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{{Gravitational Lensing}}
In [[statistics]], the '''score''', '''score function''', '''efficient score'''<ref name=Cox1>Cox & Hinkley (1974), p 107</ref> or '''informant'''<ref>{{SpringerEOM| title=Informant |id=i/i051030 |first=N.N. |last=Chentsov}}</ref> indicates how sensitively a [[likelihood function]] <math>L(\theta; X)</math> depends on its [[parametric model|parameter]] <math>\theta</math>. Explicitly, the score for <math>\theta</math> is the [[gradient]] of the log-likelihood with respect to <math>\theta</math>.
[[Image:Einstein Rings.jpg|thumb||Some observed Einstein rings]]
In observational [[astronomy]] an '''Einstein ring''' is the deformation of the light from a source (such as a [[galaxy]] or [[star]]) into a ring through [[gravitational lens]]ing of the source's light by an object with an extremely large mass (such as another galaxy, or a [[black hole]]). This occurs when the source, lens and observer are all aligned. The first complete Einstein ring, designated B1938+666, was discovered by collaboration between astronomers at the [[University of Manchester]] and [[Nasa|NASA's]] [[Hubble Space Telescope]] in 1998.<ref>{{cite web | url=http://www.merlin.ac.uk/press/PR9801/press.html | title=A Bull's Eye for MERLIN and the Hubble | publisher=University of Manchester | date=27 March 1998}}</ref>


== Introduction ==
The score plays an important role in several aspects of [[statistical inference|inference]]. For example:
Gravitational lensing is predicted by [[Albert Einstein]]'s theory of [[general relativity]]. Instead of light from a source traveling in a straight line (in three dimensions), it is bent by the presence of a massive body, which distorts [[spacetime]]. An Einstein Ring is a special case of gravitational lensing, caused by the exact alignment of the source, lens and observer. This results in a symmetry around the lens, causing a ring-like structure.
:*in formulating a [[test statistic]] for a locally most powerful test;<ref>Cox & Hinkley (1974), p 113</ref>
:*in approximating the error in a [[maximum likelihood]] estimate;<ref name="Cox & Hinkley 1974, p 295">Cox & Hinkley (1974), p 295</ref>
:*in demonstrating the asymptotic sufficiency of a [[maximum likelihood]] estimate;<ref name="Cox & Hinkley 1974, p 295"/>
:*in the formulation of [[confidence interval]]s;<ref>Cox & Hinkley (1974), p 222–3</ref>
:*in demonstrations of the [[Cramér–Rao bound|Cramér–Rao inequality]].<ref>Cox & Hinkley (1974), p 254</ref>


[[Image:Gravitational lens geometry.svg|thumb|The geometry of a gravitational lens]]
The score function also plays an important role in [[computational statistics]], as it can play a part in the computation of
The size of an Einstein ring is given by the [[Einstein radius]]. In [[radians]], it is
maximum likelihood estimates.


:<math>\theta_E = \sqrt{\frac{4GM}{c^2}\;\frac{d_{LS}}{d_L d_S}},</math>
==Definition==


where
The score or efficient score <ref name="Cox1"/> is the [[gradient]] (the vector of [[partial derivative]]s), with respect to some parameter <math>\theta</math>, of the [[logarithm]] (commonly the [[natural logarithm]]) of the [[likelihood function]] (the log-likelihood).
If the observation is <math>X</math> and its likelihood is <math>L(\theta;X)</math>, then the score <math>V</math> can be found through the [[chain rule]]:


: <math>G</math> is the [[gravitational constant]],
:<math>
: <math>M</math> is the mass of the lens,
V \equiv V(\theta, X)
: <math>c</math> is the [[speed of light]],
=
: <math>d_L</math> is the [[angular diameter distance]] to the lens,
\frac{\partial}{\partial\theta} \log L(\theta;X)
: <math>d_S</math> is the [[angular diameter distance]] to the source, and
=
: <math>d_{LS}</math> is the [[angular diameter distance]] between the lens and the source.
\frac{1}{L(\theta;X)} \frac{\partial L(\theta;X)}{\partial\theta}.
</math>


Note that, over cosmological distances <math>d_{LS}\ne d_S-d_L</math> in general.
Thus the score <math>V</math> indicates the [[Sensitivity analysis|sensitivity]] of <math>L(\theta;X)</math> (its derivative normalized by its value). Note that <math>V</math> is a function of <math>\theta</math> and the observation <math>X</math>, so that, in general, it is not a [[statistic]]. However in certain applications, such as the [[score test]], the score is evaluated at a specific value of <math>\theta</math> (such as a null-hypothesis value, or at the maximum likelihood estimate of  <math>\theta</math>), in which case the result is a statistic.


== History ==
In older literature, the term "linear score" may be used to refer to the score with respect to infintesimal translation of a given density. This convention arises from a time when the primary parameter of interest was the mean or median of a distribution. In this case, the likelihood of an observation is given by a density of the form <math>L(\theta;X)=f(X+\theta)</math>. The "linear score" is then defined as
The bending of light by a gravitational body was predicted by Einstein in 1912, a few years before the publication of General Relativity in 1916 (see Renn et al. 1997). The ring effect was first mentioned in [[academic journal|academic literature]] by [[Orest Chwolson]] in 1924. [[Albert Einstein]] remarked upon this effect in 1936 in a paper prompted by a letter by a Czech engineer, R W Mandl [http://www.slac.stanford.edu/pubs/beamline/31/1/31-1-maurer.pdf], but stated
{{quote|Of course, there is no hope of observing this phenomenon directly. First, we shall scarcely ever approach closely enough to such a central line. Second, the angle β will defy the resolving power of our instruments.|''Science'' vol 84 p 506 1936}}
In this statement, β is the Einstein Radius currently denoted by <math>\theta_E</math> (see above). However, Einstein was only considering the chance of observing Einstein rings produced by stars, which is low; however, the chance of observing those produced by larger lenses such as galaxies or black holes is higher since the angular size of an Einstein ring increases with the mass of the lens.


=== Known Einstein rings ===
:<math>
Hundreds of gravitational lenses are currently known. About half a dozen of them are partial Einstein rings with diameters up to an [[arcsecond]], although as either the mass distribution of the lenses is not perfectly axially symmetrical, or the source, lens and observer are not perfectly aligned, we have yet to see a perfect Einstein ring. Most rings have been discovered in the radio range.
V_{\rm linear}
=
\frac{\partial}{\partial X} \log f(X)
</math>


The first Einstein ring was discovered by Hewett et al. (1988), who observed the radio source MG1131+0456 using the [[Very Large Array]].<ref>{{cite web | url=http://www.nrao.edu/pr/2000/vla20/background/ering/ | title=Discovery of the First "Einstein Ring" Gravitational Lens | publisher=[[NRAO]] | date=2000 | accessdate=2012-02-08}}</ref> The first complete Einstein ring to be discovered was B1938+666, which was found by King et al. (1998) via optical follow-up with the Hubble Space Telescope of a gravitational lens imaged with [[MERLIN]].<ref>{{cite web | url=http://www.merlin.ac.uk/press/PR9801/press.html | title=A Bull's Eye for MERLIN and the Hubble | publisher=University of Manchester | date=27 March 1998}}</ref><ref>{{cite news| url=http://query.nytimes.com/gst/fullpage.html?res=9906EFDF103BF932A05750C0A96E958260 | work=The New York Times | title='Einstein Ring' Caused by Space Warping Is Found | first=Malcolm W. | last=Browne | date=1998-03-31 | accessdate=2010-05-01}}</ref>
==Properties==
===Mean===
Under some regularity conditions, the [[expected value]] of <math>V</math> with respect to the observation <math>x</math>, given <math>\theta</math>, written <math>\mathbb{E}(V\mid\theta)</math>, is zero.
To see this rewrite the likelihood function L as a [[probability density function]] <math>L(\theta; x) = f(x; \theta)</math>. Then:


{| class="wikitable"
:<math>
! Name
\mathbb{E}(V\mid\theta)
! Location ([[Right ascension|RA]], [[Declination|dec]])
=\int_{-\infty}^{+\infty}
! Radius
f(x; \theta) \frac{\partial}{\partial\theta} \log L(\theta;X)
! Arc size
\,dx
! [[Optical]]/[[radio frequency|radio]]
=\int_{-\infty}^{+\infty}
! Discovery
\frac{\partial}{\partial\theta} \log L(\theta;X) f(x; \theta) \, dx
|-
</math>
| [[FOR J0332-3557]]
| 03<sup>h</sup>:32<sup>m</sup>:59<sup>s</sup>:94, -35°57'51".7, [[J2000]]
| 1".48
| Partial, 260°
| Radio
| Cabanac (2005)
|-
| [[SDSSJ0946+1006]]
| 09<sup>h</sup> 46<sup>m</sup> 56.<sup>s</sup>68, +10° 06' 52."6 [[J2000]]
|
|
| Optical
| Gavazzi (2008)
|-  
| [[MG1131 + 0456]]
|
|
|
|
|
|}


{{Expand section|date=June 2008}}
:<math>
=\int_{-\infty}^{+\infty}
\frac{1}{f(x; \theta)}\frac{\partial f(x; \theta)}{\partial \theta}f(x; \theta)\, dx
=\int_{-\infty}^{+\infty} \frac{\partial f(x; \theta)}{\partial \theta} \, dx
</math>


== Extra rings ==
If certain differentiability conditions are met (see [[Leibniz integral rule]]), the integral may be rewritten as
[[Image:SDSSJ0946+1006.jpg|thumb|left|SDSSJ0946+1006 is a Double Einstein Ring. Credit: [[Hubble Space Telescope|HST]]/[[NASA]]/[[ESA]]]]


Using the [[Hubble Space Telescope]], a double ring has been found by [[Raphael Gavazzi]] of the [[STScI]] and [[Tommaso Treu]] of the [[University of California, Santa Barbara]]. This arises from the light from three galaxies at distances of 3, 6 and 11 billion light years. Such rings help in understanding the distribution of [[dark matter]], [[dark energy]], the nature of distant [[galaxies]], and the [[curvature of the universe]]. The odds of finding such a double ring are 1 in 10,000. Sampling 50 suitable double rings would provide astronomers with a more accurate measurement of the dark matter content of the universe and the equation of state of the dark energy to within 10 percent precision.<ref>{{cite web |url=http://hubblesite.org/newscenter/archive/releases/2008/04/full/ |title=Hubble Finds Double Einstein Ring |accessdate=2008-01-26 |work=http://hubblesite.org |publisher=Space Telescope Science Institute }}</ref>
:<math>
\frac{\partial}{\partial\theta} \int_{-\infty}^{+\infty}
f(x; \theta) \, dx
=
\frac{\partial}{\partial\theta}1 = 0.
</math>


=== A simulation ===
It is worth restating the above result in words: the expected value of the score is zero.
[[Image:EnsteinRingZoomOptimised.gif|thumb|Einstein rings near a black hole]]
Thus, if one were to repeatedly sample from some distribution, and repeatedly calculate the score, then the mean value of the scores would tend to zero as the number of repeat samples approached infinity.
To the right is a simulation depicting a zoom on a [[Schwarzschild metric|Schwarzschild black hole]] in front of the [[Milky Way]]. The first Einstein ring corresponds to the most distorted region of the picture and is clearly depicted by the [[Disc (galaxy)|galactic disc]]. The zoom then reveals a series of 4 extra rings, increasingly thinner and closer to the black hole shadow. They are easily seen through the multiple images of the galactic disk.  The odd-numbered rings correspond to points which are behind the black hole (from the observer's position) and correspond here to the bright yellow region of the galactic disc (close to the galactic center), whereas the even-numbered rings correspond to images of objects which are behind the observer, which appear bluer since the corresponding part of the galactic disc is thinner and hence dimmer here.
{{clearleft}}


== See also ==
===Variance===
* [[Einstein cross]]
{{Main|Fisher information}}
* [[Einstein radius]]
The variance of the score is known as the [[Fisher information]] and is written <math>\mathcal{I}(\theta)</math>.  Because the expectation of the score is zero, this may be written as
* [[Gravitational lens]]


== References ==
:<math>
{{reflist}}
\mathcal{I}(\theta)
=
\mathbb{E}
\left\{\left.
\left[
  \frac{\partial}{\partial\theta} \log L(\theta;X)
\right]^2
\right|\theta\right\}.
</math>


=== Journals ===
Note that the Fisher information, as defined above, is not a function of any particular observation, as the random variable <math>X</math> has been averaged out.
<div class="references-small">
This concept of information is useful when comparing two methods of observation of some [[random process]].
* {{cite journal | first = R. A. | last = Cabanac | coauthors = et al. | title = Discovery of a high-redshift Einstein ring | year = 2005 | journal = Astronomy and Astrophysics. | volume = 436 | issue = 2 | pages = L21–L25 | url = http://www.arxiv.org/astro-ph/0504585 | doi = 10.1051/0004-6361:200500115 | bibcode=2005A&A...436L..21C|arxiv = astro-ph/0504585 }} (refers to FOR J0332-3357)
* {{cite journal | first = O | last = Chwolson | title = Über eine mögliche Form fiktiver Doppelsterne | journal = Astronomische Nachrichten | volume = 221 | issue = 20 | pages = 329 | year = 1924 | bibcode = 1924AN....221..329C | doi = 10.1002/asna.19242212003}} (The first paper to propose rings)
* {{cite journal | first = Albert | last = Einstein | authorlink = Albert Einstein | title = Lens-like Action of a Star by the Deviation of Light in the Gravitational Field | journal = Science | volume = 84 | pages = 506–507 | year = 1936 | url = http://www.to.infn.it/~zaninett/projects/storia/einstein1936.pdf | doi = 10.1126/science.84.2188.506 | pmid = 17769014 | issue = 2188|bibcode = 1936Sci....84..506E }} (The famous Einstein Ring paper)
* {{cite journal | first=J | last=Hewitt | title=Unusual radio source MG1131+0456 - A possible Einstein ring | journal=Nature | volume=333 | pages=537 | year=1988 | bibcode=1988Natur.333..537H|doi = 10.1038/333537a0 }}
* {{cite journal | first = Jurgen | last = Renn | coauthors = Tilman Sauer and John Stachel | title =The Origin of Gravitational Lensing: A Postscript to Einstein's 1936 Science paper | journal = Science | volume = 275 | pages = 184–186 | year = 1997 | doi = 10.1126/science.275.5297.184 | pmid =8985006 | issue = 5297|bibcode = 1997Sci...275..184R }}
* {{cite journal | first=L | last=King | title=A complete infrared Einstein ring in the gravitational lens system B1938 + 666 | journal=MNRAS | volume = 295 | pages=41 | year=1998 | bibcode=1998MNRAS.295L..41K|arxiv = astro-ph/9710171 |doi = 10.1046/j.1365-8711.1998.295241.x }}
</div>


=== News ===
==Examples==
<div class="references-small">
* {{cite news | url = http://www.universetoday.com/am/publish/perfect_einstein_ring.html | title = Nearly perfect Einstein ring discovered | publisher = Universe Today | first = Jeff | last = Barbour | date = 2005-04-29 | accessdate = 2006-06-15}} (refers to FOR J0332-3357)


* {{cite news | url = http://www.sciencedaily.com/releases/2008/01/080110102319.htm | title = Hubble Finds Double Einstein Ring | publisher = Science Daily | date = 2008-01-12 | accessdate = 2008-01-14}}
===Bernoulli process===
</div>


== Further reading ==
Consider a [[Bernoulli process]], with ''A'' successes and ''B'' failures; the probability of success is&nbsp;''θ''.
* {{cite journal | first = C.S. | last = Kochanek | coauthors = C.R. Keeton and B.A. McLeod | title = The Importance of Einstein Rings | journal = The Astrophysical Journal | year = 2001 | volume = 547 | issue = 1 | pages = 50–59 | arxiv = astro-ph/0006116 | doi = 10.1086/318350 | bibcode=2001ApJ...547...50K}}


{{Commons category|Einstein Rings}}
Then the likelihood ''L'' is


{{DEFAULTSORT:Einstein Ring}}
:<math>
[[Category:Effects of gravitation]]
L(\theta;A,B)=\frac{(A+B)!}{A!B!}\theta^A(1-\theta)^B,</math>
[[Category:Albert Einstein|Ring]]
[[Category:Optical phenomena]]
[[Category:Gravitational lensing]]


[[ar:حلقة آينشتاين]]
so the score ''V'' is
[[cs:Einsteinův prstýnek]]
 
[[de:Einsteinring]]
:<math>
[[es:Anillo de Einstein]]
V=\frac{1}{L}\frac{\partial L}{\partial\theta} = \frac{A}{\theta}-\frac{B}{1-\theta}.
[[gl:Anel de Einstein]]
</math>
[[ko:아인슈타인 링]]
 
[[hu:Einstein-gyűrű]]
We can now verify that the expectation of the score is zero.  Noting that the expectation of ''A'' is ''n''θ and the expectation of ''B'' is ''n''(1&nbsp;&minus;&nbsp;θ) [recall that ''A'' and ''B'' are random variables], we can see that the expectation of ''V'' is
[[nl:Einsteinring]]
 
[[pl:Pierścień Einsteina]]
:<math>
[[sk:Einsteinov prsteň]]
E(V)
[[sl:Einsteinov obroč]]
= \frac{n\theta}{\theta} - \frac{n(1-\theta)}{1-\theta}
[[sv:Einsteinring]]
= n - n
[[uk:Кільця Ейнштейна]]
= 0.
[[zh:愛因斯坦環]]
</math>
 
We can also check the variance of <math>V</math>.  We know that ''A'' + ''B'' = ''n'' (so ''B'' =&nbsp;''n''&nbsp;&minus;&nbsp;''A'') and the variance of ''A'' is ''n''θ(1&nbsp;&minus;&nbsp;θ) so the variance of ''V'' is
 
:<math>
\begin{align}
\operatorname{var}(V) & =\operatorname{var}\left(\frac{A}{\theta}-\frac{n-A}{1-\theta}\right)
=\operatorname{var}\left(A\left(\frac{1}{\theta}+\frac{1}{1-\theta}\right)\right) \\
& =\left(\frac{1}{\theta}+\frac{1}{1-\theta}\right)^2\operatorname{var}(A)
=\frac{n}{\theta(1-\theta)}.
\end{align}
</math>
 
===Binary outcome model===
 
For models with binary outcomes (''Y'' = 1 or 0), the model can be scored with the logarithm of predictions
 
<math> S = Y \log( p ) + ( Y - 1 ) ( \log( 1 - p ) ) </math>
 
where ''p'' is the probability in the model to be estimated and ''S'' is the score.<ref name=Steyerberg2010>Steyerberg EW, Vickers AJ, Cook NR, Gerds T, Gonen M,  Obuchowski N, Pencina MJ and Kattan MW (2010) Assessing the performance of prediction models. A framework for traditional and novel measures. Epidemiology 21 (1) 128–138 [[DOI: 10.1097/EDE.0b013e3181c30fb2]]</ref>
 
==Applications==
===Scoring algorithm===
{{Main|Scoring algorithm}}
The scoring algorithm is an iterative method for numerically determining the [[maximum likelihood]] [[estimator]].
 
===Score test===
{{Main|Score test}}
{{Expand section|date=December 2009}}
 
==See also==
*[[Fisher information]]
*[[Information theory]]
*[[Score test]]
*[[Scoring algorithm]]
*[[Support curve]]
 
==Notes==
{{Reflist}}
==References==
*Cox, D.R., Hinkley, D.V. (1974) ''Theoretical Statistics'', Chapman & Hall. ISBN 0-412-12420-3
*{{cite book
| last = Schervish
| first = Mark J.
| title = Theory of Statistics
| publisher =Springer
| date =1995
| location =New York
| pages = Section 2.3.1
| isbn = 0-387-94546-6
| nopp = true}}
 
[[Category:Estimation theory]]

Revision as of 10:14, 12 August 2014

In statistics, the score, score function, efficient score[1] or informant[2] indicates how sensitively a likelihood function L(θ;X) depends on its parameter θ. Explicitly, the score for θ is the gradient of the log-likelihood with respect to θ.

The score plays an important role in several aspects of inference. For example:

The score function also plays an important role in computational statistics, as it can play a part in the computation of maximum likelihood estimates.

Definition

The score or efficient score [1] is the gradient (the vector of partial derivatives), with respect to some parameter θ, of the logarithm (commonly the natural logarithm) of the likelihood function (the log-likelihood). If the observation is X and its likelihood is L(θ;X), then the score V can be found through the chain rule:

VV(θ,X)=θlogL(θ;X)=1L(θ;X)L(θ;X)θ.

Thus the score V indicates the sensitivity of L(θ;X) (its derivative normalized by its value). Note that V is a function of θ and the observation X, so that, in general, it is not a statistic. However in certain applications, such as the score test, the score is evaluated at a specific value of θ (such as a null-hypothesis value, or at the maximum likelihood estimate of θ), in which case the result is a statistic.

In older literature, the term "linear score" may be used to refer to the score with respect to infintesimal translation of a given density. This convention arises from a time when the primary parameter of interest was the mean or median of a distribution. In this case, the likelihood of an observation is given by a density of the form L(θ;X)=f(X+θ). The "linear score" is then defined as

Vlinear=Xlogf(X)

Properties

Mean

Under some regularity conditions, the expected value of V with respect to the observation x, given θ, written 𝔼(Vθ), is zero. To see this rewrite the likelihood function L as a probability density function L(θ;x)=f(x;θ). Then:

𝔼(Vθ)=+f(x;θ)θlogL(θ;X)dx=+θlogL(θ;X)f(x;θ)dx
=+1f(x;θ)f(x;θ)θf(x;θ)dx=+f(x;θ)θdx

If certain differentiability conditions are met (see Leibniz integral rule), the integral may be rewritten as

θ+f(x;θ)dx=θ1=0.

It is worth restating the above result in words: the expected value of the score is zero. Thus, if one were to repeatedly sample from some distribution, and repeatedly calculate the score, then the mean value of the scores would tend to zero as the number of repeat samples approached infinity.

Variance

Mining Engineer (Excluding Oil ) Truman from Alma, loves to spend time knotting, largest property developers in singapore developers in singapore and stamp collecting. Recently had a family visit to Urnes Stave Church. The variance of the score is known as the Fisher information and is written (θ). Because the expectation of the score is zero, this may be written as

(θ)=𝔼{[θlogL(θ;X)]2|θ}.

Note that the Fisher information, as defined above, is not a function of any particular observation, as the random variable X has been averaged out. This concept of information is useful when comparing two methods of observation of some random process.

Examples

Bernoulli process

Consider a Bernoulli process, with A successes and B failures; the probability of success is θ.

Then the likelihood L is

L(θ;A,B)=(A+B)!A!B!θA(1θ)B,

so the score V is

V=1LLθ=AθB1θ.

We can now verify that the expectation of the score is zero. Noting that the expectation of A is nθ and the expectation of B is n(1 − θ) [recall that A and B are random variables], we can see that the expectation of V is

E(V)=nθθn(1θ)1θ=nn=0.

We can also check the variance of V. We know that A + B = n (so Bn − A) and the variance of A is nθ(1 − θ) so the variance of V is

var(V)=var(AθnA1θ)=var(A(1θ+11θ))=(1θ+11θ)2var(A)=nθ(1θ).

Binary outcome model

For models with binary outcomes (Y = 1 or 0), the model can be scored with the logarithm of predictions

S=Ylog(p)+(Y1)(log(1p))

where p is the probability in the model to be estimated and S is the score.[7]

Applications

Scoring algorithm

Mining Engineer (Excluding Oil ) Truman from Alma, loves to spend time knotting, largest property developers in singapore developers in singapore and stamp collecting. Recently had a family visit to Urnes Stave Church. The scoring algorithm is an iterative method for numerically determining the maximum likelihood estimator.

Score test

Mining Engineer (Excluding Oil ) Truman from Alma, loves to spend time knotting, largest property developers in singapore developers in singapore and stamp collecting. Recently had a family visit to Urnes Stave Church. Template:Expand section

See also

Notes

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References

  • Cox, D.R., Hinkley, D.V. (1974) Theoretical Statistics, Chapman & Hall. ISBN 0-412-12420-3
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  1. 1.0 1.1 Cox & Hinkley (1974), p 107
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  3. Cox & Hinkley (1974), p 113
  4. 4.0 4.1 Cox & Hinkley (1974), p 295
  5. Cox & Hinkley (1974), p 222–3
  6. Cox & Hinkley (1974), p 254
  7. Steyerberg EW, Vickers AJ, Cook NR, Gerds T, Gonen M, Obuchowski N, Pencina MJ and Kattan MW (2010) Assessing the performance of prediction models. A framework for traditional and novel measures. Epidemiology 21 (1) 128–138 DOI: 10.1097/EDE.0b013e3181c30fb2