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Black Hole Masses of Active Galaxies with Double-peaked Balmer Emission Lines
We have obtained near-IR spectra of five AGNs that exhibit double-peakedBalmer emission lines (NGC 1097, Pictor A, PKS 0921-213, 1E0450.30-1817, and IRAS 0236.6-3101). The stellar velocity dispersions ofthe host galaxies were measured from the Ca II λλ8494,8542, 8662 absorption lines and were found to range from 140 to 200 kms-1. Using the well-known correlation between the black holemass and the stellar velocity dispersion, the black hole masses in thesegalaxies were estimated to range from 4×107 to1.2×108 Msolar. We supplement theobservations presented here with estimates of the black holes masses forfive additional double-peaked emitters (Arp 102B, 3C 390.3, NGC 4579,NGC 4203, and M81) obtained by other authors using similar methods.Using these black hole masses, we infer the ratio of the bolometricluminosity to the Eddington luminosity,(Lbol/LEdd). We find that two objects (Pictor Aand PKS 0921-213) have Lbol/LEdd~0.2, whereas theother objects have Lbol/LEdd<~10-2(nearby, low-luminosity double-peaked emitters are the most extreme,with Lbol/LEdd<~10-4). The physicaltimescales in the outer regions of the accretion disks (atr~103GM/c2) in these objects were also estimatedand range from a few months for the dynamical timescale to severaldecades for the sound crossing timescale. The profile variability inthese objects is typically an order of magnitude longer than thedynamical time, but we note that variability occurring on the dynamicaltimescale has not been ruled out by the observations.Based on observations carried out at Cerro Tololo Inter-AmericanObservatory, which is operated by AURA, Inc., under a cooperativeagreement with the National Science Foundation.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Interstellar polarization at high galactic latitudes from distant stars. V. First results for the South Galactic Pole
We present the first results of our interstellar polarization programmefor the South Galactic Pole (b<-70degr ). The new observations (43stars) combined with previously published data show that there is asubstantial interstellar polarization in this area of the sky. Startingat a distance of 300 pc, we have found stars with P > 0.3% includingone for which P ~ 0.6%. These measurements lead to the conclusion thatthere is a significant amount of interstellar dust at high southgalactic latitudes. Futhermore, there is a remarkable alignment seenover the South Polar Cap: for most stars the directions of polarizationvectors are aligned with the longitude l ~ 80degr , close to theexpected direction of the global magnetic field. In this respect the SGPseems to differ strongly from its northern counterpart.
| A catalog of K giants at the South Galactic Pole - Broadband and DDO photometry and radial velocities
We describe a sample of K giants at the South Galactic Pole, selected toexamine the chemical and kinematical properties of stars perpendicularto the galactic plane and to measure the local column density of thedisk. We report velocities, abundances, absolute magnitudes, andbroadband BV photometry for over 500 giants.
| Local dark matter from a carefully selected sample
The precise data obtained by Flynn and Freeman (1991) on K giants at thesouth Galactic pole are used to analyze the amount of local dark matterin which the systematic effects can be modeled easily and evaluatedaccurately. The method of Bahcall (1984) is employed to solve theself-consistent equations for the distribution of dark matter. TheK-giant survey is found to provide significant evidence for disk darkmatter. Taking into account all recognized sources of error using astatistical test devised by Gould (1989, 1990), a model with no darkmatter is inconsistent with the data at the 86-percent confidence level.The best-fit P-model (in which dark matter is distributed proportionallyto known matter) has 53 percent more dark matter than visible matter.
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Datos observacionales y astrométricos
| Constelación: | Ballena |
| Ascensión Recta: | 00h24m49.63s |
| Declinación: | -18°28'18.7" |
| Magnitud Aparente: | 6.893 |
| Distancia: | 337.838 parsecs |
| Movimiento Propio en Ascensión Recta: | -6.5 |
| Movimiento Propio en Declinación: | -63.7 |
| B-T magnitude: | 8.776 |
| V-T magnitude: | 7.049 |
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