Home     Getting Started     To Survive in the Universe    
Inhabited Sky
    News@Sky     Astro Photo     The Collection     Forum     Blog New!     FAQ     Press     Login  

NGC 3147



Upload your image

DSS Images   Other Images

Related articles

Supernovae 2006gi in NGC 3147
IAUC 8755 available at Central Bureau for Astronomical Telegrams.

Supernovae 2006gi and 2006gj
IAUC 8751 available at Central Bureau for Astronomical Telegrams.

Low-Luminosity Active Galaxies and Their Central Black Holes
Central black hole masses for 117 spiral galaxies representingmorphological stages S0/a through Sc and taken from the largespectroscopic survey of Ho et al. are derived using Ks-banddata from the Two Micron All Sky Survey. Black hole masses are foundusing a calibrated black hole-Ks bulge luminosity relation,while bulge luminosities are measured by means of a two-dimensionalbulge-disk decomposition routine. The black hole masses are correlatedagainst a variety of parameters representing properties of the nucleusand host galaxy. Nuclear properties such as line width (FWHM [N II]), aswell as emission-line ratios (e.g., [O III]/Hβ, [O I]/Hα, [NII]/Hα, and [S II]/Hα), show a very high degree ofcorrelation with black hole mass. The excellent correlation with linewidth supports the view that the emission-line gas is in virialequilibrium with either the black hole or bulge potential. The very goodemission-line ratio correlations may indicate a change in ionizingcontinuum shape with black hole mass in the sense that more massiveblack holes generate harder spectra. Apart from theinclination-corrected rotational velocity, no excellent correlations arefound between black hole mass and host galaxy properties. Significantdifferences are found between the distributions of black hole masses inearly-, mid-, and late-type spiral galaxies (subsamples A, B, and C) inthe sense that early-type galaxies have preferentially larger centralblack holes, consistent with observations that Seyfert galaxies arefound preferentially in early-type systems. The line width distributionsshow a marked difference among subsamples A, B, and C in the sense thatearlier type galaxies have larger line widths. There are also cleardifferences in line ratios between subsamples A+B and C that likely arerelated to the level of ionization in the gas. Finally, aKs-band Simien & de Vaucouleurs diagram shows excellentagreement with the original B-band relation, although there is a largedispersion at a given morphological stage.

UBVRI Light Curves of 44 Type Ia Supernovae
We present UBVRI photometry of 44 Type Ia supernovae (SNe Ia) observedfrom 1997 to 2001 as part of a continuing monitoring campaign at theFred Lawrence Whipple Observatory of the Harvard-Smithsonian Center forAstrophysics. The data set comprises 2190 observations and is thelargest homogeneously observed and reduced sample of SNe Ia to date,nearly doubling the number of well-observed, nearby SNe Ia withpublished multicolor CCD light curves. The large sample of U-bandphotometry is a unique addition, with important connections to SNe Iaobserved at high redshift. The decline rate of SN Ia U-band light curvescorrelates well with the decline rate in other bands, as does the U-Bcolor at maximum light. However, the U-band peak magnitudes show anincreased dispersion relative to other bands even after accounting forextinction and decline rate, amounting to an additional ~40% intrinsicscatter compared to the B band.

On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies
We investigate the relation between X-ray nuclear emission, opticalemission line luminosities and black hole masses for a sample of 47Seyfert galaxies. The sample, which has been selected from the Palomaroptical spectroscopic survey of nearby galaxies (Ho et al. 1997a, ApJS,112, 315), covers a wide range of nuclear powers, from L2-10keV ~ 1043 erg/s down to very low luminosities(L2-10 keV ~ 1038 erg/s). Best available data fromChandra, XMM-Newton and, in a few cases, ASCA observations have beenconsidered. Thanks to the good spatial resolution available from theseobservations and a proper modeling of the various spectral components,it has been possible to obtain accurate nuclear X-ray luminosities notcontaminated by off-nuclear sources and/or diffuse emission. X-rayluminosities have then been corrected taking into account the likelycandidate Compton thick sources, which are a high fraction (>30%)among type 2 Seyferts in our sample. The main result of this study isthat we confirm strong linear correlations between 2-10 keV,[OIII]λ5007, Hα luminosities which show the same slope asquasars and luminous Seyfert galaxies, independent of the level ofnuclear activity displayed. Moreover, despite the wide range ofEddington ratios (L/L_Edd) tested here (six orders of magnitude, from0.1 down to ~10-7), no correlation is found between the X-rayor optical emission line luminosities and the black hole mass. Ourresults suggest that Seyfert nuclei in our sample are consistent withbeing a scaled-down version of more luminous AGN.

Continuum emission in NGC 1068 and NGC 3147: indications for a turnover in the core spectra
We present new interferometric observations of the continuum emission atmm wavelengths in the Seyfert galaxies NGC 1068 and NGC 3147. Three mmcontinuum peaks are detected in NGC 1068, one centered on the core, oneassociated with the jet and the third one with the counter-jet. This isthe first significant detection of the radio jet and counter-jet at mmwavelengths in NGC 1068. While the fluxes of the jet components agreewith a steep spectral index extrapolated from cm-wavelengths, the corefluxes indicate a turnover of the inverted cm- into a steep mm-spectrumat roughly ~50 GHz which is most likely caused by electron-scatteredsynchrotron emission. As in NGC 1068, the spectrum of the pointlikecontinuum source in NGC 3147 also shows a turnover between cm andmm-wavelengths at ~25 GHz resulting from synchrotron self-absorptiondifferent to NGC 1068. This strongly resembles the spectrum of Sgr A*,the weakly active nucleus of our own galaxy, and M 81*, a link betweenSgr A* and Seyfert galaxies in terms of activity sequence, which maydisplay a similar turnover.

A high-frequency radio survey of low-luminosity active galactic nuclei
We investigate the high-frequency radio spectra of 20 low-luminosityactive galactic nuclei (LLAGNs) with compact radio cores. Our millimetresurvey with the Nobeyama Millimetre Array (NMA) and analyses ofsubmillimetre archival data that had been obtained with theSubmillimetre Common User Bolometer Array (SCUBA) on the James ClerkMaxwell Telescope (JCMT) reveal the following properties. At least halfof the LLAGNs show inverted spectra between 15 and 96 GHz; we use thepublished data at 15 GHz with the Very Large Array (VLA) in a0.15-arcsec resolution and our measurements at 96 GHz with the NMA in a7-arcsec resolution. The inverted spectra are not artificially made dueto their unmatched beam sizes, because of little diffuse contaminationfrom dust, HII regions, or extended jets in these LLAGNs. Suchhigh-frequency inverted spectra are apparently consistent with a`submillimetre bump', which is predicted by an advection-dominatedaccretion flow (ADAF) model. We find a strong correlation between thehigh-frequency spectral index and low-frequency core power measured withvery-long-baseline-interferometry (VLBI) instruments. The invertedspectra are found exclusively in low-core-power sources, while steepspectra are in high-core-power ones with prominent pc-scale jets. Thissuggests that the ADAF and non-thermal jets may coexist. The flux ratiosbetween disc and jet seem to be different from LLAGN to LLAGN; disccomponents can be seen in nuclear radio spectra only if the jets arefaint.

A further argument for the iron lines in active galactic nuclei arising from cerenkov line-like radiation - Calculation for an optically thin case
Not Available

Molecular Gas at High Redshift
The Early Universe Molecular Emission Line Galaxies (EMGs) are apopulation of galaxies with only 36 examples that hold great promise forthe study of galaxy formation and evolution at high redshift. Theclassification, luminosity of molecular line emission, molecular mass,far-infrared (FIR) luminosity, star formation efficiency, morphology,and dynamical mass of the currently known sample are presented anddiscussed. The star formation rates derived from the FIR luminosityrange from about 300 to 5000 Mȯ year 1 andthe molecular mass from 4 × 109 to 1 ×1011 Mȯ. At the lower end, these starformation rates, gas masses, and diameters are similar to those of localultraluminous infrared galaxies and represent starbursts in centrallyconcentrated disks, sometimes, but not always, associated with activegalactic nuclei. The evidence for large (>5 kpc) molecular disks islimited. Morphology and several high angular resolution images suggestthat some EMGs are mergers with a massive molecular interstellar mediumin both components. A critical question is whether the EMGs, inparticular those at the higher end of the gas mass and luminositydistribution, represent the formation of massive, giant ellipticalgalaxies in the early Universe. The sample size is expected to growexplosively in the era of the Atacama Large Millimeter Array (ALMA).

Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae
We study the effect of environment on the properties of Type Iasupernovae by analyzing the integrated spectra of 57 local Type Iasupernova host galaxies. We deduce from the spectra the metallicity,current star formation rate, and star formation history of the host andcompare these to the supernova decline rates. Additionally, we comparethe host properties to the difference between the derived supernovadistance and the distance determined from the best-fit Hubble law. Fromthis we investigate possible uncorrected systematic effects inherent inthe calibration of Type Ia supernova luminosities using light-curvefitting techniques. Our results indicate a statistically insignificantcorrelation in the direction of higher metallicity spiral galaxieshosting fainter Type Ia supernovae. However, we present qualitativeevidence suggesting that progenitor age is more likely to be the sourceof variability in supernova peak luminosities than is metallicity. We donot find a correlation between the supernova decline rate and hostgalaxy absolute B magnitude, nor do we find evidence of a significantrelationship between decline rate and current host galaxy star formationrate. A tenuous correlation is observed between the supernova Hubbleresiduals and host galaxy metallicities. Further host galaxyobservations will be needed to refine the significance of this result.Finally, we characterize the environmental property distributions forType Ia supernova host galaxies through a comparison with two larger,more general galaxy distributions using Kolmogorov-Smirnov tests. Theresults show the host galaxy metallicity distribution to be similar tothe metallicity distributions of the galaxies of the NFGS and SDSS.Significant differences are observed between the SN Ia distributions ofabsolute B magnitude and star formation histories and the correspondingdistributions of galaxies in the NFGS and SDSS. Among these is an abruptupper limit observed in the distribution of star formation histories ofthe host galaxy sample, suggesting a Type Ia supernovae characteristicdelay time lower limit of approximately 2.0 Gyr. Other distributiondiscrepancies are investigated and the effects on the supernovaproperties are discussed.

The Size of the Radio-Emitting Region in Low-Luminosity Active Galactic Nuclei
We have used the VLA to study radio variability among a sample of 18low-luminosity active galactic nuclei (LLAGNs) on timescales of a fewhours to 10 days. The goal was to measure or limit the sizes of theLLAGN radio-emitting regions in order to use the size measurements asinput to models of the radio emission mechanisms in LLAGNs. We detectvariability on typical timescales of a few days at a confidence level of99% in half the target galaxies. Either variability that is intrinsic tothe radio-emitting regions or that is caused by scintillation in theGalactic interstellar medium is consistent with the data. For eitherinterpretation, the brightness temperature of the emission is below theinverse Compton limit for all our LLAGNs and has a mean value of about1010 K. The variability measurements plus VLBI upper limitsimply that the typical angular size of the LLAGN radio cores at 8.5 GHzis 0.2 mas, plus or minus a factor of 2. The ~1010 Kbrightness temperature strongly suggests that a population ofhigh-energy nonthermal electrons must be present, in addition to ahypothesized thermal population in an accretion flow, in order toproduce the observed radio emission.

Reddening, Absorption, and Decline Rate Corrections for a Complete Sample of Type Ia Supernovae Leading to a Fully Corrected Hubble Diagram to v < 30,000 km s-1
Photometric (BVI) and redshift data corrected for streaming motions arecompiled for 111 ``Branch-normal,'' four 1991T-like, seven 1991bg-like,and two unusual supernovae of Type Ia (SNe Ia). Color excessesE(B-V)host of normal SNe Ia, due to the absorption of thehost galaxy, are derived by three independent methods, giving excellentagreement leading to the intrinsic colors at maximum of(B-V)00=-0.024+/-0.010 and (V-I)00=-0.265+/-0.016if normalized to a common decline rate of Δm15=1.1. Thestrong correlation between redshift absolute magnitudes (based on anarbitrary Hubble constant of H0=60 km s-1Mpc-1), corrected only for the extrinsic Galactic absorption,and the derived E(B-V)host color excesses leads to thewell-determined yet abnormal absorption-to-reddening ratios ofRBVI=3.65+/-0.16, 2.65+/-0.15, and 1.35+/-0.21.Comparison with the canonical Galactic values of 4.1, 3.1, and 1.8forces the conclusion that the law of interstellar absorption in thepath length to the SN in the host galaxy is different from the localGalactic law, a result consistent with earlier conclusions by others.Improved correlations of the fully corrected absolute magnitudes (on thesame arbitrary Hubble constant zero point) with host galaxymorphological type, decline rate, and intrinsic color are derived. Werecover the result that SNe Ia in E/S0 galaxies are ~0.3 mag fainterthan in spiral galaxies for possible reasons discussed in the text. Thenew decline rate corrections to absolute magnitudes are smaller thanthose by some authors for reasons explained in the text. The fourspectroscopically peculiar 1991T-type SNe are significantly overluminousas compared to Branch-normal SNe Ia. The overluminosity of the seven1999aa-like SNe is less pronounced. The seven 1991bg types in the sampleconstitute a separate class of SNe Ia, averaging in B 2 mag fainter thanthe normal Ia. New Hubble diagrams in B, V, and I are derived out to~30,000 km s-1 using the fully corrected magnitudes andvelocities, corrected for streaming motions. Nine solutions for theintercept magnitudes in these diagrams show extreme stability at the0.02 mag level using various subsamples of the data for both low andhigh extinctions in the sample, proving the validity of the correctionsfor host galaxy absorption. We shall use the same precepts for fullycorrecting SN magnitudes for the luminosity recalibration of SNe Ia inthe forthcoming final review of our Hubble Space Telescope Cepheid-SNexperiment for the Hubble constant.

EGRET Upper Limits and Stacking Searches of Gamma-Ray Observations of Luminous and Ultraluminous Infrared Galaxies
We present a stacking analysis of EGRET γ-ray observations at thepositions of luminous and ultraluminous infrared galaxies. The latterwere selected from the recently presented HCN survey, which is thoughtto contain the most active star-forming regions of the universe.Different sorting criteria are used, and since there is no positivecollective detection of γ-ray emission from these objects, wedetermined both collective and individual upper limits. The uppermostexcess we find appears in the case of ULIRGs ordered by redshift, at avalue of 1.8 σ.

Radio sources in low-luminosity active galactic nuclei. IV. Radio luminosity function, importance of jet power, and radio properties of the complete Palomar sample
We present the completed results of a high resolution radio imagingsurvey of all ( 200) low-luminosity active galactic nuclei (LLAGNs) andAGNs in the Palomar Spectroscopic Sample of all ( 488) bright northerngalaxies. The high incidences of pc-scale radio nuclei, with impliedbrightness temperatures ≳107 K, and sub-parsec jetsargue for accreting black holes in ≳50% of all LINERs andlow-luminosity Seyferts; there is no evidence against all LLAGNs beingmini-AGNs. The detected parsec-scale radio nuclei are preferentiallyfound in massive ellipticals and in type 1 nuclei (i.e. nuclei withbroad Hα emission). The radio luminosity function (RLF) of PalomarSample LLAGNs and AGNs extends three orders of magnitude below, and iscontinuous with, that of “classical” AGNs. We find marginalevidence for a low-luminosity turnover in the RLF; nevertheless LLAGNsare responsible for a significant fraction of present day massaccretion. Adopting a model of a relativistic jet from Falcke &Biermann, we show that the accretion power output in LLAGNs is dominatedby the kinetic power in the observed jets rather than the radiatedbolometric luminosity. The Palomar LLAGNs and AGNs follow the samescaling between jet kinetic power and narrow line region (NLR)luminosity as the parsec to kilo-parsec jets in powerful radio galaxies.Eddington ratios {l_Edd} (=L_Emitted/L_Eddington) of≤10-1{-}10-5 are implied in jet models of theradio emission. We find evidence that, in analogy to Galactic black holecandidates, LINERs are in a “low/hard” state (gas poornuclei, low Eddington ratio, ability to launch collimated jets) whilelow-luminosity Seyferts are in a “high” state (gas richnuclei, higher Eddington ratio, less likely to launch collimated jets).In addition to dominating the radiated bolometric luminosity of thenucleus, the radio jets are energetically more significant thansupernovae in the host galaxies, and are potentially able to depositsufficient energy into the innermost parsecs to significantly slow thegas supply to the accretion disk.

A catalogue of ultraluminous X-ray sources in external galaxies
We present a catalogue of ultraluminous X-ray sources (ULXs) in externalgalaxies. The aim of this catalogue is to provide easy access to theproperties of ULXs, their possible counterparts at other wavelengths(optical, IR, and radio), and their host galaxies. The cataloguecontains 229 ULXs reported in the literature until April 2004. Most ULXsare stellar-mass-black hole X-ray binaries, but it is not excluded thatsome ULXs could be intermediate-mass black holes. A small fraction ofthe candidate ULXs may be background Active Galactic Nuclei (AGN) andSupernova Remnants (SNRs). ULXs with luminosity above 1040ergs s-1 are found in both starburst galaxies and in thehalos of early-type galaxies.Table 1 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr ( or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/429/1125

The complex structure of low-luminosity active galactic nuclei: NGC 4579
We have modelled the low-luminosity active galactic nucleus (AGN) NGC4579 by explaining both the continuum and the line spectra observed withdifferent apertures. It was found that the nuclear emission is dominatedby an AGN such that the flux from the active centre (AC) is relativelylow compared with that of the narrow emission-line region (NLR) ofSeyfert galaxies. However, the contribution of a young starburst cannotbe neglected, as well as that of shock-dominated clouds with velocitiesof 100, 300 and 500kms-1. A small contribution from an olderstarburst with an age of 4.5 Myr, probably located in the externalnuclear region, is also found. HII regions appear in the extendedregions (~1 kpc), where radiation and shock-dominated clouds withVs= 100kms-1 prevail. The continuum SED of NGC4579 is characterized by the strong flux from an old stellar population.Emissions in the radio range show synchrotron radiation from the base ofthe jet outflowing from the accretion disc within 0.1 pc from the activecentre. Radio emission within intermediate distances (10-20 pc) isexplained by the bremsstrahlung from gas downstream of low-velocityshocks (Vs= 100kms-1) reached by a relatively lowradiation flux from the AC. In extended regions (>100 pc) the radioemission is synchrotron radiation created by the Fermi mechanism at theshock front. The shocks are created by collision of clouds with the jet.All types of emissions observed at different radius from the centre canbe reconciled with the presence of the jet.

Mid-Infrared Galaxy Morphology along the Hubble Sequence
The mid-infrared emission from 18 nearby galaxies were imaged with theInfrared Array Camera (IRAC) on the Spitzer Space Telescope, samplingthe spatial distributions of the reddening-free stellar photosphericemission and the warm dust in the interstellar medium. These twocomponents provide a new framework for galaxy morphology classificationin which the presence of spiral arms and their emission strengthrelative to the starlight can be measured directly and with highcontrast. Four mid-infrared classification methods are explored, threeof which are based on quantitative global parameters (colors andbulge-to-disk ratio) that are similar to those used in the past foroptical studies; in this limited sample, all correlate well withtraditional B-band classification. We suggest reasons why infraredclassification may be superior to optical classification.

Spatial Distribution of Warm Dust in Early-Type Galaxies
Images taken with the Infrared Array Camera on the Spitzer SpaceTelescope show that the spatial distribution of warm dust emission inlenticular galaxies is often organized into dynamically stablestructures strongly resembling spiral arms. These galaxies havebulge-to-disk ratios and colors for their stellar content that areappropriate for their morphological classification. Two of the threegalaxies with warm dust detected at 8.0 μm also show far-IR emissionexpected from that dust. More importantly, the [5.8]-[8.0] color of thedust emission matches the colors found for late-type, star-forminggalaxies, as well as theoretical predictions for polycyclic aromatichydrocarbon emission from dust grains. The spatially resolved duststructures may be powerful indicators of the evolutionary history of thelenticular class of galaxies, either as a tracer of ongoing quiescentstar formation or as a fossil record of a previous episode of moreactive star formation.

The Star Formation Rate and Dense Molecular Gas in Galaxies
HCN luminosity is a tracer of dense molecular gas,n(H2)>~3×104cm-3, associatedwith star-forming giant molecular cloud (GMC) cores. We present theresults and analysis of our survey of HCN emission from 65 infraredgalaxies, including nine ultraluminous infrared galaxies (ULIGs,LIR>~1012Lsolar), 22 luminousinfrared galaxies (LIGs,1011Lsolar0.06 are LIGs or ULIGs. Normal spiralsall have similar and low dense gas fractionsLHCN/LCO=0.02-0.05. The global star formationefficiency depends on the fraction of the molecular gas in a densephase.

Low-Luminosity Active Galactic Nuclei at the Highest Resolution: Jets or Accretion Flows?
Six low-luminosity active galactic nuclei (AGNs) have been imaged atmultiple frequencies from 1.7 to 43 GHz (2.3-15 GHz for three of thegalaxies) using the Very Long Baseline Array. In spite of dynamic rangesof about 100 in several frequency bands, all six galaxies remainunresolved, with size limits at 8.4 GHz of 103-104times the Schwarzschild radii of the black holes inferred at theirgalactic centers. The galaxy spectra are roughly flat from 1.7 to 43GHz, rather than steepening to classical optically thin synchrotronspectra at high frequencies. Although the spectral slopes somewhatresemble predictions for advection-dominated accretion flows, theluminosities are too high for the black hole masses of the galaxies, andthe slight spectral steepening at high frequencies cannot be explainedby standard simple models of such accretion flows. In contrast, compactjets can accommodate the average spectral index, the relatively highradio luminosity, and the unresolved appearance, but only if the jets inall six galaxies are fairly close to our line of sight. This constraintis in agreement with inclination angle predictions for five of the sixAGNs based on the dusty torus unification model.

Stacking Searches for Gamma-Ray Emission above 100 MeV from Radio and Seyfert Galaxies
The EGRET telescope on board Compton Gamma Ray Observatory detected morethan 60 sources of high-energy gamma radiation associated with activegalactic nuclei (AGNs). All but one of those belong to the blazarsubclass; the only exception is the nearby radio galaxy Centaurus A.Since there is no obvious reason other than proximity to expect Cen A tobe the only nonblazar AGN emitting in high-energy gamma rays, we haveutilized the ``stacking'' technique to search for emission above 100 MeVfrom two nonblazar AGN subclasses, radio galaxies and Seyfert galaxies.Maps of gamma-ray counts, exposure, and diffuse background have beencreated, then co-added in varying numbers based on sorts by redshift, 5GHz flux density, and optical brightness, and finally tested forgamma-ray emission. No detection significance greater than 2 σ hasbeen found for any subclass, sorting parameter, or number of objectsco-added. Monte Carlo simulations have also been performed to validatethe technique and estimate the significance of the results.

A New Nonparametric Approach to Galaxy Morphological Classification
We present two new nonparametric methods for quantifying galaxymorphology: the relative distribution of the galaxy pixel flux values(the Gini coefficient or G) and the second-order moment of the brightest20% of the galaxy's flux (M20). We test the robustness of Gand M20 to decreasing signal-to-noise ratio (S/N) and spatialresolution and find that both measures are reliable to within 10% forimages with average S/N per pixel greater than 2 and resolutions betterthan 1000 and 500 pc, respectively. We have measured G andM20, as well as concentration (C), asymmetry (A), andclumpiness (S) in the rest-frame near-ultraviolet/optical wavelengthsfor 148 bright local ``normal'' Hubble-type galaxies (E-Sd) galaxies, 22dwarf irregulars, and 73 0.05

Motion and properties of nuclear radio components in Seyfert galaxies seen with VLBI
We report EVN, MERLIN and VLBA observations at 18 cm, 6 cm and 3.6 cm ofthe Seyfert galaxies NGC 7674, NGC5506, NGC 2110 and Mrk1210 to study their structure and proper motions on pc scalesand to add some constraints on the many possible causes of theradio-quietness of Seyferts. The component configurations inNGC 7674 and NGC 2110 are simple,linear structures, whereas the configurations in NGC5506 and Mrk 1210 have multiple componentswith no clear axis of symmetry. We suggest that NGC7674 is a low-luminosity compact symmetric object. Comparingthe images at different epochs, we find a proper motion in NGC7674 of (0.92±0.07) c between the two centralcomponents separated by 282 pc and, in NGC 5506, wefind a 3 σ upper limit of 0.50 c for the components separated by3.8 pc. Our results confirm and extend earlier work showing that theoutward motion of radio components in Seyfert galaxies isnon-relativistic on pc scales. We briefly discuss whether thisnon-relativistic motion is intrinsic to the jet-formation process orresults from deceleration of an initially relativistic jet byinteraction with the pc or sub-pc scale interstellar medium. We combinedour sample with a list compiled from the literature of VLBI observationsmade of Seyfert galaxies, and found that most Seyfert nuclei have atleast one flat-spectrum component on the VLBI scale, which was not seenin the spectral indices measured at arcsec resolution. We found alsothat the bimodal alignment of pc and kpc radio structures displayed byradio galaxies and quasars is not displayed by this sample of Seyferts,which shows a uniform distribution of misalignment between0° and 90°. The frequent misalignmentcould result from jet precession or from deflection of the jet byinteraction with gas in the interstellar medium.

Deprojecting spiral galaxies using Fourier analysis. Application to the Frei sample
We present two methods that can be used to deproject spirals, based onFourier analysis of their images, and discuss their potential andrestrictions. Our methods perform particularly well for galaxies moreinclined than 50° or for non-barred galaxies moreinclined than 35°. They are fast and straightforward touse, and thus ideal for large samples of galaxies. Moreover, they arevery robust for low resolutions and thus are appropriate for samples ofcosmological interest. The relevant software is available from us uponrequest. We use these methods to determine the values of the positionand inclination angles for a sample of 79 spiral galaxies contained inthe Frei et al. (\cite{frei96}) sample. We compare our results with thevalues found in the literature, based on other methods. We findstatistically very good agreementTable 7 is only available in electronic form at the CDS via anonymousftp to cdsarc.u-strasbg.fr ( or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/415/849

Disk-bulge decompositions of spiral galaxies in UBVRI
A sample of 26 bright spiral galaxies (Btot < 12.7) withlow to medium inclination and without a bar was observed with UBVRIfilters. The CAFOS focal reducer camera at the Calar Alto 2.2 mtelescope was used. The surface-brightness distributions were fittedusing a 2-dimensional algorithm with corresponding functions for thedisk- and bulge-structure. For the disks an exponential function wasused, for the bulges a Sérsic Rβ law, was appliedwith the concentration parameter β = 1/n as another fit variable.Correlations of the resulting structural parameters of disks and bulgesin UBVRI are investigated, giving clues to the formation history of thebulges.We confirm that the large and bright bulges of early-type spirals aresimilar to elliptical galaxies. They were probably formed prior to thedisks in a monolithic collapse or via early mergers. Late-type spiralshave tiny and faint bulges with disk-like profiles. These bulges wereprobably formed after the disk in secular evolution processes, e.g. froma disk instability. The comparison of the color indices of correspondingspirals and bulges with population synthesis computations support aboveformation scenarios.Tables 2-4 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr ( or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/415/63

A scheme to unify low-power accreting black holes. Jet-dominated accretion flows and the radio/X-ray correlation
We explore the evolution in power of black holes of all masses, andtheir associated jets, within the scheme of an accretion rate-dependentstate transition. Below a critical value of the accretion rate allsystems are assumed to undergo a transition to a state where thedominant accretion mode is optically thin and radiatively inefficient.In these significantly sub-Eddington systems, the spectral energydistribution is predicted to be dominated by non-thermal emission from arelativistic jet whereas near-Eddington black holes will be dominatedinstead by emission from the accretion disk. Reasonable candidates forsuch a sub-Eddington state include X-ray binaries in the hard andquiescent states, the Galactic Center (Sgr A*), LINERs, FR I radiogalaxies, and a large fraction of BL Lac objects. Standard jet physicspredicts non-linear scaling between the optically thick (radio) andoptically thin (optical or X-ray) emission of these systems, which hasbeen confirmed recently inX-ray binaries. We show that this scaling relation is also a function ofblack hole mass and only slightly of the relativistic Doppler factor.Taking the scaling into account we show that indeed hard and quiescentstate X-ray binaries, LINERs, FR I radio galaxies, and BL Lacs can beunified and fall on a common radio/X-ray correlation. This suggests thatjet domination is an important stage in the luminosity evolution ofaccreting black hole systems.

Asteroid database
The development and significance of asteroid database are reviewed inthis paper. Some of online database of asteroid are presented andcompared briefly, including asteroid orbital elements database, asteroidphotometric database, asteroid infrared database, near earth asteroiddatabase and asteroid database. Ephemeris service based on asteroiddatabase is mentioned. The trend of development of asteroid database hasalso been discussed.

A Fundamental Plane of black hole activity
We examine the disc-jet connection in stellar mass and supermassiveblack holes by investigating the properties of their compact emission inthe X-ray and radio bands. We compile a sample of ~100 active galacticnuclei with measured masses, 5-GHz core emission, and 2-10 keVluminosities, together with eight galactic black holes with a total of~50 simultaneous observations in the radio and X-ray bands. Using thissample, we study the correlations between the radio (LR) andthe X-ray (LX) luminosity and the black hole mass (M). Wefind that the radio luminosity is correlated with bothM andLX, at a highly significant level. In particular, we showthat the sources define a `Fundamental Plane' in the three-dimensional(logLR, logLX, logM) space, given bylogLR= (0.60+0.11-0.11)logLX+ (0.78+0.11-0.09) logM+7.33+4.05-4.07, with a substantial scatter ofσR= 0.88. We compare our results to the theoreticalrelations between radio flux, black hole mass, and accretion ratederived by Heinz & Sunyaev. Such relations depend only on theassumed accretion model and on the observed radio spectral index.Therefore, we are able to show that the X-ray emission from black holesaccreting at less than a few per cent of the Eddington rate is unlikelyto be produced by radiatively efficient accretion, and is marginallyconsistent with optically thin synchrotron emission from the jet. On theother hand, models for radiatively inefficient accretion flows seem toagree well with the data.

First results from the HI Jodrell All Sky Survey: inclination-dependent selection effects in a 21-cm blind survey
Details are presented of the HI Jodrell All Sky Survey (HIJASS). HIJASSis a blind neutral hydrogen (HI) survey of the northern sky (δ> 22°), being conducted using the multibeam receiver on theLovell Telescope (full width at half-maximum beamwidth 12 arcmin) atJodrell Bank. HIJASS covers the velocity range -3500 to 10 000 kms-1, with a velocity resolution of 18.1 km s-1 andspatial positional accuracy of ~2.5 arcmin. Thus far about 1115deg2 of sky have been surveyed. The average rms noise duringthe early part of the survey was around 16 mJy beam-1.Following the first phase of the Lovell Telescope upgrade (in 2001), therms noise is now around 13 mJy beam-1. We describe themethods of detecting galaxies within the HIJASS data and of measuringtheir HI parameters. The properties of the resulting HI-selected sampleof galaxies are described. Of the 222 sources so far confirmed, 170 (77per cent) are clearly associated with a previously catalogued galaxy. Afurther 23 sources (10 per cent) lie close (within 6 arcmin) to apreviously catalogued galaxy for which no previous redshift exists. Afurther 29 sources (13 per cent) do not appear to be associated with anypreviously catalogued galaxy. The distributions of peak flux, integratedflux, HI mass and cz are discussed. We show, using the HIJASS data, thatHI self-absorption is a significant, but often overlooked, effect ingalaxies with large inclination angles to the line of sight. Properlyaccounting for it could increase the derived HI mass density of thelocal Universe by at least 25 per cent. The effect that this will haveon the shape of the HI mass function will depend on how self-absorptionaffects galaxies of different morphological types and HI masses. We alsoshow that galaxies with small inclinations to the line of sight may alsobe excluded from HI-selected samples, since many such galaxies will haveobserved velocity widths that are too narrow for them to bedistinguished from narrow-band radio-frequency interference. This effectwill become progressively more serious for galaxies with smallerintrinsic velocity widths. If, as we might expect, galaxies with smallerintrinsic velocity widths have smaller HI masses, then compensating forthis effect could significantly steepen the faint-end slope of thederived HI mass function.

Submit a new article

Related links

  • - No Links Found -
Submit a new link

Member of following groups:

Observation and Astrometry data

Right ascension:10h16m53.30s
Aparent dimensions:4.169′ × 3.631′

Catalogs and designations:
Proper Names   (Edit)
NGC 2000.0NGC 3147

→ Request more catalogs and designations from VizieR