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	A follow-up study,<ref name=Emsellem>{{cite journal \|last=Emsellem \|first=Eric \|title=Is the black hole in NGC 1277 really overmassive? \|journal=] \|volume=433 \|issue=3 \|pages=1862–1870 \|date=Aug 2013 \|doi=10.1093/mnras/stt840 \|bibcode = 2013MNRAS.433.1862E \|arxiv = 1305.3630 }}</ref> based on the same data and published the following year, reached a very different conclusion. The black hole that was initially suggested at {{math\|{{val\|1.7\|e=10\|u=solar mass}}}} was not as massive as once thought. The black hole was estimated to be between 2 and 5 billion solar masses. This is less than a third of the previously estimated mass, a significant decrease. Models with no black hole at all were also found to provide reasonably good fits to the data, including the central region.		A follow-up study,<ref name=Emsellem>{{cite journal \|last=Emsellem \|first=Eric \|title=Is the black hole in NGC 1277 really overmassive? \|journal=] \|volume=433 \|issue=3 \|pages=1862–1870 \|date=Aug 2013 \|doi=10.1093/mnras/stt840 \|bibcode = 2013MNRAS.433.1862E \|arxiv = 1305.3630 }}</ref> based on the same data and published the following year, reached a very different conclusion. The black hole that was initially suggested at {{math\|{{val\|1.7\|e=10\|u=solar mass}}}} was not as massive as once thought. The black hole was estimated to be between 2 and 5 billion solar masses. This is less than a third of the previously estimated mass, a significant decrease. Models with no black hole at all were also found to provide reasonably good fits to the data, including the central region.

	Subsequent investigations employed ] to acquire a better estimate of the mass of the black hole.<ref name=walsh>{{cite journal\|last1=Walsh\|first1=Jonelle L.\|last2=van den Bosch\|first2=Remco C. E.\|last3=Gebhardt\|first3=Karl\|last4=Yildirim\|first4=Akin\|last5=Richstone\|first5=Douglas O.\|last6=Gültekin\|first6=Kayhan\|last7=Husemann\|first7=Bernd\|title=A 5 x 109 Msun Black Hole in NGC 1277 from Adaptive Optics Spectroscopy\|journal=The Astrophysical Journal\|date=1 January 2016\|volume=817\|issue=1\|pages=2\|doi=10.3847/0004-637X/817/1/2\|issn=0004-637X\|bibcode=2016ApJ...817....2W\|arxiv = 1511.04455 \|s2cid=118487689}}</ref><ref name=graham>{{cite journal\|last1=Graham\|first1=Alister W.\|last2=Durré\|first2=Mark\|last3=Savorgnan\|first3=Giulia A. D.\|last4=Medling\|first4=Anne M.\|last5=Batcheldor\|first5=Dan\|last6=Scott\|first6=Nicholas\|last7=Watson\|first7=Beverly\|last8=Marconi\|first8=Alessandro\|title=A Normal Supermassive Black Hole in NGC 1277\|journal=The Astrophysical Journal\|date=1 March 2016\|volume=819\|issue=1\|pages=43\|doi=10.3847/0004-637X/819/1/43\|issn=0004-637X\|bibcode=2016ApJ...819...43G\|arxiv = 1601.05151 }}</ref>		Subsequent investigations employed ] to acquire a better estimate of the mass of the black hole.<ref name=walsh>{{cite journal\|last1=Walsh\|first1=Jonelle L.\|last2=van den Bosch\|first2=Remco C. E.\|last3=Gebhardt\|first3=Karl\|last4=Yildirim\|first4=Akin\|last5=Richstone\|first5=Douglas O.\|last6=Gültekin\|first6=Kayhan\|last7=Husemann\|first7=Bernd\|title=A 5 x 109 Msun Black Hole in NGC 1277 from Adaptive Optics Spectroscopy\|journal=The Astrophysical Journal\|date=1 January 2016\|volume=817\|issue=1\|pages=2\|doi=10.3847/0004-637X/817/1/2\|issn=0004-637X\|bibcode=2016ApJ...817....2W\|arxiv = 1511.04455 \|s2cid=118487689}}</ref><ref name=graham>{{cite journal\|last1=Graham\|first1=Alister W.\|last2=Durré\|first2=Mark\|last3=Savorgnan\|first3=Giulia A. D.\|last4=Medling\|first4=Anne M.\|last5=Batcheldor\|first5=Dan\|last6=Scott\|first6=Nicholas\|last7=Watson\|first7=Beverly\|last8=Marconi\|first8=Alessandro\|title=A Normal Supermassive Black Hole in NGC 1277\|journal=The Astrophysical Journal\|date=1 March 2016\|volume=819\|issue=1\|pages=43\|doi=10.3847/0004-637X/819/1/43\|issn=0004-637X\|bibcode=2016ApJ...819...43G\|arxiv = 1601.05151 \|s2cid=36974319 }}</ref>
	One group made observations using the Gemini Near Infrared Integral Field Spectrometer to better determine the mass of the black hole at the center of NGC 1277.<ref name="walsh"/> The group used similar models to that of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they came to a mass of {{math\|{{val\|4.9\|e=9\|u=solar mass}}}}, similar to the estimate from the follow-up study done by Emsellem,<ref name="Emsellem"/> which estimated a mass between 2–5 billion solar masses.		One group made observations using the Gemini Near Infrared Integral Field Spectrometer to better determine the mass of the black hole at the center of NGC 1277.<ref name="walsh"/> The group used similar models to that of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they came to a mass of {{math\|{{val\|4.9\|e=9\|u=solar mass}}}}, similar to the estimate from the follow-up study done by Emsellem,<ref name="Emsellem"/> which estimated a mass between 2–5 billion solar masses.
	More recently, a new group<ref name="graham"/> made observations using the larger ] with superior spatial resolution, and calculated that a black hole with mass {{math\|{{val\|1.2\|e=9\|u=solar mass}}}} fits best. Moreover, this value is an order of magnitude smaller than first reported by van den Bosch,<ref name="vandenBosch"/> and was noted to probably be an upper limit due to the edge-on rotating disk in NGC 1277.		More recently, a new group<ref name="graham"/> made observations using the larger ] with superior spatial resolution, and calculated that a black hole with mass {{math\|{{val\|1.2\|e=9\|u=solar mass}}}} fits best. Moreover, this value is an order of magnitude smaller than first reported by van den Bosch,<ref name="vandenBosch"/> and was noted to probably be an upper limit due to the edge-on rotating disk in NGC 1277.

Revision as of 02:28, 30 October 2022

Lenticular galaxy in the constellation Perseus

NGC 1277
NGC 1277 as seen by the HST
Observation data (J2000 epoch)
Constellation	Perseus
Right ascension	03 19 51.5
Declination	41° 34′ 25″
Redshift	0.016898
Heliocentric radial velocity	5066 km/s
Galactocentric velocity	5168 km/s
Distance	73 Mpc (240 Mly)
Group or cluster	Perseus Cluster
Apparent magnitude (V)	14.66
Characteristics
Type	S0^+, pec
Size	~52,700 ly (16.16 kpc) (estimated)
Apparent size (V)	1.0 x 0.4
Other designations
PGC 12434, LGG 088
References:

NGC 1277 is a lenticular galaxy in the constellation of Perseus. It is a member of the Perseus Cluster of galaxies and is located approximately 73 Mpc (megaparsecs) or 220 million light-years from the Milky Way. It has an apparent magnitude of about 14.7. It was discovered on December 4, 1875 by Lawrence Parsons, 4th Earl of Rosse.

NGC 1277 has been called a "relic of the early universe" due to its stars being formed during a 100 million year interval about 12 billion years ago. Stars were formed at a rate of 1000 times that of the Milky Way galaxy's formation rate in a short burst of time. After this process of stellar formation ran its course, NGC 1277 was left populated with metal-rich stars that are about 7 billion years older than the Sun. It is still uncertain whether or not NGC 1277 is a "relic galaxy"; current studies are still researching the possibility. However, observations with Hubble Space Telescope indicate that NGC 1277 lacks metal-poor globular clusters, suggesting that it has accreted little mass over its lifetime and supporting the relic galaxy hypothesis.

Supermassive black hole

Initial observations made using the Hobby–Eberly Telescope at Texas's McDonald Observatory suggested the presence of a black hole with a mass of about 1.7×10 M_☉ (17 billion solar masses), equivalent to 14% of the total stellar mass of the galaxy, due to the motions of the stars near the center of the galaxy. This resulted in the initial claim that the black hole in NGC 1277 is one of the largest known in relation to the mass of its host galaxy.

A follow-up study, based on the same data and published the following year, reached a very different conclusion. The black hole that was initially suggested at 1.7×10 M_☉ was not as massive as once thought. The black hole was estimated to be between 2 and 5 billion solar masses. This is less than a third of the previously estimated mass, a significant decrease. Models with no black hole at all were also found to provide reasonably good fits to the data, including the central region.

Subsequent investigations employed adaptive optics to acquire a better estimate of the mass of the black hole. One group made observations using the Gemini Near Infrared Integral Field Spectrometer to better determine the mass of the black hole at the center of NGC 1277. The group used similar models to that of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they came to a mass of 4.9×10 M_☉, similar to the estimate from the follow-up study done by Emsellem, which estimated a mass between 2–5 billion solar masses. More recently, a new group made observations using the larger Keck Telescope with superior spatial resolution, and calculated that a black hole with mass 1.2×10 M_☉ fits best. Moreover, this value is an order of magnitude smaller than first reported by van den Bosch, and was noted to probably be an upper limit due to the edge-on rotating disk in NGC 1277.

References

^ "NASA/IPAC Extragalactic Database". Results for NGC 1277. Retrieved November 29, 2012.
^ Trujillo, Ignacio; Ferré-Mateu, Anna; Balcells, Marc; Vazdekis, Alexandre; Sánchez-Blázquez, Patricia (1 January 2014). "NGC 1277: A Massive Compact Relic Galaxy in the Nearby Universe". The Astrophysical Journal Letters. 780 (2): L20. arXiv:1310.6367. Bibcode:2014ApJ...780L..20T. doi:10.1088/2041-8205/780/2/L20. ISSN 0004-637X. S2CID 53866417.
Brunzendorf, J.; Meusinger, H. (October 1, 1999). "The galaxy cluster Abell 426 (Perseus). A catalogue of 660 galaxy positions, isophotal magnitudes and morphological types". Astronomy and Astrophysics Supplement Series. 139 (1): 141–161. Bibcode:1999A&AS..139..141B. doi:10.1051/aas:1999111. ISSN 0365-0138.
^ Walsh, Jonelle L.; van den Bosch, Remco C. E.; Gebhardt, Karl; Yildirim, Akin; Richstone, Douglas O.; Gültekin, Kayhan; Husemann, Bernd (1 January 2016). "A 5 x 109 Msun Black Hole in NGC 1277 from Adaptive Optics Spectroscopy". The Astrophysical Journal. 817 (1): 2. arXiv:1511.04455. Bibcode:2016ApJ...817....2W. doi:10.3847/0004-637X/817/1/2. ISSN 0004-637X. S2CID 118487689.{{cite journal}}: CS1 maint: unflagged free DOI (link)
^ Graham, Alister W.; Durré, Mark; Savorgnan, Giulia A. D.; Medling, Anne M.; Batcheldor, Dan; Scott, Nicholas; Watson, Beverly; Marconi, Alessandro (1 March 2016). "A Normal Supermassive Black Hole in NGC 1277". The Astrophysical Journal. 819 (1): 43. arXiv:1601.05151. Bibcode:2016ApJ...819...43G. doi:10.3847/0004-637X/819/1/43. ISSN 0004-637X. S2CID 36974319.{{cite journal}}: CS1 maint: unflagged free DOI (link)
Beasley, Michael A.; Trujillo, Ignacio; Leaman, Ryan; Montes, Mireia (2018-03-12). "A single population of red globular clusters around the massive compact galaxy NGC 1277". Nature. 555 (7697): 483–486. arXiv:1803.04893. Bibcode:2018Natur.555..483B. doi:10.1038/nature25756. ISSN 0028-0836. PMID 29531319. S2CID 4440393.
^ van den Bosch, Remco C. E.; et al. (29 Nov 2012). "An over-massive black hole in the compact lenticular galaxy NGC 1277". Nature. 491 (7426): 729–731. arXiv:1211.6429. Bibcode:2012Natur.491..729V. doi:10.1038/nature11592. PMID 23192149. S2CID 205231230.
^ Emsellem, Eric (Aug 2013). "Is the black hole in NGC 1277 really overmassive?". Monthly Notices of the Royal Astronomical Society. 433 (3): 1862–1870. arXiv:1305.3630. Bibcode:2013MNRAS.433.1862E. doi:10.1093/mnras/stt840.{{cite journal}}: CS1 maint: unflagged free DOI (link)

External links

Media related to NGC 1277 at Wikimedia Commons

v t e Astronomical catalogs
NGC	NGC 1272 NGC 1273 NGC 1274 NGC 1275 NGC 1276 NGC 1277 NGC 1278 NGC 1279 NGC 1280 NGC 1281 NGC 1282
PGC	PGC 12530 PGC 12531 PGC 12532 PGC 12533 PGC 12534 PGC 12535 PGC 12536 PGC 12537 PGC 12538

v t e New General Catalogue 1000 to 1499
1000 1001 1002 1003 1004 1005 1006 1007 1008 1009 1010 1011 1012 1013 1014 1015 1017 1018 1019 1020 1021 1022 1023 1024 1025 1026 1027 1028 1029 1030 1031 1032 1033 1034 1035 1036 1037 1038 1039 1040 1041 1042 1043 1044 1045 1046 1047 1048 1049 1050 1051 1052 1053 1054 1055 1056 1057 1058 1059 1060 1061 1062 1063 1064 1065 1066 1067 1068 1069 1070 1071 1072 1073 1074 1075 1076 1077 1078 1079 1080 1081 1082 1083 1084 1085 1086 1087 1088 1089 1090 1091 1092 1093 1094 1095 1096 1097 1098 1099 1100 1101 1102 1103 1104 1105 1106 1107 1108 1109 1110 1111 1112 1113 1114 1115 1116 1117 1118 1119 1120 1121 1122 1123 1124 1125 1126 1127 1128 1129 1130 1131 1132 1133 1134 1135 1136 1137 1138 1139 1140 1141 1142 1143 1144 1145 1146 1147 1148 1149 1150 1151 1152 1153 1154 1155 1156 1157 1158 1159 1160 1161 1162 1163 1164 1165 1166 1167 1168 1169 1170 1171 1172 1173 1174 1175 1176 1177 1178 1179 1180 1181 1182 1183 1184 1185 1186 1187 1188 1189 1190 1191 1192 1193 1194 1195 1196 1197 1198 1199 1200 1201 1202 1203 1204 1205 1206 1207 1208 1209 1210 1211 1212 1213 1214 1215 1216 1217 1218 1219 1220 1221 1222 1223 1224 1225 1226 1227 1228 1229 1230 1231 1232 1233 1234 1235 1236 1237 1238 1239 1240 1241 1242 1243 1244 1245 1246 1247 1248 1249 1250 1251 1252 1253 1254 1255 1256 1257 1258 1259 1260 1261 1262 1263 1264 1265 1266 1267 1268 1269 1270 1271 1272 1273 1274 1275 1276 1277 1278 1279 1280 1281 1282 1283 1284 1285 1286 1287 1288 1289 1290 1291 1292 1293 1294 1295 1296 1297 1298 1299 1300 1301 1302 1303 1304 1305 1306 1307 1308 1309 1310 1311 1312 1313 1314 1315 1316 1317 1318 1319 1320 1321 1322 1323 1324 1325 1326 1327 1328 1329 1330 1331 1332 1333 1334 1335 1336 1337 1338 1339 1340 1341 1342 1343 1344 1345 1346 1347 1348 1349 1350 1351 1352 1353 1354 1355 1356 1357 1358 1359 1360 1361 1362 1363 1364 1365 1366 1367 1368 1369 1370 1371 1372 1373 1374 1375 1376 1377 1378 1379 1380 1381 1382 1383 1384 1385 1386 1387 1388 1389 1390 1391 1392 1393 1394 1395 1396 1397 1398 1399 1400 1401 1402 1403 1404 1405 1406 1407 1408 1409 1410 1411 1412 1413 1414 1415 1416 1417 1418 1419 1420 1421 1422 1423 1424 1425 1426 1427 1428 1429 1430 1431 1432 1433 1434 1435 1436 1437 1438 1439 1440 1441 1442 1443 1444 1445 1446 1447 1448 1449 1450 1451 1452 1453 1454 1455 1456 1457 1458 1459 1460 1461 1462 1463 1464 1465 1466 1467 1468 1469 1470 1471 1472 1473 1474 1475 1476 1477 1478 1479 1480 1481 1482 1483 1484 1485 1486 1487 1488 1489 1490 1491 1492 1493 1494 1495 1496 1497 1498 1499
Astronomical catalog List of NGC objects 1001–2000

New General Catalogue 1000 to 1499

Constellation of Perseus

Stars

Bayer	α (Mirfak) β (Algol) γ δ ε ζ η (Miram) θ ι κ (Misam) λ μ ν ξ (Menkib) ο (Atik) π (Gorgonea Secunda) ρ (Gorgonea Tertia) σ τ φ ψ ω (Gorgonea Quarta) b
Flamsteed	1 2 3 4 (g) 5 7 8 9 (i) 10 11 12 14 16 17 20 21 24 29 30 31 32 (l) 34 36 40 (o) 42 (n) 43 (A) 48 (c) 49 50 52 (f) 53 (d) 54 55 56 57 (m) 58 (e) 59 1 Aur
Variable	S T U V X Z RS RT RV RW RY ST SU SV TZ UV UX UY VX XX XY XZ YZ AB AG AR AS AW AX BM DM DY FO GK IK IP IQ IU IW IX IZ KP KS KT KW LX V351 V356 V357 V361 V376 V380 V386 V392 V396 V400 V423 V432 V440 V459 V461 V471 V472 V473 V480 V490 V492 V505 V509 V518 V520 (61 And) V521 V545 V551 V572 V573 V575 V576 V621 V718 V1024
HR	470 526 529 538 540 621 641 787 792 810 820 831 842 846 849 864 865 876 885 886 890 894 918 (k) 920 923 930 949 950 956 964 966 969 973 975 979 986 991 1001 1019 1034 1037 1041 1047 1051 1056 1059 1074 1097 1113 1127 1130 1133 1141 1160 1164 1176 1191 1197 1198 1207 1215 1226 1234 1286 1301 1330 1333 1337 1344 1371 1390 1419 1424 1482 1489 1493 1500 1514
HD	13519 14433 14434 16691 16760 17092 17245 17605 21684 22781 23301 23596 25329 26702 29587
Other	BD+31 643 BD+48 740 G 38-29 G 95-57 GD 61 HAT-P-15 (Berehynia) HAT-P-29 (Muspelheim) IRAS 04296+3429 L1448-IRS2E LkHα 101 LRLL 54361 NGC 1333 13 NGC 1333 IRAS 2A NGC 1333 IRAS 4A NGC 1333 IRAS 4B NGC 1624-2 PSR B0355+54 PSR J0357+3205 WR 4

Exoplanets	WASP-11b/HAT-P-10b

Star
clusters

NGC	869 (h) 884 (χ) 957 1039 1220 1285 1342 1444 1513 1528 1545 1624
Other	Alpha Persei Cluster IC 348 Trumpler 2

Nebulae

NGC	650 (Little Dumbbell Nebula) 1333 1491 1499 (California Nebula) 1579
Other	Barnard 203 Wreath Nebula

Galaxies

NGC	1003 1023 1058 1077 1086 1159 1160 1161 1167 1169 1175 (Peanut Galaxy) 1198 1250 1259 1260 1264 1265 1267 1268 1270 1271 1272 1273 1274 1275 1277 1278 1279 1281 1282 1283 1293 1294 1334
Other	1H 0323+342 IC 310 NRAO 140 UGC 2885 (Godzilla galaxy) 4C +37.11

Galaxy clusters	Perseus Cluster

Astronomical events	SN 2006gy Perseids

Revision as of 20:18, 20 October 2022 editColonies Chris (talk \| contribs)Autopatrolled, Extended confirmed users, Pending changes reviewers, Rollbackers445,668 editsm Redirect bypass from Hobby-Eberly Telescope to Hobby–Eberly Telescope using popups ← Previous edit		Revision as of 02:28, 30 October 2022 edit undoCitation bot (talk \| contribs)Bots5,426,107 edits Add: s2cid. \| Use this bot. Report bugs. \| Suggested by Whoop whoop pull up \| #UCB_webform 249/976Next edit →
Line 42:		Line 42:
	A follow-up study,<ref name=Emsellem>{{cite journal \|last=Emsellem \|first=Eric \|title=Is the black hole in NGC 1277 really overmassive? \|journal=] \|volume=433 \|issue=3 \|pages=1862–1870 \|date=Aug 2013 \|doi=10.1093/mnras/stt840 \|bibcode = 2013MNRAS.433.1862E \|arxiv = 1305.3630 }}</ref> based on the same data and published the following year, reached a very different conclusion. The black hole that was initially suggested at {{math\|{{val\|1.7\|e=10\|u=solar mass}}}} was not as massive as once thought. The black hole was estimated to be between 2 and 5 billion solar masses. This is less than a third of the previously estimated mass, a significant decrease. Models with no black hole at all were also found to provide reasonably good fits to the data, including the central region.		A follow-up study,<ref name=Emsellem>{{cite journal \|last=Emsellem \|first=Eric \|title=Is the black hole in NGC 1277 really overmassive? \|journal=] \|volume=433 \|issue=3 \|pages=1862–1870 \|date=Aug 2013 \|doi=10.1093/mnras/stt840 \|bibcode = 2013MNRAS.433.1862E \|arxiv = 1305.3630 }}</ref> based on the same data and published the following year, reached a very different conclusion. The black hole that was initially suggested at {{math\|{{val\|1.7\|e=10\|u=solar mass}}}} was not as massive as once thought. The black hole was estimated to be between 2 and 5 billion solar masses. This is less than a third of the previously estimated mass, a significant decrease. Models with no black hole at all were also found to provide reasonably good fits to the data, including the central region.

	Subsequent investigations employed ] to acquire a better estimate of the mass of the black hole.<ref name=walsh>{{cite journal\|last1=Walsh\|first1=Jonelle L.\|last2=van den Bosch\|first2=Remco C. E.\|last3=Gebhardt\|first3=Karl\|last4=Yildirim\|first4=Akin\|last5=Richstone\|first5=Douglas O.\|last6=Gültekin\|first6=Kayhan\|last7=Husemann\|first7=Bernd\|title=A 5 x 109 Msun Black Hole in NGC 1277 from Adaptive Optics Spectroscopy\|journal=The Astrophysical Journal\|date=1 January 2016\|volume=817\|issue=1\|pages=2\|doi=10.3847/0004-637X/817/1/2\|issn=0004-637X\|bibcode=2016ApJ...817....2W\|arxiv = 1511.04455 \|s2cid=118487689}}</ref><ref name=graham>{{cite journal\|last1=Graham\|first1=Alister W.\|last2=Durré\|first2=Mark\|last3=Savorgnan\|first3=Giulia A. D.\|last4=Medling\|first4=Anne M.\|last5=Batcheldor\|first5=Dan\|last6=Scott\|first6=Nicholas\|last7=Watson\|first7=Beverly\|last8=Marconi\|first8=Alessandro\|title=A Normal Supermassive Black Hole in NGC 1277\|journal=The Astrophysical Journal\|date=1 March 2016\|volume=819\|issue=1\|pages=43\|doi=10.3847/0004-637X/819/1/43\|issn=0004-637X\|bibcode=2016ApJ...819...43G\|arxiv = 1601.05151 }}</ref>		Subsequent investigations employed ] to acquire a better estimate of the mass of the black hole.<ref name=walsh>{{cite journal\|last1=Walsh\|first1=Jonelle L.\|last2=van den Bosch\|first2=Remco C. E.\|last3=Gebhardt\|first3=Karl\|last4=Yildirim\|first4=Akin\|last5=Richstone\|first5=Douglas O.\|last6=Gültekin\|first6=Kayhan\|last7=Husemann\|first7=Bernd\|title=A 5 x 109 Msun Black Hole in NGC 1277 from Adaptive Optics Spectroscopy\|journal=The Astrophysical Journal\|date=1 January 2016\|volume=817\|issue=1\|pages=2\|doi=10.3847/0004-637X/817/1/2\|issn=0004-637X\|bibcode=2016ApJ...817....2W\|arxiv = 1511.04455 \|s2cid=118487689}}</ref><ref name=graham>{{cite journal\|last1=Graham\|first1=Alister W.\|last2=Durré\|first2=Mark\|last3=Savorgnan\|first3=Giulia A. D.\|last4=Medling\|first4=Anne M.\|last5=Batcheldor\|first5=Dan\|last6=Scott\|first6=Nicholas\|last7=Watson\|first7=Beverly\|last8=Marconi\|first8=Alessandro\|title=A Normal Supermassive Black Hole in NGC 1277\|journal=The Astrophysical Journal\|date=1 March 2016\|volume=819\|issue=1\|pages=43\|doi=10.3847/0004-637X/819/1/43\|issn=0004-637X\|bibcode=2016ApJ...819...43G\|arxiv = 1601.05151 \|s2cid=36974319 }}</ref>
	One group made observations using the Gemini Near Infrared Integral Field Spectrometer to better determine the mass of the black hole at the center of NGC 1277.<ref name="walsh"/> The group used similar models to that of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they came to a mass of {{math\|{{val\|4.9\|e=9\|u=solar mass}}}}, similar to the estimate from the follow-up study done by Emsellem,<ref name="Emsellem"/> which estimated a mass between 2–5 billion solar masses.		One group made observations using the Gemini Near Infrared Integral Field Spectrometer to better determine the mass of the black hole at the center of NGC 1277.<ref name="walsh"/> The group used similar models to that of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they came to a mass of {{math\|{{val\|4.9\|e=9\|u=solar mass}}}}, similar to the estimate from the follow-up study done by Emsellem,<ref name="Emsellem"/> which estimated a mass between 2–5 billion solar masses.
	More recently, a new group<ref name="graham"/> made observations using the larger ] with superior spatial resolution, and calculated that a black hole with mass {{math\|{{val\|1.2\|e=9\|u=solar mass}}}} fits best. Moreover, this value is an order of magnitude smaller than first reported by van den Bosch,<ref name="vandenBosch"/> and was noted to probably be an upper limit due to the edge-on rotating disk in NGC 1277.		More recently, a new group<ref name="graham"/> made observations using the larger ] with superior spatial resolution, and calculated that a black hole with mass {{math\|{{val\|1.2\|e=9\|u=solar mass}}}} fits best. Moreover, this value is an order of magnitude smaller than first reported by van den Bosch,<ref name="vandenBosch"/> and was noted to probably be an upper limit due to the edge-on rotating disk in NGC 1277.

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