Difference between revisions of "List of accreting X-ray pulsars"
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! Notes | ! Notes | ||
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− | | [[CXOU J005047.9-731817]] || 12.699963 || -73.305018 || | + | | [[CXOU J005047.9-731817]] || 12.699963 || -73.305018 || 62<ref name="graczyk14">Distance to SMC. See Graczyk, D. et al., ApJ 780, 59 ([https://ui.adsabs.harvard.edu/#abs/2014ApJ...780...59G/abstract NASA ADS])</ref> || 292 || || [[List of Be X-ray Binaries|BeXRB]]? || || T || aka SXP 292 |
|- | |- | ||
− | | [[RX J0059.2-7138]] || 14.803112 || -71.645828 || | + | | [[RX J0059.2-7138]] || 14.803112 || -71.645828 || 62<ref name="graczyk14" /> || 2.76 || 82|| [[List of Be X-ray Binaries|BeXRB]]? || [[List of cyclotron line sources|C]]? || T || aka SXP 2.76 |
|- | |- | ||
− | | [[RX J0101.8-7223]] || 15.467910 || -72.392796 || 12.3 (+2.0, -1.7) || 175 || || [[List of Be X-ray Binaries|BeXRB]] || || T || | + | | [[RX J0101.8-7223]] || 15.467910 || -72.392796 || 12.3 (+2.0, -1.7)<ref name="bailerjones18">Bailer-Jones, C.A.L. et al., submitted to ApJ as of 11 July 2018 ([https://ui.adsabs.harvard.edu/#abs/2018arXiv180410121B/abstract NASA ADS])</ref> || 175 || || [[List of Be X-ray Binaries|BeXRB]] || || T || |
|- | |- | ||
− | | [[SMC X-1]] || 19.271456 || -73.443343 || | + | | [[SMC X-1]] || 19.271456 || -73.443343 || 62<ref name="graczyk14" /> || 0.71 || 3.892 || SG || || P || eclipsing |
|- | |- | ||
− | | [[3A 0114+650]] || 19.511228 || 65.291623 || | + | | [[3A 0114+650]] || 19.511228 || 65.291623 || 7.2 <ref name="reig96">Reig, P. et al., 1996, ApJ 311, 879 ([https://ui.adsabs.harvard.edu/#abs/1996A&A...311..879R NASA ADS])</ref> || 9828 || 11.6 || SG || || P || 30.7 d superorbital modulation |
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− | | [[SXP 265]] || 23.214439 || -74.429258 || | + | | [[SXP 265]] || 23.214439 || -74.429258 || 62<ref name="graczyk14" /> || 264.52 || || [[List of Be X-ray Binaries|BeXRB]] || || PT || SMC region, persistent low luminosity, one type I outburst |
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− | | [[LXP 169]] || 76.981153 || -68.418135 || | + | | [[LXP 169]] || 76.981153 || -68.418135 || 50<ref name="pietrzynski13">Distance to LMC. See Pietrzynski, G. et al., 2013, Nature 495, 76 ([https://ui.adsabs.harvard.edu/#abs/2013Natur.495...76P])</ref> || 168.8 || 24.3 || [[List of Be X-ray Binaries|BeXRB]] || || T? || NS eclipsing companion, LMC source |
|- | |- | ||
− | | [[Swift J053041.9-665426]] || 82.675788 || -66.907566 || | + | | [[Swift J053041.9-665426]] || 82.675788 || -66.907566 || 50<ref name="pietrzynski13" /> || 28.78 || || [[List of Be X-ray Binaries|BeXRB]] || || T? || LMC source |
|- | |- | ||
− | | [[LMC X-4]] || 83.206501 || -66.370332 || | + | | [[LMC X-4]] || 83.206501 || -66.370332 || 50<ref name="pietrzynski13" /> || 13.5 || 1.4 || SG || || P || superorbital variation ~30 d |
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− | | [[GRO J1008-57]] || 152.439620 || -58.292035 || 5 || 93.7 || 249.48 || [[List of Be X-ray Binaries|BeXRB]] || [[List of cyclotron line sources|C]]? || T || outbursts predicted precisely | + | | [[GRO J1008-57]] || 152.439620 || -58.292035 || 5.8<ref name="riquelme12">Riquelme, M., Torrejon, J.M., and Negueruela, I., 2012, A&A 539, 114 ([https://ui.adsabs.harvard.edu/#abs/2012A&A...539A.114R/abstract NASA ADS]</ref> || 93.7 || 249.48 || [[List of Be X-ray Binaries|BeXRB]] || [[List of cyclotron line sources|C]]? || T || outbursts predicted precisely |
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− | | [[IGR J16358-4726]] || 249.124997 || -47.623903 || | + | | [[IGR J16358-4726]] || 249.124997 || -47.623903 || 5-6 or 12-13 <ref name="lutovinov05">Lutovinov, A., Revnivtsev, M., Gilfanov, M., et al. 2005, A&A, 444 ([https://ui.adsabs.harvard.edu/#abs/2005A&A...444..821L/abstract NASA ADS])</ref> || 5880 || || [[List of symbiotic X-ray binaries|SyXB]] || || || Distances estimates depend on which part of the Norma arm the source is assumed to reside in. |
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− | | [[GRO J1750-27]] || 267.291434 || -26.639700 || || 4.45 || 29.82 || [[List of Be X-ray Binaries|BeXRB]]? || || P || a.k.a. AX J1749.1-2639 | + | | [[GRO J1750-27]] || 267.291434 || -26.639700 || 18<ref name="scott97">Scott, D.M., et al., 1997, ApJ 488, 831 ([https://ui.adsabs.harvard.edu/#abs/1997ApJ...488..831S/abstract NASA ADS])</ref>|| 4.45 || 29.82 || [[List of Be X-ray Binaries|BeXRB]]? || || P || a.k.a. AX J1749.1-2639 |
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− | | [[1RXS J180431.1-273932]] || 271.130284 || -27.659214 || || 494 || || [[List of symbiotic X-ray binaries|SyXB]] || || || | + | | [[1RXS J180431.1-273932]] || 271.130284 || -27.659214 || 10<ref name="nucita07">Nucita, A.A., Carpano, S., and Guainazzi, M., 2007, A&A 474, L1 ([<https://ui.adsabs.harvard.edu/#abs/2007A%26A...474L...1N/abstract NASA ADS])</ref> || 494 || || [[List of symbiotic X-ray binaries|SyXB]] || || || Likely a magnetic CV, not a SyXB, according to Masetti et al. (2012)<ref name="masetti12">Masetti, N., Nucita, A.A., and Parisi, P., 2012, A&A 544, 114 ([https://ui.adsabs.harvard.edu/#abs/2012A&A...544A.114M/abstract NASA ADS])</ref> |
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− | | [[AX J1820.5-1434]] || 275.122921 || -14.571809 || | + | | [[AX J1820.5-1434]] || 275.122921 || -14.571809 || 3.5-6<ref name="segreto13">Segreto, A. et al., 2013, A&A 558, 99 ([https://ui.adsabs.harvard.edu/#abs/2013A&A...558A..99S/abstract NASA ADS])</ref> || 152 || || HMXB || || ? || Distance assumes a B0 companion. |
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− | | [[Sct X-1]] || 278.857602 || -7.614004 || | + | | [[Sct X-1]] || 278.857602 || -7.614004 || 4-10 <ref name="nebot15">Nebot Gomez-Moran, A., et al., MNRAS 452, 884([https://ui.adsabs.harvard.edu/#abs/2015MNRAS.452..884N/abstract NASA ADS])</ref>|| 112 || 111 || [[List of symbiotic X-ray binaries|SyXB]] || || || Distance estimates depend on assumed spectral class of companion. |
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− | | [[2S 1845-024]] || 282.075590 || -2.419729 || || 94.8 || 242.2 || [[List of Be X-ray Binaries|BeXRB]]? || || T || a.k.a. GS 1843-02 | + | | [[2S 1845-024]] || 282.075590 || -2.419729 || 10<ref name="finger99">Finger, M., et al., 1999, ApJ 517, 449 ([https://ui.adsabs.harvard.edu/#abs/1999ApJ...517..449F/abstract NASA ADS])</ref> || 94.8 || 242.2 || [[List of Be X-ray Binaries|BeXRB]]? || || T || a.k.a. GS 1843-02; distance based on spiral arm location |
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|} | |} | ||
− | + | ||
+ | All distances with uncertainties are from Gaia data release 2, as described by Bailer-Jones et al. (see [https://ui.adsabs.harvard.edu/#abs/2018arXiv180410121B/abstract this paper] and [http://www.mpia.de/homes/calj/gdr2_distances/main.html this webpage]). Note that these should be taken with a grain of salt and are dependent on the priors selected by Bailer-Jones et al. - as an example, the Magellanic cloud sources show up in Gaia DR2 as having distances of ~7 kpc, when they are actually 45 or 60 kpc away. | ||
Revision as of 20:34, 11 July 2018
List of accreting X-ray pulsars
Source | RA | Dec | Distance (kpc) | Pspin (s) | Porbit (d) | Type | CRSF? | Persistent? | Notes |
---|---|---|---|---|---|---|---|---|---|
CXOU J005047.9-731817 | 12.699963 | -73.305018 | 62[1] | 292 | BeXRB? | T | aka SXP 292 | ||
RX J0059.2-7138 | 14.803112 | -71.645828 | 62[1] | 2.76 | 82 | BeXRB? | C? | T | aka SXP 2.76 |
RX J0101.8-7223 | 15.467910 | -72.392796 | 12.3 (+2.0, -1.7)[2] | 175 | BeXRB | T | |||
SMC X-1 | 19.271456 | -73.443343 | 62[1] | 0.71 | 3.892 | SG | P | eclipsing | |
3A 0114+650 | 19.511228 | 65.291623 | 7.2 [3] | 9828 | 11.6 | SG | P | 30.7 d superorbital modulation | |
4U 0115+634 | 19.633194 | 63.742522 | 7.2 (+1.5, -1.1) | 3.6 | 24.3 | BeXRB | C | T | 5 or more lines |
SXP 265 | 23.214439 | -74.429258 | 62[1] | 264.52 | BeXRB | PT | SMC region, persistent low luminosity, one type I outburst | ||
RX J0146.9+6121 | 26.750876 | 61.356573 | 2.50 (+0.22, -0.19) | 1412 | 330 | BeXRB | T | a.k.a. V* V831 Cas | |
IGR J01583+6713 | 29.577033 | 67.223185 | 7.4 (+1.1, -0.9) | 469 | BeXRB | C? | T | controversial claim of CRSF features | |
Swift J0243.6+6124 | 40.918432 | 61.434378 | 6.9 (+1.6, -1.2) | 9.86 | 27.587 | BeXRB | T | Galactic ULX? | |
V 0332+53 | 53.749630 | 53.173140 | 5.1 (+1.1, -0.8) | 4.37 | 34.25 | BeXRB | C | T | multiple lines |
X Per | 58.846151 | 31.045836 | 0.79 +/- 0.04 | 830 | 250.3 | BeXRB | P | magnetar? | |
RX J0440.9+4431 | 70.247207 | 44.530344 | 3.2 (+0.7, -0.5) | 203 | 155 | BeXRB | P | a.k.a. LS V+44 17, persistent, but with outbursts | |
LXP 169 | 76.981153 | -68.418135 | 50[4] | 168.8 | 24.3 | BeXRB | T? | NS eclipsing companion, LMC source | |
Swift J053041.9-665426 | 82.675788 | -66.907566 | 50[4] | 28.78 | BeXRB | T? | LMC source | ||
LMC X-4 | 83.206501 | -66.370332 | 50[4] | 13.5 | 1.4 | SG | P | superorbital variation ~30 d | |
1A 0535+26 | 84.727393 | 26.315776 | 2.13 (+0.26, -0.21) | 103 | 111.1 | BeXRB | C | T | |
SAX J0635.2+0533 | 98.822528 | 5.553870 | 1.6 (+2.2, -0.8) | 0.0338 | BeXRB | T | low luminosity | ||
MXB 0656-07 | 104.572030 | -7.209774 | 5.1 (+1.4, -1.0) | 160.4 | 101.2 | BeXRB | C | a.k.a XTE J0658-073 | |
3A 0726-260 | 112.223241 | -26.108019 | 9.5 (+3.1, -2.2) | 103.2 | 34.5 | BeXRB | T | ||
RX J0812.4-3114 | 123.118149 | -31.247807 | 6.8 (+1.2, -1.0) | 31.9 | 80 | BeXRB | T | ||
GS 0834-430 | 128.981072 | -43.185598 | 5.5 (+2.5, -1.7) | 12.3 | 105.8 | BeXRB | T | ||
Vela X-1 | 135.528560 | -40.554654 | 2.42 (+0.19, -0.17) | 283 | 8.96 | SG | C | P | eclipsing |
GRO J1008-57 | 152.439620 | -58.292035 | 5.8[5] | 93.7 | 249.48 | BeXRB | C? | T | outbursts predicted precisely |
4U 1036-56 | 159.397094 | -56.798840 | 5.0 (+1.1, -0.8) | 862 | BeXRB | P? | a.k.a. RX J1037.5-564/LS 1698 | ||
1A 1118-616 | 170.238174 | -61.916707 | 2.93 (+0.26, -0.22) | 407 | 24 | BeXRB | C | T | |
Cen X-3 | 170.312856 | -60.623776 | 6.4 (+1.4, -1.1) | 4.8 | 2.09 | SG | C | P | disk-fed HMXB |
1E1145.1-6141 | 176.868942 | -61.953720 | 9.1 (+2.2, -1.6) | 297 | 14.4 | SG | (V* V830 Cen) varying luminosity states | ||
4U 1145-619 | 177.000032 | -62.206910 | 2.23 (+0.20, -0.17) | 292 | 187.5 | BeXRB | PT | ||
GX 301-2 | 186.656453 | -62.770359 | 3.5 (+0.6, -0.5) | 686 | 41.5 | SG | C | P | very massive companion, strong orbital variability |
3A 1239-599 | 190.508997 | -60.200951 | 2.9 (+2.4, -1.3) | 191 | |||||
GX 304-1 | 195.321198 | -61.601845 | 2.01 (+0.15, -0.13) | 272 | 132.2 | BeXRB | C | T | Strong spectral parameter variations |
SAX J1324.4-6200 | 201.108853 | -62.016515 | 3.5 (+2.6, -1.7) | 171 | 22 | BeXRB? | |||
2S 1417-624 | 215.303896 | -62.698168 | 3.8 (+2.8, -1.8) | 17.6 | 42.12 | BeXRB | T | ||
SAX J1452.8-5949 | 223.207002 | -59.820983 | 3.0 (+2.6, -1.5) | 437 | BeXRB? | ||||
4U 1538-52 | 235.597300 | -52.386011 | 6.6 (+2.2, -1.5) | 526 | 3.72 | SG | C | P | |
2S 1553-542 | 239.452345 | -54.416113 | 3.5 (+2.6, -1.5) | 9.3 | 29.56 | BeXRB? | P | Occasional outbursts | |
IGR J16194-2810 | 244.888926 | -28.127773 | 2.3 (+0.8, -0.5) | SyXB | |||||
Swift J1626.6-5156 | 246.652146 | -51.941848 | 9.8 (+3.2, -2.4) | 15.4 | 132.9 | BeXRB | C | T | strong flares |
IGR J16318-4848 | 247.951259 | -48.816876 | 5.2 (+2.8, -1.9) | SG | P | super absorbed source | |||
IGR J16320-4751 | 248.009669 | -47.874785 | 1.3 (+0.6, -0.4) | 1309 | 8.986 | SG | P | aka 2FGL J1632.4-4753c | |
4U 1626-67 | 248.069509 | -67.461207 | 3.5 (+2.3, -1.3) | 7.7 | 0.029 | WD? | C | Torque reversals. Only UCXB with a CRSF. | |
IGR J16358-4726 | 249.124997 | -47.623903 | 5-6 or 12-13 [6] | 5880 | SyXB | Distances estimates depend on which part of the Norma arm the source is assumed to reside in. | |||
IGR J16393-4643 | 249.772382 | -46.704006 | 4.0 (+2.7, -1.7) | 912 | 3.7 | SyXB | a.k.a. AX J1639.0-4642 | ||
IGR J16465-4507 | 251.646902 | -45.117960 | 2.7 (+0.5, -0.4) | 228 | 30.243 | P | aka 2MASS J16463526-4507045 | ||
Her X-1 | 254.457539 | 35.342324 | 5.0 (+0.8, -0.6) | 1.24 | 1.7 | IMXB | C | P | |
AX J1700.1-4157 | 255.018132 | -41.968217 | 3.4 (+2.6, -1.5) | 715 | BeXRB? | ||||
OAO 1657-415 | 255.202665 | -41.654882 | 2.2 (+0.7, -0.5) | 37.7 | 10.4 | SG | C? | P | eclipsing |
4U 1700-37 | 255.986566 | -37.844121 | 1.75 (+0.24, -0.19) | 3.4 | SG | P | No pulsations, eclipsing source | ||
4U 1700+24 | 256.643762 | 23.971820 | 0.536 +/- 0.010 | 404 | SyXB | ||||
EXO 1722-363 | 261.296681 | -36.284621 | 4.0 (+2.3, -1.3) | 9.74 | HMXB | a.k.a. IGR J17252–3616, heavily absorbed, eclipsing | |||
GX 1+4 | 263.008955 | -24.745600 | 7.6 (+4.3, -2.8) | 170 | 1161 | SyXB | P | Pulse period evolving rapidly | |
2XMM J174016.0-290337 | 265.067079 | -29.060569 | 1.4 (+1.6, -0.5) | 626 | SyXB | a. k.a. AX_J1740.2-2903 | |||
GRO J1744-28 | 266.139419 | -28.744480 | 1.3 (+1.2, -0.5) | 0.47 | 11.8 | LMXB | T | "Bursting Pulsar" | |
GRO J1750-27 | 267.291434 | -26.639700 | 18[7] | 4.45 | 29.82 | BeXRB? | P | a.k.a. AX J1749.1-2639 | |
IGR J17544-2619 | 268.605299 | -26.331274 | 2.7 (+0.5, -0.4) | 4.93 | SFXT? | C | T | ||
SAX J1802.7-2017 | 270.665728 | -20.286816 | 1.5 (+2.8, -0.7) | 139.6 | 4.57 | SG | P | a.k.a. IGR J18027-2016 | |
1RXS J180431.1-273932 | 271.130284 | -27.659214 | 10[8] | 494 | SyXB | Likely a magnetic CV, not a SyXB, according to Masetti et al. (2012)[9] | |||
SAX J1808.4-3658 | 272.114166 | -36.979379 | 5.1 (+4.3, -2.6) | 0.0025 | 0.837 | LMXB | a.k.a. V* V4580 Sgr, disk accretor(?) | ||
Swift J1816.7-1613 | 274.176846 | -16.222949 | 1.4 (+2.5, -0.7) | 142.9 | 151 | BeXRB? | T | ATel 6253 ATel 1457 | |
IGR J18179-1621 | 274.467048 | -16.359400 | 11.82 | C? | T | ATel 3947 ATel 3949 | |||
AX J1820.5-1434 | 275.122921 | -14.571809 | 3.5-6[10] | 152 | HMXB | ? | Distance assumes a B0 companion. | ||
3A 1822-371 | 276.445028 | -37.105158 | 6.1 (+2.7, -1.6) | 0.59 | 0.23 | LMXB | |||
Sct X-1 | 278.857602 | -7.614004 | 4-10 [11] | 112 | 111 | SyXB | Distance estimates depend on assumed spectral class of companion. | ||
GS 1843+00 | 281.403474 | 0.863160 | 2.3 (+2.0, -1.0) | T | |||||
2S 1845-024 | 282.075590 | -2.419729 | 10[12] | 94.8 | 242.2 | BeXRB? | T | a.k.a. GS 1843-02; distance based on spiral arm location | |
XTE J1855-026 | 283.876680 | -2.604678 | 8.1 (+2.6, -1.8) | 361 | 6.1 | SG | |||
XTE J1858+034 | 284.678379 | 3.439739 | 1.55 (+0.28, -0.21) | 221 | T | ||||
XTE J1859+083 | 284.778177 | 8.246352 | 2.7 (+2.4, -1.5) | 9.8 | T | ATel 7037 | |||
4U 1901+03 | 285.903524 | 3.190426 | 2.2 (+2.2, -1.3) | T | |||||
XTE J1906+090 | 286.197769 | 9.044912 | 2.8 (+2.4, -1.4) | 89.2 | BeXRB? | ||||
4U 1907+09 | 287.408533 | 9.829777 | 4.4 (+2.1, -1.3) | 442 | 8.37 | SG | C | P | |
4U 1909+07 | 287.700872 | 7.597657 | 2.6 (+2.3, -1.4) | 604 | 4.4 | SG | P | ||
IGR J19140+0951 | 288.517606 | 9.882865 | 2.8 (+2.4, -1.4) | 13.55 | HMXB | ? | |||
IGR J19149+1036 | 288.728311 | 10.612245 | 3.0 (+2.5, -1.6) | 22.25 | SG | C | P | very close to GRS1915 | |
IGR J19294+1816 | 292.482927 | 18.310607 | 2.9 (+2.5, -1.5) | 12.5 | 116 | BeXRB? | T | ||
XTE J1946+274 | 296.413975 | 27.365400 | 12.6 (+3.9, -2.9) | 15.8 | 169.2 | BeXRB | C | T | |
KS 1947+300 | 297.397839 | 30.208809 | 15.2 (+3.7, -2.8) | 18.8 | 40.4 | BeXRB | C | T | |
3A 1954+319 | 298.926399 | 32.096931 | 3.3 (+1.0, -0.7) | 19100 | SyXB | ||||
EXO 2030+375 | 308.063627 | 37.637433 | 3.6 (+1.4, -0.9) | 41.8 | 46.03 | BeXRB | T | regular outbursts | |
GRO J2058+42 | 314.698059 | 41.776980 | 8.0 (+1.2, -1.0) | T | |||||
SAX J2103.5+4545 | 315.898770 | 45.751533 | 6.4 (+0.9, -0.7) | 359 | 12.7 | BeXRB | T | ||
IGR J21343+4738 | 323.584869 | 47.633380 | 7.8 (+1.4, -1.1) | 320.35 | 20.85 | BeXRB | P? | Varying levels of activity | |
Cep X-4 | 324.877853 | 56.986219 | 10.2 (+2.2, -1.6) | 66.32 | 20.85 | BeXRB | C | T | |
4U 2206+54 | 331.984289 | 54.518433 | 3.3 +/- 0.4 | 5560 | 19.25 | SG | P | magnetar? | |
SAX J2239.3+6116 | 339.836831 | 61.274053 | 8.0 (+1.4, -1.1) | 1247 | 262 | BeXRB | T | ||
IGR J22534+6243 | 343.479672 | 62.726882 | 8.1 (+2.3, -1.6) | 46.7 | Be? | P? |
All distances with uncertainties are from Gaia data release 2, as described by Bailer-Jones et al. (see this paper and this webpage). Note that these should be taken with a grain of salt and are dependent on the priors selected by Bailer-Jones et al. - as an example, the Magellanic cloud sources show up in Gaia DR2 as having distances of ~7 kpc, when they are actually 45 or 60 kpc away.
Location in the Galaxy
The figure below displays the position of accreting X-ray pulsars in the Galaxy as far as known at this moment. Click on the figure for a larger version. Labels indicate the ordinal number in the first column of the table. Uncertainties in the distances are not indicated. Empty symbols represent sources for which there is no distance info in the literature; they have been artificially set to a distance of 7.6 kpc. HEASARC source class identifiers are also given. The spiral arms are from Vallée et al. (2008)[13]. Figure and data provided by Arash Bodaghee, SSL, UC Berkeley.
# | Source | Class | Dist. [kpc] | # | Source | Class | Dist. [kpc] | |
---|---|---|---|---|---|---|---|---|
1 | GRO_J1744-28 | 1490 | 8.5 | 33 | 3A_0656-072 | 1316 | 3.9 | |
2 | GX_1+4 | 1410 | 4.5 | 34 | 3A_0726-260 | 1310 | 6.1 | |
3 | GRO_J1750-27 | 1316 | ? | 35 | RX_J0812.4-3114 | 1316 | 8.8 | |
4 | 1RXS_J180431.1-273932 | 1410 | ? | 36 | Ginga_0834-430 | 1316 | 4 | |
5 | AX_J1820.5-1434 | 1316 | 8.2 | 37 | Vela_X-1 | 1213 | 1.4 | |
6 | XTE_J1855-026 | 1213 | 10 | 38 | LMC_X-4 | 1210 | 55 | |
7 | Sct_X-1 | 1116 | 7 | 39 | GRO_J1008-57 | 1316 | 5 | |
8 | Ginga_1843+009 | 1316 | 12.5 | 40 | 4U_1036-56 | 1316 | 5 | |
9 | 4U_1901+03 | 1366 | ? | 41 | Cen_X-3 | 1263 | 10 | |
10 | 4U_1909+07 | 1210 | 7 | 42 | 1A_1118-615 | 1366 | 5 | |
11 | XTE_J1906+090 | 1316 | 10 | 43 | 1E_1145.1-6141 | 1210 | 8.5 | |
12 | H_1907+097 | 1216 | 5 | 44 | H_1145-619 | 1316 | 3.1 | |
13 | 4U_1700+24 | 1400 | 0.42 | 45 | GX_301-2 | 1211 | 4.1 | |
14 | IGR_J19294+1816 | 1316 | ? | 46 | SMC_X-1 | 1213 | 60 | |
15 | Her_X-1 | 1413 | 6.56 | 47 | 3A_1239-599 | 1110 | ? | |
16 | XTE_J1946+274 | 1316 | 9.5 | 48 | RX_J0101.8-7223 | 1310 | 60 | |
17 | KS_1947+300 | 1316 | 9.5 | 49 | GX_304-1 | 1316 | 2.4 | |
18 | 3A_1954+319 | 1416 | 1.7 | 50 | SAX_J1324.4-6200 | 1310 | 10 | |
19 | EXO_2030+375 | 1366 | 7.1 | 51 | H_1417-624 | 1316 | 6 | |
20 | GRO_J2058+42 | 1316 | 9.0 | 52 | SAX_J1452.8-5949 | 1010 | 9 | |
21 | SAX_J2103.5+4545 | 1366 | 6.8 | 53 | 4U_1626-67 | 1410 | 9.0 | |
22 | Cep_X-4 | 1316 | 3.8 | 54 | H_1538-522 | 1213 | 6.4 | |
23 | 3A_2206+543 | 1260 | 2.6 | 55 | SWIFT_J1626.6-5156 | 1366 | ? | |
24 | 3A_0114+650 | 1213 | 4.5 | 56 | AX J1700.1-4157 | 9999 | ? | |
25 | H_0115+634 | 1386 | 8 | 57 | OAO_1657-415 | 1213 | 7.1 | |
26 | IGR_J01583+6713 | 1316 | 4 | 58 | IGR_J16358-4726 | 1110 | 7 | |
27 | RX_J0146.9+6121 | 1310 | 2.3 | 59 | IGR_J16393-4643 | 1210 | 10.6 | |
28 | V_0332+53 | 1366 | 7.5 | 60 | IGR_J16194-2810 | 1400 | 3.7 | |
29 | RX_J0440.9+4431 | 1310 | 3.3 | 61 | SAX_J1808.4-3658 | 1416 | 3.6 | |
30 | X_Per | 1310 | 0.7 | 62 | 3A_1822-371 | 1419 | 2.5 | |
31 | 1A_0535+262 | 1366 | 2 | 63 | AX_J1740.2-2903 | 1410 | ? | |
32 | SAX_J0635.2+0533 | 1310 | 5 |
Correlation between luminosity and CRSF energy
In recent years more and more sources have been observed at different luminosities, allowing us to find correlation between the luminosity and the cyclotron line energy. A summary of the current state of the observations can be found on this page: CRSF energy as function of luminosity
Assignments
Our collaboration has assigned one or two sources to each member to take care of, i.e., to put together the most important information and keep the page up to date in case new data are available or new papers are published. The list can only be accessed if logged in.
- ↑ 1.0 1.1 1.2 1.3 Distance to SMC. See Graczyk, D. et al., ApJ 780, 59 (NASA ADS)
- ↑ Bailer-Jones, C.A.L. et al., submitted to ApJ as of 11 July 2018 (NASA ADS)
- ↑ Reig, P. et al., 1996, ApJ 311, 879 (NASA ADS)
- ↑ 4.0 4.1 4.2 Distance to LMC. See Pietrzynski, G. et al., 2013, Nature 495, 76 ([1])
- ↑ Riquelme, M., Torrejon, J.M., and Negueruela, I., 2012, A&A 539, 114 (NASA ADS
- ↑ Lutovinov, A., Revnivtsev, M., Gilfanov, M., et al. 2005, A&A, 444 (NASA ADS)
- ↑ Scott, D.M., et al., 1997, ApJ 488, 831 (NASA ADS)
- ↑ Nucita, A.A., Carpano, S., and Guainazzi, M., 2007, A&A 474, L1 ([<https://ui.adsabs.harvard.edu/#abs/2007A%26A...474L...1N/abstract NASA ADS])
- ↑ Masetti, N., Nucita, A.A., and Parisi, P., 2012, A&A 544, 114 (NASA ADS)
- ↑ Segreto, A. et al., 2013, A&A 558, 99 (NASA ADS)
- ↑ Nebot Gomez-Moran, A., et al., MNRAS 452, 884(NASA ADS)
- ↑ Finger, M., et al., 1999, ApJ 517, 449 (NASA ADS)
- ↑ Vallée, Jacques P., 2008, ApJ 681, 303 (NASA ADS)