0019.8+21 + Supersoft. Dist (kpc) = 2, kT_{bb}(keV)= 0.022, L_{x}= 6xE36 erg/s, L_{opt}= 6xE35 erg/s, N_{H}= 7.7 E 20 atoms/cm^{2}, Beuermann, K., Reinsch, K., Barwig, H., et.al., 1995, AA, 294, L1. 0019.8+21.56 + Supersoft, discovered by ROSAT, {alpha}_{2000}= 00 19 55.5, {delta}_{2000}= +21 57 27.5, Matsumoto, K., 1996, PASJ , 48, 827. + Short PSPC and HRI observations on 1993 J une 20 and 1994 J uly 11-12 gave count rates 1.81 +/- 0.17 and 0.22 +/- 0.01 cts/s, Beuermann, K., Reinsch, K., Barwig, H., et al. 1995, AA, 294, L1. + Supersoft, orbital P = 15.85 hr, Beuermann, K., Reinsch, K., Barwig, H., et al. 1985, AA, 284, L1. Matsumoto, K., PASJ , 1996, AA, 284, L1. + Supersoft. Mx = 1Mo , M opt = 1 Mo , i = 15^{o}- 26^{o}, K = 67+/- 3 km/s, Vg = -59 +/- 2 Km/s, f(M) =0.021 +/- 0.002 Mo , Beuermann, K., Reinsch, K., Barwig, H., et.al., 1995, AA, 294, L1. + Supersoft. V = 13.01 +/- 0.01, B-V = 0.70 +/- 0.03, V-R = 0.53 +/- 0.01, V-I = 0.99 +/- 0.02, Matsumoto, K., PASJ., 1996, 48, 827. + White Dwarf, E(B-V)= 0.1+/- 0.03, Beuermann, K., Reinsch, K., Barwig, H., et.al., 1995, AA, 294, L1. 0035.4-7230 + Supersoft, SMC, {alpha}_{2000}= 00 37 20.3, {delta}_{2000}= - 72 14 15, Schmidtke, P.C., Cowley, A.P., McGrath, T.K., 1996, AJ , 111, 788. + Was discovered during the first Einstein survey, Seward, F.D., Mitchell, M., 1981, ApJ , 293, 736. Wang, Q., Wu, X., 1982, ApJ Supp. Ser., 78, 391. + As orbital period lies outside the predicted range of orbital for high mass WD's, this source mass be a recurrently burning lower mass WD, Kahabka, P., 1996, AA, 306, 795. + Supersoft, SMC. Orbital period P = 0.1719256 d, Schmidtke, P.C., Cowley, A.P., McGrath, T.K., 1996, AJ , 111, 788. + Orbital period p=0.171925+/- 0.000001 d, Crampton, D., Hutchings, J. B., Cowley, A. P., and Schmidtke, P. C., 1997, ApJ 489, 903. + SMC, Supersoft. T = (4.5 - 5) E5^{o}K, N_{H}<= 4 E20 cm^{-2}, Kahabka, P., 1996, AA, 306, 795. + SMC, supersoft kT < 40 eV, in the Einstein L_{x}~ 1E37 erg/s, Hasinger, G., 1994, in "Reviews of Modern Astronomy", ed. G. Klare, (Astron. Gesch., Hamburg), Vol. 7, p.129. + Blackbody temperature ~ 40 eV, N_{H}= 5 E20 cm^{-2}, Kahabka, P., Pietsch, W., Hasinger, G., 1994, AA, 288, 538. + SMC Supersoft. M_{x}=0.5-1.5M_{o}, M_{opt}=0.4-0.5M_{o}, K_{x}=100 km/s, f(M)=0.0178 M_{o}, i ~ 78^{o}, Crampton, D., Hutchings, J. B., Cowley, H. P., and Schmidtke, P. C., 1997, ApJ 489, 903. + SMC, Supersoft. Optical counterpart a faint variable star, Orio, M., Della Valle, M., Massone, G., Ogelman, H., 1994, AA, 289, L11. + Vmax = 20.2, B-V = -0.15, U-B = -1.06, Schmidtke, P.C., Cowley, A.P., McGrath, T. K., 1996, AJ, 111, 788. + V = 21^{m}, Hasinger, G., 1994, in Review of Modern Astronomy, ed. G. Klare, (Astron. Geschl., Hamburg), Vol. 7, p. 129. + V~20.4, M_{v}~ +1.4, E(B-V)=0.1 mag, Crampton, D., Hutchings, J. B., Cowley, A. P., and Schmidtke, P. C., 1997, ApJ 489, 903. 0142+614 + Flux F_{x}= 5.5 E-10 erg/cm^{2}s, Mereghetti, S., Stella, L., 1995, ApJ , 442, L17. + F_{x}= 4.2 E-11 erg/cm^{2}s,White, N. E., Mason, K. O., Giommi, P., et al. 1987, MNRAS, 226, 64. + 1994 ASCA, 0.5-10 keV, F = 1.3 E-10 erg/cm^{2}s, White, N.E., Angelini, L., Ebisawa, K., et al. 1996, ApJ , 463, L83. + 4U 0142+61, Mereghetti, S., Stella, L., 1995, ApJ , 442, L17. + p= 8.687s, Hellier, W.C., 1994, MNRAS, 271, L21. Israel, G.L., Mereghetti, S., Stella, L., 1994, ApJ , 433, L25. + p/P' = 1.2 E5 / yr, Hellier, W.C., 1994, MNRAS, 271, L21. + P'= 7 E-5 s/yr, Steinle, H., Pietsch,W., Gottwald, M., Grazer, U., 1987, Astrophys. Space Sci., 131,687. Mereghetti, S., Stella, L., 1995, ApJ , 442, L17. + in 1979 p_{pulse}= 8.68736 +/- 0.00070 s, P'/p ~ (6.63 +/- 0.57) E-5 yr, in 1994 p_{pulse}= 8.68791 +/- 0.00015 s, White, N.E., Angelini, L., Ebisawa, K., et al. 1996, ApJ , 463, L83. + p_{pulse}= 8.68732 s, Israel, G.L., Mereghetti, S., Stella, L., 1994, ApJ , 433, L25. + Spin P'/p = (6.63 +/- 0.57) E-5 s/yr, White, N.E., Angelini, L., Ebisawa, K., et al. 1996, ApJ , 463, L83. + p_{pulse}= 8.68791 +/- 0.00015 s (68% confidence), White, N.E., Angelini, L., Ebisawa, K., et al. 1996, ApJ , 463, L83. + Dist (kpc) = 1.5, Mereghetti, S., Stella, L., 1995, ApJ, 442, L17. + Fx = 4.2 E-11 erg/cm^{2}s, Lx ( erg/s )= 2.4E37; and E35 (at 5 Kpc and 0.1-2.4 (keV) energy band), Lx/Lo 1E4, Log N_{H}(cm-2) = 21.99, Hellier, 1994, MNRAS, 271, L21. + Log N_{H}(cm-^{2}) = 23.6, White, N.E., Mason, K.O., Giommi, P., 1987, MNRAS, 226, 645. + Log N_{H}(cm-^{2}) = 22.18, Leisawitz, D., Bash, F.N., Thaddeus, P. 1989, ApJ, Supp. Ser., 70, 731. + N_{H}= 8 E21 cm^{-2}, White, N.E., Mason, K.O., Giommi, P., et al. 1987, MNRAS, 226, 645. + A_{v}= 4.7 mag., Predehl, P., Schmitt, J.H.M.M., 1995, AA, 293, 889. + d = 0.5 - 1 kpc, Mereghetti, S., Stella, L., 1995, ApJ, 442, L17. + L_{x}estimation (4.8 - 7.2 ) d^{2}_{kpc}E34, kT = 0.39 - 0.93 keV, kT = 0.4 - 0.9 keV, photon index 1.6 - 3.7, N_{H}= 9 E21 cm^{-2}, White, N.E., Angelini, L., Ebisawa, K., et al. 1996, ApJ, 463, L83. + N_{H}= ( 9.7 +/- 0.7) E21, L_{x}= 2.4 E37 at d = 5 kpc (0.1 - 2.4 keV), Hellier, C., 1994, MNRAS, 271, L21. + V 23^{m}, Hellier, C., 1994, MNRAS, 271, L21. + V 24^{m}, Steinle, H., Pietsch, W., Gottwald, M., Graser, U., 1987, Astrophys. Space Sci., 131, 687. + No optical counterpart with m_{v}< 23, White, N.E., Mason, K.O., Giommi, P., et al. 1987, MNRAS, 226, 645. 0422+32 + 1994 BATSE, 2-11 keV, maximum Fx = 9.3 E-9 erg/cm^{2}s, Callanan, P.J., Garciha, M.R., McClintock, J .E., et al. 1995, ApJ , 441, 786. + The X-ray Nova was discovered on 5.8.1992 by the BATSE instrument on board the GRO observatory. By 8 August the flux in the 20 - 300 keV band had reached >> 3 Crab, Paciesas, W., Briggs, M.S., Harmon, B.A., et al. 1992, IAU Circ. No. 5580. + Intensity, (0.1- 2.4) , 0.3 Crab, Pietsch, W., Briggs, M.S., Harmon, B.A., 1993, AA, 273, L11. + Intensity, At brightness maximum, X-ray novae are among the brightets X-ray sources. GRO J 0422+32 in its maximum was as bright as 3 Crab units, Sunyaev, S.A., Kaniovsky, A.S., Borozdin, K.N., 1993, AA, 280, L1. + Other Name, GRO J 0422+32 appears to be a member of a class of X-ray novae including at least 6 obJ ects which have been investigated in detail in the X-ray range: Mon X-Nova = A0620-00, OphiuchiX-Nova = H1705-25, Vul X-Nova = GS2000+25, V404 Cyg = GS2023 + 338, Musca X-Nova = GRS1124-648 and now GRO J 0422 + 32 in Perseus, Sunyaev, S.A., Kaniovsky, A.S., Borozdin, K.N., et al. 1993, AA, 280, L1. + 2 -11 keV, Fx = 9.3 E-9 ergs cm^{=2}at outburst max, Callanan, P.J., Garcia, M.R., McClintock, J .E., et al. 1995, ApJ , 1995, ApJ , 461, 351. + P_{orb}= 0.211 - 0.2157 day, Dominant Period of 5.06 hours, Chevalier, C., Ilovaisky, S.A., 1995, AA, 297, 103. Sunyaev, R.A., Kaniovsky, A.S., Borozdin, K.N., et al. 1993, AA, 288, L1. Kato, T., Mineshige, S., Hirata, R., 1995, PASJ , 47,31. + A transient 5.1/10.2 hr. modulation, which may be releated to the orbital period, has been observed during roughly half of our observations. however, confirmation of the orbital period must await obsevations in quiescence, Callanan, P.J., Garchia, M.R., McClintock, J .E., et al. 1995, ApJ , 441, 786. + l = 165.9, b = -11.9, Castro-Tirado, A.J., Pavlenko, E.P., et al. 1993, AA, 276, L37. + P = 0.21159 +/- 0.00057 d, Filippenko, A.V., Matheson, T., Ho, L.C., 1995, ApJ , 455, 614. + P = 0.2107 +/- 0.0012 d, Orosz, J.A., Bailyn, C.D., 1995, ApJ , 446, L59. + Weak ellipsoidal modulation at a period of 5.1 hr, Callanan, P.J., Garcia, M.R., McClintock, J .E., et al. 1996, ApJ , 461, 351. + Orbital period P = 0.212140 +/- 0.000003 d, Chevalier, C., Ilovaisky, S.A., 1996, AA, 312, 105. + Reached maximum flux in 6d. The decay with T = 40 to 44 days, Harmon, B.A., Zhang, S.N., Wilson, C.H., et al. 1994, "The second Compton Symposium", ed. L.E. Fitchel, et al. p. 210, New York AIP Conference Series. Vikhlinin, A., Churazov, E., Gilfanov, M., et al. 1995, ApJ , 441, 779. + Total outburst energy ~ 1.2 E44 erg, Tanaka, Y., Shibazaki, N., 1996, ARAA, 34, 607. + A_{v}= 1.2 +/- 0.1, d < 2.2 Kpc, Callanan, P.J., Garcia, M.R., McClintock, J.E., et al. 1996, ApJ, 461, 351. + d 1 kpc, Lx (2-11 keV) / L (opt+UV) >> 4 - 75, Callanan, P.J., Garcia, M. R., McClintock, J. E., et al. 1995, ApJ, 441, 786. + Dist ( kpc ) = 2, Av =1.25, Chevalier, C., Ilovaisky, S.H., 1995, AA, 297, 103. Castro-Trado, A.J., Pavlenko, E.P., Shlyapkinov, A.A., et al. 1993, AA, 276, L37. + Fx = 3000, (F max reaching an intensity 3 times that of the Crab Nebula), Harmon, B.A., Wison, R.B., Fishmann, G.J., Meegsn, C.A.,1992, IAU Circ. No. 5584. + d = 2.4 kpc, Bradt, H., McClintock, J.E., 1983, ARAA, 21, 13. + Lx/Lo = 44, Lo =1.8E35 erg/s, Lx max = 2.7 E37 erg/s in 2 - 300 keV band (for dist.= 2 kpc), photon index ~ 1.5, Sunyaev, R.A., Kaniovsky, A.S., Borozdin, K.N., et al.1993, AA, 280, L1. + Lx max = 8E36 erg/s in the 8-13 keV at d = 2 kpc, Castro-Trado, A.J., Pavlenko, E.P., Shyapkinov, A. A.,et al. 1993, AA, 276, L37. + kT (keV) =2 keV (Black Body), Kato, T., Mineshige, S., Hirata, R., 1995, PASJ, 47, 31. + Log N_{H}= 21.23, Pietsch, W., Haberl, F., Gehrels, N., Petre, R., 1993, AA, 273, L11. + log N_{H}(cm^{-2}) <21.7, Sunyaev, R.A., Kaniovsky, A.S., Borozdin, K.N., et al. 1993, AA, 280, L1. + Lx ( erg/s ) = 4.5 E36 in the 40-150(keV) Dist (Kpc) = 1, Vikhilin, A., Churazov, E.,Gilfanov, M., et al. ApJ, 1995, 441, 779. + Lx/Lo = 500, van Paradijs, J., Verbunt, F., 1984, in Nodley, S. (Ed.), "High Energy Transient in Astrophysics", p. 49. + Dist(kpc)=1.2, Vargas, M., Goldwurm, A., Laurent, P., et al., 1997, ApJ 476, L23. + Mx 2.4Mo , Mx = 3 - 6 Mo , Kato, T., Mineshige, S., Hirata, R., 1995, PASJ, 47, 31. + f(M) = 1.21 +/- 0.06 Mo , Mx = 3.57 +/- 0.34 Mo , M opt = 0.39 +/- 0.02 Mo , i = 48^{o}+/- 3, Kopt = 380.6 +/- 6.5 km/s, Kx = 41.6 +/- 3.2 km/s, Filippenko, A.V., Matheson, T., Ho, L.C., 1995, ApJ, 455, 614. + 2.9 Mo < Mx < 6.2 Mo , Mineshige, S., Hirose, M., Osaki, Y., 1992, PASJ, 44, L15. + Mx >= 3.4 Mo , i <= 45^{o}, Callanan, P.J., Garchia, M.R., McClintock, J.E., et al. 1996, 461, 351. + fx(M) = 3.1 +/- 0.4 Mo ,, M = 4 - 6 Mo , (Probable), Remillard, R.A., McClintock, J.E., Bailyn, C.D., 1992, ApJ, 399, L145. + Mx = 2.5 - 5 Mo , i = 41^{o}- 43^{o}, f(M) = 0.85 +/- 0.3 Mo , Kopt = 340 km/s, Casares, J., Martin, A.C., Charles, P.A., et al. 1995, MNRAS, 276, L35. + Mx 3 Mo , Mopt < 0.5 Mo , i < 59^{o}, K = 300 - 400 km/s, f(M) = 0.9 +/- 0.4 Mo , Orosz, J.A., Bailyn, C.D., 1995, ApJ, 446, L59. + Spec. Type M2V, Filipenko, A.V., Matheson, T., Ho, L.C., 1995, ApJ, 455, 614. Bessel, M., 1990, PASP, 102, 1181, Chevalier, C., Ilovaisky, S.A., 1996, AA, 312, 105. Castro- Tirado, A.J., et al. IAU, Circ. No. 5588. + Optical photometry, O'Donoghue, D., Charles, P.A., 1996, MNRAS, 282, 191. + Spec. Type, M0 V, with the disk contributing ~ 40% of the total light V about 13-20.7, Chevalier,C., llovaisky, S.H., 1995, AA, 297, 103. + V = 12.6^{m}, B ~ 13.5, optical counterpart,V 518 Per, Castro-Tirado, A.J., Pavlenko, P., Shlyapnikov, A., et al. 1993, AA, 276, L37. + Optical counterpart V 518 Per, Spect. Type, M2 +/- 2 V, Black Hole candidate, Orosz, J.E., Bailyn, C.D., 1995, ApJ, 446, L59. Casares, J., Martin, A.C., Charles, P,A., 1995, MNRAS, 276, L35. + At the maximum of mini-outburst, B-V = 0.38 +/- 0.02, primary outburst (B-V) = 0.15, Beskin, G., Neizvestny, S.I., Bartolini, C., et al. 1992, IAU, Circ. No. 5610. Callanan, P.J., Garcia, M.R., McClintock, J.E., et al. 1995, ApJ, 441, 786. + In December 1994, V = 22^{m}.24 +/- 0.14, R = 20.97 +/- 0.10, I = 20.22 +/- 0.07, Casares, J., Martin, A.C., Charles, P.A., et al. 1995, MNRAS, 276, L35. + The optical light curve exhibited a very slow decay and the presence of several mini-outburst during the following 18 months, Callanan, P., Garchia, M.R., McClintock, J.E., 1995, ApJ, 441, 786. Chevallier, C., Ilavaisky, S.A., 1995, AA, 297, 103. + Before it finally reached quiescence at V = 22.4, Zhao, D., Callanan, P., Carcia, M., McClintock, J. E., 1994, IAU, Circ. No. 6072. + Optical counterpart, E(B-V) = 0.3, 0.4, 0.2, Castro-Tirado, A.J., Pavlenko, E.P., Shlyapkinov, A A., et al. 1993, AA, 276, L37. Chevailer, C., llovaisky, S., 1995, AA, 297, 103. Harlaftis, E.T., Charles, P.A., 1993, IAU Cir. No. 5728. + E(B-V) = 0.3, Callanan, P.J., Michel R., Jeffery E., et al. 1995, ApJ, 442, 786. + E(B-V) = 0.2, Shrader, C.R., Wagner R. M., Starrfield S. G., et al. 1993, in the Second Compton Symposium, (ed) C.E. Fichtel, N. Gehrels and J.P. Norris (New York:AIP), 365. 0512-401 + Optical counterpart, E(B-V) = 0.02, Da Costa, G.S., Armandroff, T.E., 1990, AJ, 100, 162. 0513.9-6951 + LMC Supersoft, {alpha}_{2000}= 05 13 50.8, {delta}_{2000}= - 69 51 47 error +/- 1", Cowley, A.P., Schmidtke, P.C., Hutchings, J .B. et al. 1993, ApJ , 418, L63. Schaeidt, S., Hasingert, G., Trumper, J ., 1993, AA, 270, L9. + The X-ray variability of this source was discovered by ROSAT. The source brightened by a factor ~ 20 over 10 days, Cowley, A.P., Schmidtke, P.C., Hutching, J .B., et al. 1993, ApJ , 418, L63. + Was discovered by, Schaeidt, S., Hasinger, G., Trumper, J ., 1993, AA, 270, L9. + Supersoft. Transient P_{orb}= 0.76 d, Crampton, D., Hutchings, J .B., Cowley, A.P., et al. 1995, ApJ , 456, 320. + P_{orb}= 0.76278 +/- 0.00005 d, Alcock, C., Allsman, R.A., Alves, D., et al. 1996, MNRAS, 280, L94. + Orbital P = 0.43 d, Cowley, A.P., Schmidtke, P.C., Crampton, D., et al. 1995, "Supersoft X-ray sources in the LMC", IAU Symposium 165, Compact Stars in Binaries. + LMC, Supersoft. kT = 0.04 keV, L_{bol}= 2.5 E38, erg/s, Kahabka, P., 1995, in "The Lives of Neutron Stars", eds. M.A. Alpar, J. van PadiJs, U. Kiziloglu, p.409. + Supersoft. 0.4 < Mx < 1.2 Mo , Mopt < 0.2 Mo , fopt(M) =0.00011 Mo , i =15^{o}, Kopt =11+/- 2, Crampton, D., Hutchings, J.B., Cowley, A.P., et al. 1995, ApJ, 456, 320. + Kopt = 14.5 +/- 3 Km/s, Vg = 297 +/- 1 Km/s, i <= 7^{o}, Mx = 0.8 - 1.4 Mo , Southwell, K.A., Livio, M., Charles, P.A., et al. 1996, ApJ, 470, 1065. + 0.6M_{o}< M_{x}< 1.4 M_{o}. Southwell, K.A., Livio, M., and Pringle, J. E., 1997, ApJ 478, L29. + LMC, Supersoft. Optic counterpart HV 5682, during 1992 December and March 1993, V = 16.769 +/- 0.044, B-V = -0.112 +/- 0.012, Mv = -1.6, The optical counterpart has a faint red companion ( V = 19.067 +/- 0.067), (high velocity (4000 km/s) bipolar outflows or jets, Southwell, K.A., Livio, M., Charles, P.A., et al. 1996, ApJ, 470, 1065. Cowley, A.P., Schmidtke, P.C., Hutchings, J.B., et al. 1993, ApJ, 418, L63. + D (B-V) ~ 0.1 - 0.2, D (V-R) ~ 0.1, V = 19.8 +/- 0.2, B = 19.6 +/- 0.3, Reinsch, K., van Teeseling, A., Beuerman, K., Abbott, T.M.C., 1996, AA, 309, L11. Pakull, M.W., Motch, C., Bianchi, L., et al. 1993, AA, 278, L39. + V = 16.8, Mv = -2, E(B-V) = 0.1, V = 16.7 - 16.8 when it is "bright" and V = 17.0 - 17.1 when it is "faint" several higher ionization emission features, Crampton, D., Hutchings, J.B., Cowley, A.P., et al. 1995, ApJ, 456, 320. + The system probably comprises a relatively massive white dwarf accreting at a high state ( E-6 Mo yr^{1}), Southwell, K.A., Livio, M., Charles, P.A., et al. 1996, ApJ, 470, 1065; Southwell, K. A., Livio, M., and Pringle, J. E., 1997, ApJ 478, L29. + V = 16.6 - 16.8, show strong He II {lambda} 4686 line, O VI {lambda} {lambda} 3811, 34 lines, an indication of the {lambda} 4640 line complex and relatively strong H{alpha} and H{beta} Balmer emission lines, Hasinger, G., 1994, in Reviews of Modern Astronomy, ed. G. Klare, (Astron. Gescl., ) Hamburg, V7, p.129. 0521-720 + LMC, Dist ( kpc ) = 50, Av = 0.3, Smale, S.A., Corbet, R.H.D., Charles, P.A., et al. 1988, MNRAS, 223, 51. + Log N_{H}(cm-2) ~ 22, Bonnet-Bidaud, J.M., Motch, C., Beuermann, K., et al. 1989, AA, 213, 97. + LMC, Suppersoft. Mx = 1.4 Mo , Mopt ~ 0.8 Mo , i < 70^{o}, Bonnet-Bidaud, J.M., Motch, C., Beuermann, K., et al. 1989, AA, 213, 97. + LMC. Spec. Type, Blue Star, Bonnet-Bidaud, J.M., Motch, C., Beuermann, K., et al. 1989, AA, 213, 97. + Mv = -0.3, V = 18.5, E(B-V) = 0.1, van Paradijs, J., McClintock J.E., 1994, AA, 290, 133. 0527.8-6954 + LMC, Supersoft. Was detected with the ROSAT PSPC in an X-ray survey of the LMC, in J une 16-17 1990, ROSAT in the 0.1-2.4 keV band Fx=0.11 cnt/s, Trumper, J., Hasinger, G., Aschenbach, B., et al. 1991, Nature, 349, 579. + a_{2000}= 05 27 48.3, {delta}_{2000}= -69 54 16, ROSAT PSPC 6 November, 1992 Fx = 0.06 count/s, Cowley, A.P., Schmidtke, P.C., Hutchings, J .B., et al. 1993, ApJ , 418, L63. + a_{2000}= 05 27 48.5, {delta}_{2000}= -69 54 10.6, Hasinger, G., 1994, Reviews of Modern Astronomy, Vol. 7, p. 129. + ROSAT PSPC May 1992, Fx= 0.07 counts/s, Orio, M., Ogelman, H., 1993, AA, 273, L56. + Supersoft. Probably transient, Trumper, J., Hasinger, G., Aschenbach, B., et al. 1991, Nature, 349, 579. + LMC, Supersoft. kT (keV) = 0.016, Log N_{H}(cm-2) ~ 21.65, Greiner, J., Hasinger, G., Kahabka, P., 1991, AA, 246, L17. + LMC, supersoft N_{H}= 1.5 E21 cm^{-2}, Cowley, A.P., Schmidtke, P.C., Hutchings, J.B., et al. 1993, ApJ, 418, L63. + kT = 0.03 keV, Kahabka, P., 1995, in "The Lives of Neutron Stars", eds. M.A. Alpar, J. van PadiJs, U. Kiziloglu, p.409. + bolometric luminosity = 5 E38 erg/s, Kahabka, P., Pietsch, W., Hasinger, G., 1994, AA, 288, 538. + kT(keV) = 0.02-0.05, log N_{H}= 20.78 cm^{-2}, L(0.1-0.3 keV) = 2 E36 erg/s, Trumper, J., Hasinger, G., Aschenbach, B., et al. 1991, Nature, 349, 578. + LMC, Supersoft. Possible optical counterpart HV2554 at V = 15.8, Cowley, A.P., Schmidtke, P.C., Hutchings, J.B., et al. 1993, ApJ, 418, L63. + HV 2554 inlikely to be counterpart, counterpart is fainter than 17^{m}, Hasinger, G., 1994, Reviews af Modern Astronomy, ed. G. Klare, (Astron. Gescl., Hamburg), V7, p.129. 0543.6-6822 + LMC, Supersoft. Discovered in the original Einstein survey of the LMC, Long, K.S., Helfand, D.J ., Grabelsky, D.A., 1981, ApJ , 248, 925. + Optical position 2000 yr RA= 05 43 34.2, Dec= -68 22 21.7, Schmidtke, P.C., Cowley, A.P., Frattare, L.M., McGrath, T.K., 1994, PASP, 106, 843. + Supersoft. LMC. P_{orb}= 1.08 day, van ParadiJ s, J ., McClintock, J .E., 1994, AA, 290, 133. Smale, A.P., Corbert, R.H.D., Charles, P.A., et al. 1988, MNRAS, 233, 51. + P_{orb}= 1.04 d, Cowley, A.P., Crampton, D., Hutchings, J .B., et al. 1984, ApJ , 286, 196. + LMC, Supersoft. Dist ( kpc ) = 55, Mv = -1.2, Crampton, D., Cowley, A.P., Hutchings, J.B., et al. 1987, ApJ, 321, 745. + LMC, supersoft Mv = -1.6, Lx ( erg/s ) = 3.2 E36 (in 0.15-4.5 keV), Lx / Lo ~ 0.7, Smale, A.P., Corbet, R.H.D., Charles, P.A., et al. 1988, MNRAS, 233, 51. + kTbb, (keV) = 0.025, Log N_{H}(cm-^{2}) ~ 21.48, Greiner, J., Hasinger, G., Kahabka, P., 1991, AA, 246, L17. + kT_{bb}(keV) = 0.040, Kahabka, P., 1995, in "The Lives of Neutron Stars", eds. M.A. Alpar, J. van Paradijs, U. Kiziloglu, p.409. + Lx (erg / s) ~ 2 E36, Crampton, D., Cowley, A.P., Hutchings, J.B., et al. 1987, ApJ, 321, 745. + Lx (erg / s) 3 E37, Remillard, R.A., Rappaport, S., Macri, L.M., 1995, ApJ, 439, 646. + LMC, Supersoft. Mx < 3.2 Mo , Mopt < 1 Mo , Kopt (km/s) = 40, f(M) = 6.9 E-4 Mo , Smale, A.P., Corbet, R.H.D., Charles, P.A.,1988, MNRAS, 233, 51. + i < 20^{o}, Kahabka, P., 1996, AA, 306, 795. + LMC, Supersoft. Spec. Type,WR pec. em., Ables, J.G., 1969, Proc. Astron. Soc. Aust. 1, 237. + V = 16.2-17.3, Mv = - 2.1, E (B-V) = 0.1, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + V ~ 17, Cowley, A.P., Crampton, D., Hutchings, J.B., et al. 1984, ApJ, 286, 196. + Mv = -1.6, Smale, A.P., Corbert, R.H.D, Charles, P.A., et al. 1988, MNRAS, 233, 51. Pakull, M.W., Beuermann, K., van der Klis, M., van Paradijs J., 1988, AA, 203, 127. Cowley, A.P., Schmditke, P.C., Crampton, D., Hutchings J.B., 1990, ApJ, 350, 288. + Mv = -1.2, B - V = - 0.023, U - B = - 1.1, Crampton, D., Cowley, A.P., Hutchings, J.B., et al. 1987, ApJ, 321, 745. + E(B-V) = 0.1, Remillard, R.A., Rappaport, S., Macri, L.M., 1995 ApJ 439, 976. 0547-711 + Supersoft. Range (2-10), The two spectra associated with the lowest X-ray fluxes 1.2, 1.1 E -9 erg/cm^{2}s. Two other spectra with slightly larger X-ray fluxes 1.5 E-9 erg/cm^{2}s , Barret, D., Grindlay J .E., 1995, Ap J , 440, 841. + Range (0.5-20), Intensity, Christian, D.J., 1993, Ph.D. thesis, Univ. Maryland. + Discovered in the original Einstein survey of the LMC , Long, K.S., Helfand, D.J ., Grabelsky, D.A., 1981, ApJ , 248, 925. + Supersoft, LMC. P_{orb}= 10.6 h, van ParadiJ s, J ., McClintock, J .E., 1994, AA, 290, 133, Cowley, A.P., Schmidtke, P.C., Crampton, D.,Hutchings, J .B., 1990, ApJ , 350, 288. Pakull, M.W., Buermann, K., van der Klis, M., van ParadiJ s, J .,1988, ApJ , 203, 229. + P_{orb}= 0.442 d, Schmidtke, P.C., McGrath, T.K., Cowley, A.P., et al. 1993, PASP, 105, 863. + LMC, Supersoft. Dist (Kpc)= 55, Cowley, A.P., Schmidtke, P.C., Crampton, D., Hutchings, J.B., 1990, ApJ, 350, 288. + LMC, supersoft kT_{bb}(keV) = 0.055, Kahabka, P., 1995, in "The Lives of Neutron Stars", eds. M.A. Alpar, J. van Paradijs, U. Kiziloglu, p.409. + Lx (erg / s) = 8 E35, Lx / Lo = 6, Khruzina, T.S., Cherepashchuk, A. M., 1994, Astron Report., 38, 386. + Bolometric luminosity 5 E38 erg/s, N_{H}= 1.5 E22 cm^{-2}, kT = 0.034 +/- 0.01 keV, Kahabka, P., Pietsch, W., Hasinger, G., 1994, AA, 288, 538. Schmidtke, P.C., McGarth, T.K., Cowley, A.P., Frattare, L.M., 1993, PASP, 103, 863. + A_{v}= 0.2, Deutsch, E.W., Margon, B.,Wachter, S., Anderson, S.F., 1996, Ap.J.,471, 979 + LMC, Supersoft. Mx = 5.2 - 7.7 Mo , Mopt = 0.6 - 0.7 Mo , Khruzina, S., Cherepashchuk, A.M., 1994, Astron. Report., 38, 386. + Mx 6 Mo , Mopt = 1 - 1.5 Mo , i 70^{o}, Cowley, A.P., Schmidtke, P.C., Crampton, D., Hutchings, J.B., 1990, ApJ, 350, 288. + M_{x}< 0.9 M_{o}. Southwell, K.A., Livio, M., and Pringle, J. E., 1997, ApJ 478, L29. + LMC, Supersoft. Black Hole?, Eclipses at both optical and X- ray wavelenghts, Schmidtke, P.C., McGrath, T.K., Cowley, A.P., Frattare, L.M., 1993, PASP, 105, 863. + Black Hole, V=18.9, B-V=-0.15 - 0.14, U-B= - 0.7 - -0.95, Deutsch, E.W., Morgan, B., Wachter, S., Anderson, S.F., 1996, Ap.J., 471, 979. Kahabka, P., 1996, AA, 306, 795. + Optical counterpart: Spec. Type: ~ d G0, V = 18.8 - 20.0, B = 16.7, Crampton, D., Cowley, A.P., Thompson, I.B., Hutchings, J.B., 1985, AJ, 90, 43. + Mv=0.5, Khruzina, T.S., Cherepashchuk, A.M., 1994, Astron. Report, 38, 386. + B - V = 0.14, Cowley, A.P., Schmidtke, P.C., Crampton, D., Hutchings, J.B., 1990, ApJ, 350, 288. + Mv= 0.0, V = 18.8, E(B-V) = 0.1, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. 0614+091 + X-ray burster. Swank, J. H., Becker, R. H., Boldt, E. A., et al., 1978, MNRAS 182, 349; Brandt, S., Castro-Tirado, A.J., Lund, N., et al., 1992, AA 262, L15. + QPOs, possible spin period 3.1 ms, Ford, E., Kaaret, P., Tavani, M., et al., 1997, ApJ 475, L123. + Dist (Kpc) = 5 +/- 3, Brandt, S., Castro-Tirado, A.J., Lund, N.,et al. 1992, AA, 262, L15. + Dist (Kpc) = 4, Davitsen, D.A., Malina, R., Bowyer, S., 1977, ApJ, 211, 866. + Dist (Kpc) = 2, Lx (erg / s) = (1-8) E36 (in 2-6 keV), (1-10) E36 (in 1-20 keV), 1 E37 (35-200 keV), Barret, D., Grindlay, J.E., 1995, ApJ, 440, 841. + kT (keV) ~ 0.6-1.6, LogN_{H}(cm-2) = 22.9, Lx ( erg/s ) = (3- 4) E36 (in 1-20 keV), Sign, K.P., Apparao, K.M.V., 1994, ApJ, 431, 826. + Lx ( erg/s ) = 8 E36 (in 0.5-20 keV) for distance 5 Kpc., Log N_{H}(cm-2) = 21.26, Christian, D.J., White, N.E., Swank, J.H., 1994, ApJ, 422, 791. + Lx ( erg/s ) ~1E37, Churazov, E., Gilfanov, M., Sunyaev, R., 1995, ApJ, 443, 341. + Spec. Type: Optically identified with a blue stars, B ~ 18.8, Davidsen, D.A., Malina, R., Smith, A., et al. 1974, ApJ, 193, L25. + B -V = 0.26, U-B=-0.5, E(B-V)~0.3, Machin, G., Callanan, P.J., Charles, P.A., et al. 1990, MNRAS, 247, 205. 0620-003 + Discovered on August 3, 1975 with ARIEL-V, Max Fx >> 25 Crab (2 -18 keV) at Aug. 14, Elwis, M., Page, C.G., Pounds, K.A. et al. 1975, Nature, 57, 656. + P = 0.325 d, McClintock, J.E., Horne, K., Remillard, R.A., 1995, ApJ , 442, 358. + X-ray light - curve, Ward, M., Penston, M., Murray, C., Clements, E., 1975, Nature, 257, 659. Amnuel, P. R., Guseinov, O.H., 1976, Sov. Astr. Lett., 2, 392. Amnuel, P.R., Guseinov, O.H., Rakhamimov, S.J ., 1974, Astrophys. Space Sci., 1974, 29, 331. Kaluzienski, L.J ., Holt, S.S., Boldt, E.A., Serlemitsos, P.J ., 1977, ApJ , 212, 203. + Porb = 0.323 +/- 0.014 d, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. McClintock, J .E., Remillard, R.A., 1986, ApJ , 308, 110. Kaluzienski, L.J ., Holt, S.S., Boldt, F.A., 1977, ApJ , 212, 209. + Dist (Kpc) = 0.6-1.4, Shahbaz, T., Sanson, A.E., Naylor, T., Dotani, T., 1994, MNRAS, 268, 763. + Log N_{H}(cm-2) = 21.59, de Kool, M., 1988, ApJ, 334, 336. + d = 1 kpc, L = 6 E30 erg/s, Log N_{H}(cm-2) = 21.20, McClintock, J.E., Horne, K., Remillard, R.A., 1995, ApJ, 442, 358. + The quiescent X-ray luminosity is the lowest value that has been repoted for any X-ray nova, and is only ~5E-8 of peak luminosity observed during the 1975 outburst. Lx max, The peak X-ray luminosity 1E38 erg/s, (1-10 keV), Elvis, M., Page, C.G., Pounds, K.A., et al. 1975, Nature, 257, 656. + Dist (Kpc) = 0.87, Lx ( erg/s ) =1 E38 (in 1-1(keV), Oke, J.B., 1977, ApJ, 217, 181. + Lx (erg / s) < 1E32, McClintock, J.E., Petro, L.D., Remillard, R.A., Ricker, G.R., 1983, ApJ, 266, L27. + Decay constant at (3-6 keV) 24 d, Kaluzienski, L.L., Holt, S.S., Boldt, E.A., Serlemitos, P.J., 1977, ApJ, 212, 203. + Photon index ~ 1.6, Ricketts, M.J., Pounds, K.A., Turner, M.J.L., 1975, Nature, 257, 657. + Mx ~ 10 Mo , Mopt = 0.6 Mo , Shahbaz, T., Ringwald, F.A., Bunn, J.C., et al. 1994, MNRAS, 271, L10. + Mx = 2.70 - 3.2 Mo , f(M) = 3.18 +/- 0.16 Mo , Mopt ~ 0.5 - 0.8 Mo , Kx < 70 km/s, Kx = 43 +/- 8 km/s, Kopt = 457 +/- 8 km/s, McClintock, J.E., Remillard, R.A., 1986, ApJ, 308, 110. + Kopt = 457 +/- 8 km/s, Kx = 43 km/s, f(M) = 3.19 +/- 0.17 Mo , Vg = -28 km/s, M_{x}= 3.19 - 3.82 Mo for i = 90^{o}, M_{opt}= 0.36 +/- 0.07 Mo, Haswell, C.A., Shafter, A., 1990, ApJ, 359, L47. + Mx = 5.17 Mo , Shahbaz, T., Naylor, T., Charles, P.A., 1994, MNRAS, 268, 756. + Kopt = 442 +/- 4 Km/s, fopt(M) = 2.9 +/- 0.08 Mo , McClintock, J.E., Remillard, R.A., 1989, BAAS, 21, 1206. + Spec. Type: K4 - K5 V, V = 18.3, Murdin, P., Allen, D.A., Morton, D.C., et al. 1980, MNRAS, 192, 709. K3, Shazbaz, T., Sansom, A.E., Naylor T., Dotani, T., 1994, MNRAS, 268, 756. + K4 V - K7 V, V = 18.5 at quiescence, Oke, J.B., 1977, ApJ, 217, 181. Whelan, J. A., Ward, M.J., Allen, D.A., 1976, MNRAS, 180, 657. Murdin, P., Allen, D.A., Morton, D.C., et al. 1980, MNRAS, 192, 709. + V = 11.2, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + V ~ 12 - 18.3, preoutburst brightness, optical counterpart V616 Mon, Boley, F., Wolfson, R., Bradt, H., et al. 1976, ApJ, 203, L13. + B ~ 12, at the peak of out burst, B ~ 18.5, at the quiescence, Haswell, C.A., Shafter A.W., 1990, AA, 359, L47- L50. + During the 18 months (after the eruption) the optical counterpart, V616 Mon, faded some 6 mag from B ~ 12 at the peak of the out burst to B ~ 18.5 at quiescence, Oke, J.B., 1977, ApJ, 217, 181. + B -V = 1.4, McClintock, J.E., Remillard, R., 1986, ApJ, 308, 110. + Mv = 0.7, E (B-V) = 0.4, van Paradijs, J., McClintock, J.E., 1994, AA, 227, 133. + E (B-V) = 0.35, V = 18.3 preoutburst brightness, E (B-V) = 0.35, McClintock, J.E., Horne, K., Remillard, R.A., 1995, ApJ, 442, 358. 0656-072 + Spec. Type: K, Amnuel, P.R., Guseinov, O.H., Rakhaminov, S. H., 1974, Astrophys. Space. Sci., 29, 331. 0748-676 + Discovered by EXOSAT in 1985 February and displays 8 minute eclipses with a period of 3.8 hr, Parmar, A.N., White, N.E., Giommi, P., Haberl, F., 1985, IAU Circ. No. 4039. + EXOSAT 8 dates from 15 February 1985, 10.5-13.2 E-10 erg/cm^{2}s (0.1-20 keV) up to 19 J uly 1985, 13.5 E-10 erg/cm^{2}s, Gottwald, M., Haberl, F., Parmar, A.N., White, N.E., 1986, ApJ , 308, 213. + Porb = 0.159 d, van ParadiJ s, J .P, McClintock, J .E., 1994, AA, 290, 133. The 5.6 hours orbital period is increasing on a timescale of 2.9 E6 yr, Hellier, C., Mason, K.O., Smale, A.P., Kilkenny, O., 1990, MNRAS, 224, 390. + P_{orb}= 3.82 h, orb. P'/P = 2 E-7 /yr, Parmar, A.N., Smale, A.P., Verbunt, F., Corbert, R.H.D., et al. 1991, ApJ , 366, 253. + Dist (Kpc) = 6, Crampton, D., Cowley, A.P., Stauffer, J., et al. 1986, ApJ, 306, 599. + Dist (kpc) = 2.1, Schoembs, R., Zoeschinger, G., 1990, AA, 227, 105. + kT (keV) = 1.6 keV, the correspondig radii are 8.7 km and 4.4 km.,Lx ( erg/s ) = (3.6-22) E36, Lx max = 3.9 E38, d=10kpc, (in 0.1-2(keV), Gottwald, M., Haberl, F. Parmar, A. N., White, N. E., 1986, ApJ, 308, 213. + Mx = 1.4 Mo , van Paradijs, J., van der Klis, M., Pedersen, H., 1988, AA Supp. Ser., 76,185. + Kopt (km/s) = 210 +/- 92, Crampton, D., Cowley, A.P., Stauffer, J., et al. 1986, ApJ, 306, 599. + a_{2}Sin i = 1.46 Ro , Schoembs, R., Zoeschinger, G., 1990, AA, 227, 105. + Optical counterpart UY Vol, Spec. Type: O6 V, B - V = 0.14, U - B = - 0.86, Schoembs, R., Zoeschinger, G., 1990, AA, 227, 105. + Mv = 1.2, V = 16.9, E(B-V) = 0.42, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. 0834-430 + ROSAT, 13-16 Nov. 1990 and May 1991 in (1-24 keV) F_{x}= 0.49 cts/s, RA = 08 35 55.1, Decl. = -43 11 22 (2000.0), Belloni, T., Hasinger, G., Pietsch, W., et al. 1993, AA, 271, 487. + pulse p =12.3203+/- 0.0015s Lx = (1.3+/- 0.3) E36 (d/10 kpc)^{2}erg/s in (1-2.4 keV) range, N_{H}= (2.4+/- 0.3) E22 cm^{-2}, Belloni, T., Hasinger, G., Pietsch, W., et al. 1993, AA, 271, 487. 0836-42 + Intensity, 0.74 (cts/s), Range, 1-2.4 KeV (ROSAT), RA = 08 37 23.6, Decl. = -42 54 02, (2000.0), ROSAT 13-16 Nov. 1990 and May 1991 (1-2.4 keV), Fx = (1.2 +/- 0.3) E-10 erg/cm^{2}s, Belloni, T., Hasinger, G., Pietsch, W., et al. 1993, AA, 271, 487. 0836-429 + kT (keV) = 4, Cominsky, L., Jones, C., Forman, W., Tananbaum, H., 1978, ApJ, 224, 46. + Log N_{H}(atoms cm^{-2}) <= 22.5, Markert, T.H., Canizares, C.R., Clark, G.W., et al. 1977, ApJ, 218, 801. + Lx(1.0-2.4 keV) = (1.4+/- 0.3) E36 (d/10 kpc)^{2}, N_{H}= (2.2+/- 0.3) E22 cm^{-2}, Belloni, T., Haqsinger, G., Pietsch, W., et al. 1993, AA, 271, 487. 0918-549 + Dist (Kpc) =15, Lx ( erg/s ) = 5.2 E35, Lx / Lo = 800, Av =1.0, Chevalier, C., Ilovaisky, S. A., 1987, AA, 172, 167. 0921-630 + Porb = 9.012 d, Mason, K.O., Branduardi - Raymont, G., Cordova, F., Corbert, R.H.D., 1987, MNRAS, 226, 253. + Dist (Kpc) = 1.2 - ~ 8, Smale, S.A., Corbet, R.H.D., Charles, P.A., et al. 1988, MNRAS, 223, 51. + kT (keV) = 13.4 +/- 0.5, Log N_{H}(cm-2) = 21.76, Av = 2.7 +/- 0.8, Brundiardi-Raymont, G., Corbet, R.H.D., Mason, K.O., et.al 1983, MNRAS, 205, 403. + d = 7-10 kpc, Cowley, A.P., Crampton, D., Hutchings, J. B., 1982, ApJ, 256, 605. + L = 8.8 E36 ergs/s, Murray, S.D., Woods, D.T., Castor, J. I., et al. 1996, ApJ,______ + Mx = 1.4 Mo , Mopt = 0.6 Mo , i = 85^{o}, a = 1.9 E12 cm, Murray, S.D., Woods, D.T., Castor, J.I., et al. 1996, ApJ, ***. 0925.7-4758 + Supersoft, Hasinger, G., 1994, Reviews of Modern Astronomy, ed.G. Klare, (Astron. Ges.,Hamburg) Vol.7, p. 129. + P_{orb}= 3.5 d, Hasinger, G., 1994, on Rewievs of Modern Astronomy, ed. G. Klare, (Astron. Geschl. Hamburg), Vol.7, p.129. + Dist (kpc)_{min}0.4, kT (keV) = 0.030-0.055, N_{H}= (1.4-3.7) E22 cm^{-2}, Hasinger, G., 1994, "Rewievs of Modern Astronomy", ed. G. Klare, (Astron. Geschl. , Hamburg), Vol. 7, p.129. + 0.6 M_{o}< M_{x}< 1.4 M_{o}. Southwell, K.A., Livio, M., and Pringle, J. E., 1997, ApJ 478, L29. + The object could be spectroscopically identified with a 17^{m}star with an H{alpha} ,He II 4686 and Bowen NIII/CIII 4640-60 emission line spectrum very similar to conventional LMXB, Motch, C., Hasinger, G., Pietsch, W., 1994, AA, 284, 827.. 1009-45 + Discovered by Granat, Lapsov, I., Sazonov, S., Sunyaev, R.A. et al. 1993, IAU, Circ., No: 5864. + P_{orb}= 6.86 +/- 0.12 h, Shahbaz, T., van der Hooft, F., Charles, P.A., et al. 1996, MNRAS, 282, L47. + Dist(kpc)=2.6, Vargas, M., Goldwurm, A., Laurent, P., et al., 1997, ApJ 476, L23. + i 37^{o}, Shahbaz, T., van der Hooft, F., Charles, P.A., et al. 1996, MNRAS, 282, L47. + Spec. Type: Blue Star, V = 14.6, Della Valle, M., Benetti, S., 1993, IAU, Circ. No. 5890. + V = 14-20, R = 20.6, ellipsoidal modulation with amplitude 0.23 mag, Shahbaz, T., van der Hooft, F., Charles, P.A., et al. 1996, MNRAS, 268, 763. 1048.1-5937 + Intensity 2.2 E -11 (erg/cm^{2}s), Range, 2-10 KeV, Mereghetti, S., Caraveo, P.A., Bignami, G.F., et al. 1992, AA, 263, 172. + RA= 10 50 07.83, Dec. = -59 53 15.50 (2000), Mereghetti, S., 1995, ApJ, 455, 598. + F_{x}=5.8 E-12 ergs/cm^{2}s for 2-10 keV band, ASCA observations on 1994 March 2 and 5, Corbet, R.H.D., Mihara, T., 1997, ApJ 475, L127. + Spin down (9.19 +/- 0.42) E-4 syr^{-1}during 1992, slow than p' ~ 5 E-4 syr^{-1}, Mereghetti, S., ApJ, 1995, 455, 598. Mereghetti, S., Caraveo, P., Bignami, G.F., 1992, AA, 263, 172. + spin p'/p = 7.1 E-5 yr^{-1}, p' = 5 E-4 syr^{-1}, Corbert, R.H.D., Day, C.S.R., 1990, MNRAS, 243,553. + p-pulse= 6.64 - 6.44, Mereghetti, S., Stella, L., 1995, ApJ, 442, L17. Seward, F., Charles, P.A., Smale, A.P., 1986, ApJ, 305, 814. + p = 6.4 s, p' = 5 E-4 s / yr, Mereghetti, S., Caraveo, P. A., Bignami, G. F., 1992, AA, 1992, 263, 172. Smale, A. P., Corbert, R.H.D., Charles, P.A., et al. 1988, MNRAS, 233, 51. + p = 6.44 s, Seward, F., Charles, P.A., Smale, A.P., 1986, ApJ, 305, 814 + p'= 5 E-4 s / yr, Corbert, R.H.D., Day, C.S.R., 1990, MNRAS, 243, 553. + p-pulse=6.446645+/- 0.000001s, p'=(10.41+/- 0.10)E-4 s/yr. Corbet, R.H.D. and Mihara, T., 1997, ApJ 475, L 127. + Dist (Kpc) =10.6, Lx (erg/s) =2.8 E35, Mereghetti, S., Stella, L. 1995, ApJ, 442, L17. + A_{v}~ 8, 7, Mereghetti, S., Caraveo, P.A., Bignami, G.F., 1992, AA, 263, 172. + L_{x}(erg/s) < 1 E36, Log N_{H}(cm^{-2}) = 22.3, Seward, F., Charles, P.A., Smale, A.P., 1986, ApJ, 305, 814. + Dist (Kpc) = 10, kT (keV) &sup3; 1, L (0.5 - 2.5 keV) = (1 - 4) E35 at d = 10 Kpc, N(H) = 5 E21 - 1.5 E22 (cm^{-2}), N(H) = 1.6 E22, Seward, F., Charles, P.A., Smale, A.P., 1986, ApJ, 305, 814. + Blackbody kT=0.55+/- 0.02 keV, N_{H}=(0.55-1.62) E22 cm^{-2}, L_{x}=6.3 E33 ergs/cm^{2}s for d=3 kpc, 2-10 keV, ASCA on 1994 March 2 and 5, Corbet, R.H.D., and Mihara, T., 1997, ApJ 475, L127. 1124-684 + Detected on J anuary 8,1991 with GINGA all sky monitor, Makino, F., et al. 1991, IAU Circ. No. 5161. + GINGA, 1-6 keV, 5.1.1991 the Fx < 50mCrab, 8.1.1991 the Fx ~ 0.8 Crab or 1.6 counts/cm^{2}s, Kitamoto, S., Tsunami, H., Miyamoto, S., Hayashida, K., 1992, ApJ , 394, 609. Brandt, S., Castro-Tirado, A.J ., Lund, N., et al. 1992, AA, 254, L39. + Independently with the GRANAT / WATCH, Sunyaev, R.A., 1991, IAU Circ. No. 5176. Lund, N., Brand, S., 1991, IAU, Circ. No. 5161. + Granat: Soft emission (belov 8 keV) changed gradually with characteristics decay time ~ 30 days. On J anuary 20-21, 1991 detected emission line near 500 keV with flux ~ 7 E-3 phot/cm^{2}s, Gilfanov, M., Sunyaev, R., Churazov, J ., et al. 1991, Astronomy Lett., 17, 1059. + GRANAT, (35-100 keV), 1991, J an. 9-10, (14.5 +/- 0.53) E-2 phot/cm^{2}s, May 31, (0.50+/- 0.14) E-2 phot/cm^{2}s; Aug. 14-15, (1.01+/- 0.14) E-2 phot/cm^{2}s, Sunyaev, R., Churazov, E., Gilfanov, M., et al. 1992, ApJ , 389, L75. + GRANAT (6-15 keV), 8-13 J an 1991. Teaching a peak flux of 2.2 Crab, Brandt, S., Castro-Tirado, A.J ., Lund, N., et al., 1992, AA, 254, L39. + RA = 11 24 10, Dec. = -68 24 (1950), West, R., 1991, IAU circ. No: 5165. + P_{orb}= 0.4332 days, Remillard, R.H., McClintok, J .E., Bailyn, C.D., 1992, ApJ , 399, L145. + l =297, b= -7^{o}, Shrader, C.R., Gonzales Riestra, R., AA, 1993, 276, 373. + Orbital photometric period 0.436044 +/- 0.0000034 d, spectroscopic orbital period 0.4326058 +/- 0.0000031 s, Orosz, J.A., Bailyn, C.D., McClintock, J .E., Remillard, R.A., 1996, ApJ , 468, 380. + With a rise time from 10 to 90% of the peak in 4-5 days, it reached a maximum of -2.5 E38 erg/s (d=3 kpc). The count rate (1-20 keV) decayed exponentialy with T=30 d, while bolometric L with T=40d, Ebisawa, K., Ogawa, M., Aoki, T., et al. 1994, PASJ , 46, 375. + X-ray light curve are very similar A620-003. the total outburst energy E45 erg, Tanaka, Y., Shibazaki, N., 1996, ARAA, 34, 607. + kT (keV) = 0.96, Log N_{H}(cm-2) = 21.34, Greiner, J., Hasinger, G., Molendi, S., Ebisawa, K., 1994, AA, 285, 509. + d = 3 kpc, West, R.M., 1991, in Proc. Workshop on Nova Muscae 1991, Lyngby, (ed) S. Brandt, p. 143. + Lx (2-11 keV) / Lbol (Opt.+UV) ~ 75 at minimum., Della Valle, M., Pakull, M.,1991, IAU Circ. No. 5165. Kitamoto, S., Tsunemi, H., Miyamoto, S., Hayashida, K., 1992, ApJ, 394, 609. + kT (keV) ~ 1, (The typical dereddened continue which were measured for Nova Muscae 1991 are approximately fitted by a power laws indices ranging from -2.2 to -2.7)., Dist (Kpc) = 1 - 4, Shrader, C.R., Gonzales-Riestra, R., 1993, AA, 276, 373. + Dist (Kpc) = 0.5 - 5, Grebenev, S.A., Sunyaev, R.A., Pavlinsky, M.N., 1991, in Brandt, S.(ed.) Proc. Workshop on Nova Muscea 1991. + Dist (Kpc) = 1.4, Della Valle, M., Jarvis, B.J., West, R.M., 1991, Nature, 353, 50. + Dist (kpc) = 5.5 +/- 1.0, Orosz, J.A., Bailyn, C.D., McClintock, J.E., Remillard, R.A., 1996, ApJ, 468, 380. + L_{max}(at d=3) =2.5 E38 erg/s, Tanaka, Y., Shibazaki, N., 1996, ARAA, 34, 607. + The 3-300 keV luminosity of the source changed from 6 E36 erg/s (at d=1 kpc) on 16.01.91 to 2 E35 erg/s on 15.08.91, Gilfanov, M., Churazov, E., Sunyaev, R., et al. 1995, in "The Lives of Neutron Stars", eds. Alpar, M.A., ParadiJs, J., Kiziloglu, U., p.331. + Photon index of 2.5 - 2.7 extended to ~ 500 keV, Sunyaev, R., Churazov, E., Gilfanov, M., et al. 1992, ApJLett., 389, L75. + Dist(Kpc) = 3.9, West, R.M., 1991, in Proc.Workshop on Nova Mus 91, ed. S.Brandt, (Lyngby: DSRI), 143. + Dist(kpc)=2.2, Vargas, M., Goldwurm, A., Laurent, P., et al., 1997, ApJ 476, L23. + Mx = 6 +/- 1.5 Mo , f(M) = 3.1 +/- 0.4 Mo , Greiner, J., Hasinger, G., Molendi, S., Ebisawa, K., 1994, AA, 285, 509. + Mx = 5.92 +/- 0.62 Mo , i = 60^{o}, Mopt = 0.7 Mo , f(M)opt = 3.1 +/- 0.4 Mo , Kopt (km/s) = 409 +/- 18, Vg (km/s) = 48 +/- 17, Remillard, R.E., McClintock, J.E., Bailyn, C.D., 1992, ApJ, 399, L145. + 5 < Mx < 7.5 Mo , 0.6 < Mopt < 1.1 Mo , Kopt = 406 +/- 7 Km/s, Vg = 16 +/- 5 Km/s, f(M)opt = 3.01 +/- 0.15 Mo , 54^{o}< i < 65^{o}, Orosz, J.A., Bailyn, C.D., McClintock, J.E., Remillard, R.A., 1996,ApJ, 468, 380. + Optical counterpart: XN Mus (Black hole), Spectral Type: K0-4 V, Component star K0V to K4V, Remillard, R.A., McClintock, J.E., Bailyn, C.D., 1992, ApJ, 399, L145. + V ~ 13.5, Della Valle, M., Jarvis B.J., West R.M., 1991, Nature, 353, 50. + Optical photometry, O'Donoghue, D., Charles, P.A., 1996, MNRAS, 282, 191. + E(B-V) = 0.29, Cheng, F.H., Horne, K., Panagia, N., et al. 1992, ApJ, 397, 664. + Spec. Type K 3-5 V, B-V = 1.3, V= 20.3 - 20.5, Orosz, J.A., Bailyn, C.D., McClintock, J.E., Remillard, R.A., 1996, ApJ, 468, 380. McClintock, J.E., Bailyn, C.D., Remillard, R.H., et al. 1992, IAU Circ. No. 5499. + V ~ 13.3, B = 13.5, V ~ 20.4, B = 20.9, R = 19.4, E(B-V) = 0.30, With d = 1.4 kpc and B = 19.8 (Magnitude at a minimum after reddening correction), Mbol. = 9.2, Della Valle, M., Jarvis B.J., West R.M., 1991, AA, 247, L33-L36. + E(B-V) = 0.20, Gonzales-Riestra, R., Wamsteker, W., 1991, IAU, Circ. No. 5174. 1254-690 + Dist (Kpc) = 8 -15, Av ~ 1.1, Motch, C., Pedersen, H., Beuermann, K., et al. 1987, ApJ, 313, 792. + Log N_{H}(cm-2) = 21.48, Mason, K.O., Middleditch, J., Nelson, J.E., White, N.E., 1980, Nature, 287,516. + Mx = 1.4 Mo , Mopt = 0.5 Mo , Motch, C., Pedersen, H., Beuermann,K., et al. 1987, ApJ, 313, 792. + Kopt (km/s) = 114, f(M) = 0.025 Mo, Cowley, A.P., Hutchings, J.B., Crampton, D., 1988, ApJ, 333, 906. + B -V = 0.31, E(B-V) = 0.4, Motch, C., Pedersen, H., Beuermann, K., et al. 1987, ApJ, 313, 792. 1323-619 + P_{orb}= 0.122 days, Type I x-ray burst, l = 307.1, b = + 0.2^{o}, Parmar, A.N., White, N., E., Giommi, P., et al. 1986, ApJ , 308,199. + Dist (Kpc) = 10-20, Log N_{H}(cm-2) = 22.60, Parmar, A.N., Gottwald, M., van der Klis, M., van ParadiJs, J., 1989, ApJ, 338, 1024. + kT (keV) = 1.4-1.8, Log N_{H}(cm-2) = 22.32, van der Klis, M., Jansen, F., van ParadiJs, J., Stollmann, G., 1985, Space Sci. Rev., 40, 287. + Lx (0.1-10 keV) = 2 E36 at 10 kpc, Smale, A.P., 1995, AJ, 110, 1292. + i<80^{o}, Parmar, A.N., Gottwald, M., van der Klis M., van Paradijs, J., 1989, ApJ, 338, 1024. + No optical counterpart is dedected on the SERC-J plates down to their limiting wagnitude of ~21-22, Smale, A.P., 1995, AJ, 110, 1292. + Possible candidates for the counterparts of the LMXBs GX13+1 and GX5-1 with K = 13 - 15 have recently been found using IR Photometry, Naylor, T., Charles, P.A., Longmore, A.J., 1991, MNRAS, 252, 203. 1354-645 + (2.9 +/- 0.1) E-9 erg / cm^{2}s in the (1 - 10 keV) Ginga Satellite, 13.02.1987, Macino, F., 1987, IAU Circ.No. 4342. Kitamoto, S., Tsunami, H., Pedersen, H., et al. 1990, ApJ , 361, 590. + Log N_{H}(cm-2) = 22.5, Kitamoto, S., Tsunemi, H., Pedersen, H., et al. 1990, ApJ, 361, 590. + Lmax (1-10 keV) at 10 kpc >> 3.5 E37 erg/s, Tanaka, Y., Lewin, W.N.G., in "X-ray Binaries", (eds) W.N.G. Lewin, J. van ParadiJs, E.P.J. van der Heuvel, Cambridge University Press, 1994. + Optical counterpart BW Cir, B - V = 1.08, Kitamoto, S., Tsunemi, H., Pedersen, H., et al. 1990, ApJ, 361, 590. + U - B = - 0.13, E(B-V) ~ 1, V = 16.92 on 28. 03.1987, Kitamoto, S., Tsunemi, H., Pedersen, S.A., et al. 1990, ApJ, 361, 590. 1455-314 + Discovered in 1969, Conne, J.P., Evans, W.D., Belian, R.D., 1969, ApJ , 157, L157. + The 1979 outburst of the soft X-ray transient Cen X-4 was discovered by Ariel V (in 3-6 keV photon flux ~ 1.4 photon/cm^{2}s), Kaluzienski, L.J., Holt, S.S., Swank, J .H., 1980, ApJ , 241, 779. Matsuoka, M., Inoue, H., Koyama, K., et al. 1980, ApJ , 240, L37. + Hard X-rays (13-163 keV) by Signe 2 MP, Bouchacourt, P., Chambon, G., Niel, M., et al.1984, ApJ , 285, L67. + Two outbursts of Gen X-4 have been observed the first in J uly 1969, Evans, W.D., Belian, R.D., Conner, J .P., 1970, ApJ , 159, L57. + and second in May 1978, Kaluzienski, L.J., Holt, S.S., Swank, J .H., 1980, ApJ , 271, 779. + P_{orb}= 0.628925 days, van Paradijs, J., McClintock, J .E., 1994, AA, 290, 133. Sahbaz, T., Smale, A.P., Naylor, T., et al. 1996, MNRAS, 282, 1437. Cowley, A.P., Hutchings, J .P.,Schmidtke, P.C., et al. 1988, AJ , 95, 1231. + The first outburst in J uly 1969, Ewans, W.D., Belian, R.D., Conner, J .P., 1970, ApJ , Lett., 159, L57. + The second outburst in May 1979, Kaluzienski, L.J., Holt, S.S., Swank, J .H., 1980, ApJ , 241, 779. + Log N_{H}(cm-2) = 22.15, Matsioka, M., Inoue,H., Koyama, K., et al. 1980, ApJ, 240, L137. + Dist (kpc) = 1.2, L_{max}= E38, Tanaka, Y., Shibazaki, N., 1996, ARAA, 34, 607. + Dist (kpc) 2.5, Chevalier, C., Ilovaisky, S.A., van ParadiJs, J., et al. 1989, AA, 210, 114. McClintock, J.E., Remillard, R.A., 1990, ApJ, 350, 386. + kT = 0.16 - 0.7 keV, L = E32 - E33 erg/s, N_{H}= 3 E20 - 7 E21 cm^{-2}, Asai, K., Dotani, K., Mitsuda, K., et al. 1996, PASJ, 48, 257. + d = 1.2 kpc, Matsuoka, M., Inoue, H., Koyama, K., et al. 1980, ApJ, 240, L137. + The total energy emitted during an outburst was ~ 3 E44 erg for the 1969 outburst and ~ 3 E43 erg for the 1979 outburst, van Paradijs, J., Verbunt, F., 1984, "High Energy Transients in Astrophysics" Ney York AIP Conforence Series + For Cen X-4 in quiesence L ~ ( 4 - 8 ) E32 erg/s in 0.5 - 4.5 keV band at d = 1.2 kpc, van ParadiJs, J., Verbunt, F., Shafer, R.A., Arnoud, K.A., 1987, AA, 182, 47. + Mx = 1.4 Mo , M_{opt}= 0.1 - 0.2 Mo , < 0.7 Mo , Kopt (km/s) = 150, Vg = 137 km/s, f(M) = 0.2 Mo , i < 80^{o}, Whitlock, L., Imamura, J., Priedhorsky, W., 1990, AA, 219, 158. + Mx = 0.5 - 2.1 Mo , Shahbaz, T., Naylor, T., Charles, P.A., 1993, MNRAS, 265, 655. + Kopt = 146 +/- 12 km/s, f(M)opt = 0.20 +/- 0.05 Mo , Cowley, A.P., Hutchings, J.P., Schmidtke, P.C., et al. 1988, AJ, 95, 1231. McClintock, J.E., Remillard, R.A., 1990, ApJ, 350, 386. + Spectral Type: K4 V, B822 Cen, Blair, W.P., Raymond, J.C., Dupree, A.K., 1984, ApJ, 278, 270. + Mv = 1.5, V = 12.8, E(B-V) = 0.1, van Paradijs, J., McClintock J.E., 1994, AA, 290, 133. + V = 12.8 - 18.3, Spectral type K5-7 V, van Paradijs, J., Verbunt, F., van den Linden, T., et al. 1980, ApJ, 241, L161. Cowley, A.P., Hutchings, J.P., Schmidke, P.C., et al. 1988, AJ, 95, 1231. McClintock, J.E., Remillard, R.A., 1990, ApJ, 350, 386. + Mean brightness V= 18.35 -18.5, In 1985-1986,V=16.57, B- V=0.71, U-B=0.21, E(B-V)=0.1, K7 V, Chevalier, C., Ilovaisky, S. H., van Paradijs, J. et.al., 1989, AA, 210, 114. + V=19.1, K5 V, E(B-V)=0.1, Many Lines, Shahbaz, T., Smale, A.P., Naylor, T., et.al., 1996, MNRAS, 282, 1437. 1516-569 + The high L_{x}/ L_{opt}indicates that Cir X-1 is a low-mass X-ray binary, Oosterbroek, T., van der Klis, M., Kuulkerse, E., et al. 1995, AA, 297, 141. + P_{orb}= 16.6 days, Nicolson, G.D., 1980 IAU, Cir. No. 3449. Stewart, R.T.,Nelson, G.J ., Penninx, W, et al. 1991, MNRAS, 253, 212. + Possibly emits radio J ets, Stewart, R.T., Caswell, J .L., Haynes, R.F., et al. 1993, MNRAS, 261, 593. + See reviews, van der Klis, M., 1989, Ann. Rev. of AA, 27, 517. van der Klis, M., 1991, on "Neutron Stars Observations and Theory", Ventura, J ., Pines, D. L., eds. Kluwer Academic Publishers, p. 319. + Dist (kpc) 6, Log N_{H}(cm-2) ~ 22, Glass, I.S., 1994, MNRAS, 268, 742. + Dist (kpc) = 10, Z(kpc)=0, van OiJen, J.G.J., 1989, AA, 217, 115. + Lx ( erg/s ) = 8E38 (The high Lx/Lopt indicates that Cir X-1 is a low mass X-ray binary), Oosterbrook, T., van der Klis, M., Kuulkers, E., et al. 1995, AA, 297, 141. + Av = ~11; ~14; ~5, Moneti, A., 1992, AA, 260, L7; Glass, I.S., 1994, MNRAS, 268, 742. + Spectral Type: Faint red star BR Cir, the optical counterpart of Cir X-1 is a faint red star, Moneti, A., 1992, AA, 260, L7. 1524-617 + This soft X-ray transient (A1524-617) was discovered on 1974 November with Ariel 5, max flux >> 0.9 Crab (3-6 keV), Kaluzienski, L.J., Holt, S.S., Bolt, E.A., et al. 1975, ApJ , 201, L121. Pounds, K.A., 1974, IAU Circ. No. 2729. + TrA X-1 ( A1524-617) was discovered on 1974 November 22 by Ariel 5 SSI experiment, Pounds, K.A., 1974, IAU Circ. No. 2729. + Dist (Kpc)= 4.4, Barret, D., Roques, J.P., Mandrov, P., et al. 1992, ApJ, 392, L19. van ParadiJs, J., Verbunt, F., 1984, in "High Energy Transient Astrophysics, Ed. Woosley, New York AIP Conf. Proc. 115. + kT(keV)= 0.3-0.7 (Blackbody, at 0.1-2.4 (keV), An Upper limit (2-10)E33 has been derived for its quiescent X-ray luminosity 4.5 E36-8E35 variable, Maximum X ray Luminosity at d=4.4 Kpc. is about 7E37???s, Barret, D., Motch, C., Pietsch, W., Voges, W., 1995, AA, 296, 459. + Lx max= 1E38, Tanaka, Y., Lewin 1994, in X-ray Binaries. eds. Lewin, ParadiJs, van den Heuvel ,Cambridge Univ.Press. + Optical counterpart KY TrA, E (B-V) = 0.7, B = 17.5, R 21, Murdin, P., ***, et al. 1977, MNRAS, 178, 27p. 1543-475 + Recorded in 1971 by, Matilsky, T., et al. 1972, ApJ , 174, L53. + In 1971 the source rise to maximum flux >> 2 Crab (2-6 keV) and become undetectable about a year later when the flux had decreased by a factor >> E3, Le, F.K., et al. 1976, ApJ , 203, 187. + In 1983, the source was detected with Tenma, on August 17, at F >> 50 mCrab, Tanaka, Y., 1983, IAU Circ. No. 3854. + I >> 6 Crab (1.5 - 7 keV) on August 20, Kitamoto, S., Miyamoto, S., Tsunami, H., et al. 1984, PASJ , 36, 799. + the soft X-ray transient erupted in 1971, Li, F.K., Sprott, G., Clark, G., et al. 1976, ApJ , 203, 187. + the soft X-ray transient erupted in 1983, Kitomoto, S., Miyamoto, S., Tsunami, H., et al. 1984, PASJ , 36, 799. + the soft X-ray transient erupted in 1992, Harmon, B.A., Wilson, R.B., Finger, M.H., et al. 1992, IAU, Circ. No: 5504. + kT (keV)= 37, Log N_{H}(cm-2)= 22.23, Singh, K.P., Apparao, K.M.V.,Kraft, R.P., 1994, ApJ, 421, 753. + A_{v}= 2.2, d = 4kpc, Chevalier, C., 1989, in two Topics in X-ray Astronomy, 23rd ESLAB Symp. Bologna (ESA Paris), p.341. + L_{max}= 5 E38 erg/s, (1.5-7 keV) at a distance 4 kpc, Tanaka, Y., Lewin, W.H.G., in "X-ray Binaries", eds. W.H.G., Lewin, J. van ParadiJs, E.P.J. van den Heuvel, Cambridge University Press. + kT = 1.6 keV, photon index = 5.3, Kitomoto, S., Miyamoto, S., Tsunami, H., et al. 1984, PASJ, 36, 799. + kT_{bb}(keV) = 0.6 - 1 (kT_{bb}), log N_{H}(cm^{-2}) = 21.6, L_{x}( erg/s ) = (4-6) E36, L_{x}max = 1 E38 erg/s, (in 1-10 keV) at distance 10 kpc, Motch, C., Pakull, M.W., Mouchet, M., Beuermann, K., 1989, AA, 219, 158. + Opt. Spec. Type: A1-A2 V, V ~ 14.5-16.7, Chevalier, C., 1989, in Two Topics in X-Ray Astronomy, 23rd ESLAB Symp, Bologna. ESA, Paris, p. 341. + The Optical counterpart was discovered near X-Ray maximum at V = 14.9, Petersen, H., 1983, ESO Mesenger, 34, 21. + A2V, V = 16.7, Chevalier, C., eds. Kunt, J., Patrick, B., Proc. 23rd ESLAB Symp. Bologna, ESA SP-296, p.341 1556-605 + kT_{bb}(keV)= ~0.6-1, Log N_{H}(cm-2) = ~21.6, Lx ( erg/s )=(4-6) E36, Lx max= 1E38 Erg/s, Motch, C., Pakull, M.W., Mouchet, M., Beuermann, K., 1989, AA, 219, 158. + Mx = 1.4 Mo , Motch, C., Pakuli, M.W., Mouchet, M., Beuermann, K., 1989, AA, 219, 158. + E(B-V) = 0.55, Motch, C., Pakull, M.W., Mouchet, M., Beuermann, K., 1989, AA, 219, 158. 1603.6+2600 + Found by Einstein observatory, Gioia, I.M., Maccacaro, T., Schild, R.E., et al. 1990, ApJ , Sup. Ser. 72, 567. + Einstein, 0.3- 3.5 keV, Fx= 1.14 E-12 erg/cm^{2}s, Morris, S.L., Liebert, J., Stocke,, J .T., et al. 1990, ApJ , 365, 686. + Orbital P = 112.5 min, Vilhu, O., Hakala, P., Ergma, E., 1993, 2nd Haifa Conference on CV and Releated Objects, + RA= 16 03 40.5, Dec. = 25 59 48.1 (1950), l = 42^{0}.8, b = 46^{0}8, Orbital P = 111.04 min, Morris, S.L., Liebert, J ., Stocke, J .T., et al. 1990, 365, 686. + Dist (Kpc) = 30-80, L_{x}(0.3-3.5 keV) = 1.4 E34 (d/10 kpc)^{2}erg/s, Morris, S.L., Liebert, J., Stocke, J.T., et al. 1990, ApJ, 365, 686. + Mopt = 0.2 Mo , Morris, S.L., Liebert, J., Stocke, J.T., et al. 1990, ApJ, 365, 686. + V = 19.7, R = 19.4, Eclipsing, Morris, S.L., Liebert, J., Stocke, J. T., et al. 1990, ApJ, 365, 686. 1608-522 + Recur. transient. Many outburst have been observed. No significant correlation between the outburst energy and the waiting time, Lochner, J.C., Roussel - Dupre, D., 1994, ApJ , 435, 840. + Frequent type-1 X-ray bursts, Lewin, W.H.G., van ParadiJ s, J ., Team, R.E., 1995, in "X-Ray Binaries" eds. W.H.G., Lewin, J . van ParadiJ s, E.P.J ., van den Heuvel, Cambridge University Press; van Paradijs, J. And McClintock, J. E., 1995, in "X-Ray Binaries" eds. W.H.G., Lewin, J . van ParadiJ s, E.P.J ., van den Heuvel, Cambridge University Press, p.97. + Recently, a 800 Hz QPO has been detected, Berger, M., et al., 1996, ApJ 469, L13. + Dist (Kpc)= 3, Lx ( erg/s )= (6-30) E36, Mitsuda, K., Inoue, H., Nakamura, N., Tanaka, Y., 1989, PASJ, 41, 97. + Av ~6.0, Bradt, H.V.D., McClintock, J.E., 1983, Ann. Rev. Astron. Astrophys., 21,13. + L ~ 6 E32 erg/s, in 0.5 - 10 keV, at d = 3.6 kpc, Asai, K., dotani, T., Mitsuda, K., et al. 1996, PASJ, 48, L57. + Dist (Kpc) = 3.6, Lmax = 4 E37, Nakamura, N., Dotani, T., Inoue, H., et al. 1989, PASJ, 41, 617. + Dist (Kpc) = 4.1, Tanaka, Y., "X-ray binaries and the formation of binary and milisecond stars radio pulsars", 1991, California. + kT = 0.3 keVC, Lx = E32 - E33 erg/s, N_{H}= (0.9 - 2.3) E22 cm^{-2}, Asai, K., Dotani, T., Mitsuda, K., et al. 1996, PASJ, 48, 257. + The total energy per outburst E34 - E44 erg. No significant correlation between the outburst energy and the waiting time, Lochner, J.C., Roussel - Dupre, D., 1994, ApJ, 435, 840. + Data from 3 to 5 months after the outburst show the counterpart at a mean magnitude of R=20.2 and variable on timescales of days. A comparison with identical observations in 1995 implies that the object has brightened by at least 1.8 mag in R following the X-ray outburst, Wachter, S., 1997, ApJ 485, 839. + The optical counterpart of X 1608-52, QX Nor. It was discovered after an outburst in 1977. E(B-V) = 1.5, I = 18.2, I 20, Grindlay, J.E., Liller, W., 1978, ApJ, 220, L127. Penninx, W., Damen, E., Tan, J., et al., 1989, AA, 208, 146. 1617-155 + P_{orb}= 0.787313 days, van Paradijs, J., Mclintock, J.E., 1994, AA, 290, 133. Shahbaz, T., Smale, A.P., Naylor, T., et al. 1996, MNRAS, 282, 1473. Schachter, J ., Filipenko, A., Khan, S.M., 1989, ApJ , 362, 379. + QPO, Hasinger, G., van der Klis, M., 1989, AA, 225, 79. (and see therein references). + Dist (Kpc) = 0.3-1;0.7, Mv=2.4, Smale, S.A., Corbet, R.H.D., Charles, P.A., et al. 1988, MNRAS, 223, 51. + Mx = 1.3 Mo , M_{opt}= 0.8 - 1.2 Mo , a = 11 lt s, i = 25 - 30^{o}, Petro, L.D., Bradt, H.V., Kelley, et al. 1981, ApJ, 251, L7. + Mv = - 0.7, V = 12.2, E(B-V) = 0.3, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + E(B-V) = 0.13 - 0.23, Schacter, J., Flippenko, A.V., Kahn, S.M., 1990, ApJ, 340, 1049 + E(B-V) = 0.2, Gallagher, D., Cash, W., Green, J., 1995, ApJ, 439, 976. + V818 Sco, Kallman, T.R., Raymond, J.C., Vrtilek, S.D., 1991, ApJ, 370, 717.;Wu, C.C., 1979, ApJ, 227, 291. + V=12.9, E(B-V)=0.15, lines, Shahbaz, T., Smale, A.P., Naylor, T., et.al., 1996, MNRAS, 282, 1437. 1624-490 + kT(keV)= 1.4- 5, Log N_{H}(cm-2)=22.7, Watson, M.G., Willingale, R., King, A.R., et al. 1985, Space. Sci. Rev., 40, 195. Churc, M.J., Balucinska, - Churc, M., 1995, AA, 300, 441. 1627-673 + Coordinates, Zhang, N.S., Wilson, C.A., Harmon, B.A., et al. 1994, IAU Cir. 6046. + Satellite-BeppoSAX, range 0.1-10 keV, count rate=1.029+/- 0.005 s^{-1}, on 1996 Aug 6-11, Owens, A., Oosterbroek, T. and Parmar, A. N., 1997, AA 324, L9. + F_{x}=(5.4+/- 0.3) E-10 ergs/cm^{2}s, Einstein, in 2-10 keV, on 1979 Feb/Mar, Elsner, R.F., Darbro, W., Leahy, D., et al., 1983, ApJ 266, 769. + F_{x}=(5.6+/- 0.5) E-10 ergs/cm^{2}s, EXOSAT, in 2-10 keV, on 1983 Aug 30, Mavromatakis, F., 1994, AA 285, 503. + F_{x}=(12.9+/- 0.1) E-10 ergs/cm^{2}s, Ginga, in 2-24 keV, on 1990 Apr 20, Mihara, T., 1995, Ph.D. thesis, Univ. of Tokyo. + F_{x}=(2.9+/- 0.2) E-10 ergs/cm^{2}s, ASCA, in 0.5-10 keV, on 1993 Aug 11, Angelini, L., White, N. E., and Nagase, F., 1995, ApJ 449, L41. + Porb = 0.0288 days, Levine, A., Ma, C.P., McClintock, J ., et al. 1988, ApJ , 327, 732. J oss, P.C., Avni, Y., Rappaport, S., 1978, ApJ , 221, 645. + Porb = 0.02875 days and p_{pulse}= 7.66 s, Mereghetti, S., Stella, L., 1995, ApJ , 442, L17. Lutovinov, A., Grebenev, S., Sunyaev, R., Pavlinsky, M., 1995, In The Lives of Neutron Stars, M.A. Alpar, U. Kiziloglu and J . van ParadiJ s, eds. NATO ASI Ser. C, Vol. 450, Kluwer Academic Publ. Rappaport, S., A., 1977, ApJ , 217, L29. + p/ p' = - 4.9 E 3 yrs, P' = -1.6 E -3 s/yr, Hellier, W.C., 1994 MNRAS, 271, L21. Mereghetti, S., Stella, L., 1995 ApJ , 442, L17. Nagase, F., 1989, PASJ , 411,1. + p/p'_{pulse}= 5 E3, van ParadiJ s, J .E., Taam, R.E., van den Heuvel, E.P.J ., 1995, AA, 299, L41. + QPO-observations by Ginga and the Advanced Satellite for Cosmology and Astrophysics (ASCA), Shinoda, K., Kii, T., Mutsuda, K., et al., 1990, PASJ 42, L27; Angelini, L., White, N. E., Nagase, F., et al., 1995, ApJ 449, L41. + Many data about pulse period. In 1990, switching to steady spin-down after 13 yrs of steady spin-up. The current spin- down rate is nearly equal to the previous spin-up rate, with a spin evolution timescale of | p/p'| =5 E3 yrs in both states. Timing noise seen in young radio pulsars, Chakrabarty, D., Bildsten, L., Grunsfeld, J. M., et al., 1997, ApJ 474, 414. + P_{pulse}=7.66794+/- 0.00004s, Owens, A., Oosterbroek, T., and Parmar, A. N., 1997, AA 324, L9. + Dist (Kpc) =1.7, Fx = 1.4E-9 erg/cm^{2}s, Lx ( erg/s ) =1.9 E36, Mereghetti, S., Stella, L., 1995, ApJ, 442, L17. + kT(keV) = 1.8, Log N_{H}(cm-2) = 21.4 and 21, Mavromatakis, F., 1994, AA, 285, 503. + d = 3 -6 kpc, Lx = 2 E36 - E37 erg/s, Levine, A.M., Ma, C.P., McClintock, J., et al. 1988, ApJ, 327, 732. + Spec. Inedx = 1.5, blackbody temp. = 0.6 keV, (0.5 - 10 keV) luminosity obs. by ASCA, 3.3 E34 erg/s d^{2}_{kpc}, Angelini, L., White, N.E., Nagase, F., et al. 1995, ApJ, 449, L41. + Spec. Index =1.7, Hellier, W.C., 1994, MNRAS, 271, L21. + Spec.Index = 0.61+/- 0.02, kT=0.33+/- 0.02 keV, N_{H}=(6.9+/- 2.0) E20 cm^{-2}, Owens, A., Oosterbroek, T., and Parmar, A. N., 1997, AA 324, L9. + Dist (kpc) ~ 8, Lx~ E37 ergs/s, Chakrabarty, D., 1998, ApJ, 492, 342. + a_{x}Sin i < 0.01 lt-s, Levine, A., Ma, C.P., McClintock, J., et al. 1988, ApJ, 327, 732; Chakrabarty, D., Bildsten, L., and Grunsfeld, J. M., 1997, 474, 414. + E ~ 18, Optical counterpart: KZ TrA, B-V ~ 0, U-B = - 1.2, V=17.52, McClintock, J.E., Canizares, C.R., Bradt, H.V., et al. 1978, Nature, 270, 320. + Low mass He star has been suggested for 4U1626-67 with strong neon line emission, Angelini, L., White, N.E., Nagase, F., et al. 1995, ApJ, 449, L41. 1630-47 + Mx > 3.4 Mo , Parmar, A.N., Stella, L., White, N.E., 1986, ApJ, 304, 664. 1630-472 + Satellite, Range, Intensity, Corbet, R.H.D., Smale, A.P., Charles, P.A., et al. 1989, MNRAS, 239, 533. + Rosat (PSPC) during 20.9.1992-26.8.1993 flux changed 0.173 q/s to 8.7 E-3 q/s, Parmar, A.N., Angelini, L., White, N.E., 1995, ApJ , 452, 129. + F_{x}=7.0 E-9 ergs/cm^{2}s or 240 mCrab in 2-60 keV, Rossi X- ray Timing Explorer, dip flux, which drops by a factor of about 3, (RXTE) observation, on 1996 May 3, Tomsick, J.A., Lapshov, I. , and Kaaret, P., 1998, ApJ 494, 747. + F_{x}~3000 counts/s, 2-13 keV, RXTE on 1996 May 3, Kuulkers, E., Wijnands, R., Belloni, T., et al., 1998, ApJ 494, 753. + Recurrent periodic outburst, Periodic ossilation 601.7 +/- 3.0 d, Parmar, A.N., Angelini, L., White, N.E., Predhorsky, W.C., 1986, ApJ Supp. Ser., 126, 29. + Recurrent transient, Jones, C., Forman, W., Tananbaum, H,. Turner, M.J .L., 1976, ApJ , 210, L9. + Outburst recurrence time is relatively short and regular, staying between 600 and 700 days, Kuulkers, E., Parmar, A. N., Kitamoto, S., et al., 1997, MNRAS 291, 81. + Dist (kpc) = 10, kT(keV) =1.15, Lx ( erg/s ) ~2.8E38, 4 E36 (1 -150 keV) (assuming distance is 10 kpc), Log N_{H}(cm- 2)=22.81, Parmar, A.N., Stella, L., White, N.E., 1986, ApJ, 304, 664. + N_{H}in dip = 8.6 E23 cm^{-2}, N_{H}in non-dip = 7.3 E22 cm^{-2}, kT_{max}= 1.145, spectral index {alpha} =4.20+/- 0.15, Tomsick, J.A., Lapshov, I., and Kaaret, P., 1998, ApJ 494, 747. + N_{H}= (1.23+/- 0.03) E23 cm^{-2}, T~ 1.2 keV, Kuulkers, E., Wijnands, R., Belloni, T., et al., 1998, ApJ 494, 753. 1636-536 + Redshift (1+Z) = 1.6 P_{orb}= 0.159 days, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + r shift (1+z) = 1.6, Dist (Kpc) = 2-10, Av = 2.5 +/- 0.3, Lawrence, A., Cominsky, L., et al. 1983, ApJ, 271, 793. + Dist (kpc) = 6.9, Tanaka, Y., 1991, on "X-Ray Binaries and the Formation of Binary and Millisecond Radio Pulsars", California. + redshift (1+z) = 1.6, M_{x}= 1.45 M_{o}, M_{opt}= 0.2 M_{o}, Kopt (km/s) = 215 +/- 65, Cowley, A.P., Hutchings, J.B., Crampton, D., 1988, ApJ, 333, 906. + redshift (1+z) = 1.6, V = 17.5, Mv = 1.3, E(B-V) = 0.8, van Paradijs, J., McClintock J.E., 1994, AA, 290, 133. 1642-455 + QPO, Hasinger, G., van der Klis, M., 1989, AA, 225, 79. (and see their references). + Av~20, Penninx, W., Zwarthoed, G.A.A., van ParadiJs, J., et al. 1993, AA, 267, 92. 1655-40 + Discovered 27.07.1994 by BATSE, (20-100 keV), F = 1.1 Crab, 28.07.1994 - 11.08.1994, BATSE 0.19 photon/cm^{2}s, (20-100 keV), Harmon, B.A., Wilson, C.A., Zhang, S.N., et al. 1995, Nature, 374, 703. + a_{2000}= 16 53 59.9, {delta}_{2000}= - 39 50 44, Greiner, J., Predehl, P., Pohl, M., 1995, AA, 297, L67. + a_{2000}= 16 54 00.137, {delta}_{2000}= -39 50 44.90, Superluminal X-Ray transient, Tavani, M., Fruchter, A., Zhang, S.H., et al. 1996, ApJ , 473, L103. + Discovered in outburst on J uly 27, 1994 with the CGRO BATSE (20-300 keV), Zhang, S.N., Wilson, C.A., Harmon, B.A., et al. 1994, IAU Circ. No. 6046. + flux in September 1994 and February 1995 differed by a factor 3, Alexandrovich, N., Borozdin, K., Sunyaev, R., Efremov, Y., 1994, IAU Circ. No. 6087. Alexandrovich, N., Borozdin, K., Sunyaev, R., 1995, IAU Circ. No. 6143. + Outburst in 1995 late March, Wilson, C.A., Harmon, B. A., Zhang, S. N., et al., 1995, IAU Circ. 6152. + Another outburst in 1995 late July, Harmon, B.A., et al., 1995, IAU Circ. 6205. + F_{x}=4.5 E-9 ergs/cm^{2}s on 1994 Aug 23, F_{x}=1.2 E-9 ergs/cm^{2}s on 1994 Sep 28, F_{x}=4.7 E-8 ergs/cm^{2}s on 1995 Aug 16, F_{x}=2 E-13 ergs/cm^{2}s on 1996 Mar 25, 2-10 keV, ASCA, Ueda, Y., Inoue, H., Tanaka, Y., et al., 1998, ApJ 492, 782. + F_{x}~11500 counts/s, 2-13 keV, RXTE on 1997 Feb 26, Kuulkers, E., Wijnands, R., Belloni, T., et al., 1998, ApJ 494, 753. + Short recurrence time between the X-ray outbursts, Orosz, J.A., Bailyn, C.D., 1997, ApJ 477, 876. + Superluminal X-ray transient, P = 2.62 days, Bailyn, C. D., Orozs, J . A., Remillard, R. H., 1995, IAU Circ. 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HJ elming, R.M., Rupen, M.P., 1995, Nature, 375, 464. + Dist (Kpc)=3-5 (derived from HI Observation), Tingay, S.J., Jauncey, D.L., Preston, R.A., 1995, Nature, 374, 141. + Dist (Kpc)=3 (from the dusty scattering halo), Log N_{H}(cm- 2)=21.8, Av= 5.6 (estimated), Lx ( erg/s )=2E37 (unobserved luminosity under the distance 3 Kpc in the band of 0.1- 2.4(keV), Greiner, J., Predehl, P., Pohl, M., 1995, AA, 297, L67. + Dist (kpc) = 3.5, Bailyn, C.D., Orosz, J.A., Girard, T.M., et.al., 1995, Nature, 374, 701. + Dist (kpc) =3.2+/-0.2, Jets, radio emission E29 -E32 erg/s, Hjelming, R.M., Rupen, M.P., 1995, Nature, 375, 464.; Tavani, M., Fruchter, H., Zhang, S.N., et.al., 1996, Ap.J., 473, L103. + N_{H}= (3.6-6.2) E22 cm^{-2}, Ueda, Y., Inoue, H., Tanaka, Y., et al., 1998, ApJ 492, 782. + N_{H}= 2.17 E22 cm^{-2}, T=1.1 keV, Kuulkers, E., Wijnands, R., Belloni, T., et al., 1998, ApJ 494, 753. + Mx= 4 - 5.2 Mo , Mopt = 0.4 -1.3 Mo , Kopt (km/s) = 231, f(M) = 3.35 +/- 0.14 Mo , i @ 90^{o}, f(M_{2}) = 3.16 +/- 0.15 Mo , Bailyn, J.D., Orosz, J.A., McClintock, J., Remillard, R.A., 1995, IAU, Cir. 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Ecl, Optical counterpart: Spectral Type: F-G, V=14.2, and V=17.3 in quiescent, (in August 10, 1994) eclipses primary and secondary, Nova Sco 1994, Bailyn, C.D., Orosz, J.A., Remillard, R.H., 1995, IAU, Cir. No. 6173. Bailyn, C.D., Jogee, S., Orosz, J., 1994, IAU, Cir. No. 6050 and 6060. 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I., Dotani, T., and Nagase, F., 1997, ApJ 476, L81. + Mx= 1.3 M_{o}, M_{opt}= 2 - 2.2 M_{o}, e_{2}= 0.34, Kopt (km/s) = 85, Crampton, D., 1974, ApJ, 187, 345. + e_{1}= 0.1, Vg = -75 km/s, Crampton, D., Hutchings, J.B., 1974, ApJ, 191, 483. + a = 8.6 Ro , Choi, C.S., Naase, F., Makino, F., et al. 1994, ApJ, 422, 799. + Kopt = 83 +/- 3 km/s, Hutchings, J.B., Gibson, E.M., Crampton, D., Fisher, W.A., 1985, ApJ, 292, 670. + Kopt = 110 +/- 17 km/s, Koo, D.C., Kron, R.G., 1977, PASP, 89, 285. + Mx = 1.2 Mo , Mopt = 2.2 Mo , i 72^{o}, e < 0.0003, Kopt = 90 +/- 20 km/s, van Kerkwijk, M.H., van Paradijs, J., Zuiderwijk, E. J., 1996, AA, 303, 497. + f(M)_{x}=0.8513 +/- 0.0001 Mo , f(M)_{opt}= 0.1 Mo , M_{x}= 0.98 +/- 0.12 Mo , a_{x}sini = 13.1831 +/- 0.0003 lt-s, Deeter, J.E., Boynton, P.E., Miyomoto, S., 1991, ApJ, 383, 324. + Spectral Type: A8 - B0, Crampton, D., 1974, ApJ, 187, 345. + HZ Her, Howarth, I.D., Wilson, R., MNRAS, 204, 1091. 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Doxsey, R., Grindlay, J., Griffiths, R.E., et al. 1979, ApJ, 228, L67. + V=20.7, E(B-V)=0.3, No spectral features., Shahbaz, T., Smale, A.P., Naylor, T. et.al., 1996, MNRAS, 282, 1437. + In 1979 June V=21.5 and about a month later V > 23, Cominsky, L., Ossmann, W., and Lewin, W. H. G., 1983, ApJ 270, 226. + For V2134 Oph RA=17^{h}02^{m}06^{s}.42, dec= -29^{o} 56' 44''.33 (2000 yr), p_{orb}=7.1 hr, spectral type later than K2, Wachter, S., Smale, A.P., 1998, ApJ 496, L21. 1659-487 + Rec. ~ 460 d. Discovered by, Markert, T.H., Canizares, C.R., Clark, G.W., et al. 1973, ApJ , 184, L67. + P_{orb}= 0.87 days, Cowley, A.P., Crampton, D., Hutchings, J .B., 1987, ApJ , 92, 195. + P = 14.8 h, Honey, W.B., Charles, P.A., 1988, IAU Circ. No. 4532. Callanan, P. J ., Charles, P.A., Honey, W.B., Thorstensen, J .R., et al. 1992, MNRAS, 259, 395. + QPO, Markert, T.H., 1973, ApJ , 184, L67. Dolan, J . F., Crannell, C.J ., Dennis, B.R., Orwig, L.E., 1987, ApJ , 322, 324, + Rec ~460d, Dist (Kpc)=4, Cowley, A.P., Crampton, D., Hutchings, J.B., 1987, AJ, 92, 195 + kT(keV)= 1.28 (soft), 4 (hard x-ray), Corbert, R.H.D., Thorstensen, J.R., Charles, P.A., et al. 1987, MNRAS, 227, 1055. + Lx/Lopt= 750, Av~3.5, Grindlay, J.E., 1979, ApJ, 232, L33. Makishima, K., MaeJima, Y., Mitsuda,K., et al. 1986, ApJ, 308, 653. + Spectral index = 0.37+/- 0.06, Lx ( erg/s )=5E35, for d=4Kpc and 5-20(keV)band; 2E37 for d~4Kpc and 50-400(keV)band., Grabelsky, D.A., Matz, S.M.,Pursell, M., et al. 1995, ApJ, 441, 800. + L_{max}(erg/s) = 6 E37 for d = 4 kpc and in 1.2-3.7 keV, 20% intensity variation in less than 100 ms, Miyamoto, S., Kitamoto, S., 1989, Nature, 342, 773.Miyamoto, S., Kitamoto, S., 1991, ApJ, 374, 741. + Mx < 2.5 Mo , Kopt = 124 +/- 13 Mo , i < 60^{o}, Cowley, A.P., Crampton, D., Hutchings, J.B., 1987, AJ, 92, 195. + Rec ~400d, Opt. Counterpart V821 Ara, Spec. Type: Early-Mid B V star, Grindlay, J.E., 1979, ApJ, 232, L33. + V = 15.4 - 20, Cowley, A.P., Schmidtke, P.C., Crampton, D., et al. 1991, ApJ, 373, 228. 1702-363 + Intensity, (2-11), Intensity,(0.3-8.3), Bradt, H.V., McClintock, J .E., 1984, Ann. Rev. Astr. Ap., 21,87. + Date, Satellite, (EXOSAT), Range, Intensity, Langmeier, A., StaJ no, M.,Hasinger,, G., et al. 1987, ApJ , 323, 288. + Intensity, The bolometric maximum flux of the main burst is about 14 E-9 ergs cm^{-2}s^{-1}assuming bl`ckbody spectrum. The peak fluxes of the burst remain approximately the same in all observation. A peak flux of 18.4 E-9 erg cm^{-2}s^{-1}and for the first burst in observation a value of 1.31 E-9 ergs cm^{-2}s^{-1}was derived, Langmeier, A., StaJ no, .,Hasinger, G., et al. 1987, ApJ , 323, 288. + Intensity, The X-ray flux (1-20 keV) varied from 1.3 to 10.7 E-9 erg cm^{-2}s^{-1}on a time scale of months, Langmeier, A., StaJ no, M., Hasinger, G., et al. 1987, ApJ , 323, 288. + Satellite, Range, Intensity, Gottwald, M., Haberl, F., Langmeier, A., et al. 1989, ApJ , 339, 1044. + RA= 17 05 44.42, dec= -36 25 22.82, Wachter, S., 1997, ApJ 490, 401. + QPO, Hasinger, G., van der Klis, M., 1989 AA, 225, 79. (and see therein references). + p_{orb}= 21.85 +/- 0.4 h, Watchter, S., Margon, B., 1996, AJ , 112, 2684. + p_{orb}=22.5+/- 0.1 hr, Wachter, S., 1997, ApJ 490, 401. + Dist (Kpc) = 8.5, Wachter, S., Margon, B., 1996, AJ., 112, 2684. + Av = 4 - 6, Penninx, W., AugusteiJn, T., 1991, AA., 246, L81; Cooke, B.A., Ponmann, T.J., 1991, AA., 244, 358. + V = 18.6, Mv = -0.4, E(B-V) = 1.3, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + V = 18.56 +/- 0.04, R = 17.55, J = 15.0, H =14.5, K = 14.6, Wachter, S., Margon, B., 1996, AJ, 112, 2684. + V = 18.4 +/- 0.1, B = 20.0 +/- 0.1, Penninx, W., Augusteijn, T., 1991, AA, 246, L81. 1702-429 + Dist (Kpc) ~7, Log N_{H}(cm-2)=21.90, Av ~4.5, Oosterbroek, T., Pennix, W., van der Klis, M., et al. 1991, AA, 250, 389. + Log N_{H}(cm-2)=22.7, Makishima, K., Inoue, H., Koyama, K., et al. 1982, ApJ, 255, L49. 1704+240 + Dist (Kpc)=0.73, kT(keV) ~15, LogN_{H}(cm-2)=20.86, Garcia, M., Baliunas, S.L., Doxey, R., et al. 1983, ApJ, 267, 291. + Optical counterpart:HD 154791, Spec. Type: M3 II, V=7.3, Garcia, M., Baliunas, S.L., Doxsey, R., et al. 1983, ApJ, 267, 291. 1705-250 + Nova Oph 1977, Longmore, A., Camnon, R., Murdin, P., Malin, D., 1977, IAU Circ. No. 3110. + Orbital P = 16.8 +/- 0.1 h, Martin, A.C., Casares, P. A., Charles, P.A., et al. 1995, MNRAS, 274, L46. + P = 12.51 +/- 0.03 h, Remillard, R. A., Orosz, J . A., McClintock, J .E., Bailyn, C. D., 1996, ApJ , 459, 226. + kT(keV) ~4 (soft), ~17 (hard X ray), Cooke, B.A., Levine, A.M., Lang, F.L., et al. 1984, ApJ, 285, 258. + LogN_{H}(cm-^{2}) = 21.95, Wilson, C.K., Rothschild, R.E., 1983, ApJ, 274, 717. + Dist (kpc) = 3, A_{v}= 1.4, Griffiths, R., Johnson, J., Doxey, R., et al. 1977, IAU, Circ. No. 3110. + Dist (kpc) = 2-8.4, Martin, A.C., Cezares, J., Charles, P.A., et al. 1995, MNRAS, 274, L46. + Dist (kpc) = 6, Remillard, R.A., Orosz, J.A., McClintock, J.E., Bailyn, C.D., 1996, ApJ, 459, 226. + X-Ray spectrum consist optically thin component (kT = 1.8 +/- 0.1 keV) and hard power-low componnet (photon index = 2.19 +/- 0.06), Wilson, C.K., Rothshild, R.E., 1983, ApJ, 274, 717. + 48^{o}< i < 51^{o}, Mx 3 Mo , Mopt 0.15 Mo , Martin, A.C., Casares, J., Charles, P.A., et al. 1995, MNRAS, 274, L46. + Mx = 6 +/- 1 Mo , if companion is a K3 star, i = 60^{o}- 80^{o}, Kopt = 420 +/- 30 km/s, f(M) = 4.0 +/- 0.8 Mo , Remillarad, R.A., Orosz, J.A., McClintock, J.E., Bailyn, C.D., 1996, ApJ, 459, 226. + V2107 Oph, Nova Oph 77 reached B = 16.55, Longmore, A., Cannon, R., Murdin, P., Malin, D., 1977, IAU, Circ, No. 3110. Griffits, R.E., Bradt, H., Doxsoy, R., et al. 1978, ApJ, 221, L63. + Spec. Type: K3, quiescent V = 21.5, Remillard, R.A., Orosz, J.A., McClintock, J.E., Bailyn, C.D., 1986, ApJ, 459, 226. + E(B-V) = 0.5, V=16.6, E(B-V)=0.5, No spectral features, Griffits, R.E., Gursky, H., Schwartz, D.A., et al. 1971, Nature, 276, 247; Shahbaz, T., Smale, A.P., Naylor, T., 1996, MNRAS, 282,1437. 1705-440 + EXOSAT, 2-11 keV, Fx = (0.7-8.3) E-9 egrs/cm^{2}s, Langmeier, A., Hasinger, G., Trumper, J ., 1989, ApJ , 340, L21. + Intensity dips with a quasi period of 0.05416 days, Langmeier, A., StaJ no, M., Trumper, J ., 1985 in Proc. Int. Symp. "X- Ray Astronomy", held in Bologna, p. 121. + Dist (kpc)= 10, kT (keV) = 1.5, Blackbody fit to the burst net counts (persistent emmision substracted) during the maximum gives a blackbody temperature of kT = 2.3 +/- 0.1 keV. In the burst decay the temperature decreases to kT = 1.25 +/- 0.15 keV, typical for type I X-ray bursts. Fx = (13- 10.7) E-9 (1-20 keV) erg/cm2s, Lx ( erg/s ) = 1.7 E38, Log N_{H}(cm-2) = 21.87-22.15, Longmeir, A., Sztaino, M., Hasinger, G., Trumper, J., Gottwald, M., 1987, ApJ, 323, 288. + Dist (Kpc) = 10, Fx (erg/cm^{2}s) = (1.7-6) E-9 (in 0.1- 20(keV), Lxmax ( erg/s )=1.6E38 (for type I); 2.4E38 (for type II) (0.1-20(keV) (EXOSAT), Gottwald, M., Haberl, F., Langmeir, A. et al. 1989, ApJ, 339, 1044. + Fx = (0.7-8.3 keV)E-9 erg/cm^{2}s, the spectrally very hard low-intensity state, the source has the highhest burst frequency (~0.5 h-1) and the hardest spectrum (kT~20 keV) for a thermal Bremsstrahlung representation, Langmeier, A., Hansinger, G., Trumper, J., 1989, ApJ, 340, L21. + Dist (Kpc)=7.4, Haberl, F., Titarchux, L., 1995, AA, 299, 419. 1715-321 + LogN_{H}(cm-2) = 22.60 +/- 0.48, Hoffman, J.A., Lewin, W.H.G., Doty, J., et al. 1978, ApJ, 221, L57. 1716-249 + X-ray Nova in Ophiuchi has been discovered on Sept. 25, 1993 with Granat, Ballet, J., Denis, M., Gilfanor, M., Sunyaev, R., 1993, IAU Circ. No. 5874. + Independently discovered GRO, The source reached a max. flux at ~ 1.4 Crab (20-100 keV) on September 30, Harmon, B.A., Zang, S.N., Paciesas, W.S., Fishman, G.J ., 1993, IAU Circ. No. 5874. + Koordinates, Tanaka, Y., 1993, IAU Circ. No. 5877. + On Octeber, 3-4, 1993 in the range 2-300 keV flux 3.9 E-8, in Spring 1994, in the range 40-150 keV F = 15.8 +/- 5.5 mCrab, Revnivtsev, M., Gilfanov, M., Churazov, E. et al. 1995, Proceedings of the Wurzburg, Germany Meeting `Rontgen Strahlung from Universe` September 25-29. + From December 9 (day 75 of the outburst) the 20-100 keV flux GRO J 1719-24 suddenly decreased within six days from 1.1 +/- 0.1 to 0.4 +/- 0.08 Crab, and on December 16-18 it dropped below the BATSE detection limit of 0.1 Crab, Harmon, B.A., Paceisas, W.S., 1993, IAU Circ. No. 5913. + QPO, van der Hooft, F., Kouveliotou, C., van ParadiJ s, J ., et al. 1996, ApJ , 458, L75. + l = 0.1, b = +7.1, Della Valle, M., Mirabel, F., Roriguez, I.F., 1994, AA, 290, 803. + Dist (kpc) = 2.4, L_{x}= 2 E38 erg/s, L_{x}/ L_{opt}= 1 E3, Fx(erg/cm^{2}s) =3E-7, Lx/Lopt = +1.4 E3, Lx max = 2.1E38 (in 0.1-100 keV), Av = 2.88, Della Valle, M., Mirabell, I.F., Rodriguez, L.F., 1994, AA, 290, 803. + L (2 - 300 keV) = at d= 2 kpc for 3 - 4 Oct. 1994, 2 E37 erg/s and 2 E36 erg/s for 20-22 Sept. 1994, Revnivtsev, M., Gilfanov, M., Churazov, E., et al. 1995, Proceeding of thr Wursburg (Germany) Meeting " Roentgen Strahlung from the Universe", September 20-25. + Optical counterpart: Nova Oph 1993, Spec. Type: K?, V 21, E(B-V) = 0.9 +/- 0.2, R >= 20, B >= 21, outburst amplitude >= 4.4 mag., V 16.55, d = 2.4 kpc, Opt. Counterpart; K V, Mv >= 6, Della Valle, M., Mirabel I.F., Rodriguez L.F., 1994, AA, 290, 803. 1724-307 + Dist (Kpc) ~10, Bradt, H.V.D., McClintock, J.E., 1983, Ann. Rev. Astron. Astrophys., 21, 13. + GC Ter 2. kT (keV) = 8.6, LogN_{H}(cm-2) = 21.85, Av ~ 3 - 4, Grinlay, J.E., Marshall, H.L., Hertz, P., et al. 1980, ApJ, 240, L121. + Av = 3.85, Christian, C.A., Friel, E.D., 1992, AJ, 103, 142. + Mx = 1.4 Mo , Grindlay, J.E., Marshall, H.L., Hertz, P., et al. 1980, ApJ, 240, L121. + E(B-V) = 1.25 +/- 0.15, Christian, C.A., Frigel, E.D., 1992, AJ, 103, 142. 1728-169 + Porb = 0.17492 d, Schaefer, B.E., 1990, ApJ , 354, 720. + Dist (kpc) = 4.4, Davidsen, A., Malina, R., Bowyer, S., 1976, ApJ, 203, 448. + B -V ~ 0.0, U-B= - 0. 5, E(B-V) = 0.35, Davidsen, A., Malina, R., Bowyer, S., 1976, ApJ, 203, 448. + V = 16.7, G-K V, E(B-V) = 0.25, No other features, Shahbaz, T., Smale, A.P., Naylor, T., 1996, MNRAS, 282,1437. 1728-247 + RA = 17 32 02.1, Decl.= -24 44 44 (J 2000), Intensity 1.3 E - 11 (erg/cm^{2}s), Range,0.1-2.4 keV, 18.08.1993, ROSAT, Predehl, P., Friedrich, S., Staubert, R., 1995 AA 294, L33. + Other name V2116 Oph, Shahbaz, T., Smale, A.P., Naylor, T., 1996, MNRAS, 282, 1437. + Oph type; PSR with magnetic field H=E14 Gauss, White, N.E., 1988, Nature, 333, 708. + RA(2000)=17 32 02.1, dec(2000)= -24 44 44, Predehl, S., Friedrich, R., Stanbert, R., 1995, AA 294, L33. + p_{pulse}=120.657s, Finger, M.H., 1993, IAU Circ. No.5859. + p_{spin}=112.68s, p'= -2.68 s/yr, p'/p = -2.7 E-2 yr^{-1}, Elsner, R.F., Weisskopf, M. C., Apparao, K. M., et al., 1985 ApJ 297, 288. + p'_{spin}=1.6+/- 1.4 s/yr, Rao, A.R., Paul, B., Chitnis, V. R., Agraval, P. C., Manchanda, R. K., 1994, AA 289, 143. + Spin p'/p=1.2 E-2 yr^{-1}, Dotani, T., Kii, T., Nagase, F., 1989, PASJ 41, 427. + Pulse period decreased from 135s to 110s, p'~2 s/yr, Manchanda, R.K., Janes, J. D., et al., 1995, AA 293, L32. + p'~1.5 s/yr, Greenhil, J.G., Giles, A. B., Sharma, D. P., et al., 1989, AA 208, L1. + The neutron star surface magnetic field is > 10^{13}Gauss remarkably large for an object believed to be very old, Mony, B., et al., 1989, in Hunt, J., Battrick, B., (eds) proc. 23^{rd}ESLAB Symp. on two topics in X-ray Astronomy, Vol. 1, European Space Agency, Paris, p. 541. + V = 19, Manchanda, R.K., James, S.D., Lawson, W.A., et al. 1985, AA, 293, L29. + Optical counterpart = V2116 Oph from Mv = -0.5 for a M III star to Mv = 3 and the spectral type to M IV accordingly, Predehl, P., Friedrich, S., Staubert, R., 1995, AA, 294, L33. + Optic flare 1.5 mag. 1993 July, Greenhill, J.G., Watson, R.D., Tobin, W., et al. 1995, MNBRAS, 274, L59. + Optical counterpart V2116 Oph, M6 III, Davidsen, A., Malina, R., Rower, S., 1977, ApJ, 211, 866. + E(B-V) = 2.30+/- 0.06, M5 III, Lines, V = 19.6, Shahbaz, T., Smale, A.P., Naylor, T., et al. 1996, MNRAS, 282, 1437. 1728-337 + Rapid burster position (2000yr) {alpha} = 17 33 19+/- 7, , Decl.= -33 23+/- 0.5, ASCA 26 - 27 August 1992, ASCA, 1-10 keV, Fx = 0.004 count/s, Asai, K., Dotani, T., Kunieda, H., Kawai, N., 1996, PASJ , 48, L28. + kT (keV) = 7.8, Parmar, A.N., Angelini, L., Roche, P., White,N.E., 1993, AA, 279, 179. + L_{x}~3 E 33 erg/s (quiescent), 1-10 KeV, at d = 10 Kpc, Photon index ~ 2, Asai, K., Dotani, T., Kunieda, H.,Kawai, N., 1996, PASJ., 48, L27. 1730-220 + kT (keV) = 4 +/- 1, Cominsky, L., Jones, C., Forman, W., Tananbaum, H., 1978, ApJ, 224, 46. 1730-312 + has been discovered on Sept 23, 1994 simultaneously by MIR- KVANT, Borozdin, K., Alexandrowich, N., Sunyaev, R., et al. 1984, IAU, Circ. No. 6083. + and GRANAT, Churazov, E., et al. 1994, IAU Circ 6083. + Average flux during flare are 105 +/- 10 and 80 +/- 21 mCrab in 35-75 and 75-150 keV bands; flux (2-10 keV) 22-23 September 1994, 1.2 E-9 erg/cm^{2}s, (2-10 keV) 25-26 September 1994, 9.52 E-9 erg/cm^{2}s, (2-10 keV) 26-27 September 1994, 11.3 E-9 erg/cm^{2}s, Trudolyubov, S., Gilfanov, M., Churazov, E., et al. in "Roentgen Strahlung from the Universe" Wurtzburg , Germany, 25-29 September 1995. + Transient, {alpha}_{1950}= 17 33 47, {delta}_{1950}= -31 11 37, Trudolyubov, S., Gilfanov, M., Churazov, E., et al. 1995, in "Roentgen Strahlung from the Universe", Wurtzburg, Germany, 25-29 September. + Dist (kpc) = 8.5, photon index = 2.09 - 3.81, kT = 26 -50 keV, L_{x}(1 - 300 keV) = 2.2 E38 erg/s, N_{H}= ( 4.7 - 11.1) E22, Trudolyubov, S., Gilfanov, M., Churazov, E., et al. 1995, Proceeding of the Wurzburg (Germany) Meeting " Roentgen Strahlung from the Universe", September 20-25. + kT = 70 keV, photon index = 2.5, Vargas, M., Goldwurm, A., Paul, J., et al. 1996, AA, 313, 828. 1730-335 + Transient, rapid burster was discovered, Lewin, W.H.G., 1976, IAU, Circ. No. 2922. + In GC Lil 1, Asai, F., Dotani, T., Kawai, N., 1996, PASJ , 48, L27. + Dist (kpc)=10 (GC Lil 1) , Lx (2-10 keV) = 3 (+2, -1) E33 in 1993, Aug. 26-27, ASCA, N_{H}=1 E22, Asai, F., Dotani, T., Kawai, N., 1996, PASJ, 48, L27. + The total energy emitted in one outburst ~ ( 0.3-1) E44 erg/s, Tanaka, Y., Shibazaki, N., ARAA, 1996, 34, 607. 1731-260 + Dist (kpc) = 8.5, Barret, D., Bouchet, L., Mandrov, P., et al. 1992, ApJ, 394, 615. 1732-304 + GC Ter 1 (R.A. = 17 35 47.2, Decl.= -30 28 54) 2000y, contain the XB 1733-30 (R.A. = 17 35 47.4, Decl.= -30 28 58, 2000yr), Johnston, H.M., Verbunt, F., Hasinger, G., 1995, AA, 288, L21. + GRANAT 4-20 keV, 9. 09 - 18. 10. 1990, F_{x}= (3.44 +/- 0.1) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R ., et al. 1992, Astronomy Lett., 18, 291. + SLX 1732-304 (in the globular cluster Terzan 1) has on avaraged flux of ~ 7.4 mCrab (35-75 keV), Goldwurm, A., Denis, M., Paul, J ., et al. 1995, Adv. Space Res., 15, 41. + LogN_{H}(cm-2) = 22.48, Inoue, H., Koyama, K. et.el. 1981, ApJ, 250, L71. + Lx (4-20 keV) = (3.33 +/- 0.15) E36 erg/s at d = 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. + d = 5.9 Kpc (GC Ter 1), N_{H}= 1.8 E 22 cm^{-2}, Log L_{x}= 36.10, Johnston, H.M., Verbunt, F., Hasinger, G., 1995, AA., 298, L21 1734-292 + GRANAT, 4-20 keV, 0.006 cnt/s, 6.10.1990 in (3-12 keV) band Fx = 3.4 +/- 0.4 mCrab, 9.09 - 18.10.1990, F_{x}= (0.62 +/- 0.08) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Lx ( 4-20 keV) = (7.9 +/- 1.3) E35 erg/s at d= 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1735-269 + GRANAT, 4-20 keV, 9.09 - 18.10.1990, F_{x}= (1.68 +/- 0.35) E-2 photon/cm^{2}s, , Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Lx ( 4-20 keV) = (2.32 +/- 0.43) E36 erg/s at d = 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1735-444 + EXOSAT, August 1985, 1.4-20 keV, Fx = (4.4-6.4) E-9 erg/cm^{2}s, Not periodic modulation, van Paradijs, J., Penninx, W., Lewin, W.H.G., et al. 1988, AA, 192, 147. + P_{orb}= 0.152 days, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + Dist (kpc) = 5-10, Lx / Lopt = 2100, McClintock, J.E., Canizares, C.R., 1978, ApJ, 223, L73. + Dist (kpc) 2, Smale, A.P., Charles, P.A., Tuohy, I.R., Thorstensen, J.R., 1984, MNRAS, 207, 29P. + Kopt = 68 km/s, Vg = -152 km/s, i = 10 - 20^{o}, Smale, A.P., Corbert, R.H.D., 1991, ApJ, 383, 853. + Spectral Type: F0 - K5 V, V926 Sco, Hammerschlag-Hensberge, G., McClintock, J.E., van Paradijs, J., 1982, ApJ, 254, L1. Smale, A.P., Charles, P.A., Tuohy,I.R., Thorstensen, J.R., 1984, MNRAS, 207, 29. + E(B-V) = 0.3, Canizares, C.R., McClintock, J.E., Grindlay, J.E., 1979, ApJ, 234, 556. + Magnetic X-ray Binary, B - V = 0.22, U - B = - 0.82, McClintock, J.E., Canizares, C.R., Backman, D.E., 1978, ApJ, 273, L75. + Mv = 2.5, Smale, A.P., 1988, MNRAS, 233, 51. + E(B-V) = 0.15, V = 17.5, Mv = 2.2, van Paradijs, J., McClintock, J.E., 1994, AA, 290, 133. + possible HMXB, McClintock, J.E., Canizares, C.R., Backman, D.E., 1978, ApJ, 273, L75. + HVg CaII, NaI lines indicate different spectral type, Canizares, C.R., McClintock, J.E., Grindlay, J.E., 1979, ApJ, 234, 556. 1736-297 + GRANAT, 4-20 keV, 9.09 - 18.10.1990, F_{x}= (0.44 +/- 0.06) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Lx (4-20 keV) = (5.7 +/- 1) E35 erg/s at d= 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1739-278 + X-ray transient, discovered in 1996 March with SIGMA telescope (Granat space observatory). Intensities F_{x}=70+/- 7 mCrab and 58+/- 10 mCrab in the 40-75 keV and 75-150 keV. Coordinates RA=17^{h}39^{m}31^{s}, dec= -27^{o} 45' 52'' (1950 yr). Rossi X-ray Timing Explorer (RXTE) detected GRS 1739-278 in the 2-10 keV band ~250 mCrab in early March, reaching a peak of ~800mCrab around March 20 and declining to ~350 mCrab in late April, Vargas, M., Goldwurm, A., Laurent, P., et al., 1997, ApJ 476, L23. + Hardness ratio of 0.83+/- 0.13, Power-law (PI) {alpha} = 2.2+/- 0.3, kT=68, N_{H}= (4.1+/- 0.7) E22 cm^{-2}, Peak luminosity L_{x}=(8.6+/- 2.0) 10^{36}ergs/s in the 40-300 keV band at d=8.5 kpc, Vargas, M., Goldwurm, A., Laurent, P., et al., 1997, ApJ 476, L23. 1740.7-2942 + In October 1991 F_{x}= (4-150 keV) = 20-30 mCrab by GRANAT, Churazov, E., Gilfanov, M., Sunyaev, R., et al. 1992, ApJ , 407, 752. + GRANAT, 4-20 keV, 9.09 -18.10.1990, F_{x}= (4.11 +/- 0.06) E- 2 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Was discovered by Einstein in soft X-rays (< 4 keV), Hertz, P., Grindlay, J ., 1984, ApJ , 278, 137. + In 1993 - 1994 ASCA 1-10 keV, F = 2.435 E-10 erg/cm^{2}s, Sheth, S., Liang, E., Luo, C., Murakami, T., 1996, ApJ , 468, 755. + 1985, Spartan-1, Fx = 2.5 E-10 erg/cm^{2}s (2-10 keV), Kawai, N., Fenimore, E.E., Middleditch, J ., et al. 1988, ApJ , 330, 130. + kT(keV)=14.3, Photon index = 2.0, LogN_{H}(cm-2)=23.16 - 23.2 (for Thermal Bremsstrahlung); 23.21, (for Power-law), Kawai, N., Fenimore, E.E., Middleditch, J., et al. 1988, ApJ, 330, 130 + Av = 25-175, ~100, N_{H}= 4 E22, Skinner, G.K., Pan, H.C., Maisack, M., 1991, AA, 252, 172. + L ( 4 -300 keV) = 3.2 E37 erg/s at d = 8.5 kpc, Sunyaev, R., Gilfanov, M., Churazov, E., et al. 1991, Astronomy Lett., 17, 116. + photon index = 1.11 +/- 0.014, N_{H}= 8 E22 cm^{-2}, Sheth, S., Liang, E., Luo, C., Murakami, T., 1996, ApJ, 468, 755. + Lx (4-20 keV) = (5.50 +/- 0.09) E36 at d= 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. + N_{H}= E23 cm^{-2}due to molecular cloud in front of source, Churazov, E., Gilfanov, M., Sunyaev, R., 1996, ApJ, 464, L71. + N_{H}= 4 E22 cm^{-2}, Skinner, G.K., Pan, H.C., Maisack, M., et.al., 1991, Ap.J., 252, 172. 1741-322 + An outburst of this transient was observed with Ariel 5 and HEAO-1 in August 1977, Kaluzensky, L.J., Holt, S.S., 1977, IAU Circ. No. 3099 and No. 3106. + Average flux (2-10 keV) in the period J uly 29 - August 6, 1985 was < 4 E-11 erg / cm^{2}s, (< 0.002 Crab), Skinner, G.K., Griffin, I., Whitmore, B., et al. 1990, MNRAS, 243, 72. + On March 12-18, 1978 the flux in the range 1-10 keV was E-9 erg / cm^{2}s (~ 0/03 Crab), Wood, K.S., Meekins, J .F., Yentis, D.J ., et al. 1981, ApJ , 56, 507. 1741.9-2853 + GRANAT, 4-20 keV, 9.09 - 18.10.1990, (1.47 +/- 0.09) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. 1742-289 + Discovered in February 7, 1975 by Ariel-V, ({alpha}_{1950}= 17 42 26.0, {delta} ._{1950}= -28 59.8), Max Fx = 4 E-8 erg/cm^{2}s (3-10 keV) at 16 February, Eyles, C.J., Skinner, G.K., Willmore, A.P., Rosenberg, F.D., 1975, Nature, 257, 291. + In 1993 - 1994 ASCA, in 3 -10 keV, F = ( 0.8 - 4 ) E-11 erg/cm^{2}s, Maeda, Y., Koyama, K., Sakano, M., et al. 1996, PASJ , 48, 417. + Dist (kpc) =1.2, Lx max ~7 E36 erg/s, LogN_{H}(cm-2) ~23, Murdin, P., Allen, D.A., Morton, D.C., et al. 1980, MNRAS, 192, 709. + Dist (kpc) =1.2, Av ~1.2, Bradth, H.V.D., McClintock, J.E., 1983, Ann.Rev.Astron.Astrophys., 21, 13. + kT(keV) ~ 4.5, LogN_{H}(cm-2) ~23, Brunduardy, G., Ives, J.C., Brinkman, A.C., Maraschl, L., 1976, MNRAS, 175, 47P. + photon index = 2.1 (low-state), 2.5 (high - state), 5.6 (eclipse), N_{H}= 2.6 E23, Lx (3-10 keV) = (2-10) E35 erg/s, Meade, Y., Koyama, K., Sakano, M., et al. 1996, PASJ, 48, 417. + Spec. Type: K3 V, V = 18.2, U - B = 1.35, E(B-V) = 0.35, Murdin, P., Allen, D.A., Morton, D.C., et al. 1990, MNRAS, 192, 709. 1742-294 + In 1992 flux in 35-100 keV was 31+/- 5.4 mCrab, L=3 E36 erg/s (at d=8.5 kpc), Churazov, E., Gilfanov, M., Sunyaev, R., 1995, ApJ , 443, 341. + GRANAT, 4-20 keV, 9.09- 18.10.1990, F_{x}= (5.23 +/- 0.06) E- 2 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + In 1990 Spring - 1992 Spring the flux in the 8-20 keV was 20 - 40 mCrab, the brightest state ~70 mCrab in September 3, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1994, ApJ , 425, 110. + 1985, September 1, Fx = 1.1 E-9 ergs/cm^{2}s (2-10 keV) Spartan-1, Kavai, N., Fenimore, E.E., Middledith, J ., et al. 1988, ApJ , 330, 130. + Dozen X-ray burst, Pavlinsky, M. N., Grebenev, S. A., Sunyaev, R. A., 1994, ApJ , 425, 110. + Transient hard state was detected by Granat / Sigma in 1992, Churazov, E., Gilfanov, M., Sunyaev, R., et al. 1995, ApJ , 443, 341. + kT(keV) = 5.1, Photon index = 2.8, LogN_{H}(cm-2) = 22.913 - 23.0, Kawai, N., Fenimore, E.E., Middleditch, J., et al. 1988, ApJ, 330, 130. + L (3-30 keV) = 1.3 E37 erg/s at d= 8.5 kpc, Skinner, G.K., Willmore, A.P., Eyles, C.J., et al. 1978, Nature, 330, 544. + L (35-100 keV) = 3 E36 at d = 8.5 kpc, Churazov, E., Gilfanov, M., Sunyaev, R., et al. 1995, ApJ, 443, 341. 1743-288 + LogN_{H}(cm-2)= 23.45, Proctor, P.J., Skinner, G.K., Willmore, A.P., 1978, MNRAS, 185, 745. 1743-290 + 19-31 March 1995, ROSAT, 1-20 keV, F = 8 E-11 erg/cm^{2}s, Barret, D., Grindlay, J .E., 1996, AA, 311, 239. + Dist (kpc) = 8.5, L(1-20 keV) = 7 E35 erg/s, N_{H}= 6 E22 cm^{-2}, Barret, D., Grindlay, J.E., 1996, AA, 311, 239. 1743-2926 + Lx ( erg/s ) = 9 E36, LogN_{H}(cm-2) = 22.7 - 23.3 (GCX-1) d=10 kpc, Cruddace, R.G., Fritz, G., Shulman, S., et al. 1978, ApJ, 222, L95. 1743.1-2843 + GRANAT, 4-20 keV, 9.09-18.10.1990, F_{x}=(1.77+/- 0.08) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + 1985, Spartan-1, Fx = 1.9 E-10 ergs/cm^{2}s (2-10 keV), Kawai, N., Feniore, E.E., Middledith, J ., et al. 1988, ApJ , 330, 130. + kT(keV) = 11.2, Photon index = 2.2, LogN_{H}(cm-2) = 23.29 - 23.37, Kawai, N., Fenimore, E.E., Middleditch, J., et al. 1988, ApJ, 330, 130. + Lx (4-20 keV) = ( 2.03 +/- 0.12) E36 erg/s at d = 2.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1744-265 + GRANAT, 4-20 keV, 9.09 - 18.10.1990, F_{x}= 0.32 +/- 0.01 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + 1985, Spartan-1, Fx = 7.6 E-10 ergs/cm^{2}s, (2-10 keV), Kavai, N., Fenimore, E.E., Middleditch, J ., et al., 1988, ApJ , 330, 130. + Lx (4-20 keV) = (3.18 +/- 2) E37 erg/s at d = 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. + kT = 5.6 keV, Photon index = 2.49, log N_{H}(cm^{-2})= 22.58 - 22.67, Kawai, N., Fenimore, E.E., Middleditch, J., et.al., 1988, Ap.J., 330, 130. 1744-28 + Discovered on December 2, 1995, with BATSE (GRO), kT = 6 keV, N(H) = 2 E22 cm^{-2}, Fishman, G.J., Kouveliotu, C., van ParadiJ s, J ., et al. 1995, IAU, Cir. No. 6272. Lewin, W.H.G., Rutledge, R.E., Kommers, J .M., et al. 1996, ApJ , 462, L39. AugusteiJ n, T., van de Steene, G., van de Hooft, F., et al., 1966, IAU Circ. No. 6326. + BATSE (20-50 keV) on 15.1.1996, flux = 2 E-7 erg/cm^{2}s, Fishman, G.J., Kommers, J., Lewin, W.H.G., 1996, IAU Cir. No. 6290. + Mid J une 1996, in (20-100 keV) ~ 2.5 Crab, Mid J anuary 1996, GRANAT 8-20 keV, 4.4 +/- 0.3 Crab, Sazonov, S., Sunyaev, R., 1996, IAU Cir. No. 6191. + BATSE (GRO) 20-60 keV, mid December 1995, Fx <= E-9 erg/cm^{2}s, mid February 1996, Fx ~ 4E-8 erg/cm^{2}s, van Paradijs, J., van den Heuvel, E.P.J ., Kouveliotou, C., et al. 1997, AA, 317, L9. + Transient rapid burster, Lewin, W.H.G., Rutlege, R.E., Kommers, J .M., et al. 1996, ApJ , 462, L39. + Orbital period 11.8 d, pulsar pulse period 467 ms, Finger, M.H., Wilson, R.B., van Paradijs, 1996, IAU Circ, No. 6286. Strichman, M.S., Dermer, C.D., Grove, J .E., et al. 1996, ApJ , 464, L131. Kouveliotu, C., van ParadiJ s, J ., Fishman, G.J ., et al. 1996, IAU, Circ, No. 6286. + Magnetic field E12 Gauss, Daumerie, P., Kalogera, V., Lamb, F.K., Psaltis, D., 1996, Nature, 382, 141. + QPO, Zhang, W., Morgan, E. H., Jahoda, K., et al., 1996, ApJ 469, 29. + The mean time interval between bursts is evidently constant, t_{ave}~29.6 minutes, for the whole period of observation from 1995 December 18 to 1996 March 15, Aptekar, R.L., Butterworth, P. S., Cline, T. L. et al., 1998, ApJ 493, 404. + kT (keV) = 6 keV, Briggs, M.S., Harmon, B.A., van ParadiJs, J., et al. 1996, IAU Circ. No. 6290. + Photon index = 1.2, Swank, J., 1996, IAU Circ. No. 6291.Lewin, W.H.G., Rutlege, R. E., Kommers, J.M., et al. 1996, ApJ, 462, L39. + N_{H}= 2 E22 cm^{-2}, AugusteiJn, T., van der Steene, G., van der Hooft, F., et al. 1996, IAU Circ. No. 6326. + i < 18^{o}, M_{x}= 1.4 Mo , Mopt = 0.065 - 0.14 Mo , fx(M) = (1.31 +/- 0.04) E-4 Mo , Finger, M.H., Wilson, R.B., van Paradijs, J., 1996, IAU Circ. No. 6286. 1744-299 + GRANAT, 4-20 keV, 9.09 - 18.10.1990, F_{x}= (3.36 +/- 0.08) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebener, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Lx (4-20 keV) = (3.76 +/- 0.12) E36 erg/s at d = 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1744-300 + Name, 1744.2-2959, Discovery in 1985 by Spartan-1 free-flying shuttle payload. Fx = 20 E-11 erg/cm^{2}s (2-10 keV), Kawai, N., Fenimore, E.E., Middleditch, J ., et al. 1988, ApJ , 330, 130. + kT(keV)= 4.4, Photon index = 2.86, LogN_{H}(cm-2)= 22.756 - 22.86, Kawai, N., Fenimore, E.E., Middleditch, J., et al. 1988, ApJ, 330, 130. 1745-203 + GC NGC 6440, (RA = 17 48 52.7, Dec. = -20 21 37, 2000 yr) contain MX 1746-20 (RA = 17 48 53.4, Dec. = -20 21 43, 2000 yr), Johnston, H.M., Verbunt, F., Hasinger, G., 1995, AA, 298, L21. + Dist (kpc) = 5.8, Martins, D.H., Harvel, C.A., Miller, D.H., 1980, AJ, 85, 521. + LogN_{H}(cm-2) = 22.04, Markert, J.H., Backman, D.E., Canizares, C.R., et al. 1975, Nature, 257, 32. + Dist for GCNGC 6440, 7 Kpc, N_{H}= 5 E21 cm^{-2}, for MX 1746-20, Log L_{x}= 33.09, Johnston, H.M., Verbunt, F., Hasinger, G., 1995, AA., 298, L21. + B-V = 1.44, U-B = 1.96, E(B-V) = 1.17, Martins, D.H., Harvel, C.A., Miller, D.H., 1980, AJ, 85, 521. 1745-248 + GC Ter 5, ( RA = 17 48 04.6, Dec. = -24 46 48, 2000 yr) contain XB 1745-25 (RA = 17 48 05.0, Dec. = -24 46 47, 2000 yr), Johnston, H.M., Verbunt, F., Hasinger, G., 1995, AA, 298, L21. + Ter 5 , Dist (kpc) = 7.6 Kpc, N_{H}= 2 E22 cm^{-2}, For XB 1745-25, Log L_{x}= 34.62, Johnston, H.M., Vcerbunt, F., Hasinger, G., 1995, AA, 298, L21. 1746-370 + X-ray sources in GC NGC 6441, Katz, J.I., 1975, Nature 253,698; Clark, G. W., 1975, ApJ 199, L143. + E(B-V) = 0.46, Hesser, J.E., Hartwick, F.D.A., 1976, ApJ, 203, 97. + The probable optical counterpart NGC 6441 Star U1, E(B- V)=0.42, B_{o}=18.18, (U-B)_{o}= -1.06, M_{B}=3.03. Ultraviolet intensity variation of 30% for this object over 0.5 hr, Deutsch, E. W., Anderson, S. F., Margon, B., and Downes, R. A., 1998, ApJ 493, 775. 1747-214 + LogN_{H}(cm-2) = 22, Magnier, E., Lewin, W.H.G., van ParadiJs,J., et al. 1989, MNRAS, 237, 729. 1747-313 + GRANAT, 3-12 keV, 9.09 - 18.10.1990, F_{x}= ( 7.85 +/- 1.27) E-2 photon/cm^{2}s, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R., et al. 1992, Astronomy Lett., 18, 291. + Lx (3-12 keV) = (5.68 +/- 0.84) E36 at d = 8.5 kpc, Pavlinsky, M.N., Grebenev, S.A., Sunyaev, R.A., 1992, Astronomy Lett., 18, 291. 1747-341 + 19-31 March 1995 Rosat, 1-20 keV, F =4 E-11 erg/cm^{2}s, Barret, D., Grindlay, J .E., 1996, AA, 311, 239. + Dist (kpc) = 8.5, Lx (1-20 keV) = 3.4 E35 erg/s, N_{H}= 6 E22 cm^{-2}, Barret, D., Grindlay, J.E., 1996, AA, 311, 239. 1755-338 + Kvant, 1989, Mach -September, (2-10 keV), 35 - 105 mCrab, Pan, H.C., Skinner, G.K., Sunyaev, R.A., Borozdin, K.N., 1995, MNRAS, 274, L15. + Recurrent dips of 30 minutes duration with a period of 4.4 hr, White, N.E., Parmar, A. N., Sztajno, M., et al., 1984, ApJ 283, L9. + kT(keV) = 1.87, LogN_{H}(cm-2) = 21.39 - 22.39 (variable), Church, M.J., Blauciska-Church, M., 1993, MNRAS, 260, 59. + Lx ( 1-20 keV) = 4 E36 erg/s at d = 3 kpc, White, N.E., Parmar, A.N., Sztajno, M. et al. 1984, ApJ, 283, L9. + N_{H}= (2.2 +/- 1.2) E21 cm^{-2}, White, N.E., Marshall, F.E., 1984, ApJ, 281, 354. + N_{H}= E21 - 6 E21 cm^{-2}, photon index = 1.9 - 2.7, Pan, H.C., Skinner, G.K., Borozdin, K.N., 1995, MNRAS, 274, L15. + ROSAT(PSPC),observation on 1993, March 29, show decrease of count rate of 10% in the bound 0.5-2.0 keV(periodic dips), N_{H}= 5.29+/- 0.22 E21 atoms/cm^{2}, Photon index = 2.6-2.8, Church, M.J., Balucinska,-Church, M., 1997, AA, 317, L47. + d > 4 kpc, Wachter, S., Smale, A.P., 1998, ApJ 496, L21. + Opt. Counterpart is a blue 19th mag. star, McClintock, J.E., Canizares, C.R., Backman, D.E.,1978, ApJ, 223, L75. + The spectrum showed very weak He II lines, Cowley, A.P., Hutchings, J.P., Schmidtke, P.C., et al. 1988, ApJ, 333, 906. + Sinusoidal modulation in the V band with an amplitude of 0.4 mag and a period of 4.46 hr confirmed the identification of the counterpart V4134 Sgr, V=18.5 mag, Mason, K.O., Parmar, A. N., and White, N. E., 1985, MNRAS 216, 1033. + The counterpart has faded from its on-state brightness of V=18.5 to V > 22, R > 21.5, and I > 21. Spectral type M0V, d > 4 kpc, Wachter, S., Smale, A. P., 1998, ApJ 496, L21. 1758-205 + Dist (Kpc)= 9, LogN_{H}(cm-2) = 22.5, Church, M.J., Blauciska-Church, M., 1993, MNRAS, 260, 59. 1758-250 + QPO, Hasinger, G., van der Klis, M., 1989, AA, 225, 79. (and see their references). Kuulkers, E., van der Klis, M., Ooesterbrock, T., et al. 1994, AA, 289, 795. + LogN_{H}(cm-2) = 22.48, Asai, K., Kazumi, A.S.A.I., Dotani, T., et al. 1994, PASJ, 46, 479. 1758-258 + Discovered with Granat in March- April 1990, Mandrov, P., ***** et al. 1990, IAU Circ. No. 5032. Sunyaev, R.A., Pavlinskii, M., Gilfanov, M., et al. 1991, Sov. Astron. Lett., 17, 50. + Lx ( erg/s ) = (4.6 - 8.2) E36 (in the 4-30 keV band), LogN_{H}(cm-2) = 23.25, Sunyaev, R., Churazov, E., Gilfanov, M., et al. 1991, AA, 247, L29. + Lx (4 - 300 keV) = 2.2 E37 erg/s at d = 8.5 kpc, Sunyaev, R., Gilfanov, M., Churazov, E., et al. 1991, Astronomy Lett., 17, 116. + Variations by a factor 2 over several days were observed in the 4-30 keV and 5-170 keV bands, Sunyaev, R., Pavlinskii, M., Gilfanov, M., et al. 1991, Astronomy Lett., 17, 50. 1811-171 + EXOSAT,1985 year in (1-20 keV) F= 8 E-9 erg / cm^{2}s, Garchia, M.R., Grindlay, J .E., Molnar, L.A., et al. 1988, ApJ , 328, 552. + EXOSAT 1983 year in (1-12 keV) F = 6 E-9 erg / cm^{2}s, Stella, L., White, N.E., Taylor, B.G., 1985, in ESA Sp-236, 552. + Ginga 1989 year in (1-20 keV), F = (7-10) E-9 erg / cm^{2}s, Matsuba, E., Dotani, T., Mitsuda, K., et al. 1995, PASJ , 47, 575. + Lx = 2.3 E39 (D/7 kpc)^{2}, N_{H}= 2 E22 cm^{-2}, A_{v}= 13- 18, d = 8-9 kpc, Lx = (4-6) E37 (d/7 kpc)^{2}erg/s, Matsuba, E., Dotani, T., Mitsuda, K., et al. 1995, PASJ, 47, 575. + Radio flux is variable around 1 mJy is not correlated with the X-ray flux, Garchia, M.R., Grindlay, J.E., Molnar, L.A., et al. 1988, ApJ, 358, 552. 1813-140 + QPO, Hasinger, G., van der Klis, M., 1989, AA, 225, 79. (and see therein references). + Dist (kpc) = 1.4, Hoag, A., Weisberg, J.M., 1976, ApJ, 209, 908. + Spec. 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