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

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Table 2:

Name, year, number of detected pulsars ( $N_{\rm real}$ ), number of simulated detected pulsars ( $N_{\rm sim}$ ) and frequency observed at ( $\nu$ ) for the eight surveys simulated.
Survey	Year	$N_{\rm real}$	$N_{\rm sim}$	$\nu$ (MHz)
Jodrell	1972	51	20 $\pm$ 2	408
UMass-Arecibo	1974	50	39 $\pm$ 4	430
MolongloII	1978	224	227 $\pm$ 7	408
UMass-NRAO	1978	50	54 $\pm$ 6	400
ParkesII	1991-1994	298	335 $\pm$ 10	400
Cambridge 80MHz	1993-1994	20	27 $\pm$ 5	82
Parkes Multibeam	1997-2000	987	801 $\pm$ 41	1374
LOFAR	2010-2012	-	1100 $\pm$ 100	140

The error on $N_{\rm sim}$ is the standard variation in the outcomes when simulating the model described in the text with different random number seeds. The $N_{\rm real}$ data is taken from Shrauner et al. (1998); Hulse & Taylor (1975); Manchester et al. (1996,1978); Damashek et al. (1978); Davies et al. (1977) and Manchester et al. (2005) respectively. The LOFAR numbers are for the incoherent 25-day reference design described in the text.

Source LaTeX | All tables | In the text

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