Finding pulsars with LOFAR | Astronomy & Astrophysics (A&A)

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Table 1:

Figure of merit *FoM* per Eq. (2) for the three different survey set ups as described in the text: Full Incoherent, Core Coherent and Superstation Coherent.
Type	$A/T_{\rm sys}$ (m²/K)	$N_{\rm beams}$	$\Omega$ (deg²)	B (MHz)	$1\vert N_{\rm stations}$	FoM
Full Incoherent	260	1	27	32	54	1.0
Core Coherent	170	128	0.006	32	1	0.8
Superstation Coherent	40	128	0.23	32	1	1.2

All parameters derived using the lowest observing frequency, 120 MHz. In the first column, $A/T_{\rm sys}$ , we use 54, 36 and 12 stations respectively, of 24 tiles at 28 m², and 140 K, while for the Superstation Coherent case we also multiply by 0.70 to correct for the lower sensitivity at the station beam edge.

Source LaTeX | All tables | In the text

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