Table 2: Summary of the IR fluxes measurements for all types of isolated NSs with an identified IR counterpart i.e. rotation-powered pulsars (rows 1-5) and magnetars (rows 6-11). The columns give the observed $J, H, K, K_{\rm s}$ magnitudes (an hyphen stands for non-detection, values in italics have been extrapolated), the distance, and the interstellar extinction AV either derived from existing optical measurements (O) or from the $N_{\rm H}$ derived from the fits to the X-ray spectra (X) by using the relation of Predehl & Schmitt (1995). K-band flux values in italics have been derived from the extrapolation of the J and H-band fluxes.
NS Name J H K $K_{\rm s}$ $d{\rm (kpc)}$ AV Ref.
Crab 14.8 $\pm$ 0.05 14.3 $\pm$ 0.05 13.8 $\pm$ 0.05 - 1.730 $\pm$ 0.28 1.62 (O) 1, 2, 3
PSR B1509-58 - 20.6 $\pm$ 0.20 - 19.4 $\pm$ 0.1 4.181 $\pm$ 0.60 4.8 (O) 4, 2, 5
Vela 22.7 $\pm$ 0.10 22.0 $\pm$ 0.16 21.3 $\pm$ 0.4 - $\rm0.294^{+0.019}_{-0.017}$ 0.20 (O) 6, 7, 8
PSR B0656+14* 24.4 $\pm$ 0.10 23.2 $\pm$ 0.08 22.6 $\pm$ 0.13 - $\rm0.288^{+0.033}_{-0.027}$ 0.09 $\pm$ 0.06(O) 9, 10, 11
Geminga* 25.1 $\pm$ 0.10 24.3 $\pm$ 0.10 23.4 $\pm$ 0.4 - $\rm0.157^{+0.059}_{-0.034}$ 0.12 $\pm$ 0.09(O) 9, 12, 13
4U 0142+61** - - 19.7 $\pm$ 0.05 20.1 $\pm$ 0.08 $\ge$5 5.1 (X) 14, 15
1E 1048.1-5937 21.7 $\pm$ 0.30 20.8 $\pm$ 0.30 - 21.3 $\pm$ 0.30 3 $\pm$ 1 6.1 (X) 16, 17, 15
1RXS J170849-400910$^{\rm x}$ 20.9 $\pm$ 0.10 18.6 $\pm$ 0.10 - 18.3 $\pm$ 0.10 5 7.8 (X) 18, 15
XTE J1810-197 - 22.0 $\pm$ 0.10 - 20.8 $\pm$ 0.10 4 $\pm$ 1+ 5.1 (X) 19, 20, 15
1E 2259+586 - - - 21.7 $\pm$ 0.20 3.0 $\pm$ 0.5 5.7 $\pm$ 0.1 (O) 21, 22, 23
SGR 1806-20 - - - 20.1 $\pm$ 0.14 $15.1\pm1.6$ 29 $\pm$ 2 (O) 24, 25, 26
(1) Sollerman (2003); (2) radio dispersion measure, Cordes & Lazio (2002); (3) Sollerman et al. (2000); (4) Kaplan & Moon (2006); (5) Lortet et al. (1987); (6) Shibanov et al. (2003); (7) radio parallax, Dodson et al. (2003); (8) Mignani et al. (2003); (9) Koptsevich et al. (2001); (10) radio parallax, Brisken et al. (2003); (11) Pavlov et al. (1997); (12) optical parallax, Caraveo et al. (1996); (13) Kargaltsev et al. (2005); (14) Hulleman et al. (2004); (15) present work; (16) Wang & Chakrabarty (2002); (17) Gaensler et al. (2005); (18) Israel et al. (2003); (19) Israel et al. (2004); (20) Rea et al. (2004); (21) Hulleman et al. (2001); (22) Kothes et al. (2002); (23) Woods et al. (2004); (24) Israel et al. (2005); (25) Mc Clure-Griffiths & Gaensler (2005); (26) Eikenberry et al. (2004); * magnitudes refer to the HST/NICMOS filters 110W, 160W, 187W, which overlap the J, H and K passbands; ** K and $K_{\rm s}$ magnitudes have been taken at different epochs; $^{\rm x}$ IR counterpart still to be confirmed (Safi-Harb & West 2005; Durant & van Kerkwijk 2006; Rea et al. 2007a); + revised downward to 2.5 kpc (Gotthelf & Halpern 2005).

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