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Background

Josh Lande recently ran some consistency tests comparing the Monte Carlo point source parameters to the values fit by binned likelihood for point sources. For the spacecraft data, he used a one-day interval of the idealized +/-50 deg rocking provided by gtobssim. For one location on the sky, location 0: (RA, Dec) = (176.31, 44.28), the fitted flux in the 0.1-100 GeV band was too high relative to the MC value by ~8%, whereas at location 1: (RA, Dec) =

...

(-176.31,

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-44.28),

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the

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disparity

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appeared

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negligible.

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For

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such

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a

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short

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time

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scale

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(1

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day),

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these

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two

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sky

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locations

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have

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very

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different

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off-axis

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profiles.

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Here

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are

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histograms

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of

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the

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livetime

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as

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a

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function

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of

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off-axis

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angle

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for

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the

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two

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locations.

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The

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black

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histogram

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corresponds

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to

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location

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0,

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and

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the

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red

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corresponds

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to

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location 1.

Image Added

Diagnosis

The bug lay in the code that computes the exposure averaged PSF. This is given by

Wiki Markup
 1.

!off_axis_histograms.png|thumbnail!

h3. Diagnosis

The bug lay in the code that computes the exposure averaged PSF. This is given by
{latex}
\newcommand{\e}{\varepsilon}
\newcommand{\Int}{{\displaystyle \int}}
\begin{eqnarray}
P(\psi, \e) &=& \frac{\Int dt P(\psi, \e, \theta) A(\e, \theta)}
        {\Int dt A(\e, \theta)}\\
        &=& \frac{\Int d\theta P(\psi, \e, \theta(t)) 
                       A(\e, \theta(t))|\partial\theta/\partial t|^{-1}}
                 {\Int d\theta A(\e, \theta(t))
                       |\partial\theta/\partial t|^{-1}}
\end{eqnarray}
{latex}

Here 

Here

Wiki Markup
{latex}$P${latex}

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and
Wiki Markup
{latex}$A${latex}

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are

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the

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PSF

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and

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effective

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area,

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respectively,

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and

Wiki Markup
{latex}$\theta=\theta(t)${latex}

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is

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the

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angle

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of

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the

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source

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relative

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to

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the

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instrument

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z-axis.

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The

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phi-dependence

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of

Wiki Markup
{latex}$P${latex}

...

and
Wiki Markup
{latex}$A${latex}

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is

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suppressed

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for

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clarity.

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Wiki Markup
{latex}$\psi${latex}

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is

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the

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angle

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between

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true

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and

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measured

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photon

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direction,

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and

Wiki Markup
{latex}$\varepsilon${latex}

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is

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the

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photon

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energy.

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In

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the

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second

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line

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of

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the

...

above

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equation,

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the

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integrals

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have

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been

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recast

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as

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integrations

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over

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theta.

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These

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integrations

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are

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performed

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using

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the

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livetime

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cubes

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computed

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with

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gtltcube.

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In

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ST-09-27-01

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and

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earlier,

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there

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is

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a

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cutoff

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at

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theta=70

...

deg

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for

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the

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mean

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PSF

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calculation.

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The

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original

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reason

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for

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this

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cutoff

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is

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unclear,

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but

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it

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was

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probably

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motivated

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by

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some

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poor

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behavior

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of

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the

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PSF

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at

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large

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theta

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angles

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for

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an

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early

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version

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of

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the

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IRFs.

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As

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far

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as

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the

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shape

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of

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the

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PSF

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is

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concerned,

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this

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truncation

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does

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not

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have

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a

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significant

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effect.

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As

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part

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of

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some

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recent

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refactoring,

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this

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truncation

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was

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removed

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in

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Likelihood-17-22-04

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(22

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Feb

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2012).

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Unfortunately,

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I

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had

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thought

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that

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the

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truncation

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only

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affected

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the

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PSF

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shape

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calculation.

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In

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fact,

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for

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point

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sources,

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the

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binned

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analysis

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code

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has

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been

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using

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the

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exposure

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calculation

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in

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the

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denominator

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of

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the

...

mean

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PSF

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expression

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for

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computing

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the

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model

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counts

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rather

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than

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using

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the

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exposure

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from

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the

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binned

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exposure

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map.

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Hence,

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all

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point

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source

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fits

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will

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be

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affected

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by

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this

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truncation.

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For

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location

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0

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(black

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histogram

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in

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above

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figure),

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a

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significant

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fraction

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of

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its

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time

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is

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spent

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just

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beyond

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the

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theta=70

...

deg

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cutoff.

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This

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is

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the

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cause

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of

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the

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8%

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disparity

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that

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Josh

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found

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in

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his

...

tests.

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Effects

One can estimate the impact of the theta=70

...

deg

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cutoff

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by

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running

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gtexpcube2

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with

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the

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option

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thmax=180

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in

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the

...

nominal

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case

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(this

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is

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the

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default)

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and

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thmax=70

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in

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the

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truncation

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case.

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Assuming

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a

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photon

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index

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of

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-2,

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which

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Josh

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used

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in

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his

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gtobssim

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runs,

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one

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can

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estimate

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the

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expected

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fractional

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offset

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in

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measured

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flux

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(Fmeas)

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relative

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to

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the

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MC

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value

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(Fmc),

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(Fmeas

...

-

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Fmc)/Fmc,

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using

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the

...

spectrally

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weighted

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exposures,

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exposure

Wiki Markup
{latex}$= \left.\int \varepsilon^{-2} A(\varepsilon, \theta(t)) dt d\varepsilon\right/\int \varepsilon^{-2} d\varepsilon${latex}
,

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and

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computing

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(exposure180

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-

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exposure70)/exposure70.

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For

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the

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one-day

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simulation,

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here

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is

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a

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map

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of

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the

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estimated

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fractional

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offset

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in

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Galactic

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coordinates:

...

  • One

...

  • day
    Image Added

The green point near the Northern Galactic pole is location 0 and has a fractional flux offset of 8%, and the green point nearer the Galactic plane has flux offset of 1.5%. The peak offsets can be has high as 16.3%.

On longer time scales, these offsets are considerably smaller. Here are maps for the 18 month and 2 year livetime cubes used by the catalog group for 2FGL:

  • 18 months (/afs/slac/g/glast/groups/catalog/P6_V8_DIFFUSE/ltcube_18months_rock52.fits)

...


  • Image Added
  • 2 years (/afs/slac/g/glast/groups/catalog/P6_V8_DIFFUSE/ltcube_2years_rock52.fits)

...


  • Image Added

I've

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computed

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livetime

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cubes

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for

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30

...

day

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intervals

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and

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have

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estimated

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the

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fractional

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offset

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as

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a

...

function

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of

...

time

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for

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the

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Vela,

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Crab,

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and

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Geminga

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pulsars.

...


Image Added
There is a DC offset of about 1.5%

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and

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an

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additional

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dispersion

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of

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about

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the

...

same

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size.

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NB:

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These

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estimates

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assume

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a

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power-law

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spectrum

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with

...

photon

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index

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-2

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over

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the

...

entire

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integration

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range

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0.1-100

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GeV.

...