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Infrared 3-4 μm Spectroscopic Investigations of a Large Sample of Nearby Ultraluminous Infrared Galaxies
We present infrared L-band (3-4 μm) nuclear spectra of a large sampleof nearby ultraluminous infrared galaxies (ULIRGs). ULIRGs classifiedoptically as non-Seyfert galaxies (LINERs, H II regions, andunclassified) are our main targets. Using the 3.3 μm polycyclicaromatic hydrocarbon (PAH) emission and absorption features at 3.1 μmdue to ice-covered dust and at 3.4 μm produced by bare carbonaceousdust, we search for signatures of powerful AGNs deeply buried alongvirtually all lines of sight. The 3.3 μm PAH emission, the signaturesof starbursts, is detected in all but two non-Seyfert ULIRGs, but theestimated starburst magnitudes can account for only a small fraction ofthe infrared luminosities. Three LINER ULIRGs show spectra typical ofalmost pure buried AGNs, namely, strong absorption features with verysmall equivalent width PAH emission. Besides these three sources, 14LINER and three H II ULIRGs' nuclei show strong absorption featureswhose absolute optical depths suggest an energy source more centrallyconcentrated than the surrounding dust, such as a buried AGN. In total,17 out of 27 (63%) LINER and 3 out of 13 (23%) H II ULIRGs' nuclei showsome degree of evidence for powerful buried AGNs, suggesting thatpowerful buried AGNs may be more common in LINER ULIRGs than in H IIULIRGs. The evidence of AGNs is found in non-Seyfert ULIRGs with bothwarm and cool far-infrared colors. These spectra are compared with thoseof 15 ULIRGs' nuclei with optical Seyfert signatures taken forcomparison. The overall spectral properties suggest that the totalamount of dust around buried AGNs in non-Seyfert ULIRGs issystematically larger than that around AGNs in Seyfert 2 ULIRGs. Weargue that the optical (non)detectability of Seyfert signatures inULIRGs is highly dependent on how deeply buried the AGNs are, and thatit is essential to properly evaluate the energetic importance of buriedAGNs in non-Seyfert ULIRGs.
| Absolute declinations with the photoelectric astrolabe at Calern Observatory (OCA)
A regular observational programme with a photoelectric astrolabe havebeen performed at ``Observatoire du Calern" (Observatoire de laCôte d'Azur, OCA, phi = +43() o44′55.011″; lambda =-0() h27() m42.44() s, Calern, Caussols, France) for the last twentyyears. It has been almost fully automatized between 1984 and 1987. Since1988 the photoelectric astrolabe was used without any modification. Inaddition to determining the daily orientation of the local vertical, theyearly analysis of the residuals permits to derive corrections to theused star catalogue \cite[(Vigouroux et al. 1992)]{vig92}. A globalreduction method was applied for the ASPHO observations. The new form ofthe equations \cite[(Martin & Leister 1997)]{mar97} give us thepossibility of using the entire set of the observing program using datataken at two zenith distances (30() o and 45() o). The program containsabout 41648 stars' transits of 269 different stars taken at``Observatoire du Calern" (OCA). The reduction was based on theHIPPARCOS system. We discuss the possibility of computing absolutedeclinations through stars belonging simultaneously to the 30() o and45() o zenith distances programmes. The absolute declination correctionswere determined for 185 stars with precision of 0.027arcsec and thevalue of the determined equator correction is -0.018arcsec +/-0.005arcsec . The instrumental effects were also determined. The meanepoch is 1995.29. Catalogue only available at CDS in electronic from viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Integrated Ultraviolet Spectra and Line Indices of M31 Globular Clusters and the Cores of Elliptical Galaxies
We present observations of the integrated light of four M31 globularclusters (MIV, MII, K280, and K58) and of the cores of six ellipticalgalaxies (NGC 3605, 3608, 5018, 5831, 6127, and 7619) made with theFaint Object Spectrograph on the Hubble Space Telescope. The spectracover the range 2200-4800 Å at a resolution of 8 Å withsignal-to-noise ratio of more than 20 and flux accuracy of ~5%. To thesedata we add from the literature IUE observations of the dwarf ellipticalgalaxy M32, Galactic globular clusters, and Galactic stars. The stellarpopulations in these systems are analyzed with the aid of mid-UV andnear-UV colors and absorption line strengths. Included in the measuredindices is the key NH feature at 3360 Å. We compare these lineindex measures with the 2600 - 3000 colors of these stars and stellarpopulations. We find that the M31 globular clusters, Galactic globularclusters/Galactic stars, and elliptical galaxies represent threedistinct stellar populations, based on their behavior in color-linestrength correlations involving Mg II, NH, CN, and several UV metallicblends. In particular, the M31 globular cluster MIV, as metal-poor asthe Galactic globular M92, shows a strong NH 3360 Å feature. Otherline indices, including the 3096 Å blend that is dominated bylines of Mg I and Al I, show intrinsic differences as well. We also findthat the broadband line indices often employed to measure stellarpopulation differences in faint objects, such as the 4000 Å andthe Mg 2800 breaks, are disappointingly insensitive to these stellarpopulation differences. We find that the hot (T > 20,000 K) stellarcomponent responsible for the ``UV upturn'' at shorter wavelengths canhave an important influence on the mid-UV spectral range (2400-3200Å) as well. The hot component can contribute over 50% of the fluxat 2600 Å in some cases and affects both continuum colors and linestrengths. Mid-UV spectra of galaxies must be corrected for this effectbefore they can be used as age and abundance diagnostics. Of the threestellar populations studied here, M31 globular clusters and ellipticalgalaxies are more similar to each other than either is to the Galacticstellar populations defined by globular clusters and nearby stars.Similarities between the abundance-pattern differences currentlyidentified among these stellar populations and those among globularcluster stars (N, Al enhancements) present a curious coincidence thatdeserves future investigation. Based on observations with the NASA/ESAHubble Space Telescope, obtained at the Space Telescope ScienceInstitute, which is operated by the Association of Universities forResearch in Astronomy, Inc., under NASA contract NAS 5-26555.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| Absorption line gradients in the blue and near-ultraviolet spectra of bright elliptical galaxies, and implications for studies of intermediate redshift objects
Long-slit spectroscopic observations covering the wavelength interval3000 to 4000 A are used to investigate the radial behavior of atomic andmolecular absorption features in the elliptical galaxies NGC 2693, NGC3348, NGC 3379, NGC 4278, NGC 4486, and NGC 5044. There is a generaltendency for metallic absorption features to weaken and continuumindices to flatten with increasing radius, in qualitative agreement withwhat is seen at visible wavelengths. All six galaxies containsignificant (i.e., at the 3 sigma level) gradients in the 4000 A break.The rate of change of the 4000 A break with radius, Delta 4000/Deltalog(r), is correlated with Delta Mg2/Delta log(r), and thegalaxy-to-galaxy scatter in Delta 4000/Delta log(r) is larger thanexpected from experimental uncertainties alone. We compare the spectralindices of the various galaxies at the radius where Mg2 = 0.28, whichcorresponds roughly to (Fe/H) = 0, and find small galaxy-to-galaxyscatter. NGC 4486 is peculiar in that it has a very steep 4000 A breakgradient has been very different from that of most other ellipticals.The data are also used to investigate aperture effects in spectroscopicobservations of intermediate redshift galaxies. It is demonstrated thatthe failure to compensate for aperture effects in galaxies out to z =0.2 can introduce an apparent redshift dependence in the strength of the4000 A break which closely follows trends previously attributed toevolution.
| Multiplicity among solar type stars in the solar neighbourhood. I - CORAVEL radial velocity observations of 291 stars
Results obtained on stellar radial velocity of 291 stars of spectraltypes FO to G9, measured with CORAVEL spectrometers at theHaute-Provence and la Silla Observatories, are discussed. The paperdescribes the observational procedure, reduction technique, andvelocity-data calibration and presents a list of individualradial-velocity measurements. Few histograms describing the survey arealso presented.
| Multiplicity among solar-type stars in the solar neighbourhood. II - Distribution of the orbital elements in an unbiased sample
An unbiased sample of 164 primary G-dwarf stars in the solarneighborhood are studied with the aid of 4200 radial velocities obtainedduring almost 13 yrs. Several present-day distributions of the orbitalelements are derived. For systems with M(2)/M(1) above 0.1 in the nearbyG-dwarf sample, the following results are obtained: (1) The orbitalperiod distribution is unimodal and can be approximated by aGaussian-type relation with a median period of 180 yrs. (2) The shortbinaries are circularized up to orbital periods of about 11 d due to thetidal evolution effects - a result compatible with the mean age of theGalactic disk. (3) The tight binaries not affected by tidal effects (inthe range between 11 and 1000 d) may reflect the initial binaryformation process, and they have a mean eccentricity of 0.31 +/-0.04.For systems with M(2)/M(1) not greater than 0.1, the proportion of browndwarf companions among the IAU velocity standards is estimated at 10percent of the primaries, a value in good agreement with that found inthe G-dwarf sample.
| Narrow-band photometry of late-type stars. II
This paper presents extensive narrow-band photometry in the Uppsalasystem supplementing earlier published mesurements so that data now areavailable for all late-type stars brighter than V = 6.05 and a number ofgalactic cluster members. Numerous UBV and BV measurements are alsopublished. The data are used to determine relations for the predictionof UBV intrinsic colors for late-type stars from the narrow-bandmeasurements. The main purpose of the data is to constitute the basisfor the determination of solar-neighborhood space densities of late-typestars, mainly giants of different kinds; these space densities will becombined with narrow-band data for fainter stars in the north Galacticpole region to yield the decrease of space density with distance fromthe galactic plane for many kinds of late-type stars.
| Radial velocities of standard stars
Radial-velocity observations obtained over a five-year period with theMcDonald Observatory photoelectric radial-velocity spectrometer arereported for those stars not known to be velocity variable. There are259 stars included in the 1650 observations of the spectral type rangeF0 to M0 and brighter than a V of 6.5 mag. For the best-observed 134stars, the standard error of the mean velocity is typically better than+ or - 0.9 km/s. Sixteen stars are shown to be constant to a sufficientlevel to warrant standard-star status. Six possible spectroscopicbinaries are found.
| HIPPARCOS and the Nearby Stars
Not Available
| Some Cross-Reference Lists for the Catalog of Possible Nearby Stars
Not Available
| Astrometric analyses of 14 Sproul plate series
Parallaxes are presented for 15 stars of spectral type G, K, and M, withinternal errors typically one-third to nearly one-fifth of the errorsgiven in current catalogs. Two central control stars suggest that theexternal errors are nearly as small as the internal errors. Most of theplate material is from the past 15 yr and shows high telescope stabilitywith yearly mean residuals as low as 5 milliarcsec (s.e.) in someseries. Most of the series have a capability of detecting astrometricorbits with amplitudes of a few times that level and with periods fromnear one year to at least a decade. Wolf 1059 has a minimum spacevelocity of 260 km/s at the 2 sigma level.
| Radial-velocity standard stars
The paper reports the results of applying an iterative procedure devisedto establish a set of velocity standard stars for monitoring thebehavior of the Fick Observatory photoelectric radial-velocityspectrometer. Data obtained during the first three years of observationwith this instrument are used to select a set of 200 velocity standardstars brighter than 7th magnitude of spectral types from late F to earlyM. All velocities have been reduced to the Fick Observatory system.
| Photoelectric observations of Fe I line in late-type steller spectra
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1966MNRAS.133...99S&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Sárkány |
| Rektaszcenzió: | 17h02m15.30s |
| Deklináció: | +64°36'02.0" |
| Vizuális fényesség: | 6.1 |
| Távolság: | 110.497 parszek |
| RA sajátmozgás: | -20.7 |
| Dec sajátmozgás: | 32.5 |
| B-T magnitude: | 7.326 |
| V-T magnitude: | 6.202 |
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