The SN progenitor radius depends on the adopted distance D to NGC 4151 and its values are R0 = 500 R-circle dot at D = 20 Mpc and R0 = 400 R-circle dot at D = 16 Mpc.doi:10.1134/S1063773721050078Tsvetkov, D. YuPavlyuk, N. N....
galaxies : individual (NGC 4151galaxies : kinematics and dynamics galaxies : SeyfertWe present the results from a detailed kinematic analysis of both ground-based, and Hubble Space Telescope/Faint Object Camera long-slit spectroscopy at sub-arcsec spatial resolution, of the narrow-line region of ...
Pictures and descriptions of New General Catalog Objects NGC 4150, NGC 4151, NGC 4152, NGC 4153, NGC 4154, NGC 4155, NGC 4156, NGC 4157, NGC 4158, NGC 4159, NGC 4160, NGC 4161, NGC 4162, NGC 4163, NGC 4164, NGC 4165, NGC 4166, NGC 4167, NGC 4168, NGC 416
Fast luminosity variations occur within a night in the Seyfert galaxy NGC 4151 as observed in many observatories. We have examined photometric observations over 30 years performed at CAO and the Shternberg State Astronomical Institute, with the addition of data published by others (including X-ray ...
We present results of a sensitive 76 ksec Chandra observation of the young stellar cluster in NGC 2024, lying at a distance of 415 pc in the Orion B giant molecular cloud. Previous infrared observations have shown that this remarkable cl... S Skinner,M Gagné,E Belzer 被引量: 11发表: 20...
We show that NGC 1087 is located at a distance of D = 17.79 +/- 0.83 Mpc and therefore does not belong to the NGC 1068 group.doi:10.1134/S199034132103010XTikhonov, N. A.Galazutdinova, O. A.Pleiades PublishingAstrophysical bulletin
The X-ray luminosity of this object is of the order of 4 × 10 43 erg s 1 if a distance of 20 Mpc is assumed and exceeds the integrated luminosity at all the other observed greater wavelengths. Long-term observations 4 by Ariel V indicate that the X-ray emission may originate from a...
We show how the response of the Lyman continuum optical depth to variations in the continuum flux may be used to derive estimates of the distance of the absorbing gas from the central object. In this case, it seems that the absorbing gas is located $\\leq 50$~pc away from the central ...
and narrow (emission) line regions (BLR and NLR).\nWe present evidence that these emission lines arise from the same gas\nresponsible for most of the high-column UV and X-ray absorption (component\n``D+E'') that we see in outflow at a distance of ~0.1 pc from the central\n...
The first results of an analysis of the spatial variations along and across the ENLR of NGC 4151 are presented. The excitation of the gas clearly decreases with distance from the nucleus. The mean energy of the ionizing continuum deduced from the He II/H-beta ratio is compatible in the SW...