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Supernovae in Early-Type Galaxies: Directly Connecting Age and Metallicity with Type Ia Luminosity
We have obtained optical spectra of 29 early-type (E/S0) galaxies thathosted Type Ia supernovae (SNe Ia). We have measured absorption-linestrengths and compared them to a grid of models to extract the relationsbetween the supernova properties and the luminosity-weightedage/composition of the host galaxies. Such a direct measurement is amarked improvement over existing analyses that tend to rely on generalcorrelations between the properties of stellar populations andmorphology. We find a strong correlation suggesting that SNe Ia ingalaxies whose populations have a characteristic age greater than 5 Gyrare ~1 mag fainter at Vmax than those found in galaxies withyounger populations. We find that SN Ia distance residuals in the Hubblediagram are correlated with host-galaxy metal abundance with higher ironabundance galaxies hosting less-luminous supernovae. We thus concludethat the time since progenitor formation primarily determines theradioactive Ni production while progenitor metal abundance has a weakerinfluence on peak luminosity, but one not fully corrected by light-curveshape and color fitters. This result, particularly the secondarydependence on metallicity, has significant implications for thedetermination of the equation-of-state parameter,w=P/(ρc2), and could impact planning for futuredark-energy missions such as JDEM. Assuming no selection effects indiscovering SNe Ia in local early-type galaxies, we find a higherspecific SN Ia rate in E/S0 galaxies with ages below 3 Gyr than in olderhosts. The higher rate and brighter luminosities seen in the youngestE/S0 hosts may be a result of recent star formation and represents atail of the ``prompt'' SN Ia progenitors.
| Inaccuracies in the spectral classification of stars from the Tycho-2 Spectral Type Catalogue
We compare the spectroscopic and trigonometric parallaxes of commonstars from the Tycho-2 Spectral Type and Hipparcos Catalogues. Thiscomparison has revealed that the distance estimations for theoverwhelming majority of stars by both methods yield very similarresults. However, there is a small fraction of stars for which thedistance estimates differ significantly. It is these stars that are thesubject of our study. We have been able to find the causes of thesedifferences.
| Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters
The availability of the Hipparcos Catalogue has triggered many kinematicand dynamical studies of the solar neighbourhood. Nevertheless, thosestudies generally lacked the third component of the space velocities,i.e., the radial velocities. This work presents the kinematic analysisof 5952 K and 739 M giants in the solar neighbourhood which includes forthe first time radial velocity data from a large survey performed withthe CORAVEL spectrovelocimeter. It also uses proper motions from theTycho-2 catalogue, which are expected to be more accurate than theHipparcos ones. An important by-product of this study is the observedfraction of only 5.7% of spectroscopic binaries among M giants ascompared to 13.7% for K giants. After excluding the binaries for whichno center-of-mass velocity could be estimated, 5311 K and 719 M giantsremain in the final sample. The UV-plane constructed from these datafor the stars with precise parallaxes (σπ/π≤20%) reveals a rich small-scale structure, with several clumpscorresponding to the Hercules stream, the Sirius moving group, and theHyades and Pleiades superclusters. A maximum-likelihood method, based ona Bayesian approach, has been applied to the data, in order to make fulluse of all the available stars (not only those with precise parallaxes)and to derive the kinematic properties of these subgroups. Isochrones inthe Hertzsprung-Russell diagram reveal a very wide range of ages forstars belonging to these groups. These groups are most probably relatedto the dynamical perturbation by transient spiral waves (as recentlymodelled by De Simone et al. \cite{Simone2004}) rather than to clusterremnants. A possible explanation for the presence of younggroup/clusters in the same area of the UV-plane is that they have beenput there by the spiral wave associated with their formation, while thekinematics of the older stars of our sample has also been disturbed bythe same wave. The emerging picture is thus one of dynamical streamspervading the solar neighbourhood and travelling in the Galaxy withsimilar space velocities. The term dynamical stream is more appropriatethan the traditional term supercluster since it involves stars ofdifferent ages, not born at the same place nor at the same time. Theposition of those streams in the UV-plane is responsible for the vertexdeviation of 16.2o ± 5.6o for the wholesample. Our study suggests that the vertex deviation for youngerpopulations could have the same dynamical origin. The underlyingvelocity ellipsoid, extracted by the maximum-likelihood method afterremoval of the streams, is not centered on the value commonly acceptedfor the radial antisolar motion: it is centered on < U > =-2.78±1.07 km s-1. However, the full data set(including the various streams) does yield the usual value for theradial solar motion, when properly accounting for the biases inherent tothis kind of analysis (namely, < U > = -10.25±0.15 kms-1). This discrepancy clearly raises the essential questionof how to derive the solar motion in the presence of dynamicalperturbations altering the kinematics of the solar neighbourhood: doesthere exist in the solar neighbourhood a subset of stars having no netradial motion which can be used as a reference against which to measurethe solar motion?Based on observations performed at the Swiss 1m-telescope at OHP,France, and on data from the ESA Hipparcos astrometry satellite.Full Table \ref{taba1} is only available in electronic form at the CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/430/165}
| Observations of Star-Forming Regions with the Midcourse Space Experiment
We have imaged seven nearby star-forming regions, the Rosette Nebula,the Orion Nebula, W3, the Pleiades, G300.2-16.8, S263, and G159.6-18.5,with the Spatial Infrared Imaging Telescope on the Midcourse SpaceExperiment (MSX) satellite at 18" resolution at 8.3, 12.1, 14.7, and21.3 μm. The large angular scale of the regions imaged (~7.2-50deg2) makes these data unique in terms of the combination ofsize and resolution. In addition to the star-forming regions, twocirrus-free fields (MSXBG 160 and MSXBG 161) and a field near the southGalactic pole (MSXBG 239) were also imaged. Point sources have beenextracted from each region, resulting in the identification over 500 newsources (i.e., no identified counterparts at other wavelengths), as wellas over 1300 with prior identifications. The extended emission from thestar-forming regions is described, and prominent structures areidentified, particularly in W3 and Orion. The Rosette Nebula isdiscussed in detail. The bulk of the mid-infrared emission is consistentwith that of photon-dominated regions, including the elephant trunkcomplex. The central clump, however, and a line of site toward thenorthern edge of the cavity show significantly redder colors than therest of the Rosette complex.
| Oxygen line formation in late-F through early-K disk/halo stars. Infrared O I triplet and [O I] lines
In order to investigate the formation of O I 7771-5 and [O I] 6300/6363lines, extensive non-LTE calculations for neutral atomic oxygen werecarried out for wide ranges of model atmosphere parameters, which areapplicable to early-K through late-F halo/disk stars of variousevolutionary stages.The formation of the triplet O I lines was found to be well described bythe classical two-level-atom scattering model, and the non-LTEcorrection is practically determined by the parameters of theline-transition itself without any significant relevance to the detailsof the oxygen atomic model. This simplifies the problem in the sensethat the non-LTE abundance correction is essentially determined only bythe line-strength (Wlambda ), if the atmospheric parametersof Teff, log g, and xi are given, without any explicitdependence of the metallicity; thus allowing a useful analytical formulawith tabulated numerical coefficients. On the other hand, ourcalculations lead to the robust conclusion that LTE is totally valid forthe forbidden [O I] lines.An extensive reanalysis of published equivalent-width data of O I 7771-5and [O I] 6300/6363 taken from various literature resulted in theconclusion that, while a reasonable consistency of O I and [O I]abundances was observed for disk stars (-1 <~ [Fe/H] <~ 0), theexistence of a systematic abundance discrepancy was confirmed between OI and [O I] lines in conspicuously metal-poor halo stars (-3 <~[Fe/H] <~ -1) without being removed by our non-LTE corrections, i.e.,the former being larger by ~ 0.3 dex at -3 <~ [Fe/H] <~ -2.An inspection of the parameter-dependence of this discordance indicatesthat the extent of the discrepancy tends to be comparatively lessenedfor higher Teff/log g stars, suggesting the preference ofdwarf (or subgiant) stars for studying the oxygen abundances ofmetal-poor stars.Tables 2, 5, and 7 are only available in electronic form, at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/402/343 and Table\ref{tab3} is only available in electronic form athttp://www.edpsciences.org
| The association of IRAS sources and 12CO emission in the outer Galaxy
We have revisited the question of the association of CO emission withIRAS sources in the outer Galaxy using data from the FCRAO Outer GalaxySurvey (OGS). The availability of a large-scale high-resolution COsurvey allows us to approach the question of IRAS-CO associations from anew direction - namely we examined all of the IRAS sources within theOGS region for associated molecular material. By investigating theassociation of molecular material with random lines of sight in the OGSregion we were able to construct a quantitative means to judge thelikelihood that any given IRAS-CO association is valid and todisentangle multiple emission components along the line of sight. Thepaper presents a list of all of the IRAS-CO associations in the OGSregion. We show that, within the OGS region, there is a significantincrease ( ~ 22%) in the number of probable star forming regions overprevious targeted CO surveys towards IRAS sources. As a demonstration ofthe utility of the IRAS-CO association table we present the results ofthree brief studies on candidate zone-of-avoidance galaxies with IRAScounterparts, far outer Galaxy CO clouds, and very bright CO clouds withno associated IRAS sources. We find that ~ 25% of such candidate ZOAGsare Galactic objects. We have discovered two new far outer Galaxystar-forming regions, and have discovered six bright molecular cloudsthat we believe are ideal targets for the investigation of the earlieststages of sequential star formation around HII regions. Finally, thispaper provides readers with the necessary data to compare othercatalogued data sets with the OGS data.Tables 1, 2 and A1 are only available in electronic form at the CDS viaanonymous ftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/1083
| 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.
| A New Method for Obtaining Stellar Velocity Distributions from Absorption-Line Spectra - Unresolved Gaussian Decomposition
We have developed a new algorithm for extracting the line-of-sightvelocity distributions (LOSVDs) of galaxies from the broadening ofabsorption lines in their spectra relative to those of a stellar`template'. This method models the LOSVD as the sum of a set of Gaussiandistributions uniformly spaced in velocity. By choosing the dispersion,{DELTA}v, of these Gaussians so that the separate components areunresolved according to the Rayleigh criterion, such a sum can model anyLOSVD that is smooth on scales smaller than {DELTA}v. The velocity scaleon which the LOSVD is forced to be smooth is thus set explicitly by theuser. The algorithm then involves solving for the amplitudes of theindividual components to produce the LOSVD that, when convolved with thestellar template, best reproduces the observed galaxy spectrum in aleast-squares sense. This procedure is an example of quadraticprogramming for which efficient algorithms exist, and, since all of theconvolutions in the analysis involve similar Gaussians, thecomputational expense in calculating the model is also small. Thephysical constraint that the LOSVD must be non-negative can be readilyincluded in the quadratic programming, and the method allows an explicittreatment of the errors in the derived LOSVD. Monte Carlo tests showthat this algorithm can, indeed, efficiently extract a wide range ofLOSVDs from absorption- line spectra with attainable signal-to-noiseratios. Application to the early-type disc galaxy UGC 12591 illustratesthe potential of this approach for constraining dynamical models ofgalaxies.
| An improved metal abundance calibration for the Washington system
The determination of metal abundances for individual giants fromWashington photometry is revised, with several significant improvementsincorporated. The solar-abundance two-color relations are revamped withthe inclusion of new observations of a large sample of solar-abundancegiants with small reddenings, especially those with late-K spectraltypes. The new relations are very similar to the original ones derivedin C76 except for a zero-point offset. A new temperature index, M-T2, isinvestigated, as well as a new abundance index, C-T1, in addition to thestandard indices. The M-T2 index has a much broader baseline and thus amuch larger range than T1-T2, and is therefore less susceptible tophotometric errors. The significant decrease in abundance sensitivityfor cooler stars, suspected by previous investigations, is confirmed byincluding observations of a number of giants with a range in temperaturein each of a large sample of open and globular clusters. A procedure forcorrecting the abundance indices for cool stars is derived whichsignificantly improves the metallicity determination.
| JHK photometry of population I CN-rich field giants
IR JHK photometry has been obtained for a sample of CN-rich field redgiants. It is found that these giants segregate according to metallicityor CN band strength in the (J-H), (H-K) two-color diagram. A delta (H-K)color-excess index is presented, which correlates with the strength ofthe 4215 wavelength CN band as measured by the delta C(m) index of theDDO photometric system (McClure, 1970). The sensitivity of delta (H-K)as a metal abundance indicator is shown to be relatively small. It issuggested that the CN-rich field giants have colors comparable to manyof the metal-rich giants in the Galactic bulge studied by Whitford andRich (1983), although a few of the bulge giants appear to have higherabundances.
| A comparison between Washington and DDO photometry of field red giants
Washington CMT1T2 photometry of a sample of field red giants is comparedwith DDO colors obtained by McClure (1970) and Janes (1975) to determinethe relative sensitivities of the metallicity indices of the twosystems. Washington line-blanketing indices delta(M-T1) and delta(C-M)were derived, and found to correlate very well with each other, inaddition to correlating quite well with the DDO metallicity index.Furthermore, any N/A or C/A abundance variations which may exist amongthe present sample of old disk giants do not appear to significantlyeffect the delta(C-M) index. The study indicates that delta(C-M) shouldprovide a useful photometric metal abundance indicator, and is capableof providing estimates accurate to about + or - 0.2 dex over the Fe/Habundance range of +0.4 to -0.8.
| A survey of galaxy redshifts. I - Data reduction techniques
A magnitude-limited redshift survey of galaxies having B magnitudes nofainter than 14.5, galactic latitudes no less than 40 deg, andnonnegative declinations is currently being undertaken. This paperpresents in some detail the methods of data reduction, which are basedon cross correlation against filtered templates. Expressions arepresented for the uncertainty of a measured redshift, for the internalbroadening of the object, and for the uncertainty of this broadening.Comparison of the optical data with previously published 21-cm datashows no systematic errors and yields excellent agreement with theinternal error analysis. The method of analyzing velocity dispersions isquite promising for further application. A series of spectra arepresented as examples to show the power and limitations of thecorrelation techniques.
| Liste de vitesses radiales mesurees AU spectrographe coude a fente dutelescope de 193 CM (dispersions de 40 et 19,5 A/mm).
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974A&AS...16..359F&db_key=AST
| Stars with Strong Cyanogen Absorption
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971ApJ...163...75S&db_key=AST
| A photoelectric investigation of strong cyanogen stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1970AJ.....75...41M&db_key=AST
| Etude pour chaque champ de l'absorption et de la repartition des vitesses radiales EN fonction de la distance.
Not Available
| La mesure des vitesses radiales au prisme objectif - X - 4e liste de vitesses radiales déterminées au prisme objectif à vision directe
Not Available
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