Оглавление
Изображения
Загрузить ваше изображение
DSS Images Other Images
Публикации по объекту
The Epochs of Early-Type Galaxy Formation as a Function of Environment
The aim of this paper is to set constraints on the epochs of early-typegalaxy formation through the ``archaeology'' of the stellar populationsin local galaxies. Using our models of absorption-line indices thataccount for variable abundance ratios, we derive ages, totalmetallicities, and element ratios of 124 early-type galaxies in high-and low-density environments. The data are analyzed by comparison withmock galaxy samples created through Monte Carlo simulations taking thetypical average observational errors into account, in order to eliminateartifacts caused by correlated errors. We find that all threeparameters, age, metallicity, and α/Fe ratio, are correlated withvelocity dispersion. We show that these results are robust againstrecent revisions of the local abundance pattern at high metallicities.To recover the observed scatter we need to assume an intrinsic scatterof about 20% in age, 0.08 dex in [Z/H], and 0.05 dex in [α/Fe].All low-mass objects withM*<~1010Msolar (σ<~130kms-1) show evidence for the presence of intermediate-agestellar populations with low α/Fe ratios. About 20% of theintermediate-mass objects with1010<~M*/Msolar<~1011[110<~σ/(kms-1)<~230 both elliptical andlenticular galaxies] must have either a young subpopulation or a bluehorizontal branch. On the basis of the above relationships, valid forthe bulk of the sample, we show that the Mg-σ relation is mainlydriven by metallicity, with similar contributions from the α/Feratio (23%) and age (17%). We further find evidence for an influence ofthe environment on the stellar population properties. Massive early-typegalaxies in low-density environments seem on average ~2 Gyr younger andslightly (~0.05-0.1 dex) more metal-rich than their counterparts inhigh-density environments. No offsets in the α/Fe ratios areinstead detected. With the aid of a simple chemical evolution model, wetranslate the derived ages and α/Fe ratios into star formationhistories. We show that most star formation activity in early-typegalaxies is expected to have happened between redshifts ~3 and 5 inhigh-density environments and between redshifts 1 and 2 in low-densityenvironments. We conclude that at least 50% of the total stellar massdensity must have already formed at z~1, in good agreement withobservational estimates of the total stellar mass density as a functionof redshift. Our results suggest that significant mass growth in theearly-type galaxy population below z~1 must be restricted to lessmassive objects, and a significant increase of the stellar mass densitybetween redshifts 1 and 2 should be present, caused mainly by the fieldgalaxy population. The results of this paper further imply the presenceof vigorous star formation episodes in massive objects at z~2-5 andevolved elliptical galaxies around z~1, both observationally identifiedas SCUBA galaxies and extremely red objects, respectively.
| Star formation history in early-type galaxies - I. The line absorption indices diagnostics
To unravel the formation mechanism and the evolutionary history ofelliptical galaxies (EGs) is one of the goals of modern astrophysics. Ina simplified picture of the issue, the question to be answered iswhether they have formed by hierarchical merging of pre-existingsubstructures (maybe disc galaxies) made of stars and gas, with eachmerging event probably accompanied by strong star formation, orconversely, whether they originated from the early aggregation of lumpsof gas turned into stars in the remote past via a burst-like episodeever since followed by quiescence so as to mimic a sort of monolithicprocess. Even if the two alternatives seem to oppose each other,actually they may both contribute to shaping the final properties of EGsas seen today. Are there distinct signatures of the underlying dominantprocess in the observational data? To this aim we have examined the lineabsorption indices on the Lick system of the normal, field EGs of Tragerand the interacting EGs (pair- and shell-objects) of Longhetti et al.The data show that both normal, field and interacting galaxies have thesame scattered but smooth distribution in the Hβ versus [MgFe]plane even if the interacting ones show a more pronounced tail towardhigh Hβ values. This may suggest that a common physical cause is atthe origin of their distribution. There are two straightforwardinterpretations of increasing complexity. (i) EGs span true large rangesof ages and metallicities. A young age is the signature of theaggregation mechanism, each event accompanied by metal enrichment. Thissimple scheme cannot, however, explain other spectro-photometricproperties of EGs and has to be discarded. (ii) The bulk population ofstars is old but subsequent episodes of star formation scatter the EGsin the diagnostic planes. However, this scheme would predict anoutstanding clump at low Hβ values, contrary to what is observed.The model can be cured by supposing that the primary star formationactivity lasted for a significant fraction of the Hubble time (5<=T<= 13 Gyr) accompanied by global metal enrichment. The`younger' galaxies are more metal-rich. The later burst of starformation should be small otherwise too many high-Hβ objects wouldbe observed. Therefore, the distribution of normal, pair- andshell-galaxies in the Hβ versus [MgFe] plane is due to global metalenrichment. Even though the above schemes provide a formal explanation,they seem to be too demanding because of the many ad hoc ingredientsthat have to be introduced. Furthermore, they neglect theobservationally grounded hint that the stellar content of EGs is likelyto be enhanced in α-elements with [α/Fe] ranging from 0.1 to0.4 dex. Here we propose a new scheme, in which the bulk dispersion ofgalaxies in the Hβ versus [MgFe] plane is caused by a differentmean degree of enhancement. In this model, neither the large age rangesnor the universal enrichment law for the old component are required andthe observed distribution along Hβ is naturally recovered.Furthermore, later bursts of stellar activity are a rare event,involving only those galaxies with very high Hβ (roughly >2.5).Finally, simulations of the scatter in broad-band colours of EGs seem toconfirm that the bulk stars have formed in the remote past, and thatmergers and companion star formation in a recent past are not likely,unless the intensity of the secondary activity is very small.
| A new catalogue of ISM content of normal galaxies
We have compiled a catalogue of the gas content for a sample of 1916galaxies, considered to be a fair representation of ``normality''. Thedefinition of a ``normal'' galaxy adopted in this work implies that wehave purposely excluded from the catalogue galaxies having distortedmorphology (such as interaction bridges, tails or lopsidedness) and/orany signature of peculiar kinematics (such as polar rings,counterrotating disks or other decoupled components). In contrast, wehave included systems hosting active galactic nuclei (AGN) in thecatalogue. This catalogue revises previous compendia on the ISM contentof galaxies published by \citet{bregman} and \citet{casoli}, andcompiles data available in the literature from several small samples ofgalaxies. Masses for warm dust, atomic and molecular gas, as well asX-ray luminosities have been converted to a uniform distance scale takenfrom the Catalogue of Principal Galaxies (PGC). We have used twodifferent normalization factors to explore the variation of the gascontent along the Hubble sequence: the blue luminosity (LB)and the square of linear diameter (D225). Ourcatalogue significantly improves the statistics of previous referencecatalogues and can be used in future studies to define a template ISMcontent for ``normal'' galaxies along the Hubble sequence. The cataloguecan be accessed on-line and is also available at the Centre desDonnées Stellaires (CDS).The catalogue is available in electronic form athttp://dipastro.pd.astro.it/galletta/ismcat and at the CDS via anonymousftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/5
| A catalogue and analysis of local galaxy ages and metallicities
We have assembled a catalogue of relative ages, metallicities andabundance ratios for about 150 local galaxies in field, group andcluster environments. The galaxies span morphological types from cD andellipticals, to late-type spirals. Ages and metallicities were estimatedfrom high-quality published spectral line indices using Worthey &Ottaviani (1997) single stellar population evolutionary models. Theidentification of galaxy age as a fourth parameter in the fundamentalplane (Forbes, Ponman & Brown 1998) is confirmed by our largersample of ages. We investigate trends between age and metallicity, andwith other physical parameters of the galaxies, such as ellipticity,luminosity and kinematic anisotropy. We demonstrate the existence of agalaxy age-metallicity relation similar to that seen for local galacticdisc stars, whereby young galaxies have high metallicity, while oldgalaxies span a large range in metallicities. We also investigate theinfluence of environment and morphology on the galaxy age andmetallicity, especially the predictions made by semi-analytichierarchical clustering models (HCM). We confirm that non-clusterellipticals are indeed younger on average than cluster ellipticals aspredicted by the HCM models. However we also find a trend for the moreluminous galaxies to have a higher [Mg/Fe] ratio than the lowerluminosity galaxies, which is opposite to the expectation from HCMmodels.
| Line-strength indices and velocity dispersions for 148 early-type galaxies in different environments
We have derived high quality line-strength indices and velocitydispersions for a sample of 148 early-type galaxies in differentenvironments. The wavelength region covered by the observations (lambda=~ 4600 to 6600 Å) includes the Lick/IDS indices Hβ,Mg1, Mg2, Mgb, Fe5015, Fe5270, Fe5335, Fe5406,Fe5709, Fe5782, NaD, TiO1 and TiO2. The data areintended to address possible differences of the stellar populations ofearly-type galaxies in low- and high-density environments. This paperdescribes the sample properties, explains the data reduction andpresents the complete list of all the measurements. Most galaxies of thesample (85%) had no previous measurements of any Lick/IDS indices andfor 30% of the galaxies we present first-time determinations of theirvelocity dispersions. Special care is taken to identify galaxies withemission lines. We found that 62 per cent of the galaxies in the samplehave emission lines, as measured by the equivalent width of the [OIII]5007Å line, EW[OIII] > 0.3 Å. Tables 5 and 6 are onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/ A+A/395/431. They are also available via ftp atftp.mpe.mpg.de in the directory people/dthomas/Beuing02 or via WWW atftp://ftp.mpe.mpg.de/people/dthomas/Beuing02.
| Near-infrared surface photometry of early-type galaxies
CCD infrared (JHKs) photometry was performed on a sample of10 elliptical and 2 lenticular galaxies. Isophotal parameters,brightness profiles, integrated colors and color gradients arepresented. Color gradients found are very weak, showing bluer colorstowards the outer regions. The colors of the sample galaxies arecompatible with stellar populations like those found in metal-richclusters of the Galaxy; objects NGC 7192, NGC 7562 and NGC 7619 arecompatible with less metal-rich populations. The brightness profile ofmost galaxies is well described by the r1/4 law. The profilesof NGC 1600 and NGC 720 are described by Sérsic's law with n ~1.5 and n ~ 1.8 respectively. The infrared effective radius of theobjects studied is typically one half of its counterpart in the B band,which can be an indication that the stellar population that dominatesthe infrared emission is more concentrated in the central regions. Weshow that the sample satisfies the Fundamental Plane relation ofelliptical galaxies in the infrared, with an rms scatter of 0.20 for Jand H and 0.23 for Ks.
| Survey of the ISM in early-type galaxies. IV. The hot dust component
We present mid-IR photometric properties for a sample of 28 early-typegalaxies observed at 6.75, 9.63 and 15 mu m with the ISOCAM instrumenton board the ISO satellite. We find total mid-IR luminosities in therange (3-42) x 108 Lsun. The spectral energydistributions (SED) of the galaxies were derived using the mid-IR datatogether with previously published UV, optical and near-IR data. TheseSEDs clearly show a mid-IR emission coming from dust heated at T =~ 260K. Dust grains properties are inferred from the mid-IR colors. Themasses of the hot dust component are in the range 10-400Msun. The relationship between the masses derived from mid-IRobservations and those derived from visual extinction are discussed. Thepossible common heating source for the gas and dust is investigatedthrough the correlations between Hα and mid-IR luminosities. Basedon observations with ISO, an ESA project with instruments funded by ESAmember states (especially the PI countries: France, Germany, theNetherlands and the UK) and with participation of ISAS and NASA.
| Cold gas in elliptical galaxies
We explore the evolution of the cold gas (molecular and neutralhydrogen) of elliptical galaxies and merger remnants ordered into a timesequence on the basis of spectroscopic age estimates. We find that thefraction of cold gas in early merger remnants decreases significantlyfor ~1-2Gyr, but subsequent evolution toward evolved elliptical systemssees very little change. This trend can be attributed to an initial gasdepletion by strong star formation, which subsequently declines toquiescent rates. This explanation is consistent with the merger picturefor the formation of elliptical galaxies. We also explore the relationbetween the HI-to-H2 mass ratio and spectroscopic galaxy age,but find no evidence for a statistically significant trend. Thissuggests little net HI-to-H2 conversion for the systems inthe present sample.
| Nearby Optical Galaxies: Selection of the Sample and Identification of Groups
In this paper we describe the Nearby Optical Galaxy (NOG) sample, whichis a complete, distance-limited (cz<=6000 km s-1) andmagnitude-limited (B<=14) sample of ~7000 optical galaxies. Thesample covers 2/3 (8.27 sr) of the sky (|b|>20deg) andappears to have a good completeness in redshift (97%). We select thesample on the basis of homogenized corrected total blue magnitudes inorder to minimize systematic effects in galaxy sampling. We identify thegroups in this sample by means of both the hierarchical and thepercolation ``friends-of-friends'' methods. The resulting catalogs ofloose groups appear to be similar and are among the largest catalogs ofgroups currently available. Most of the NOG galaxies (~60%) are found tobe members of galaxy pairs (~580 pairs for a total of ~15% of objects)or groups with at least three members (~500 groups for a total of ~45%of objects). About 40% of galaxies are left ungrouped (field galaxies).We illustrate the main features of the NOG galaxy distribution. Comparedto previous optical and IRAS galaxy samples, the NOG provides a densersampling of the galaxy distribution in the nearby universe. Given itslarge sky coverage, the identification of groups, and its high-densitysampling, the NOG is suited to the analysis of the galaxy density fieldof the nearby universe, especially on small scales.
| Star formation history of early-type galaxies in low density environments. IV. What do we learn from nuclear line-strength indices?
In this paper we analyze the line-strength indices in the Lick-systemmeasured by Longhetti et al. (1998a, b) for a sample of 51 early-typegalaxies located in low density environments (LDE) and showingsignatures of fine structures and/or interactions. The sample contains21 shell-galaxies and 30 members of interacting pairs. Firstly weperform a preliminary comparison between three different sources ofcalibrations of the line strength indices, namely Buzzoni et al. (1992,1994), Worthey (1992), Worthey et al. (1994) and Idiart et al. (1995),derived from stars with different effective temperature, gravity, andmetallicity. Looking at the three indices in common, i.e. Mg2, Fe5270,and Hβ , the calibrations by Buzzoni et al. (1992, 1994), Worthey(1992) and Worthey et al. (1994) lead to mutually consistent results.The calibration of Hβ by Idiart et al. (1995) can be compared withthe previous ones only for a limited range of ages, in which goodagreement is found. Mg2 and Mgb indices predicted by the Idiart's et al.(1995) fitting functions result to be systematically lower than thoseobtained from using Worthey (1992) calibrations. Secondly, we discussthe properties of the galaxies in our sample by comparing them both withtheoretical Single Stellar Populations (SSPs) and the normal galaxies ofthe González (1993: G93) sample. The analysis is performed bymeans of several diagnostic planes. In the sigma , Mg2, Fe5270 andFe5335 space, normal, shell- and pair-galaxies have a differentbehavior. First of all, normal and pair-galaxies follow the universalsigma vs. Mg2 relation, whereas shell-galaxies lie above it; secondlythe Fe versus Mg2 relation of normal, shell- and pair-galaxies isflatter than the theoretical expectation. This fact hints forenhancement of alpha -elements with respect to solar partition ingalaxies with strong Fe indices and/or high velocity dispersion, massand luminosity in turn. In the sigma vs. Hβ plane normal galaxiesseem to follow a nice relation suggesting that objects with shallowgravitational potential have strong Hβ values (youth signature?),whereas shell- and pair-galaxies scatter all over the plane. A group ofgalaxies with deep gravitational potential and strong Hβ is found.Is this a signature of recent star formation? In the Hβ vs. [MgFe]plane, which is perhaps best suited to infer the age of the stellarpopulations, the peculiar galaxies in our sample show nearly the samedistribution of the normal galaxies in the G93 sample. There is howevera number of peculiar galaxies with much stronger Hβ . Does thismean that the scatter in the Hβ vs. [MgFe] plane, of normal, shell-and pair-galaxies has a common origin, perhaps a secondary episode ofstar formation? We suggest that, owing to their apparent youth, shell-and pair-galaxies should have experienced at least one interaction eventafter their formation. The explanation comes natural for shell- andpair-galaxies where the signatures of interactions are evident. It ismore intrigued in normal galaxies (perhaps other causes may concur).Noteworthy, the distribution in the Hβ vs. [MgFe] plane of normal,shell- and pair-galaxies is confined within a narrow strip that runssignificantly steeper than the path followed by aging SSPs. This featureis explained as due to metal enrichment always accompanying starformation. Shell-galaxies encompass the whole range of ages inferredfrom the Hβ vs. [MgFe] plane, indicating that among them recent andold interaction/acquisition events are equally probable. If shells areformed at the same time at which the rejuvenating event took place,shells ought to be long lasting phenomena. [MgFe] = sqrt { xMgb}, = (Fe5270 + Fe5335)/2 }
| A survey of the ISM in early-type galaxies. II. The dust
We present results of a CCD optical imaging survey of the dust contentin 22 early-type luminous galaxies, selected from the RC3 Catalog. Alarge fraction (75%) of the observed galaxies show significant amountsof dust. The morphology and size of the dust distribution of theobserved galaxies follows very closely that of the ionized gas. For eachgalaxy, we have used broad band V and R filters imaging to build colourmaps and determine the AV and AR extinction maps.We have found typical AV values of 0.026 and AR of0.023 and have derived (V-R) values in the range 0.49-0.68. TheAV values together with an assumption of the dust grain sizeand composition enable us to estimate the dust masses. We have studiedthe correlations between the mass of dust and the Hα , IR andL_{{B}} luminosities. Finally, we investigate the possible mechanismsresponsible for the dust emission.
| Star formation history of early-type galaxies in low density environments. V. Blue line-strength indices for the nuclear region
We analyze the star formation properties of a sample of 21 shellgalaxies and 30 early-type galaxies members of interacting pairs,located in low density environments (Longhetti et al. 1998a, 1998b). Thestudy is based on new models developed to interpret the informationcoming from `blue' Hdelta /FeI, H+K(CaII) and Delta 4000 line-strengthindices proposed by Rose (1984; 1985) and Hamilton (1985). We find thatthe last star forming event that occurred in the nuclear region of shellgalaxies is statistically old (from 0.1 up to several Gyr) with respectto the corresponding one in the sub-sample of pair galaxies (<0.1 Gyror even ongoing star formation). If the stellar activity is somehowrelated to the formation of shells, as predicted by several dynamicalmodels of galaxy interaction, shells have to be considered long lastingstructures. Since pair members show evidence of very recent starformation, we suggest that either large reservoirs of gas have to bepresent to maintain active star formation, if these galaxies are onperiodic orbits, or most of the pair members in the present sample areexperiencing unbound encounters. Table~2 is available in electronic formonly, at CDS: via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia http://cdsweb.u-strasbg.fr/Abstract.html
| A catalogue of Mg_2 indices of galaxies and globular clusters
We present a catalogue of published absorption-line Mg_2 indices ofgalaxies and globular clusters. The catalogue is maintained up-to-datein the HYPERCAT database. The measurements are listed together with thereferences to the articles where the data were published. A codeddescription of the observations is provided. The catalogue gathers 3541measurements for 1491 objects (galaxies or globular clusters) from 55datasets. Compiled raw data for 1060 galaxies are zero-point correctedand transformed to a homogeneous system. Tables 1, 3, and 4 areavailable in electronic form only at the CDS, Strasbourg, via anonymousftp 130.79.128.5. Table 2 is available both in text and electronic form.
| Star formation history of early-type galaxies in low density environments. II. Kinematics
The present paper is a companion of two others dedicated one to themeasurement of the line-strength indices \cite[(Longhetti et al.1997a)]{Lo7a} and the second to trace back the star formation history ofa sample of early-type galaxies by comparing observed indices to thepredictions of new spectro-photometric models \cite[(Longhetti et al.1997b).]{Lo7b} The sample of 51 early-type galaxies in low densityenvironments is composed of two sub-sets of galaxies: 21 shell galaxiesfrom the \cite[Malin & Carter (1983)]{Ma3} catalogue (one of whichshows double nucleous and has been considered as two separate objects)and 30 members of isolated interacting pairs from the \cite[Reduzzi& Rampazzo (1995)]{Re5} catalogue. Most of the objects show finestructures. The paper collects nuclear kinematic data together with thevelocity and velocity dispersion curves of the stellar and gaseouscomponents as a function of the distance from the galaxies centres. Thegalaxies heliocentric systemic velocity compares within -1+/- 32 kms(-1) with RC3 data, while their central velocity dispersion compareswithin 9+/- 9 km s(-1) , 10+/- 27 km s(-1) and 2+/- 33 km s(-1) with\cite[Gonzalez (1993),]{Go3} \cite[Davies et al. (1987)]{Da7} and\cite[Carter et al. (1988)]{Ca8} respectively. The detailed comparisonbetween our velocity and velocity dispersion curves and those fromseveral authors is discussed. 9 out of 22 shell galaxies nuclei showemission lines, 4 of which, using data in the literature, have lineratios characteristic of LINERs. 10 members of pairs out of 30 showemission lines. RR 331a has a Seyfert like nucleus, while for theremaining galaxies the ([O III] lambda 5007)/Hβ ratio ischaracteristic of low ionization regions. In a small fraction of theobjects the emission component is detectable outside the central value.None of the objects in the sample shows counter-rotation of the gaseousversus the stellar component. The two components appear associated,although, in two cases there is evidence that gas and stars lie ondifferent planes. This latter phenomenon could be associated toaccretion events. Emission lines in the central part of the RR 331a showa secondary component in the emission lines profile. E 2400100 has twonuclei embedded in the main body of the galaxy. The U-shape profile ofthe stellar velocity profile shows the ongoing interaction of the twonuclei. V/sigma profile of shell galaxies is, finally, discussed inrelation to the hypothesis of the accretion/merging origin of thesegalaxies. Based on observations obtained at ESO, La Silla, Chile. Dataand and kinematical profiles are available at CDS.
| Star formation history of early-type galaxies in low density environments. I. Nuclear line-strength indices
This paper is the first of a series \cite[(Longhetti et al.1997a,b)]{lon97} dedicated to the study of the star formation history inearly-type galaxies which show fine structures and/or signatures ofinteraction. It presents nuclear line-strength indices for a samplecomposed of 21 shell galaxies, from the \cite[Malin & Carter(1983)]{mal83} southern survey, and 30 members of isolated interactingpairs, from the \cite[Reduzzi & Rampazzo (1995)]{red95} catalogue,located in low density environments. The spectral range covers 3700Angstroms < lambda < 5700 Angstroms at 2.1 Angstroms FWHMresolution. We measure 16 red (lambda > 4200 Angstroms) indicesdefined by the Lick Group. Measures have been transformed into theLick-IDS ``standard'' system. The procedure has been tested on a set of5 elliptical galaxies selected from the \cite[Gonzalez (1993)]{gon93}sample. We derive also three blue (lambda < 4200) indices, namelyDelta (4000 Angstroms) defined by \cite[Hamilton (1985)]{ham85},H+K(CaII) and Hdelta /FeI defined by \cite[Rose (1984, 1985)]{ros84}.Blue indices are correlated to the age of the last starburst occurred ina galaxy \cite[(Leonardi & Rose 1996)]{leo96}. The determination ofthese indices, the estimate of the measurement errors and the correctionfor the galaxies velocity dispersions are discussed in detail. In theAppendix A we present the indices for a set of hot stars (T> 10000 K)which may be used for extending W92 fitting functions toward hightemperatures. Based on observations obtained at ESO, La Silla, Chile.Tables 1-8 are also available in electronic form at CDS and Tables 9-15are only available in electronic form at CDS: via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Total magnitude, radius, colour indices, colour gradients and photometric type of galaxies
We present a catalogue of aperture photometry of galaxies, in UBVRI,assembled from three different origins: (i) an update of the catalogueof Buta et al. (1995) (ii) published photometric profiles and (iii)aperture photometry performed on CCD images. We explored different setsof growth curves to fit these data: (i) The Sersic law, (ii) The net ofgrowth curves used for the preparation of the RC3 and (iii) A linearinterpolation between the de Vaucouleurs (r(1/4) ) and exponential laws.Finally we adopted the latter solution. Fitting these growth curves, wederive (1) the total magnitude, (2) the effective radius, (3) the colourindices and (4) gradients and (5) the photometric type of 5169 galaxies.The photometric type is defined to statistically match the revisedmorphologic type and parametrizes the shape of the growth curve. It iscoded from -9, for very concentrated galaxies, to +10, for diffusegalaxies. Based in part on observations collected at the Haute-ProvenceObservatory.
| A survey of the ISM in early-type galaxies. I. The ionized gas.
We present results of a CCD optical imaging survey of the ionized gas in73 luminous elliptical and lenticular galaxies, selected from the RC3catalog to represent a broad variety of X-ray, radio, infrared andkinematical properties. For each galaxy we have used broad-band R imagesand narrow-band images centered at the Hα and [NII] emission linesto derive the luminosity and distribution of the ionized gas. We foundthat a large fraction of E (72%) and S0 (85%) galaxies in our samplecontain ionized gas. The gas morphology appears to be rather smooth formost galaxies; however ~12% of the sample galaxies show a very extendedfilamentary structure. According to the morphology and size of the gasdistribution, the galaxies have been classified into three broad groups,named small disk (SD), regular extended (RE) and filamentary structure(F). The mean diameter of the emitting region ranges between 1 and10kpc; the derived mass of the ionized gas ranges between 10^3^ and10^5^ solar masses. A significant correlation between Hα+[NII] andX-ray luminosities is found for those galaxies (27% of the sample) forwhich we have detected ionized gas and are also listed as X-ray sources.However, there are relatively strong X-ray emitting galaxies for whichwe have not detected Hα+[NII] emission and objects which showemission-lines but are not listed either in the EINSTEIN or in the ROSATdatabases. The distribution of datapoint and upper limits in thisdiagram suggests that galaxies with warm gas are also X-ray emitters,while there are X-ray emitters without measurable Hα+[NII]emission. Similar characteristics are present in the correlation betweenthe infrared luminosity in the 12 μm band and L_Hα+[NII]_;correlations with other infrared wavelengths are weaker. A strongcorrelation was also found between the Hα+[NII] luminosity and theluminosity in the B band inside the region occupied by the line-emittinggas. We use these correlations to discuss the possible mechanismsresponsible for the gas ionization and excitation, analyzing inparticular the role of the post-AGB stars and the thermal conductionfrom the X-ray halo in providing the necessary source of ionization.
| The fundamental plane of early-type galaxies: stellar populations and mass-to-light ratio.
We analyse the residuals to the fundamental plane (FP) of ellipticalgalaxies as a function of stellar-population indicators; these are basedon the line-strength parameter Mg_2_ and on UBVRI broad-band colors, andare partly derived from new observations. The effect of the stellarpopulations accounts for approximately half the observed variation ofthe mass-to-light ratio responsible for the FP tilt. The residual tiltcan be explained by the contribution of two additional effects: thedependence of the rotational support, and possibly that of the spatialstructure, on the luminosity. We conclude to a constancy of thedynamical-to-stellar mass ratio. This probably extends to globularclusters as well, but the dominant factor would be here the luminositydependence of the structure rather than that of the stellar population.This result also implies a constancy of the fraction of dark matter overall the scalelength covered by stellar systems. Our compilation ofinternal stellar kinematics of galaxies is appended.
| A Catalog of Stellar Velocity Dispersions. II. 1994 Update
A catalog of central velocity dispersion measurements is presented,current through 1993 September. The catalog includes 2474 measurementsof 1563 galaxies. A standard set of 86 galaxies is defined, consistingof galaxies with at least three reliable, concordant measurements. It issuggested that future studies observe some of these standard galaxies sothat different studies can be normalized to a consistent system. Allmeasurements are reduced to a normalized system using these standards.
| Total and effective colors of 501 galaxies in the Cousins VRI photometric system
Total color indices (V-R)T, (V-I)T and effectivecolor indices (V-R)e, (V-I)e in the Cousins VRIphotometric system are presented for 501 mostly normal galaxies. Thecolors are computed using a procedure outlined in the Third ReferenceCatalogue of Bright Galaxies (RC3) whereby standard color curvesapproximated by Laplace-Gauss integrals are fitted to observedphotoelectric multiaperture photometry. 11 sources of such photometrywere used for our analysis, each source being assigned an appropriateweight according to a rigorous analysis of residuals of the data fromthe best-fitting standard color curves. Together with the integrated B-Vand U-B colors provided in RC3, our analysis widens the range ofwavelength of homogeneously defined colors of normal galaxies of allHubble types. We present color-color and color-type relations that canbe modeled to understand the star formation history of galaxies.
| Integrated photoelectric magnitudes and color indices of bright galaxies in the Johnson UBV system
The photoelectric total magnitudes and color indices published in theThird Reference Catalogue of Bright Galaxies (RC3) are based on ananalysis of approximately equals 26,000 B, 25,000 B-V, and 17,000 U-Bmultiaperture measurements available up to mid 1987 from nearly 350sources. This paper provides the full details of the analysis andestimates of internal and external errors in the parameters. Thederivation of the parameters is based on techniques described by theVaucouleurs & Corwin (1977) whereby photoelectric multiaperture dataare fitted by mean Hubble-type-dependent curves which describe theintegral of the B-band flux and the typical B-V and U-B integrated colorgradients. A sophisticated analysis of the residuals of thesemeasurements from the curves was made to allow for the random andsystematic errors that effect such data. The result is a homogeneous setof total magnitudes BTA total colors(B-V)T and (U-B)T, and effective colors(B-V)e and (U-B)e for more than 3000 brightgalaxies in RC3.
| Photometrically distinct nuclei in elliptical and early-type disks galaxies.
Not Available
| Dynamics of the Pavo-Indus and Grus clouds of galaxies
A study of groups of galaxies in the above regions was carried out byselecting a sample extending one magnitude deeper than previous work inthe area, complete down to 15 mag. We report new redshift determinationsfor 58 galaxies in the region and 13 other miscellaneous galaxies, basedon La Silla observations. Using a total of 266 galaxies with measuredredshifts in the Pavo-Indus and Grus clouds, we perform a new analysisof groupings following a well-tested algorithm. A total of 18 groups issingled out, most of them known from previous work, even though a fewadditional members are added. For all the groups, we have calculateddynamical parameters and M/L ratios. All groups are found to be boundaggregates, but only one group can be virialized. For the six mostpopulated examples, having at least five members, we also calculateseveral mass estimators and discuss the wide range of observed M/Lratios, which extends from nine to nearly 500 M(solar)/L(solar). Weintroduce two parameters to measure the presence of either a dominantgalaxy or internal subcondensations, respectively, and test whether anycorrelation with the M/L ratios can be detected. No clear correlationsare found.
| General study of group membership. II - Determination of nearby groups
We present a whole sky catalog of nearby groups of galaxies taken fromthe Lyon-Meudon Extragalactic Database. From the 78,000 objects in thedatabase, we extracted a sample of 6392 galaxies, complete up to thelimiting apparent magnitude B0 = 14.0. Moreover, in order to considersolely the galaxies of the local universe, all the selected galaxieshave a known recession velocity smaller than 5500 km/s. Two methods wereused in group construction: a Huchra-Geller (1982) derived percolationmethod and a Tully (1980) derived hierarchical method. Each method gaveus one catalog. These were then compared and synthesized to obtain asingle catalog containing the most reliable groups. There are 485 groupsof a least three members in the final catalog.
| Low-luminosity early-type galaxies. I - Photometry and morphology
New multiaperture photoelectric photometry in U, B, V, R, and I for 50southern low-luminosity early-type galaxies (LLEs) is presented.Asymptotic magnitude and mean surface brightness within the effectiveaperture are derived from fits to r exp 1/4 growth curves, and colorsare reduced at an effective radius for 154 galaxies. Morphological andstructural analysis of the LLE sample, based on the ESO-LV image database, shows that the average flattening of these galaxies is high. Thesample can be divided into four main categories. There is no correlationbetween the morphological type for t of not greater than -3 and any ofthe structural and geometrical properties investigated. Only a fewgalaxies show a boxy isophote shape, while a greater fraction showsdisky isophotes.
| Multiwavelength isophotal data for southern elliptical galaxies
Isophotal data derived from CCD observations made through the Danish1.5-m telescope at La Silla during 1982 are presented for 40 ellipticalgalaxies. The primary tabulated parameters include ellipticity, positionangle, the position of the ellipse center, and the fourth-order Fouriercoefficients of the normalized radial deviations. The galaxies havebeeen observed with B, V, R, I, and Gunn z filters. The data obtainedshow excellent agreement with other CCD observations.
| Southern Sky Redshift Survey - The catalog
The catalog of radial velocities for galaxies which comprise thediameter-limited sample of the Southern Sky Redshift Survey ispresented. It consolidates the data of observations carried out at theLas Campanas Observatory, Observatorio Nacional, and South AfricanAstronomical Observatory. The criteria used for the sample selection aredescribed, as well as the observational procedures and the techniqueutilized to obtain the final radial velocities. The intercomparisonbetween radial velocity measurements from different telescopes indicatesthat the final data base is fairly homogeneous with a typical error ofabout 40 km/s. The sample is at present 90 percent complete, and themissing galaxies are predominantly objects with very low surfacebrightness for which it is very difficult to obtain optical redshifts.
| Interstellar matter in early-type galaxies. I - The catalog
A catalog is given of the currently available measurements ofinterstellar matter in the 467 early-type galaxies listed in the secondedition of the Revised Shapley-Ames Catalog of Bright Galaxies. Themorphological type range is E, SO, and Sa. The ISM tracers are emissionin the following bands: IRAS 100 micron, X-ray, radio, neutral hydrogen,and carbon monoxide. Nearly two-thirds of the Es and SOs have beendetected in one or more of these tracers. Additional observed quantitiesthat are tabulated include: magnitude, colors, radial velocity, centralvelocity dispersion, maximum of the rotation curve, angular size, 60micron flux, and supernovae. Qualitative statements as to the presenceof dust or emission lines, when available in the literature, are given.Quantities derivative from the observed values are also listed andinclude masses of H I, CO, X-ray gas, and dust as well as an estimate ofthe total mass and mass-to-luminosity ratio of the individual galaxies.
| Triaxiality in disk galaxies
Thirty-two bulges of nearby spirals have been observed, to detectmisalignment between disk and bulge apparent major axes. Suchmisalignment is unequivocally present in the majority of observedobjects. This may be due to the triaxiality of disks, bulges, or both.The probability distribution function for the axial ratios is derivedunder the two extreme hypotheses, i.e., that either only disks (case I)or only bulges (case II) are triaxial: the observational data areequally well fitted by either one. Since dynamical evidence and theinternal twisting of isophotes show that bulges are triaxial, case I isunlikely, but an intermediate case cannot be ruled out. Thesedistribution functions are compared with available constraints; inparticular, that of case II is projected and compared with thedistribution of apparent ellipticities of minor-axis dust-laneellipticals and of all ellipticals. Both tests show that the observedand derived distributions are consistent.
| The plane W(Na I) X W(Mg I) - Effects of interstellar Na I in a sample of southern galaxies
Galaxy spectra from a subsample of the Southern Sky Redshift Survey databank were used to study the equivalent width plane for the lines Na Ilambda 5893 A vs Mg I lambda 5175 A. An estimate of how important thecontribution of the interstellar gas for the sodium line is compared tothat of the stellar population. The sample is made up of galaxies withmorphological types from E to Sc and are distributed up to radialvelocities of 25,000 km/s, most of them smaller than 15,000 km/s. Mostearly type galaxies with dust lanes, particularly nearly edge-on So's,present an enhancement of the Na I line. Inclined spiral galaxies tendto present enhanced Na I with respect to face-on spirals. This tendency,previously found in a smaller sample of galaxies limited to V equal toor less than 6000 km/s, is now confirmed for more distant ones. In thelarge velocity sample it shows the global bulge rather than the verynucleus; the persistence of the effect suggests that the scale height ofthe gas layer in the central disk can reach a considerable fraction ofthe bulge radius.
|
Добавить новую статью
Внешние ссылки
- - Внешних ссылок не найдено -
Добавить внешнюю ссылку
Группы:
|
Наблюдательные данные и астрометрия
Каталоги и обозначения:
|
