Диссертация (1149494), страница 13
Текст из файла (страница 13)
– V. 12. – P.1157.[63] Tully R. Brent, Courtois Helene M., Dolphin Andrew E., Fisher J. Richard,Heraudeau Philippe, Jacobs Bradley A., Karachentsev Igor D., Makarov Dmitry,Makarova Lidia, Mitronova Sofia, Rizzi Luca, Shaya Edward J., Sorce Jenny G.,Wu Po-Feng. Cosmicflows-2: The Data. // Astron.J. – 2013. – V.
146. – P.86.[64] Tully R. Brent, Courtois H., Hoffman Yehuda, Pomarede D. The Laniakeasupercluster of galaxies. // Nature. – 2014. – V. 513. – P.71.89[65] Wang J.S., Wang F.Y., Cheng K.S., and Dai Z.G. Measuring dark energywith the Eiso − Ep correlation of gamma-ray bursts using model-independentmethods. // Astron.Astrophys.
– 2016. – V. 585. – A68.[66] Williams R.E. The Hubble Deep Field: Observations, Data Reduction, andGalaxy Photometry. // Astrophys.J. – 1996. – V. 112. – P.1335.[67] Yu H., Wang F.Y., Dai Z.G., Cheng K.S. An Unexpectedly Low-redshift Excessof Swift Gamma-ray Burst Rate. // Astrophys.J.Suppl.Ser. – 2015. – V. 218. –N 1.[68] http://cosmos.astro.caltech.edu[69] http://www.stsci.edu/ftp/science/hdf/hdf.html[70] http://www.strw.leidenuniv.nl/galaxyevolution/ULTRAVISTA/Ultravista/Data_Products_Download.html[71] https://cloud.iaa.csic.es/alhambra[72] http://archive.eso.org/cms/eso-data/data-packages/zcosmos-data-release-dr1.html[73] http://xmmssc-www.star.le.ac.uk/Catalogue/xcat_public_3XMM-DR4.html[74] https://swift.gsfc.nasa.gov/archive/grb_table/[75] http://www.grbcatalog.org[76] https://www.ipnl.in2p3.fr/projet/cosmicflows/90ПриложениеРис.
57: Модуль FDEP.Рис. 58: Основная подпрограмма FDEP.91zf0.100.200.300.400.500.600.700.800.901.001.101.201.301.401.501.601.701.801.902.002.102.202.302.402.502.602.702.802.903.00zs0.000.100.200.300.400.500.600.700.800.901.001.101.201.301.401.501.601.701.801.902.002.102.202.302.402.502.602.702.802.90406.8387.2367.2347.2327.7308.9291274.1258.3243.5229.8217.1205.2194.3184.2174.8166.1158.1150.6143.7137.2131.2125.6120.3115.4110.8106.5102.598.695.1R, M pk0.3740.2190.1860.1690.1580.1500.1440.1390.1350.1320.1300.1270.1260.1240.1220.1210.1200.1190.1180.1170.1160.1160.1150.1140.1130.1130.1120.1120.1110.1105, 1.80.4050.3100.2870.2730.2630.2550.2480.2420.2370.2320.2280.2250.2210.2180.2150.2130.2100.2080.2060.2030.2010.1990.1970.1960.1940.1920.1900.1890.1870.1865, 10.5730.4390.4060.3860.3720.3600.3500.3420.3350.3290.3230.3180.3130.3090.3050.3010.2970.2940.2910.2880.2850.2820.2790.2770.2740.2720.2690.2670.2650.2620.8110.6200.5740.5460.5260.5090.4950.4840.4740.4650.4570.4490.4430.4370.4310.4250.4200.4160.4110.4070.4030.3990.3950.3910.3870.3840.3810.3770.3740.371COSMOS10, 1 20, 1+ 0.276- 0.352- 0.104+ 0.102+ 0.003- 0.163+ 0.062+ 0.250+ 0.186+ 0.461- 0.328+ 0.856+ 0.330- 0.620+ 0.316- 0.459- 0.273- 0.493- 0.665- 0.170+ 0.254- 0.610- 0.428- 0.401- 0.443+ 0.322- 0.432+ 0.168+ 0.111- 0.107δobs0.3650.2130.1810.1650.1540.1460.1400.1360.1320.1290.1260.1240.1220.1210.1190.1180.1170.1160.1150.1140.1130.1130.1120.1110.1110.1100.1090.1090.1080.1085, 1.80.4000.3060.2830.2690.2590.2510.2440.2380.2330.2290.2250.2220.2180.2150.2120.2100.2070.2050.2030.2010.1980.1970.1950.1930.1910.1890.1880.1860.1840.1835, 10.5650.4320.4000.3810.3660.3550.3450.3370.3300.3240.3180.3130.3090.3040.3000.2970.2930.2900.2870.2840.2810.2780.2750.2730.2700.2680.2650.2630.2610.2590.8000.6110.5660.5380.5180.5020.4890.4770.4670.4580.4500.4430.4360.4300.4250.4190.4150.4100.4050.4010.3970.3930.3890.3860.3820.3790.3750.3720.3690.366UVISTA10, 1 20, 1+ 0.157- 0.223- 0.141+ 0.146- 0.172- 0.170- 0.050+ 0.033+ 0.250+ 0.241- 0.137+ 0.305+ 0.012+ 0.112+ 0.088+ 0.100- 0.088- 0.125- 0.077- 0.115- 0.216- 0.231- 0.197- 0.185- 0.090- 0.042+ 0.213+ 0.220+ 0.063- 0.043δobs0.4770.2710.2310.2130.2030.1950.1900.1860.1820.1800.1780.1760.1750.1740.1740.1730.1720.1720.1720.1710.1710.1710.1710.1710.1710.1710.1710.1710.1710.1715, 1.80.4240.3220.3010.2910.2830.2770.2720.2680.2650.2620.2590.2570.2550.2530.2510.2490.2480.2460.2450.2440.2420.2410.2400.2390.2380.2360.2350.2340.2330.2325, 1каталогов COSMOS, UVISTA и ALH/F4 по бину ∆z = 0.1 c наблюдаемыми флуктуациями.0.5990.4560.4260.4110.4000.3920.3850.3800.3750.3710.3670.3630.3600.3580.3550.3530.3510.3480.3460.3450.3430.3410.3390.3380.3360.3340.3330.3310.3300.3280.8470.6450.6030.5810.5660.5540.5450.5370.5300.5240.5190.5140.5100.5060.5020.4990.4960.4930.4900.4870.4850.4820.4800.4770.4750.4730.4710.4680.4660.464ALH/F410, 1 20, 1- 0.267+ 0.167+ 0.185+ 0.205+ 0.110- 0.239- 0.247- 0.142+ 0.167+ 0.410- 0.108- 0.002- 0.177- 0.216- 0.136+ 0.011+ 0.014+ 0.300+ 0.293+ 0.043- 0.347- 0.273+ 0.024+ 0.014δobsТаблица 15: Сравнение расчетных значений σcorr для четырех комбинаций (γ; r0 ) = (1.8; 5); (1; 5); (1; 10); (1; 20) для92Рис.
59: Распределение галактик на небесной сфере в обзоре CF2.93Рис. 60: Распределение галактик на небесной сфере в обзоре CF2.94Рис. 61: Распределение галактик на небесной сфере в обзоре 2MRS.95.