noisy", respectively. For example, the Mars-crosser1747 Wright has an "AU:" class, which means that it is anA-type asteroid, though with an unusual and noisy spectrum.[8]
This is a more recent taxonomy introduced by American astronomersSchelte Bus andRichard Binzel in 2002, based on theSmall Main-Belt Asteroid Spectroscopic Survey (SMASS) of 1,447 asteroids.[9] This survey produced spectra of a far higher resolution than ECAS(seeTholen classification above), and was able to resolve a variety of narrow spectral features. However, a somewhat smaller range of wavelengths (0.44 μm to 0.92 μm) was observed. Also,albedos were not considered. Attempting to keep to the Tholen taxonomy as much as possible given the differing data, asteroids were sorted into the 26 types given below. As for the Tholen taxonomy, the majority of bodies fall into the three broad C, S, and X categories, with a few unusual bodies categorized into several smaller types(also see§ Overview of Tholen and SMASS above):
A significant number of small asteroids were found to fall in theQ,R, andV types, which were represented by only a single body in the Tholen scheme. In the Bus and Binzel SMASS scheme only a single type was assigned to any particular asteroid.[citation needed]
The characterization of an asteroid includes the measurement of itscolor indices derived from aphotometric system. This is done by measuring the object's brightness through a set of different, wavelength-specific filters, so-called passbands. In theUBV photometric system, which is also used tocharacterize distant objects in addition to classical asteroids, the three basic filters are:
| Colors | violet | blue | cyan | green | yellow | orange | red |
|---|---|---|---|---|---|---|---|
| Wavelengths | 380–450 nm | 450–495 nm | 495–520 nm | 520–570 nm | 570–590 nm | 590–620 nm | 620–750 nm |
In an observation, the brightness of an object is measured twice through a different filter. The resulting difference in magnitude is called thecolor index. For asteroids, the U−B or B−V color indices are the most common ones. In addition, the V−R, V−I and R−I indices, where thephotometric letters stand forvisible (V), red (R) andinfrared (I), are also used. A photometric sequence such as V–R–B–I can be obtained from observations within a few minutes.[10]
| Groups | Color index | |||
|---|---|---|---|---|
| B−V | V−R | V−I | R−I | |
| Plutinos | 0.895±0.190 | 0.568±0.106 | 1.095±0.201 | 0.536±0.135 |
| Cubewanos | 0.973±0.174 | 0.622±0.126 | 1.181±0.237 | 0.586±0.148 |
| Centaurs | 0.886±0.213 | 0.573±0.127 | 1.104±0.245 | 0.548±0.150 |
| SDOs | 0.875±0.159 | 0.553±0.132 | 1.070±0.220 | 0.517±0.102 |
| Comets | 0.795±0.035 | 0.441±0.122 | 0.935±0.141 | 0.451±0.059 |
| Jupiter trojans | 0.777±0.091 | 0.445±0.048 | 0.861±0.090 | 0.416±0.057 |
These classification schemes are expected to be refined and/or replaced as further research progresses. However, for now the spectral classification based on the two above coarse resolution spectroscopic surveys from the 1990s is still the standard. Scientists have been unable to agree on a better taxonomic system, largely due to the difficulty of obtaining detailed measurements consistently for a large sample of asteroids (e.g. finer resolution spectra, or non-spectral data such as densities would be very useful).[citation needed]
Some groupings of asteroids have been correlated withmeteorite types:[citation needed]
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