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|The Chemical Properties of Milky Way and M31 Globular Clusters. II. Stellar Population Model Predictions|
We derive ages, metallicities, and abundance ratios ([α/Fe]) fromthe integrated spectra of 23 globular clusters in M31 by employingmultivariate fits to two different stellar population models. We alsoperform a parallel analysis on 21 Galactic globular clusters as aconsistency check and in order to facilitate a differential analysis.Our analysis shows that the M31 globular clusters separate into threedistinct components in age and metallicity; we identify an old,metal-poor group (seven clusters), an old, metal-rich group (10clusters), and an intermediate-age (3-6 Gyr), intermediate-metallicity([Z/H]~-1) group (six clusters). This third group is not identified inthe Galactic globular cluster sample. We also see evidence that the old,metal-rich Galactic globular clusters are 1-2 Gyr older than theircounterparts in M31. The majority of globular clusters in both samplesappear to be enhanced in α-elements, but the degree of enhancementis rather model-dependent. The intermediate-age globular clusters appearto be the most enhanced, with [α/Fe]~0.4. These clusters areclearly depressed in CN with respect to the models and the bulk of theM31 and Milky Way sample. Compared with the bulge of M31, M32, and NGC205, these clusters most resemble the stellar populations in NGC 205 interms of age, metallicity, and CN abundance. We infer horizontal branchmorphologies for the M31 clusters using the Rose Ca II index anddemonstrate that blue horizontal branches are not leading to erroneousage estimates in our analysis. We discuss and reject as unlikely thehypothesis that these objects are in fact foreground stars contaminatingthe optical catalogs. The intermediate-age clusters have generallyhigher velocities than the bulk of the M31 cluster population.Spatially, three of these clusters are projected onto the bulge region,and the remaining three are distributed at large radii. We discuss theseobjects within the context of the build-up of the M31 halo and suggestthat these clusters possibly originated in a gas-rich dwarf galaxy,which may or may not be presently observable in M31.
|The ISOPHOT 170 μm Serendipity Survey II. The catalog of optically identified galaxies%|
The ISOPHOT Serendipity Sky Survey strip-scanning measurements covering≈15% of the far-infrared (FIR) sky at 170 μm were searched forcompact sources associated with optically identified galaxies. CompactSerendipity Survey sources with a high signal-to-noise ratio in at leasttwo ISOPHOT C200 detector pixels were selected that have a positionalassociation with a galaxy identification in the NED and/or Simbaddatabases and a galaxy counterpart visible on the Digitized Sky Surveyplates. A catalog with 170 μm fluxes for more than 1900 galaxies hasbeen established, 200 of which were measured several times. The faintest170 μm fluxes reach values just below 0.5 Jy, while the brightest,already somewhat extended galaxies have fluxes up to ≈600 Jy. For thevast majority of listed galaxies, the 170 μm fluxes were measured forthe first time. While most of the galaxies are spirals, about 70 of thesources are classified as ellipticals or lenticulars. This is the onlycurrently available large-scale galaxy catalog containing a sufficientnumber of sources with 170 μm fluxes to allow further statisticalstudies of various FIR properties.Based on observations with ISO, an ESA project with instruments fundedby ESA Member States (especially the PI countries: France, Germany, TheNetherlands and the UK) and with the participation of ISAS and NASA.Members of the Consortium on the ISOPHOT Serendipity Survey (CISS) areMPIA Heidelberg, ESA ISO SOC Villafranca, AIP Potsdam, IPAC Pasadena,Imperial College London.Full Table 4 and Table 6 are only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/422/39
|Arcsecond Positions of UGC Galaxies|
We present accurate B1950 and J2000 positions for all confirmed galaxiesin the Uppsala General Catalog (UGC). The positions were measuredvisually from Digitized Sky Survey images with rms uncertaintiesσ<=[(1.2")2+(θ/100)2]1/2,where θ is the major-axis diameter. We compared each galaxymeasured with the original UGC description to ensure high reliability.The full position list is available in the electronic version only.
|An image database. II. Catalogue between δ=-30deg and δ=70deg.|
A preliminary list of 68.040 galaxies was built from extraction of35.841 digitized images of the Palomar Sky Survey (Paper I). For eachgalaxy, the basic parameters are obtained: coordinates, diameter, axisratio, total magnitude, position angle. On this preliminary list, weapply severe selection rules to get a catalog of 28.000 galaxies, wellidentified and well documented. For each parameter, a comparison is madewith standard measurements. The accuracy of the raw photometricparameters is quite good despite of the simplicity of the method.Without any local correction, the standard error on the total magnitudeis about 0.5 magnitude up to a total magnitude of B_T_=17. Significantsecondary effects are detected concerning the magnitudes: distance toplate center effect and air-mass effect.
|KISO survey for ultraviolet-excess galaxies. X.|
Presented here are the tenth list and identification charts of theultraviolet-excess galaxies which have been detected on the multi-colorplates taken with the Kiso Schmidt telescope for 10 survey fields. Inthe sky area of some 300 square degrees 490 objects are catalogued downto the photographic magnitude of about 18.
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