Table 4: Orbital and spectral parameters for XBPs with a detected soft excess (SE).
Sourcea Location Distance Companion $P_{\rm pulse}$ $L_{\rm X}^{b}$ Flux $N_{\rm H}^{c}$ $L_{\rm SE}$/$L_{\rm X}$ SE modeld $kT_{\rm BB}$ SE Pulsese
    (kpc) Star (s) (erg s-1, keV) (erg cm-2 s-1) (1021 cm-2)     (keV)  
Her X-11 Galaxy $\sim$5 A7 V 1.24 $1.0\times10^{37}$ (0.3-10) $3.3\times10^{-9}$ 0.05 0.04-0.10 BB, BB+LE 0.09-0.12 Yes
SMC X-12 SMC 65 B0 Ib 0.7 $2.4\times10^{38}$ (0.7-10) $4.7\times10^{-10}$ 2-5 0.036 BB, TB, SPL 0.15-0.18 Yes
LMC X-43 LMC 50 O7 III-O IV 13.5 $1.2\times10^{38}$ (0.7-10) $4.0\times10^{-10}$ $\sim$0.5 0.064 BB, BB+TB, COM, SPL 0.15 Yes
XTE J0111.2-73174 SMC 65 B1 IVe 30.95 $1.8\times10^{38}$ (0.7-10) $3.6\times10^{-10}$ 1.8 $\sim$0.10 SPL ... Yes
RX J0059.2-71385 SMC 65 B1 IIIe 2.76 $2.6\times10^{38}$ (0.1-10) $5.1\times10^{-10}$ 0.42-0.50 0.31 MEK, SPL ... No
4U 1626-676 Galaxy ? Low-mass 7.7 $2.6\times10^{34}D_{\rm kpc}^2$ (0.5-10) $2.2\times10^{-10}$ 0.6 0.10 BB 0.34 No
Cen X-37 Galaxy $\sim$8 O6-O8 II 4.8 $2.4\times10^{38}$ (0.1-10) $3.2\times10^{-8}$ 19.5 $\sim$0.7 BB 0.11 Yes
Vela X-18 Galaxy 1.9 B0.5 Ib 283 $2.2\times10^{36}$ (2-10) $5.1\times10^{-9}$ 4.2 $\sim$0.01 TB ... No
X Per9 Galaxy 0.95 O9.5pe 837 $1.8\times10^{34}$ (0.3-10) $1.7\times10^{-10}$ 1.5 0.24 BB 1.45 ?
EXO 053109-6609.210 LMC 50 B0.7 Ve 13.7 $4.6\times10^{37}$ (0.2-10) $1.5\times10^{-10}$ 6.9 ? MEK+PL ... Yes
A 0538-6611 LMC 50 B2 IIIe 0.069 $4.0\times10^{37}$ (0.1-2.4) $1.3\times10^{-10}$ 0.8 ? BB, TB $\sim$0.2 ?
RX J0047.3-731212 SMC 65 B2e 263 $1.5,2\times10^{36}$ (0.7-10) $3.0,4.0\times10^{-12}$ 0.96, 3.4 0.03-0.09, 0.68 BB 0.6, 2.2 Yes
RX J0101.3-721113 SMC 65 Be 452 $1.6\times10^{35}$ (0.3-10) $3.2\times10^{-13}$ 0.6 ? MEK ... ?
RX J0103.6-720114 SMC 65 O5 Ve 1323 $0.8{-}7.5\times10^{36}$ (0.2-10) $1.6{-}14.8\times10^{-12}$ 1.9 ? MEK ... No
AX J0049.5-732315 SMC 65 B2 Ve 751 $7{-}9\times10^{35}$ (0.2-10) $1.4{-}1.8\times10^{-12}$ 3.6 ? ? ... Yes
AX J0058-72013 SMC 65 Be 281 $1.2\times10^{35}$ (0.3-10) $2.4\times10^{-13}$ 0.6 ? ? ... Yes
AX J0103-72213 SMC 65 B0 IV 342 $1.8\times10^{35}$ (0.3-10) $3.6\times10^{-13}$ 0.6 ? MEK ... ?
3A 0535+26216 Galaxy 2.0 O9.7 IIIe 103.4 $3.9\times10^{33}$ (2-10) $8.2\times10^{-12}$ 6.0 0.35 BB 1.33 ?
RX J0146.9+6121 Galaxy 2.5 B0 IIIe 1395 $1.5\times10^{34}$ (0.3-10) $2.0\times10^{-11}$ 5.1 0.25 BB 1.11 ?
a References: (1) dal Fiume et al. (1998), Endo et al. (2000), Ramsay et al. (2002); (2) Woo et al. (1995), Paul et al. (2002); (3) Woo et al. (1996), La Barbera et al. (2001), Naik & Paul (2004); (4) Yokogawa et al. (2000b); (5) Kohno et al. (2000); (6) Schulz et al. (2001); (7) Burderi et al. (2000); (8) Haberl (1994), Orlandini et al. (1998), Kreykenbohm et al. (2002); (9) di Salvo et al. (1998), Coburn et al. (2001); (10) Haberl et al. (2003); (11) Mavromatakis & Haberl (1993); (12) The two set of values are base on Ueno et al. (2004) and Majid et al. (2004), respectively; (13) Sasaki et al. (2003); (14)Sasaki et al. (2003), Haberl & Pietsch (2005); (15) Yokogawa et al. (2000a), Haberl & Pietsch (2004); (16) Mukherjee & Paul (2005).
b For each source the reference energy range is also reported.
c The reported values refer only to the interstellar absorption, not to the source intrinsic absorption.
d Spectral models used for the soft excess are: BB = blackbody; TB = thermal bremsstrahlung; SPL = soft power-law or broken power-law; MEK = MEKAL thin thermal model; COM = Comptonization model; LE = broad low-energy line emission. Commas indicate separate fits, plus signs indicate fits with two components.
e Pulsation of the emission component that traces the soft excess.

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