1,723,208 research outputs found
Block Card 5252 Kellogg Road
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Craftsman Style | Dwelling | Homedale Addition (Toledo, Ohio) | Reynolds Corners Area (Toledo, Ohio) | 5252 Kellogg Road (Toledo, Ohio
Block Card 5252 Winona Drive
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Ranch houses | 5252 Winona Road (Toledo, Ohio) | Dwelling | Elizabeth Park Addition (Toledo, Ohio) | Greenwood Park Area (Toledo, Ohio
5252. Pierre de Blarru, humaniste
No full text5252. Pierre de Blarru, humaniste. In: Molinier Auguste. Les Sources de l'histoire de France - Des origines aux guerres d'Italie (1494). V. Introduction générale - Les Valois (suite), Louis XI et Charles VIII (1461-1494) Paris : A. Picard et fils, 1904. pp. 125-126
5252. Pierre de Blarru, humaniste
No full text5252. Pierre de Blarru, humaniste. In: Molinier Auguste. Les Sources de l'histoire de France - Des origines aux guerres d'Italie (1494). V. Introduction générale - Les Valois (suite), Louis XI et Charles VIII (1461-1494) Paris : A. Picard et fils, 1904. pp. 125-126
An off-nucleus nonstellar black hole in the seyfert galaxy NGC 5252
Get PDFWe report the discovery of an ultraluminous X-ray source (ULX; CXO J133815.6+043255) in NGC 5252. This ULX is an off-nuclear point source, which is 22′′ away from the center of NGC 5252, and has an X-ray luminosity of 1.5 × 1040 erg s-1. It is one of the rare examples of a ULX, which exhibits clear counterparts in radio, optical, and UV bands. A follow-up optical spectrum of the ULX shows strong emission lines. The redshift of the [O iii] emission line coincides with the systematic velocity of NGC 5252, suggesting that the ULX is gravitationally bound to NGC 5252. The flux of [O iii] appears to be correlated with both X-ray and radio luminosity in the same manner as ordinary active galactic nuclei (AGNs), indicating that the [O iii] emission is intrinsically associated with the ULX. Based on the multiwavelength data, we argue that the ULX is unlikely to be a background AGN. A more likely option is an accreting black hole with a mass of , which might be a stripped remnant of a merging dwarf galaxy
Ionized Gas Kinematics around an Ultra-luminous X-Ray Source in NGC 5252: Additional Evidence for an Off-nuclear AGN
No full textThe Seyfert 2 galaxy NGC 5252 contains a recently identified ultra-luminous X-ray (ULX) source that has been suggested to be a possible candidate off-nuclear low-mass active galactic nucleus. We present follow-up optical integral-field unit observations obtained using Gemini Multi-Object Spectrographs on the Gemini-North telescope. In addition to confirming that the ionized gas in the vicinity of the ULX is kinematically associated with NGC 5252, the new observations reveal ordered motions consistent with rotation around the ULX. The close coincidence of the excitation source of the line-emitting gas with the position of the ULX further suggests that ULX itself is directly responsible for the ionization of the gas. The spatially resolved measurements of [N II]lambda 6584/H alpha surrounding the ULX indicate a low gas-phase metallicity, consistent with those of other known low-mass active galaxies but not that of its more massive host galaxy. These findings strengthen the proposition that the ULX is not a background source but rather that it is the nucleus of a small, low-mass galaxy accreted by NGC 5252.Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning [NRF-2017R1C1B2002879]; K-GMT Science Program of Korea Astronomy and Space Science Institute (KASI) [PID: GN-2015A-Q-201]; National Key Program for Science and Technology Research and Development [2016YFA0400702]; National Science Foundation of China [11473002]; NRF grant - Korea government (MSIP) [2017R1A3A3001362]SCI(E)ARTICLE284
The Supermassive Black Hole in the Seyfert 2 Galaxy NGC 5252
Get PDFWe present results from HST/STIS long-slit spectroscopy of the gas motions in the nuclear region of the Seyfert 2 galaxy NGC 5252. The observed velocity field is consistent with gas in regular rotation with superposed localized patches of disturbed gas. The dynamics of the circumnuclear gas can be accurately reproduced by adding to the stellar mass component a compact dark mass of MBH = 0.95 (−0.45;+1.45) ×109 M⊙, very likely a supermassive black hole (BH). Contrarily to results obtained in similar studies rotational broadening is sufficient to reproduce also the behaviour of line widths. The BH mass estimated for NGC 5252 is in good agreement with the correlation between MBH and bulge mass. The comparison with the MBH vs c relationship is less stringent (mostly due to the relatively large error in c); NGC 5252 is located above the best fit line by between 0.3 and 1.2 dex, i.e. 1 - 4 times the dispersion of the correlation. Both the galaxy’s and BH mass of NGC 5252 are substantially larger than those usually estimated for Seyfert galaxies but, on the other hand, they are typical of radio-quiet quasars. Combining the determined BH mass with the hard X-ray luminosity, we estimate that NGC 5252 is emitting at a fraction ∼ 0.005 of LEdd. In this sense, this active nucleus appears to be a quasar relic, now probably accreting at a low rate, rather than a low black hole mass counterpart of a QSO
Deep Chandra Observation of the Remarkable Ionization Cones of NGC 5252
No full textInternational audienceSeyfert galaxy NGC 5252 harbors enormously extended ionization cones, which have been previously detected in the optical and X-ray band, offering a unique opportunity to investigate the interaction between the central active galactic nucleus (AGN) and the surrounding gas in the AGN host galaxy. We present deep Chandra imaging spectroscopy of NGC 5252 with a total exposure time of 230 ks. The morphology in the soft X-rays shows resolved extended structure from nucleus to a large radial distance, and for the first time we detect the outermost X-ray arc at 20 kpc. The X-ray cone mostly follows the direction of the optical ionization cones in the southeast and northwest direction, about 20 degrees misaligned with the major axis of the galactic disk of NGC 5252. Fitting the spectra extracted from radial sectors with photoionization models supports that extended emission is mainly photoionized by the central AGN. We also examine the variation of the photoionization parameter along the radial extension, and infer a decreasing ionizing continuum of the central engine by a factor of 50 over the past 64000 years. These findings are consistent with previous suggestion that NGC 5252 resembles a quasar relic with a supermassive black hole, which went through a minor merger event and switched to a low accretion rate state
NGC 5252: a pair of radio-emitting active galactic nuclei?
No full textThe X-ray source CXO J133815.6+043255 has counterparts in the UV, optical, and radio bands. Based on the multiband investigations, it has been recently proposed by Kim et al. as a rarely seen off-nucleus ultraluminous X-ray (ULX) source with a black hole mass of ≥104 M⊙ in the nearby Seyfert galaxy NGC 5252. To explore its radio properties at very high angular resolution, we performed very long-baseline interferometry (VLBI) observations with the European VLBI Network (EVN) at 1.7 GHz. We find that the radio counterpart is remarkably compact among the known ULXs. It does not show a resolved structure with a resolution of a few milliarcsecond (mas), and the total recovered flux density is comparable to that measured in earlier sub-arcsecond-resolution images. The compact radio structure, the relatively flat spectrum, and the high radio luminosity are consistent with a weakly accreting supermassive black hole in a low-luminosity active galactic nucleus. The nucleus of NGC 5252 itself has similar radio properties. We argue that the system represents a relatively rare pair of active galactic nuclei, where both components emit in the radio
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