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 1:

The observed neutron stars, their distances, and proper motions.
Object	D	$\mu_{\alpha}$	$\mu_{\delta}$
	[pc]	[mas yr^-1]	[mas yr^-1]
PSR J0108-1431	130^a	<26^a	<78^a
RX J0420.0-5022	$\geq$ 300^ass	<123^b	<123^b
Geminga	250⁺¹²⁰_-62^c	$142.2 \pm 1.2$ ^c	$107.4 \pm 1.2$ ^c
RX J0720.4-3125	361⁺¹⁷²_-88^d	$-93 \pm 1.2$ ^d	$52.8 \pm 1.3$ ^d
RX J0806.4-4123	240^ass	<86^b	<86^b
RX J1856.6-3754	167⁺¹⁸_-15^d	$326.7 \pm 0.8$ ^e	$-59.1 \pm 0.7$ ^e
PSR J1932+1059	361⁺¹⁰_-8^f	$94.03 \pm 0.14$ ^f	$43.37 \pm 0.29$ ^f
PSR J2124-3358^A	$270 \pm 20$ ^g	$-14.4 \pm 0.8$ ^h	$-50 \pm 2$ ^h
RBS 1774^K	$\geq$ 300^ass	not known	not known

^K 1RXS J214303.7+065419; ^A PSR J2124-3358 turned out to be too old for our substellar companion search. See Appendix C for a NIR limit of this neutron star; ^a Mignani et al. (2003); ^b $2\sigma$ limit of Motch et al. (2009); ^c Faherty et al. (2007); ^d Kaplan et al. (2007); ^e Walter & Lattimer (2002); ^f Chatterjee et al. (2004); ^g Gaensler et al. (2002); ^h Hotan et al. (2006); ^ass notes an assumed distance, which is a lower limit as indicated by estimations from X-ray measured hydrogen column density (e.g. Posselt et al. 2007), see also text.

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