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Daftar lubang hitam paling masif
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Berikut ini adalah sebuah daftar dari lubang hitam paling masif yang sejauh ini ditemukan (dan kandidat-kandidatnya), yang diukur dalam satuan massa matahari (M☉), sekitar 2×1030 kg.
Daftar
 | Daftar ini belum tentu lengkap. Anda dapat membantu Wikipedia dengan mengembangkannya. (Juni 2017) |
| Nama | Massa matahari (Matahari = 1) |
Catatan |
|---|---|---|
| TON 618 | 6,6×1010[1] | Perkiraan dari korelasi garis emisi kuasar Hβ. |
| Holmberg 15A | (4,0±0,8)×1010[2] | Mass specified obtained through orbit-based, axisymmetric Schwarzschild models. Earlier estimates range from ~310 billion M☉ down to 3 billion M☉, all relying on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements.[3] |
| IC 1101 | (4–10)×1010[4] | Perkiraan dari properti galaksi induk; massa belum diukur secara langsung. |
| S5 0014+81 | 4×1010[5][6][7] | Sebuah makalah 2010 mengusulkan bahwa sebuah corong mengkolimasi radiasi di sekitar sumbu jet, menciptakan ilusi optik dengan kecerahan sangat tinggi, dan dengan demikian kemungkinan terjadi sebuah overestimasi pada massa lubang hitam tersebut.[5] |
| SMSS J215728.21-360215.1 | (3,4±0,6)×1010[8] | |
| SDSS J102325.31+514251.0 | (3,31±0,61)×1010[9] | Perkiraan dari korelasi garis emisi quasar MgII. |
| H1821+643 | 3×1010[10] | Gugus galaksi terdekat yang mempunyai sebuah kuasar dalam intinya.[10] |
| NGC 6166 | 3×1010[11] | |
| APM 08279+5255 | 2,3×1010[12] 1,0+0,17 −0,13×1010[13] | Based on velocity width of CO line from orbiting molecular gas,[12] and reverberation mapping using SiIV and CIV emission lines.[13] |
| NGC 4889 | (2,1±1,6)×1010[14][15] | Best fit: the estimate ranges from 6 billion to 37 billion M☉.[14][15] |
| Central black hole of Phoenix Cluster | 2×1010[16] | This black hole is continuously growing at the rate of ~60 M☉ per year. |
| SDSS J074521.78+734336.1 | (1,95±0,05)×1010[9] | Estimated from quasar MgII emission line correlation. |
| OJ 287 primary | 1,8×1010[17] | A smaller 100 million M☉ black hole orbits this one in a 12-year period (see OJ 287 secondary below). But this measurement is in question due to the limited number and precision of observed companion orbits. |
| NGC 1600 | (1,7±0,15)×1010[18][19] | Unprecedentedly massive in relation of its location: an elliptical galaxy host in a sparse environment. |
| SDSS J08019.69+373047.3 | (1,51±0,31)×1010[9] | Estimated from quasar MgII emission line correlation. |
| SDSS J115954.33+201921.1 | (1,41±0,10)×1010[9] | Estimated from quasar MgII emission line correlation. |
| SDSS J075303.34+423130.8 | (1,38±0,03)×1010[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J080430.56+542041.1 | (1,35±0,22)×1010[9] | Estimated from quasar MgII emission line correlation. |
| Abell 1201 BCG | (1,3±0,6)×1010[20] | Estimated from the strong gravitational lensing of a background galaxy behind the BCG.[20] Beware of ambiguity between the BH mass determination and the galaxy cluster's dark matter profile.[21] |
| SDSS J0100+2802 | (1,24±0,19)×1010[22][23] | Estimated from quasar MgII emission line correlation. This object grew early in cosmic history (redshift 6.30). |
| SDSS J081855.77+095848.0 | (1,20±0,06)×1010[9] | Estimated from quasar MgII emission line correlation. |
| NGC 1270 | 1,2×1010[24] | Elliptical galaxy located in the Perseus Cluster. Also is a low-luminosity AGN (LLAGN).[25] |
| SDSS J082535.19+512706.3 | (1,12±0,20)×1010[9] | Estimated from quasar Hβ emission line |
| SDSS J013127.34-032100.1 | (1,1±0,2)×1010[26] | Estimated from accretion disk spectrum modelling.[26] |
| PSO J334.2028+01.4075 | 1×1010[27] | There are actually two black holes, orbiting at each other in a close pair with a 542-day period. The largest one is quoted, while the smaller one's mass is not defined.[27] |
| Black hole of central elliptical galaxy of RX J1532.9+3021 | 1×1010[28] | |
| QSO B2126-158 | 1×1010[5] | |
| NGC 1281 | 1×1010[29] | Compact elliptical galaxy in the Perseus Cluster. Mass estimates range from 10 billion M☉ down to <5 billion M☉.[30] |
| SDSS J015741.57-010629.6 | (9,8±1,4)×109[9] | |
| NGC 3842 | 9,7+3,0 −2,5×109[14][15] |
Brightest galaxy in the Leo Cluster |
| SDSS J230301.45-093930.7 | (9,12±0,88)×109[9] | Estimated from quasar MgII emission line correlation. |
| SDSS J075819.70+202300.9 | (7,8±3,9)×109[9] | Estimated from quasar Hβ emission line correlation. |
| CID-947 | 6,9+0,8 −1,2×109[31] |
Constitutes 10% of the total mass of its host galaxy. Estimated from quasar Hβ emission line correlation. |
| SDSS J080956.02+502000.9 | (6,46±0,45)×109[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J014214.75+002324.2 | (6,31±1,16)×109[9] | Estimated from quasar MgII emission line correlation. |
| Messier 87 "Powehi"[32] | 7,22+0,34 −0,40×109[33] 6,3×109[34] | Central galaxy of the Virgo Cluster; the first black hole directly imaged. |
| NGC 5419 | 7,2+2,7 −1,9×109[35] | Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs.[35] |
| SDSS J025905.63+001121.9 | (5,25±0,73)×109[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J094202.04+042244.5 | (5,13±0,71)×109[9] | Estimated from quasar Hβ emission line correlation. |
| QSO B0746+254 | 5×109[5] | |
| QSO B2149-306 | 5×109[5] | |
| SDSS J090033.50+421547.0 | (4,7±0,2)×109[9] | Estimated from quasar MgII emission line correlation. |
| Messier 60 | (4,5±1,0)×109[36] | |
| SDSS J011521.20+152453.3 | (4,1±2,4)×109[9] | Estimated from quasar Hβ emission line correlation. |
| QSO B0222+185 | 4×109[5] | |
| Hercules A (3C 348) | 4×109 | Notable for its million light-year long relativistic jet. |
| Abell 1836-BCG | 3,61+0,41 −0,50×109[37] | |
| SDSS J213023.61+122252.0 | (3,5±0,2)×109[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J173352.23+540030.4 | (3,4±0,4)×109[9] | Estimated from quasar MgII emission line correlation. |
| SDSS J025021.76-075749.9 | (3,1±0,6)×109[9] | Estimated from quasar MgII emission line correlation. |
| NGC 1271 | 3,0+1,0 −1,1×109[38] | Compact elliptical or lenticular galaxy in the Perseus Cluster.[39] |
| SDSS J030341.04-002321.9 | (3,0±0,4)×109[9] | Estimated from quasar MgII emission line correlation. |
| QSO B0836+710 | 3×109[5] | |
| SDSS J224956.08+000218.0 | (2,63±1,21)×109[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J030449.85-000813.4 | (2,4±0,50)×109[9] | Estimated from quasar Hβ emission line correlation. |
| SDSS J234625.66-001600.4 | (2,24±0,15)×109[9] | Estimated from quasar Hβ emission line correlation. |
| PKS 2128-123 | 2,02×109[40] | |
| ULAS J1120+0641 | 2×109[41][42] | |
| QSO 0537-286 | 2×109[5] | |
| NGC 3115 | 2×109[43] | |
| Q0906+6930 | 2×109[44] | Most distant blazar, at z = 5.47 |
| QSO B0805+614 | 1,5×109[5] | |
| Messier 84 | 1,5×109[45] | |
| J100758.264+211529.207 ("Pōniuāʻena") | (1,5±0,2)×109[46] | Second most-distant quasar known |
| PKS 2059+034 | 1,36×109[40] | |
| Abell 3565-BCG | 1,34+0,21 −0,19×109[37] |
|
| NGC 7768 | 1,3+0,5 −0,4×109[15] |
|
| NGC 1277 | 1,2×109[47] | Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories,[48] re-analysis of the data revised it downward to roughly a third of the original estimate.[49] and then one tenth.[47] |
| Black hole of central elliptical galaxy of MS 0735.6+7421 | 1×109[50][51][52] | Produced a colossal AGN outburst after accreting 600 million M☉ worth of material. BH mass not explicitly stated; just a lower limit. Requires assumptions about the efficiencies of gas accretion and jet power.[50][51][52] |
| QSO B225155+2217 | 1×109[5] | |
| QSO B1210+330 | 1×109[5] | |
| NGC 6166 | 1×109[53] | Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet. |
| Cygnus A | 1×109[54] | Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz |
| Sombrero Galaxy | 1×109[55] | Bolometrically most luminous galaxy in the local universe and also the nearest billion-solar-mass black hole to Earth. |
| Markarian 501 | 9×108–3,4×109[56] | Brightest object in the sky in very high energy gamma rays. |
| PG 1426+015 | (1,298±0,385)×109[57] 467.740.000[58] | |
| 3C 273 | (8,86±1,87)×108[57] 550.000.000[58] | Kuasar terterang di langit |
| ULAS J1342+0928 | 8×108[59] | Kuasar paling jauh[59] − saat ini tercatat sebagai kuasar terjauh dengan z=7.54[59] |
| Messier 49 | 5,6×108[60] | |
| NGC 1399 | 5×108[61] | Central galaxy of the Fornax Cluster |
| PG 0804+761 | (6,93±0,83)×108[57] 190.550.000[58] | |
| PG 1617+175 | (5,94±1,38)×108[57] 275.420.000[58] | |
| PG 1700+518 | 7,81+1,82 −1,65×108[57] 60.260.000[58] | |
| NGC 4261 | 4×108[62] | Notable for its 88.000 light-year long relativistic jet.[63] |
| PG 1307+085 | (4,4±1,23)×108[57] 281 840 000[58] | |
| SAGE0536AGN | (3,5±0,8)×108[64][65] | Constitutes 1.4% of the mass of its host galaxy |
| NGC 1275 | 3,4×108[66][67] | Central galaxy of the Perseus Cluster |
| 3C 390.3 | (2,87±0,64)×108[57] 338.840.000[58] | |
| II Zwicky 136 | (4,57±0,55)×108[57] 144.540.000[58] | |
| PG 0052+251 | (3,69±0,76)×108[57] 218.780.000[58] | |
| Messier 59 | 2,7×108[68] | Lubang hitam tersebut memiliki sebuah rotasi retrograd.[69] |
| PG 1411+442 | (4,43±1,46)×108[57] 79.430.000[58] | |
| Markarian 876 | (2,79±1,29)×108[57] 240.000.000[58] | |
| Galaksi Andromeda | 2,3×108 | Galaksi besar terdekat ke Bima Sakti |
| PG 0953+414 | (2,76±0,59)×108[57] 182.000.000[58] | |
| PG 0026+129 | (3,93±0,96)×108[57] 53.700.000[58] | |
| Fairall 9 | (2,55±0,56)×108[57] 79.430.000[58] | |
| Markarian 1095 | (1,5±0,19)×108[57] 182.000.000[58] | |
| Messier 105 | 1,4×108–2×108[70] | |
| Markarian 509 | (1,43±0,12)×108[57] 57.550.000[58] | |
| Sekunder dari OJ 287 | 1×108[17] | The smaller black hole orbiting OJ 287 primary (see above). |
| RX J124236.9-111935 | 1×108[71] | Observed by the Chandra X-ray Observatory to be tidally disrupting a star.[71][72] |
| Messier 85 | 1×108[73] | |
| NGC 5548 | (6,71±0,26)×107[57] 123.000.000[58] | |
| PG 1211+143 | (1,46±0,44)×108[57] 40.740.000[58] | |
| Messier 88 | 8×107[74] | |
| Messier 81 (Galaksi Bode) | 7×107[75] | |
| Markarian 771 | (7,32±3,52)×107[57] 7,586×107[58] | |
| Messier 58 | 7×107[76] | |
| PG 0844+349 | (9,24±3,81)×107[57] 2,138×107[58] | |
| Centaurus A | 5,5×107[77] | Also notable for its million light-year long relativistic jet.[78] |
| Markarian 79 | (5,24±1,44)×107[57] 5,25×107[58] | |
| Messier 96 | 48.000.000[79] | Estimates can be as low as 1.5 million solar masses |
| Markarian 817 | (4,94±0,77)×107[57] 4,365×107[58] | |
| NGC 3227 | (4,22±2,14)×107[57] 3,89×107[58] | |
| NGC 4151 primary | 4×107[80][81] | |
| 3C 120 | 5,55+3,14 −2,25×107[57] 2,29×107[58] | |
| Markarian 279 | (3,49±0,92)×107[57] 4,17×107[58] | |
| NGC 3516 | (4,27±1,46)×107[57] 2,3×107[58] | |
| NGC 863 | (4,75±0,74)×107[57] 1,77×107[58] | |
| Messier 82 (Cigar Galaxy) | 3×107[82] | Prototype starburst galaxy.[83] |
| Messier 108 | 2,4×107[84] | |
| M60-UCD1 | 2×107[85] | Constitutes 15% of the mass of its host galaxy. |
| NGC 3783 | (2,98±0,54)×107[57] 9.300.000[58] | |
| Markarian 110 | (2,51±0,61)×107[57] 5.620.000[58] | |
| Markarian 335 | (1,42±0,37)×107[57] 6.310.000[58] | |
| NGC 4151 secondary | 10.000.000[81] | |
| NGC 7469 | (12,2±1,4)×106[57] 6.460.000[58] | |
| IC 4329 A | 9,90+17,88 −11,88×106[57] 5.010.000[58] | |
| NGC 4593 | 5,36+9,37 −6,95×106[57] 8.130.000[58] | |
| Messier 61 | 5×106[86] | |
| Messier 32 | 1,5×106–5×106[87] | Sebuah galaksi satelit katai di Galaksi Andromeda. |
| Sagittarius A* | 4,3×106[88] | Lubang hitam di pusat Bima Sakti. |
Lihat pula
Referensi
- ↑ Shemmer, O.; Netzer, H.; Maiolino, R.; Oliva, E.; Croom, S.; Corbett, E.; di Fabrizio, L. (2004). "Near-infrared spectroscopy of high-redshift active galactic nuclei. I. A metallicity-accretion rate relationship". The Astrophysical Journal. 614 (2): 547–557. arXiv:astro-ph/0406559. Bibcode:2004ApJ...614..547S. doi:10.1086/423607. S2CID 119010341.
- ↑ Mehrgan, K.; Thomas, J.; Saglia, R.; Massalay, X.; Erwin, P.; Bender, R.; Kluge, M.; Fabricius, M. (2019). "A 40-billion solar mass black hole in the extreme core of Holm 15A, the central galaxy of Abell 85". The Astrophysical Journal. 887 (2): 195. arXiv:1907.10608. doi:10.3847/1538-4357/ab5856. S2CID 198899965. Pemeliharaan CS1: DOI bebas tanpa ditandai (link)
- ↑ López-Cruz, O.; Añorve, C.; Birkinshaw, M.; Worrall, D. M.; Ibarra-Medel, H. J.; Barkhouse, W. A.; Torres-Papaqui, J. P.; Motta, V. (2014). "The Brightest Cluster Galaxy in Abell 85: The Largest Core Known So Far". The Astrophysical Journal. 795 (2): L31. arXiv:1405.7758. Bibcode:2014ApJ...795L..31L. doi:10.1088/2041-8205/795/2/L31.
- ↑ Dullo, Bililign T.; Graham, Alister W.; Knapen, Johan H. (October 2017). "A remarkably large depleted core in the Abell 2029 BCG IC 1101". Monthly Notices of the Royal Astronomical Society. 471 (2): 2321–2333. arXiv:1707.02277. Bibcode:2017MNRAS.471.2321D. doi:10.1093/mnras/stx1635. S2CID 119000593. Pemeliharaan CS1: DOI bebas tanpa ditandai (link)
- 1 2 3 4 5 6 7 8 9 10 11 Ghisellini, G.; Ceca, R. Della; Volonteri, M.; Ghirlanda, G.; Tavecchio, F.; Foschini, L.; Tagliaferri, G.; Haardt, F.; Pareschi, G.; Grindlay, J. (2010). "Chasing the heaviest black holes in active galactic nuclei, the largest black hole". Monthly Notices of the Royal Astronomical Society. 405 (1): 387. arXiv:0912.0001. Bibcode:2010MNRAS.405..387G. doi:10.1111/j.1365-2966.2010.16449.x. S2CID 40214759.
- ↑ Ghisellini, G.; Foschini, L.; Volonteri, M.; Ghirlanda, G.; Haardt, F.; Burlon, D.; Tavecchio, F.; et al. (14 July 2009). "The blazar S5 0014+813: a real or apparent monster?". Monthly Notices of the Royal Astronomical Society: Letters. v2. 399 (1): L24 – L28. arXiv:0906.0575. Bibcode:2009MNRAS.399L..24G. doi:10.1111/j.1745-3933.2009.00716.x. S2CID 14438667.
- ↑ Gaensler, Bryan (2012-07-03). Extreme Cosmos: A Guided Tour of the Fastest, Brightest, Hottest, Heaviest, Oldest, and Most Amazing Aspects of Our Universe. ISBN 978-1-101-58701-0.
- ↑ "thirty-four billion solar mass black hole in SMSS J2157–3602, the most luminous known quasar", Monthly Notices of the Royal Astronomical Society, August 2020, doi:10.1093/mnras/staa1635
- 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 Zuo, Wenwen; Wu, Xue-Bing; Fan, Xiaohui; Green, Richard; Wang, Ran; Bian, Fuyan (2014). "Black Hole Mass Estimates and Rapid Growth of Supermassive Black Holes in Luminous $z \sim$ 3.5 Quasars". The Astrophysical Journal. 799 (2): 189. arXiv:1412.2438. Bibcode:2015ApJ...799..189Z. doi:10.1088/0004-637X/799/2/189. S2CID 73642040.
- 1 2 Walker, S. A.; Fabian, A. C.; Russell, H. R.; Sanders, J. S. (2014). "The effect of the quasar H1821+643 on the surrounding intracluster medium: Revealing the underlying cooling flow". Monthly Notices of the Royal Astronomical Society. 442 (3): 2809. arXiv:1405.7522v1. Bibcode:2014MNRAS.442.2809W. doi:10.1093/mnras/stu1067. S2CID 118724526. Pemeliharaan CS1: DOI bebas tanpa ditandai (link)
- ↑ Magorrian, J.; Tremaine, S.; Richstone, D.; Bender, R.; Bower, G.; Dressler, A.; Faber, S.~M.; Gebhardt, K.; Green, R.; Grillmair, C.; Kormendy, J.; Lauer, T. (June 1998). "The Demography of Massive Dark Objects in Galaxy Centers". The Astronomical Journal. 115 (6): 2285–2305. arXiv:astro-ph/9708072. Bibcode:1998AJ....115.2285M. doi:10.1086/300353. S2CID 17256372.
- 1 2 Riechers, D. A.; Walter, F.; Carilli, C. L.; Lewis, G. F. (2009). "Imaging The Molecular Gas in a z = 3.9 Quasar Host Galaxy at 0farcs3 Resolution: A Central Sub-Kiloparsec Scale Star Formation Reservoir in APM 08279+5255". The Astrophysical Journal. 690 (1): 463–485. arXiv:0809.0754. Bibcode:2009ApJ...690..463R. doi:10.1088/0004-637X/690/1/463. S2CID 13959993.
- 1 2 Saturni, F. G.; Trevese, D.; Vagnetti, F.; Perna, M.; Dadina, M. (2016). "A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255. II. Emission- and absorption-line variability time lags". Astronomy and Astrophysics. 587: A43. arXiv:1512.03195. Bibcode:2016A&A...587A..43S. doi:10.1051/0004-6361/201527152. S2CID 118548618.
- 1 2 3 McConnell, Nicholas J.; Ma, Chung-Pei; Gebhardt, Karl; Wright, Shelley A.; Murphy, Jeremy D.; Lauer, Tod R.; Graham, James R.; Richstone, Douglas O. (2011). "Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies". Nature. 480 (7376): 215–8. arXiv:1112.1078. Bibcode:2011Natur.480..215M. doi:10.1038/nature10636. PMID 22158244. S2CID 4408896.
- 1 2 3 4 McConnell, N. J.; Ma, C.-P.; Murphy, J. D.; Gebhardt, K.; Lauer, T. R.; Graham, J. R.; Wright, S. A.; Richstone, D. O. (2012). "Dynamical Measurements of Black Hole Masses in Four Brightest Cluster Galaxies at 100 Mpc". The Astrophysical Journal. 756 (2): 179. arXiv:1203.1620. Bibcode:2012ApJ...756..179M. doi:10.1088/0004-637X/756/2/179. S2CID 119114155.
- ↑ McDonald, M.; Bayliss, M.; Benson, B. A.; Foley, R. J.; Ruel, J.; Sullivan, P.; Veilleux, S.; Aird, K. A.; Ashby, M. L. N.; Bautz, M.; Bazin, G.; Bleem, L. E.; Brodwin, M.; Carlstrom, J. E.; Chang, C. L.; Cho, H. M.; Clocchiatti, A.; Crawford, T. M.; Crites, A. T.; De Haan, T.; Desai, S.; Dobbs, M. A.; Dudley, J. P.; Egami, E.; Forman, W. R.; Garmire, G. P.; George, E. M.; Gladders, M. D.; Gonzalez, A. H.; et al. (2012). "A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies". Nature. 488 (7411): 349–52. arXiv:1208.2962. Bibcode:2012Natur.488..349M. doi:10.1038/nature11379. PMID 22895340. S2CID 205230129.
- 1 2 Valtonen, M. J.; Ciprini, S.; Lehto, H. J. (2012). "On the masses of OJ287 black holes". Monthly Notices of the Royal Astronomical Society. 427 (1): 77–83. arXiv:1208.0906. Bibcode:2012MNRAS.427...77V. doi:10.1111/j.1365-2966.2012.21861.x. S2CID 118483466.
- ↑ Thomas, J.; Ma, C.-P.; McConnell, N. J.; Greene, J. E.; Blakeslee, J. P.; Janish, R. (2016). "A 17-billion-solar-mass black hole in a group galaxy with a diffuse core". Nature. 532 (7599): 340–342. arXiv:1604.01400. Bibcode:2016Natur.532..340T. doi:10.1038/nature17197. PMID 27049949. S2CID 4454301.
- ↑ Morrow, Ashley (5 April 2016). "Behemoth Black Hole Found in an Unlikely Place".
- 1 2 Smith, R. J.; Lucey, J. R.; Edge, A. C. (2017). "A counterimage to the gravitational arc in Abell 1201: Evidence for IMF variations or a 1010 Msun black hole?". Monthly Notices of the Royal Astronomical Society. 467 (1): 836–848. arXiv:1701.02745. Bibcode:2017MNRAS.467..836S. doi:10.1093/mnras/stx059. S2CID 59965783. Pemeliharaan CS1: DOI bebas tanpa ditandai (link)
- ↑ Smith, R. J.; Lucey, J. R.; Edge, A. C. (2017). "Stellar dynamics in the strong-lensing central galaxy of Abell 1201: A low stellar mass-to-light ratio a large central compact mass and a standard dark matter halo". Monthly Notices of the Royal Astronomical Society. 1706 (1): 383–393. arXiv:1706.07055. Bibcode:2017MNRAS.471..383S. doi:10.1093/mnras/stx1573. S2CID 54757451. Pemeliharaan CS1: DOI bebas tanpa ditandai (link)
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