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<h2>Spacelike Showers</h2>

The PYTHIA algorithm for spacelike initial-state showers is 
based on the article [<a href="Bibliography.html" target="page">Sjo05</a>], where a 
transverse-momentum-ordered backwards evolution scheme is introduced, 
with the extension to fully interleaved evolution covered in 
[<a href="Bibliography.html" target="page">Cor10a</a>]. 
This algorithm is a further development of the virtuality-ordered one 
presented in [<a href="Bibliography.html" target="page">Sj085</a>], with matching to first-order matrix 
element for <i>Z^0</i>, <i>W^+-</i> and Higgs (in the 
<i>m_t -> infinity</i> limit) production as introduced in 
[<a href="Bibliography.html" target="page">Miu99</a>]. 

<p/>
The normal user is not expected to call <code>SpaceShower</code> 
directly, but only have it called from <code>Pythia</code>, 
via <code>PartonLevel</code>. Some of the parameters below, 
in particular <code>SpaceShower:alphaSvalue</code>, 
would be of interest for a tuning exercise, however. 

<h3>Main variables</h3>

The maximum <i>pT</i> to be allowed in the shower evolution is
related to the nature of the hard process itself. It involves a
delicate balance between not double-counting and not leaving any
gaps in the coverage. The best procedure may depend on information 
only the user has: how the events were generated and mixed (e.g. with 
Les Houches Accord external input), and how they are intended to be 
used. Therefore a few options are available, with a sensible default 
behaviour.

<p/><code>mode&nbsp; </code><strong> SpaceShower:pTmaxMatch &nbsp;</strong> 
 (<code>default = <strong>0</strong></code>; <code>minimum = 0</code>; <code>maximum = 2</code>)<br/>
Way in which the maximum shower evolution scale is set to match the 
scale of the hard process itself.
<br/><code>option </code><strong> 0</strong> : <b>(i)</b> if the final state of the hard process 
(not counting subsequent resonance decays) contains at least one quark 
(<i>u, d, s, c ,b</i>), gluon or photon then <i>pT_max</i> 
is chosen to be the factorization scale for internal processes 
and the <code>scale</code> value for Les Houches input; 
<b>(ii)</b> if not, emissions are allowed to go all the way up to 
the kinematical limit. 
The reasoning is that in the former set of processes the ISR
emission of yet another quark, gluon or photon could lead to
double-counting, while no such danger exists in the latter case.
  
<br/><code>option </code><strong> 1</strong> : always use the factorization scale for an internal
process and the <code>scale</code> value for Les Houches input, 
i.e. the lower value. This should avoid double-counting, but
may leave out some emissions that ought to have been simulated.
(Also known as wimpy showers.)
  
<br/><code>option </code><strong> 2</strong> : always allow emissions up to the kinematical limit.
This will simulate all possible event topologies, but may lead to
double-counting. 
(Also known as power showers.)
  
<br/><b>Note 1:</b> Some processes contain matrix-element matching
to the first emission; this is the case notably for single 
<i>gamma^*/Z^0, W^+-</i> and <i>H^0</i> production. Then default
and option 2 give the correct result, while option 1 should never
be used. 
<br/><b>Note 2:</b> as enumerated in the text, these options take effect 
both for internal and external processes. Whether a particular option
makes sense depends on the context. For instance, if events for the same
basic process to different orders are to be matched, then option 1 would
be a reasonable first guess. But in more sophisticated descriptions 
option 2 could be combined with <code>UserHooks</code> vetoes on emissions 
that would lead to double-counting, using more flexible phase space 
boundaries. Option 0, finally, may be most realistic when only Born-level 
processes are involved, possibly in combination with a nonzero  
<code>SpaceShower:pTdampMatch</code>. The rules used for avoiding 
double-counting are not foolproof, however. As an example, for the 
<i>t</i>-channel process <i>gamma gamma -> e^+ e^-</i> its <i>pT</i> 
scale is the plausible upper shower limit, with only dampened emissions 
above it. But the initial state is not checked and, had only incoming 
quarks and gluons been taken into account, only the <i>s</i>-channel 
process <i>q qbar -> gamma^*/Z^0 -> e^+ e^-</i> would have been possible,
where indeed the whole phase space should be populated. So this is 
erroneously used, giving too much emissions. 
<br/><b>Note 3:</b> These options only apply to the hard interaction.
If a "second hard" process is present, the two are analyzed and 
set separately for the default 0 option, while both are affected
the same way for non-default options 1 and 2. 
Emissions off subsequent multiparton interactions are always constrained
to be below the factorization scale of each process itself.  
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTmaxFudge &nbsp;</strong> 
 (<code>default = <strong>1.0</strong></code>; <code>minimum = 0.25</code>; <code>maximum = 2.0</code>)<br/>
In cases where the above <code>pTmaxMatch</code> rules would imply
that <i>pT_max = pT_factorization</i>, <code>pTmaxFudge</code> 
introduces a multiplicative factor <i>f</i> such that instead
<i>pT_max = f * pT_factorization</i>. Only applies to the hardest
interaction in an event, and a "second hard" if there is such a one, 
cf. below. It is strongly suggested that <i>f = 1</i>, but variations 
around this default can be useful to test this assumption. 
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTmaxFudgeMPI &nbsp;</strong> 
 (<code>default = <strong>1.0</strong></code>; <code>minimum = 0.25</code>; <code>maximum = 2.0</code>)<br/>
A multiplicative factor <i>f</i> such that 
<i>pT_max = f * pT_factorization</i>, as above, but here for the
non-hardest interactions (when multiparton interactions are allowed).
  

<p/><code>mode&nbsp; </code><strong> SpaceShower:pTdampMatch &nbsp;</strong> 
 (<code>default = <strong>0</strong></code>; <code>minimum = 0</code>; <code>maximum = 2</code>)<br/>
These options only take effect when a process is allowed to radiate up 
to the kinematical limit by the above <code>pTmaxMatch</code> choice, 
and no matrix-element corrections are available. Then, in many processes,
the fall-off in <i>pT</i> will be too slow by one factor of <i>pT^2</i>. 
That is, while showers have an approximate <i>dpT^2/pT^2</i> shape, often 
it should become more like <i>dpT^2/pT^4</i> at <i>pT</i> values above
the scale of the hard process. Whether this actually is the case 
depends on the particular process studied, e.g. if <i>t</i>-channel 
gluon exchange is likely to dominate. If so, the options below could
provide a reasonable high-<i>pT</i> behaviour without requiring 
higher-order calculations. 
<br/><code>option </code><strong> 0</strong> : emissions go up to the kinematical limit, 
with no special dampening.
  
<br/><code>option </code><strong> 1</strong> : emissions go up to the kinematical limit,  
but dampened by a factor <i>k^2 Q^2_fac/(pT^2 + k^2 Q^2_fac)</i>, 
where <i>Q_fac</i> is the factorization scale and <i>k</i> is a 
multiplicative fudge factor stored in <code>pTdampFudge</code> below.
  
<br/><code>option </code><strong> 2</strong> : emissions go up to the kinematical limit, 
but dampened by a factor <i>k^2 Q^2_ren/(pT^2 + k^2 Q^2_ren)</i>, 
where <i>Q_ren</i> is the renormalization scale and <i>k</i> is a 
multiplicative fudge factor stored in <code>pTdampFudge</code> below. 
  
<br/><b>Note:</b> These options only apply to the hard interaction.
Specifically, a "second hard" interaction would not be affected.
Emissions off subsequent multiparton interactions are always constrained
to be below the factorization scale of the process itself.  
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTdampFudge &nbsp;</strong> 
 (<code>default = <strong>1.0</strong></code>; <code>minimum = 0.25</code>; <code>maximum = 4.0</code>)<br/>
In cases 1 and 2 above, where a dampening is imposed at around the
factorization or renormalization scale, respectively, this allows the
<i>pT</i> scale of dampening of radiation by a half to be shifted 
by this factor relative to the default <i>Q_fac</i> or <i>Q_ren</i>. 
This number ought to be in the neighbourhood of unity, but variations 
away from this value could do better in some processes.
  

<p/>
The amount of QCD radiation in the shower is determined by 
<p/><code>parm&nbsp; </code><strong> SpaceShower:alphaSvalue &nbsp;</strong> 
 (<code>default = <strong>0.137</strong></code>; <code>minimum = 0.06</code>; <code>maximum = 0.25</code>)<br/>
The <i>alpha_strong</i> value at scale <code>M_Z^2</code>. 
Default value is picked equal to the one used in CTEQ 5L.  
  

<p/>
The actual value is then regulated by the running to the scale 
<i>pT^2</i>, at which it is evaluated
<p/><code>mode&nbsp; </code><strong> SpaceShower:alphaSorder &nbsp;</strong> 
 (<code>default = <strong>1</strong></code>; <code>minimum = 0</code>; <code>maximum = 2</code>)<br/>
Order at which <i>alpha_strong</i> runs,
<br/><code>option </code><strong> 0</strong> : zeroth order, i.e. <i>alpha_strong</i> is kept 
fixed.  
<br/><code>option </code><strong> 1</strong> : first order, which is the normal value.  
<br/><code>option </code><strong> 2</strong> : second order. Since other parts of the code do 
not go to second order there is no strong reason to use this option, 
but there is also nothing wrong with it.  
  

<p/>
The CMW rescaling of <i>Lambda_QCD</i> (see the section on 
<a href="StandardModelParameters.html" target="page">StandardModelParameters</a>)
can be applied to the <i>alpha_strong</i> values used for spacelike showers. 
Note that tunes using this option need lower values of 
<i>alpha_strong(m_Z^2)</i> than tunes that do not.
<p/><code>flag&nbsp; </code><strong> SpaceShower:alphaSuseCMW &nbsp;</strong> 
 (<code>default = <strong>false</strong></code>)<br/>
<br/><code>option </code><strong> false</strong> : Do not apply the CMW rescaling.   
<br/><code>option </code><strong> true</strong> : Apply the CMW rescaling, increasing 
<i>Lambda_QCD</i> for spacelike showers by a factor roughly 1.6.
  
  

<p/>
QED radiation is regulated by the <i>alpha_electromagnetic</i>
value at the <i>pT^2</i> scale of a branching.
 
<p/><code>mode&nbsp; </code><strong> SpaceShower:alphaEMorder &nbsp;</strong> 
 (<code>default = <strong>1</strong></code>; <code>minimum = -1</code>; <code>maximum = 1</code>)<br/>
The running of <i>alpha_em</i>.
<br/><code>option </code><strong> 1</strong> : first-order running, constrained to agree with
<code>StandardModel:alphaEMmZ</code> at the <i>Z^0</i> mass.
  
<br/><code>option </code><strong> 0</strong> : zeroth order, i.e. <i>alpha_em</i> is kept 
fixed at its value at vanishing momentum transfer.  
<br/><code>option </code><strong> -1</strong> : zeroth order, i.e. <i>alpha_em</i> is kept 
fixed, but at <code>StandardModel:alphaEMmZ</code>, i.e. its value
at the <i>Z^0</i> mass.
   
  

<p/>
The natural scale for couplings and PDFs is <i>pT^2</i>. To explore 
uncertainties it is possibly to vary around this value, however, in 
analogy with what can be done for 
<a href="CouplingsAndScales.html" target="page">hard processes</a>.

<p/><code>parm&nbsp; </code><strong> SpaceShower:renormMultFac &nbsp;</strong> 
 (<code>default = <strong>1.</strong></code>; <code>minimum = 0.1</code>; <code>maximum = 10.</code>)<br/>
The default <i>pT^2</i> renormalization scale is multiplied by 
this prefactor. For QCD this is equivalent to a change of 
<i>Lambda^2</i> in the opposite direction, i.e. to a change of 
<i>alpha_strong(M_Z^2)</i> (except that flavour thresholds 
remain at fixed scales). Below, when <i>pT^2 + pT_0^2</i> is used
as scale, it is this whole expression that is multiplied by the prefactor.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:factorMultFac &nbsp;</strong> 
 (<code>default = <strong>1.</strong></code>; <code>minimum = 0.1</code>; <code>maximum = 10.</code>)<br/>
The default <i>pT^2</i> factorization scale is multiplied by 
this prefactor. 
  

<p/>
There are two complementary ways of regularizing the small-<i>pT</i> 
divergence, a sharp cutoff and a smooth dampening. These can be 
combined as desired but it makes sense to coordinate with how the 
same issue is handled in multiparton interactions.

<p/><code>flag&nbsp; </code><strong> SpaceShower:samePTasMPI &nbsp;</strong> 
 (<code>default = <strong>off</strong></code>)<br/>
Regularize the <i>pT -> 0</i> divergence using the same sharp cutoff 
and smooth dampening parameters as used to describe multiparton interactions.
That is, the <code>MultipartonInteractions:pT0Ref</code>, 
<code>MultipartonInteractions:ecmRef</code>, 
<code>MultipartonInteractions:ecmPow</code> and 
<code>MultipartonInteractions:pTmin</code> parameters are used to regularize 
all ISR QCD radiation, rather than the corresponding parameters below. 
This is a sensible physics ansatz, based on the assumption that colour 
screening effects influence both MPI and ISR in the same way. Photon 
radiation is regularized separately in either case.
<br/><b>Warning:</b> if a large <code>pT0</code> is picked for multiparton 
interactions, such that the integrated interaction cross section is 
below the nondiffractive inelastic one, this <code>pT0</code> will 
automatically be scaled down to cope. Information on such a rescaling 
does NOT propagate to <code>SpaceShower</code>, however.
   

<p/>
The actual <code>pT0</code> parameter used at a given CM energy scale, 
<i>ecmNow</i>, is obtained as
<br/><i>
    pT0 = pT0(ecmNow) = pT0Ref * (ecmNow / ecmRef)^ecmPow 
</i><br/>
where <i>pT0Ref</i>, <i>ecmRef</i> and <i>ecmPow</i> are the 
three parameters below.

<p/><code>parm&nbsp; </code><strong> SpaceShower:pT0Ref &nbsp;</strong> 
 (<code>default = <strong>2.0</strong></code>; <code>minimum = 0.5</code>; <code>maximum = 10.0</code>)<br/>
Regularization of the divergence of the QCD emission probability for 
<i>pT -> 0</i> is obtained by a factor <i>pT^2 / (pT0^2 + pT^2)</i>, 
and by using an <i>alpha_s(pT0^2 + pT^2)</i>. An energy dependence 
of the <i>pT0</i> choice is introduced by the next two parameters, 
so that <i>pT0Ref</i> is the <i>pT0</i> value for the reference 
cm energy, <i>pT0Ref = pT0(ecmRef)</i>.   
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:ecmRef &nbsp;</strong> 
 (<code>default = <strong>1800.0</strong></code>; <code>minimum = 1.</code>)<br/>
The <i>ecmRef</i> reference energy scale introduced above.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:ecmPow &nbsp;</strong> 
 (<code>default = <strong>0.0</strong></code>; <code>minimum = 0.</code>; <code>maximum = 0.5</code>)<br/>
The <i>ecmPow</i> energy rescaling pace introduced above.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTmin &nbsp;</strong> 
 (<code>default = <strong>0.2</strong></code>; <code>minimum = 0.1</code>; <code>maximum = 10.0</code>)<br/>
Lower cutoff in <i>pT</i>, below which no further ISR branchings 
are allowed. Normally the <i>pT0</i> above would be used to 
provide the main regularization of the branching rate for 
<i>pT -> 0</i>, in which case <i>pTmin</i> is used  mainly for 
technical reasons. It is possible, however, to set <i>pT0Ref = 0</i> 
and use <i>pTmin</i> to provide a step-function regularization, 
or to combine them in intermediate approaches. Currently <i>pTmin</i> 
is taken to be energy-independent.  
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTminChgQ &nbsp;</strong> 
 (<code>default = <strong>0.5</strong></code>; <code>minimum = 0.01</code>)<br/>
Parton shower cut-off <i>pT</i> for photon coupling to a coloured 
particle.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTminChgL &nbsp;</strong> 
 (<code>default = <strong>0.0005</strong></code>; <code>minimum = 0.0001</code>)<br/>
Parton shower cut-off mass for pure QED branchings. 
Assumed smaller than (or equal to) <i>pTminChgQ</i>.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:rapidityOrder &nbsp;</strong> 
 (<code>default = <strong>off</strong></code>)<br/>
Force emissions, after the first,  to be ordered in rapidity,
i.e. in terms of decreasing angles in a backwards-evolution sense. 
Could be used to probe sensitivity to unordered emissions.
Only affects QCD emissions.
  
 
<h3>Weak showers</h3>

The description of <i>W^+-</i> and <i>Z^0</i> gauge boson emission
in ISR closely parallels that of such emissions in 
<a href="TimelikeShowers.html" target="page">FSR</a>. We therefore will not repeat
the discussion here, but only report on the settings names, which again
are similar to the FSR ones. 

<p/><code>flag&nbsp; </code><strong> SpaceShower:weakShower &nbsp;</strong> 
 (<code>default = <strong>off</strong></code>)<br/>
Allow a weak shower, yes or no.
  

<p/><code>mode&nbsp; </code><strong> SpaceShower:weakShowerMode &nbsp;</strong> 
 (<code>default = <strong>0</strong></code>; <code>minimum = 0</code>; <code>maximum = 2</code>)<br/>
Determine which branchings are allowed.
<br/><code>option </code><strong> 0</strong> :  both <i>W^+-</i> and <i>Z^0</i> branchings. 
  
<br/><code>option </code><strong> 1</strong> :  only <i>W^+-</i> branchings.   
<br/><code>option </code><strong> 2</strong> :  only <i>Z^0</i> branchings.   
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:pTminWeak &nbsp;</strong> 
 (; <code>minimum = 0.1</code>; <code>maximum = 2.0</code>)<br/>
Parton shower cut-off <i>pT</i> for weak branchings.

<p/><code>parm&nbsp; </code><strong> SpaceShower:weakShowerEnhancement &nbsp;</strong> 
 (<code>default = <strong>1.</strong></code>; <code>minimum = 1.</code>; <code>maximum = 1000.</code>)<br/>
Enhancement factor for the weak shower. This is used to increase the statistics 
of weak shower emissions. Remember afterwards to correct for the additional 
weak emissions (i.e. divide the weak emissions by the same factor).
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:singleWeakEmission &nbsp;</strong> 
 (<code>default = <strong>off</strong></code>)<br/>
This parameter allows to stop the weak shower after a single emission.
<br/>on = only a single weak emission is allowed.
<br/>off = unlimited number of weak emissions possible.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:extraScaleTerm &nbsp;</strong> 
 (<code>default = <strong>0.</strong></code>; <code>minimum = 0.</code>; <code>maximum = 200.</code>)<br/>
The normal showers uses <i>pT^2</i> as ordering variable, but for 
massive particles it could be preferred to use <i>pT^2 + M^2</i> 
instead. This parameter allows to use <i>pT^2 + k * M^2</i> for 
weak showers, thus <i>k = 0</i> is the standard ordering and 
is used as default.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:dopTDampMass &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Add an extra dampening to the weak shower to lower the production
of low-<i>pT</i> <i>W/Z</i>'s. The dampening is given by
<i>(pT^2 + 0.25 M^2)/ (pT^2 + M^2)</i>, where <i>M^2</i> is the 
squared mass of the <i>W/Z</i>.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:vetoWeakJets &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
This flag will veto the 2nd emission on the same side of the process 
if it has too high "<i>pT</i>" if the primary process was weak production 
(code 221, 222, 223). This is too avoid doubling counting with 
dijet production followed by an emission of a <i>W/Z</i> boson. 
The <i>pT</i> definition used is the <i>pT</i> in the rest frame 
of the two emitted partons with respect to the incoming parton. 
This <i>pT</i> definition should be close to the <i>pT</i> 
definition of a dijet event.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:vetoWeakJetspTcut &nbsp;</strong> 
 (<code>default = <strong>20.0</strong></code>; <code>minimum = 1.0</code>; <code>maximum = 1e9</code>)<br/>
This parameter determines the cut-off <i>pT</i> used for the veto 
of emissions for weak production. For more information see 
<code>vetoWeakJets</code>.
  

<h3>Further variables</h3>

These should normally not be touched. Their only function is for
cross-checks.

<p/>
There are three flags you can use to switch on or off selected
branchings in the shower: 

<p/><code>flag&nbsp; </code><strong> SpaceShower:QCDshower &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Allow a QCD shower; on/off = true/false.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:QEDshowerByQ &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Allow quarks to radiate photons; on/off = true/false.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:QEDshowerByL &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Allow leptons to radiate photons; on/off = true/false.
  

<p/>
There are some further possibilities to modify the shower:

<p/><code>flag&nbsp; </code><strong> SpaceShower:MEcorrections &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Use of matrix element corrections; on/off = true/false.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:MEafterFirst &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Use of matrix element corrections also after the first emission,
for dipole ends of the same system that did not yet radiate.
Only has a meaning if <code>MEcorrections</code> above is 
switched on. 
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:phiPolAsym &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Azimuthal asymmetry induced by gluon polarization; on/off = true/false.
  

<p/><code>flag&nbsp; </code><strong> SpaceShower:phiIntAsym &nbsp;</strong> 
 (<code>default = <strong>on</strong></code>)<br/>
Azimuthal asymmetry induced by interference; on/off = true/false.
  

<p/><code>parm&nbsp; </code><strong> SpaceShower:strengthIntAsym &nbsp;</strong> 
 (<code>default = <strong>0.7</strong></code>; <code>minimum = 0.</code>; <code>maximum = 0.9</code>)<br/>
Size of asymmetry induced by interference. Natural value of order 0.5; 
expression would blow up for a value of 1.
  

<p/><code>mode&nbsp; </code><strong> SpaceShower:nQuarkIn &nbsp;</strong> 
 (<code>default = <strong>5</strong></code>; <code>minimum = 0</code>; <code>maximum = 5</code>)<br/>
Number of allowed quark flavours in <i>g -> q qbar</i> branchings,
when kinematically allowed, and thereby also in incoming beams. 
Changing it to 4 would forbid <i>g -> b bbar</i>, etc.
  

<h3>Technical notes</h3>

Almost everything is equivalent to the algorithm in [1]. Minor changes 
are as follows.
<ul>
<li>
It is now possible to have a second-order running <i>alpha_s</i>,
in addition to fixed or first-order running. 
</li>
<li>
The description of heavy flavour production in the threshold region 
has been modified, so as to be more forgiving about mismatches 
between the <i>c/b</i>  masses used in Pythia relative to those 
used in a respective PDF parametrization. The basic idea is that, 
in the threshold region of a heavy quark <i>Q</i>, <i>Q = c/b</i>, 
the effect of subsequent <i>Q -> Q g</i> branchings is negligible. 
If so, then
<br/><i>
   f_Q(x, pT2) = integral_mQ2^pT2  dpT'2/pT'2 * alpha_s(pT'2)/2pi
      * integral P(z) g(x', pT'2) delta(x - z x')
</i><br/>
so use this to select the <i>pT2</i> of the <i>g -> Q Qbar</i> 
branching. In the old formalism the same kind of behaviour should 
be obtained, but by a cancellation of a <i>1/f_Q</i> that diverges 
at the threshold and a Sudakov that vanishes.
<br/>
The strategy therefore is that, once <i>pT2 &lt; f * mQ2</i>, with 
<i>f</i> a parameter of the order of 2, a <i>pT2</i> is chosen 
like <i>dpT2/pT2</i> between <i>mQ2</i> and <i>f * mQ2</i>, a
nd a <i>z</i> flat in the allowed range. Thereafter acceptance
is based on the product of three factors, representing the running
of <i>alpha_strong</i>, the splitting kernel (including the mass term) 
and the gluon density weight. At failure, a new <i>pT2</i> is chosen 
in the same  range, i.e. is not required to be lower since no Sudakov 
is involved. 
</li>
<li>
The QED algorithm now allows for hadron beams with non-zero photon
content. The backwards-evolution of a photon in a hadron is identical
to that of a gluon, with <i>CF -> eq^2</i> and <i>CA -> 0</i>.
Note that this will only work in conjunction with 
parton distribution that explicitly include photons as part of the
hadron structure (such as the MRST2004qed set). Since Pythia's
internal sets do not allow for photon content in hadrons, it is thus 
necessary to use the LHAPDF interface to make use of this feature. The
possibility of a fermion backwards-evolving to a photon has not yet
been included, nor has photon backwards-evolution in lepton beams. 
</li>
</ul>

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