Table 1: Morphology of the emission assuming a 2d angular Gaussian surface brightness distribution.
Quantity Measured value

RMLR (DOF) 462.2 (5)

l₀ $-0.6\ensuremath{^\circ}\pm 0.3\ensuremath{^\circ}$

b₀ $+0.1\ensuremath{^\circ}\pm 0.3\ensuremath{^\circ}$

$\Delta l$ ( FWHM) $8.1\ensuremath{^\circ}\pm 0.9\ensuremath{^\circ}$

$\Delta b$ ( FWHM) $7.2\ensuremath{^\circ}\pm 0.9\ensuremath{^\circ}$

511 keV flux (10^-3 ph cm^-2 s^-1) $1.09 \pm 0.04$

**Table 1:** Morphology of the emission assuming a 2d angular Gaussian surface brightness distribution.
Quantity	Measured value
RMLR (DOF)	462.2 (5)
l₀	$-0.6\ensuremath{^\circ}\pm 0.3\ensuremath{^\circ}$
b₀	$+0.1\ensuremath{^\circ}\pm 0.3\ensuremath{^\circ}$
$\Delta l$ ( FWHM)	$8.1\ensuremath{^\circ}\pm 0.9\ensuremath{^\circ}$
$\Delta b$ ( FWHM)	$7.2\ensuremath{^\circ}\pm 0.9\ensuremath{^\circ}$
511 keV flux (10^-3 ph cm^-2 s^-1)	$1.09 \pm 0.04$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data preparation
	3 Background modelling
	4 Results
	5 Discussion
	6 Conclusions
	Appendix A: Summary of galactic density profiles
	References