5 31 TEMPERATURES OF COOLING NEUTRON STARS NS Log Age Log T_e Distance Period Ref Name (yrs) (K) (kpc) (sec) 3.0 1 0531+21 3.10 0.00 - 6.25 2. 0.033 BA95 Crab 5.0 1 0822-4300 3.5 6.20 - 6.30 2.2 0.075 ZTP99 in Puppis A 5.0 1 1207-52 4.00 6.05 - 6.15 2.50 0.000 ZPT98 in PKS 1209-52 5.0 1 0833-45 4.05 5.87 - 5.91 0.40 0.089 PSZ96 Vela 4.0 1 0833-45 4.05 5.81 - 5.94 0.50 0.089 OFZ93 Vela 4.0 0 0833-45 4.05 5.87 - 5.89 0.50 0.089 OFZ93 Vela 4.0 1 0002+6246 4.50 5.72 - 5.85 3.00 0.242 HC95 1.0 0 1800-21 4.20 0.00 - 6.30 3.94 0.134 BTO95 2.0 1 1706-44 4.24 0.00 - 6.10 1.82 0.102 BBT95 2.0 0 1823-13 4.33 0.00 - 6.20 4.00 0.101 FSP96 2.0 1 2334+61 4.61 5.83 - 6.07 2.50 0.495 BBT96 2.0 0 2334+61 4.61 0.00 - 6.10 2.47 0.495 SL95 1.0 1 1916+14 4.95 0.00 - 6.00 1.55 1.181 SL95 5.0 1 0656+14 5.04 5.93 - 5.97 0.5 0.384 FOK92 5.0 0 0656+14 5.04 5.81 - 5.92 0.5 0.384 Getal96 5.0 1 0656+14 5.04 5.70 - 5.76 0.3 0.384 ACPRT93 1.0 1 0740-28 5.20 0.00 - 6.00 1.89 0.167 SL95 1.0 1 1822-09 5.37 0.00 - 5.85 1.01 0.769 SL95 2.0 0 0114+58 5.44 0.00 - 6.05 2.14 0.101 SL95 5.0 0 0630+178 5.48 5.60 - 5.80 0.16 0.237 HR93 (BB+BB) Geminga 5.0 0 0630+178 5.48 5.48 - 5.77 0.16 0.237 HR93 (BB+PL) Geminga 5.0 0 0630+178 5.48 5.25 - 5.45 0.16 0.237 MPM94 (MH 12) Geminga 5.0 0 0630+178 5.48 5.48 - 5.60 0.16 0.237 MPM94 (MH 13) Geminga 5.0 1 0630+178 5.48 5.50 - 5.70 0.16 0.237 My guess 5.0 1 1055-52 5.73 5.74 - 5.82 0.5 0.197 OF93 5.0 0 1055-52 5.73 5.84 - 5.93 0.5 0.197 Getal96 2.0 0 0355+54 5.75 0.00 - 6.00 2.07 0.156 S94 2.0 0 0538+2817 5.78 0.00 - 6.00 1.50 0.143 Setal95 3.0 1 1929+10 6.49 0.00 - 5.50 0.17 0.226 YHH94 3.0 1 0950+08 7.25 0.00 - 5.10 0.13 0.000 MW94 1.0 0 0031-07 7.56 0.00 - 5.60 0.68 0.000 SL95 NOTE: first entry: `goodness' of the data: 1: neutron star not detected, 2: neutron star detected at low count rate which precludes any serious analysis of the origin of the photons, 3: neutron star clearly detected but there is evidence that the photons come mostly, or even exclusively, {\em not} from surface thermal emission, 4: neutron star clearly detected with some spectral evidence about the thermal origin of the photons and, finally, 5: neutron star clearly detected with good spectral evidence about the thermal origin of the photons second entry: to decide plotting the data or not in `subroutine plot_data'. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0531+21 (Crab): \reference{BA95} Becker, W., \& Ashenbach, B. 1995, in The Lives of the Neutron Stars, ed M. A. Alpar, \"U. Kizilo\u{g}lu, \& J. van Paradijs (Kluwer: Dordrecht), 47 % Comment: thermal emission NOT seen. It's an upper limit. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0822-4300 \reference{ZTP99} Zavlin, V. E., Tr\"umper, J., \& Pavlov, G. G., 1999, ApJ, 525, 959 %Comments: magnetized hydrogen atmosphere fits. As in the Vale case % they give much more realistic spectral fits in terms of % radius (or distance) of the neutron star. % Pulsations detected at 75 ms. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1207-52 \reference{ZPT98} Zavlin, V. E., Pavlov, G. G., \& Tr\"umper, J. 1998, A\&A, 331, 821 %Comments: magnetized hydrogen atmosphere fits. As in the Vale case % they give much more realistic spectral fits in terms of % radius (or distance) of the neutron star. % No pulsations detected yet. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0833-45 (Vela): \reference{PSZ96} Page, D., Shibanov, Yu. A., \& Zavlin, V. E. 1996, in R\"ontgen Strahlung from the Universe, MPE Report 263, ed. H.-U. Zimmermann, J.E. Truemper and H. Yorke (Garching: MPE), 173 %Comment: magnetized H atmosphere fits. % This is actually THE ONLY TEMPERATURE YOU MAY BELIEVE: it's based % on spectral fits with reallistic atmosphere models (based on sound % physics) and give meaningfull results in the sense that the distance % and interstellar absorption are OUTPUT of the fits and check with % other independent estimates (of D and N_H). % The atmosphere models are reliable because the surface temperature % (non redshifted) is about 10^6 K and the atmosphere fully ionized: % at lower T (e.g., 0656+14, 1055-52 and Geminga) the atmopshere % models are not yet good enough for serious work (but people did % use them and their results should not be trusted too much). \reference{OFZ93} {\"O}gelman, H., Finley, J. P., \& Zimmerman, H. U. 1993, Nature, 361, 136 %Comment: the quoted temperature is the EFFECTIVE temperature % obtained from the luminosity, not the BB temperature. % It's for a 14 km radius NS %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0002+6246 \reference{HC95} Hailey, Ch.~J., \& Craig, W.~W. 1995, ApJ, 455, L151 %Comment: X-ray discovered pulsar, very similar to Vela. % Pulsation seen at 10%+/-10% level. % Age is from the SNR. % ~124 photons from the point source, no evidence of nebula %Comment: the quoted temperature is the EFFECTIVE temperature % obtained from the luminosity, not the BB temperature. % It's for a 14 km radius NS %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1800-21: \reference{BTO93} Becker, W., Tr\"umper, J., \& \"Ogelman, H. 1993, in Isolated Pulsars, ed. K. A. Van Riper, R. Epstein \& C. Ho (Cambridge: Cambridge Univ. Press), 104 %Comment: from the ROSAT sky-survey, i.e., very short exposure. % `Detection' below the limit of reasonable likelihood, so it's % really undetected. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1706-44: \reference{BBT95} Becker, W., Brazier, K. T. S. \& Tr\'umper, J. 1995 A\&A, 298, 528 %Comment: Vela's twin brother. Quite far away, strong absorption. % Not possible to seperate emission of the pulsar from the % nebula (there should be a nebula as in Vela). % Too few photons for spectral fits. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1833-13: \reference{FSP96} Finley, J. P., Srinivasan, R., \& Park, S., 1996, ApJ, 466, 938 %Comment: Vela's twin brother. Quite far away, strong absorption. % No evidence that emission is thermal from surface, so % it's a rough upper limit, adjusted by hand for a 14 km radius NS. % Too few photons for spectral fits. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 2334+61: \reference{BBT96} Becker, W., Brazier, K.T.S., \& Tr\"umper, J. 1996, A\&A, 306, 464 %Comment: associated with the SNR G 114.3+0.3. % 15 photons detected. No emission detected from the SNR. % T is of course an upper limit. \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 %Comment: very far away, barely detected. Since it's about the same age % as Vela there should be a nebula but too few photons to separate % the pulsar emission from the nebula. So T is an upper-upper limit %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1916+14: \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 %Comment: not too far but in a region with very strong interstellar absorption, % Pulsar NO DETECTED: so it's an upper-upper limit. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0656+14: \reference{FOK92} Finley, J.~P., {\"O}gelman, H., \& Kizilo{\u{g}}lu, \"{U}. 1992, ApJ, 394, L21 %Comment: blackbody fits \reference{Getal96} Greiveldinger, C., et al. 1996, ApJ,465, L35 %Comment: blackbody fits \reference{ACPRT93} Anderson, S.~B., C\'{o}rdova, F.~A., Pavlov, G.~G., Robinson, C.~R., \& Thompson, Jr, R.~J. 1993, ApJ, 414, 867 %Comment: magnetized hydrogen atmosphere fits %Comment: my educated guess is that T_e should be between the BB and the % mag. H % BB gives the correct distance (i.e., compatible with the pulsar % distance estimate by radio-astronomers, while H give too small a D, % i.e. T is too low. % % The quoted distances are the distances resulting from the spectral fits. % Radio-astronomers put it usually at 0.7 kpc. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0740-28: \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 %Comment: a little bit far and probably quit absorbed. % Pulsar NO DETECTED: so it's an upper-upper limit. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1822-09: \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 %Comment: relatively far far away and in a region with very strong interstellar % absorption, % Pulsar NO DETECTED: so it's an upper-upper limit. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0114+58 \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 %Comment: far away with strong absorption, barely detected. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0630+178 (Geminga): \reference{HR93} Halpern, J. P., \& Ruderman, M. 1993, ApJ, 415, 286 %Comment: good data but low temperature makes that atmosphere models % are not reliable. Distance IS KNOWN thank to parralax measurements % with the Hubble: that put terrible constraints on the atmosphere % models and none is adequate. BB gives the correct distance at the % lower range. HR get Log T_e = 5.66 - 5.79: I cut it at 5.60 - 5.70 % using the distance constraint. % Turns out the at low temperature the atmosphere models should not be % very different from BB owing to the strong absorption edge which is % right within the ROSAT range. Present atmosphere models do not yet % handle partial ionization correctly, so they have too small an % absorption edge: final will have stronger edge and be closer to BB. % IN SHORT: BB IS NOT TOO BAD %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1055-52: \reference{OF93} \"{O}gelman, H., \& Finley, J. P. 1993, ApJ, 413, L31 \reference{Getal96} Greiveldinger, C., et al. 1996, ApJ,465, L35 %Comment: BB fits. Temperature so obtained is definitely too high: % they need a distance of 0.5 kpc while radio-astronomers put this % pulsar at 1. - 1.5 kpc (a lower temperature would push it further % away). % SO IT'S AN UPPER LIMIT. % % (The quoted distance is the distance resulting from the spectral fits.) %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0355+54 \reference{S94} Slane, P. 1993 ApJ, 437, 458 %Comment: quite far away and in a region of quite strong absorption. % Detected (70 photons) but no spectral fits possible. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0538+2817 \refernce{ABTAW95} Sun, X., Aschenbach, B., Becker, W., Tr\"umper, J. Anderson, S. \& Wolszczan, A. 1995, IAU Circ. 6187 %Comment: recently detected pulsar within SNR S147. %Detected in the All-Sky-Survey. Temperature estimate obviously very crude %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 1929+10: \reference{YHH94} Yancopoulos, S., Hamilton, T. T., \& Helfand, D. J. 1993, ApJ, 429, 832 %Comment: one of the closest pulsars. Detected clearly with a very long % observation. Spectral fits possible: emission comes from the hot % polar caps, no emission from the surface detected. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0950+08 \reference{MW94} Manning, R. A., \& Willmore, A. P. 1994, MNRAS, 266, 635 %Comment: only 50 photons, psectral fits not possible but % hardness ratios indicate high temperature, i.e. % polar cap emission. % The reported temperature is from the luminosity obtained % assuming BB emission. %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%% % 0031-07 \reference{SL95} Slane, P. \& Lloyd, N. 1995 ApJLett 452, L115 % Comment: undetected %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%