Searching for substellar companions of young isolated neutron stars

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Volume 496 / No 2 (March III 2009)

A&A, 496 2 (2009) 533-545

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Table 2:

Observational parameters for neutron stars with two epochs of observations.
Neutron star	$m_{\rm BD}$ ^a	$m_{\rm 13Jup}$ ^a	$m_{\rm lim}$ ^b	Epoch difference	$r_{\rm proj}$ ^c	refX^d	refY^d	Align_X^e	Align_Y^e
	[mag]	[mag]	[mag]	[yr]	[AU]	[mas]	[mas]	+/-	+/-
Geminga	18.2	22.3	22.4	3.05	10 000	148.4	148.4	+	-
RX J0720.4-3125	19.0	23.0	22.9	2.95	20 000	147.7	147.7	+	-
RX J1856.6-3754	17.3	21.4	21.5	3.0	10 800	147.8	147.7	+	+
PSR J1932+1059	21.5	23.5	21.5	2.9, 3.9	see text	147.5	147.3	-	+

^a $m_{\rm BD}$ and $m_{\rm 13Jup}$ are the brightest H-band magnitudes expected for a brown dwarf companion or a gas planet of 13 Jupiter mass respectively (see also text); ^b $m_{\rm lim}$ is the magnitude limit reached in both epochs; ^c $r_{\rm proj}$ is the covered projected physical separations; ^d (refX, refY) are the pixel scale of the reference ISAAC image; ^e reference image axes are roughly aligned with RA (X) and DEC (Y) to within 1 degree, although sometimes with opposite direction (indicated by ``-'' instead of ``+'').

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