Globular Cluster Formation

Do Globular Clusters Harbor Black Holes？佚名【期刊名称】《天文和天体物理学研究》【年(卷),期】2001(001)004【摘要】It has been firmly established that there exists a tight correlation be-tween the mass of the central black hole and velocity dispersion (or luminosity) in elliptical galaxies, "pseudobulges" and bulges of galaxies, although the nature of this correlation still remains unclear. We explore the possibility of extrapolating such a correlation to less massive, spherical systems like globular clusters. In par-ticular, motivated by the apparent success in the globular cluster M15, we present an estimate of the central black hole mass for a number of globular clusters with available velocity dispersion data.【总页数】5页(P291-295)【正文语种】中文【中图分类】P14【相关文献】1.The Quantization of Black Holes, Lower Mass Limit, Temperature, and Lifetime of Black Holes in a Simple Way [J], Sirus Arya Enejad2.Black Hole Clusters: The Dark Matter [J], Kenneth Dalton3.Has LIGO detected primordial black hole dark matter?——tidaldisruption in binary black hole formation [J], Yuan Gao;Xiao-Jia Zhang;Meng Su4.How a Laser Physics Induced Kerr-Newman Black Hole Can Release Gravitational Waves without Igniting the Black Hole Bomb (Explosion of a Mini Black Hole in a Laboratory) [J], Andrew Walcott Beckwith5.Looking at Quantization Conditions, for a Wormhole Wavefunction, While Considering Differences between Magnetic Black Holes, Versus Standard Black Holes as Generating Signals from a Wormhole Mouth [J], Andrew Beckwith因版权原因，仅展示原文概要，查看原文内容请购买。

银河科技名词定义中文名称：银河英文名称：Milky Way定义：地球上观测者所看到的银河系主体在天球上的投影；在晴朗夜空中呈现为一条边界不规则的乳白色亮带。

所属学科：天文学（一级学科）；恒星和银河系（二级学科）本内容由全国科学技术名词审定委员会审定公布展开编辑本段基本信息yín hé银河编辑本段基本解释完整地环绕天球伸展的一条宽而发银河风光集萃(18张)亮的不规则光带,看起来像一条河,银河只在晴天夜晚可见,它是由无数暗星(恒星)的光引起的银河不是银河系，而是银河系的一部分。

投影在天上时，地球上所能看到的亮带。

可参考“银河系”词条以区别二者。

编辑本段详细解释1. 晴天夜晚，天空呈现的银白色的光带。

银河由大量恒星构成。

古亦称云汉，又名天河、天汉、星河、银汉。

隋江总《内殿赋新诗》：“织女今夕渡银河，当见新秋停玉梭。

” 唐李白《望庐山瀑布》诗：“飞流直下三千尺，疑是银河落九天。

” 明孙仁孺《东银河风光欣赏(18张)郭记·钻穴隙》：“到而今可是难依傍，只落得一水银河隔两厢。

” 杨沫《青春之歌》第一部第二三章：“夏夜，天上缀满了闪闪发光的星星，像细碎的流沙铺成的银河斜躺在青色的天宇上。

”2. 道教称眼睛为银河。

宋赵崇绚《鸡肋·银河》：“道家以目为银河。

”一本作“ 银海”。

3. 古代一种容量很大的银质饮器。

编辑本段银河简介银河[1]（Milky Way），我国民间又称“天河”、“天汉”。

它看起来像一条白茫茫的亮带，从东北向西南方向划开整个天空。

在银河里有许多小光点，就像撒了白色的粉末一样，辉映成一片。

实际上一颗白色粉末就是一颗巨大的恒星，银河就是由许许多多恒星构成的。

太阳是其中的一颗恒星。

像太阳这样的恒星在银河中有２０００多亿颗很多恒星有卫星。

在太空俯视银河，看到的银河像个旋涡。

晴朗的夜空，当你抬头仰望天空的时候，不仅能看到无数闪闪发光的星星，还能看到一条淡淡的纱巾似靠近银心的半人马座[2]的光带跨越整个天空，好像天空中的一条大河，夏季成南北方向，冬季接近于东西方向，那就是银河。

a r X i v :a s t r o -p h /9608082v 1 13 A u g 1996A&A manuscript no.(will be inserted by hand later)Send offprint requests to :M.Kissler–Patig (Bonn)⋆Based on data collected at the Las Campanas Observatory,Chile,run by the Carnegie InstitutionsKey words:globular cluster systems –globular clus-ters –elliptical galaxies –galaxies:individual:NGC 1399,NGC 1374,NGC 1379,NGC 1387,NGC 1427–galax-ies:clusters:individual:Fornax2Globular cluster systems in FornaxTable1.General data of our target galaxies,all members of the Fornax galaxy cluster,taken from Tully(1988),Poulain(1988), and Poulain&Nieto(1994)NGC1374033516-351335236.36-54.29E111.20 1.201105NGC1379033303-352626236.72-54.13E011.20 1.191239NGC1387033657-353023236.82-53.95S010.81 1.301091NGC1399033829-352658236.71-53.64E09.27 1.251294NGC1427034219-352336236.60-52.85E311.04 1.151416Galaxy Filter Obs.date Exposure time seeing not be considered in the following:several I exposures of the SWfield were corrupted,while the SEfield includes part of NGC1404(another member of Fornax),which makes the allocation of globular clusters to the one or the other galaxy confusing.2.2.The reductionAll reductions were done in IRAF.Bias frames were sub-tracted and skyflat–fields of different nights were aver-aged toflatten the images better than1%.The different long exposures were then combined with a sigma clipping algorithm,to remove the cosmetics from thefinal frames.Object search,photometry,and the determination of the completeness factors were done with the DAOPHOT II version in IRAF.For all galaxies we computed an isophotal model in eachfilter(using the STSDAS pack-age isophote)that we subtracted from ourfinal long ex-posure to obtain aflat background for the object search and photometry.The nights of the26,27and29were photometric and the calibration was done via typically15-30standard stars from the Landolt(1992)list,taken throughout the nights, by which our Bessell V colors were transformed to John-son V.In the middle of the night of the28th cirrus passed. Frames taken at that time were calibrated via aperture photometry on the galaxy published by Poulain(1988), and Poulain&Nieto(1994)and cross–checked with over-lapping frames in the case of NGC1399.All other calibra-tions were also inter–compared and found compatible with the aperture photometry values for the individual galax-ies.Table3shows ourfinal coefficients for the calibration equations:V inst=V+v1+v2·X V+v3·(V−I)I inst=I+i1+i2·X I+i3·(V−I)where instrumental magnitudes are normalized to1sec-ond and given with an offset of25mag.The completeness calculations were done by standard artificial star experiments.We added typically10000stars over many runs on a long exposure and repeated the re-duction steps starting with the objectfinding.The com-pleteness values are given in detail in Fig.1of Paper I. The completeness limit of50%is reached at V≃23.5 mag,I≃22.5mag for our four normal galaxies,0.5magGlobular cluster systems in Fornax3 Table3.Calibration coefficients for our different nights.Col-umn5lists the RMS of the difference between our standardmagnitudes and our calibrated ones26.9.1.718±.0180.100±.012−0.019±.0070.02027.9.1.671±.0090.133fixed−0.020±.0090.02428.9.1.713±.0180.101±.012−0.018±.0070.02029.9.1.668±.0090.133fixed−0.020±.0090.02426.9.2.077±.0120.038±.008−0.013±.0050.01227.9.2.065±.0050.047fixed−0.017±.0050.01128.9.2.069±.0160.041±.010−0.006±.0070.01329.9.2.066±.0070.047fixed−0.015±.0060.0154Globular cluster systems in FornaxTable4.Number of globular clusters around our target galaxies.Column1lists the name of the galaxy,column2the background corrected counts down to the turn–over of the GCLF together with the errors from the background correction and the error in the assumed turn–over.The measured turn–over value of the GCLF is shown in column3,column4and5list the uncovered area towards the center of the galaxies and the correction,column6lists the correction for the area beyond120′′from the center,column7and8give the total amount of globular clusters within120′′and around the galaxycounts from the GCLF in Vcounts from the GCLF in ITable5.Specific frequency for our target galaxies.Column1lists the name of the galaxy,column2the derived distancemodulus,column3the absolute magnitude in V,column4the total number of globular clusters N t,column5the specificfrequency S NNGC137431.0±.2−19.8±.2410±824.9±1.3NGC137931.1±.2−19.9±.2314±633.4±0.9NGC138731.0±.2−20.2±.2389±1103.2±1.1NGC142731.0±.2−20.0±.2510±875.1±1.3NGC139931.0±.2−21.7±.25940±57012.4±3.0Globular cluster systems in Fornax5Fig.2.Histogram of the globular cluster color distribution in (V −I )around NGC 1374,NGC 1379,NGC 1387,and NGC 1427.The solid line is the gaussian fit to the distribution,the dotted one shows the broadening from the errors in (V −I )alonethe intrinsic dispersion of the distributions must be less than 0.1mag.We performed the KMM test proposed by Ashman et al.(1994),as well as fits with multiple gaus-sians,in order to detect multi–modality in the distribu-tions,but in no case the hypothesis of an unimodal distri-bution could be rejected.While the width of the distribution is almost identical for these four galaxies,the median color slightly differs.We assumed E (B −V )=0.0towards Fornax (Burstein &Heiles 1982),and derived median (V −I )colors of the globular clusters shown in Table 6,together with a median metallicity.Deriving metallicities from broadband colors is com-plicated by second parameter effects:age and metallicity can hardly be disentangled.For similar ages and metallic-ities,the V −I color of galactic globular clusters spread over about 0.2mag.From the relatively red (V −I >0.8)mean colors,the quite narrow color distributions,the fact that we see no peculiarities in the luminosity functions of the globular clusters,and that there is no sign for any recent mergers,we are encouraged to assume that the globular clusters in these four galaxies are older then 10Gyr.With this assumption on age we can roughly convert our colors to metallicities using the empirical color–to–metallicity rela-tion found for the Milky Way globular clusters.We updated the color–metallicity relation given in Couture et al.(1990),using the Mc Master catalogue (Harris 1996)of Milky Way globular clusters.Figure 3shows the metallicity of all the galactic globular clusters with a reddening E (B −V )less than 0.4(60candidates)plotted against their (V −I )0color,that we corrected for extinction assuming E (V −I )=1.38×E (B −V )(Taylor 1986).The best linear fit gives the relation:(V −I )0=0.15(±0.02)[Fe/H]+1.13(±0.03)This is valid,strictly speaking,only in the range 0.7<(V −I )<1.1.A direct comparison to the colors of theTable 6.Median V −I colors of the globular clusters around NGC 1374,NGC 1379,NGC 1387,and NGC 1379;as well as derived median metallicitiesNGC 13741.10±0.03−0.2±0.3NGC 13791.17±0.030.3±0.3NGC 13871.20±0.060.5±0.4NGC14271.03±0.03−0.7±0.36Globular cluster systems in Fornax0.60.811.21.4-2.5-2-1.5-1-0.5Fig.3.Metallicity versus (V −I )color for the globular clusters in the Milky Way with E (B −V )<0.4.Dots are bulge clusters,circles are halo clusters,the line shows the best linearfitFig.4.Histogram over the (V −I )color of the globular clusters in the Milky Way.The dashed region marks the contribution of the halo clusters,the black ones that of the bulgeThis is comparable to the intrinsic dispersion of the color distributions of our galaxies,and corresponds to a range of metallicity from [F e/H ]=−2.4to 0.2dex.Thus,from the colors alone,accurate metallicities can-not be derived,but we can conclude that:–All our early-type galaxies have median colors of their globular clusters redder than that of the Milky Way.Assuming old globular cluster populations,this would mean average metallicities of the globular clusters ranging from slightly richer than the Milky Way halo (for NGC 1427)to about solar (for NGC 1379and NGC 1387).–There is no clear evidence for multiple populations,the range of metallicities for the globular clusters in eachgalaxy could span 2dex in [Fe/H]as in the Milky Way,but is concentrated around a median value.–The median color for globular clusters in all the galax-ies is bluer by about 0.1mag in (V −I )than the inte-grated galaxy light,as already noticed in all galaxies observed up to date,but all our galaxies possess also globular clusters as red as the galaxy itself.4.2.The globular cluster colors in NGC 1399For NGC 1399we considered all the globular clusters in the NE and NW fields obeying our selection criteria.Fig-ure 5shows the color distribution of the globular clusters with errors in V −I less than 0.1mag.Here the best gaus-sian fit returns a width of σ=0.22,three times as large as expected from the errors only.For the sample com-posed by all globular clusters in the NE and NW field the KMM test rejects the unimodal hypothesis (with a confi-dence over 95%)if we impose dispersions of the color dis-tributions comparable to the dispersions observed in our normal galaxies (σ≃0.12),and favors two populations centered on V −I =0.99and V −I =1.18(correspond-ing to [Fe/H]=−0.9and 0.3dex according to our relation in the previous section).We note that the globular clus-ters do not span a much wider range of colors than in the other galaxies,but rather populate all colors more homo-geneously,i.e.they are no globular clusters with peculiar colors in NGC 1399compared to the other galaxies.From Washington photometry Ostrov et al.(1993)also derived multiple peaks in the color distribution.They find two groups,at [Fe/H]=−1.5and −0.9,as well as a pos-sible third group near −0.2dex.The shift in the color to metallicity conversion between our results demonstrates how difficult metallicity estimates are from broad band colors alone.The results from Washington photometry are probably more reliable than from the less metal sensitive V,I colors.The main result here is the confirmation of at least two groups of globular clusters in the color distribu-tion.This would suggest that two or more distinct globular cluster enrichment or formation epochs/mechanisms hap-pened in NGC 1399.4.3.A composite color distributionAs an experiment we constructed an artificial color dis-tribution with all globular clusters found around NGC 1374,NGC 1379,NGC 1387,and NGC 1427with errors in V −I <0.1mag.This is equivalent to the sum of the four histograms shown in Sect.4.1.The resulting composite color distribution is shown in Fig.6.We performed the same test on it as for the other distributions:a single gauss fit returns a width of σ=0.31;the KMM test favors a double gauss fit with 99%confi-dence if we impose individual width of σ=0.12.This color distribution would probably be classified as bi–modal,inGlobular cluster systems in Fornax7 Fig.5.Color distributions for the globular clusters in the NE(upper panel)and NW(lower panel)fields around NGC1399.The solid line is a free gaussianfit and returns a dispersionof0.22,while the dotted line shows the broadening expectedfrom our errors in photometryaloneposite histogram of the(V−I)colors of all theglobular clusters with a V−I error less than0.1mag in NGC1374,NGC1379,NGC1387,and NGC1427.The distributionseems to be bi–modal but is based on four systemscase of real data,while it is composed of four globularcluster systems.We take it as a word of caution,thatbroad and multi–modal color distribution might hide amuch more complex history than a single merger eventbetween two galaxies,as Ashman&Zepf(1992)proposein afirst approximation.4.4.Color gradientsWe present the radial color distributions of the globularclusters in Fig.7.The globular clusters plotted are thesame as used for the color distributions in the sectionsabove,i.e.objects that match our criteria for point likesources have an error in V−I of less than0.1mag,andare closer than120′′(425′′in the case of NGC1399)tothe center of the parent galaxy.Color gradients inglobu-Fig.7.Color gradients for ourfive target galaxies.Plots ex-tend to120′′for NGC1374,NGC1379,NGC1387,and NGC1427;to425′′for NGC1399.Errorbars show the dispersionaround the medianlar cluster systems is a topic of much debate.Where theyare found,such gradients are small,typically of the or-der of0.1to0.3mag in common broad band indices overhundreds of arcseconds radius(e.g.in M87,Lee&Geisler1993,in M49and NGC4649,Couture et al.1991,in NGC3923Zepf et al.1995,or in NGC3311Secker et al.1995).For most galaxies where such a gradient is found,anotherstudy exists quoting a non–detection.The most extensive data to date are probably fromGeisler et al.(1996),who recently re–examined the glob-ular cluster system of M49with deep Washington pho-tometry,and clearly showed a color gradient.However,the gradient is rather due to a different mixture of twopopulations in the inner and outer parts than to a steadyincrease of metallicity to the center as interpreted by au-thors in the past.The gradient in M49is of the order of0.4∆[Fe/H]/∆logR.This would translate into0.06∆(V−I)/∆logR according to our relation of Sect.4.1,or∆(V−I)=0.12to0.16mag over the range studied in our cases.We are therefore clearly not sensitive enough to detectsuch gradients in our data,and can only exclude gradients8Globular cluster systems in Fornaxas large a0.15∆(V−I)/∆logR(or1.0∆[F e/H]/∆logR) for our galaxies.One would need very good photome-try a couple of magnitudes deeper in a sensitive system (e.g.Washington or B and I Johnson–Cousins,Geisler et al.1996)tofind gradients,if present,in the globular clus-ter systems studied here.Bridges et al.(1991)found a decrease of0.2mag in B−V from1′to3′of the center in NGC1399.Over this range,the increase might also exists in our data,but is smaller than the scatter and can in no case be extrapolated further out.An interesting characteristic of the globular clusters in NGC1399might be noticed:the large dispersion of colors derived in Sect.4.2exists at all radii,as in the case of M49 (Geisler et al.1996).5.Spatial distributions5.1.The angular distributionsWe looked for any anisotropic distribution of globular clus-ters around NGC1374,NGC1379,NGC1387,and NGC 1427.No deep image centered on NGC1399was avail-able.We computed the counts in the same rings as for the GCLFs(i.e.excluding the centers,and out to120′′). We devided the ring in16×22.5degrees segments around NGC1374,NGC1379,NGC1387,and NGC1427,and plotted the distributions moduloπ,(i.e.rotating the west-ern side by180degrees around the center to increase a possible excess along a given axis)in Fig.8.For NGC 1374and NGC1427(E1and E3galaxies respectively), we indicated the position angle of the galaxies with dot-ted lines.The amount of background contamination in a segment is shown as a solid line.All the distributions are compatible with the globular clusters being spherically distributed around the galaxy. In NGC1374a2σexcess of objects along the major axis of the galaxy is present.For NGC1427it can be ex-cluded that the globular cluster system is as elliptical as the galaxy.For NGC1379(E0),the distribution with an ellipticity of0.2±0.1and a position angle of70±10de-greesfits the data equally well as a spherical distribution.5.2.The radial distributions5.2.1.The“normal”galaxiesFor NGC1374,NGC1379,NGC1387,and NGC1427 we computed the surface density profile for all objects found around the galaxy down to V=24.0mag without any correction for completeness.Table7shows the densi-ties computed in increasing elliptical rings22.7′′(100pix) wide.The density profiles are plotted in Fig.9,the up-per panel showing the uncorrected distribution,the lower panel showing the distribution corrected for background contamination(see Sect.5.3)together with thearbitrarily Fig.8.The angular distributions of globular clusters around NGC1374,NGC1379,NGC1387,and NGC1427.The globu-lar clusters were counted in22.5degrees wide segments around the galaxy and taken moduloπshifted galaxy light profile(squares).The excess in NGC 1374at about150′′corresponds to the distance of NGC 1375,the smaller galaxy close in projection to NGC1374, which might contribute a few globular clusters.Table7.Density profiles for the normal galaxies.Column1 shows the semi–major axis at the center of the ring in arcsecs, columns2–5the density of objects per square arcmin for our four galaxies57′′45.4±6.137.9±5.333.4±5.059.4±8.0 80′′19.8±3.121.4±3.115.2±2.621.6±3.7 102′′12.4±2.112.1±2.010.2±1.817.3±2.8 125′′7.4±1.46.9±1.35.2±1.113.8±2.2 147′′10.6±1.55.7±1.15.3±1.07.8±1.5 170′′4.0±0.97.0±1.23.6±0.810.1±1.7 193′′6.4±1.04.1±0.811.4±1.9 216′′5.4±0.94.0±0.89.4±1.7 238′′3.5±0.76.2±1.06.2±1.4 261′′4.0±1.14.4±1.16.6±1.4Globular cluster systems in Fornax9 Fig.9.The radial distribution of objects in NGC1374,NGC1379,NGC1387,and NGC1427.The left and right panels respectively show the uncorrected density profile and the density profile corrected for background contamination together withthe arbitrarily shifted galaxy light profile(squares).Surface densities are given in number per square arcminutecomputed the fraction of the ring seen in thefield,andscaled the counts up to the total area.No correction forcompleteness of the counts was necessary,since for NGC1399the counts were almost complete down to the consid-ered magnitude.The background contamination was de-termined with a backgroundfield located about40arcmineast.The backgroundfield needed a small(<5%)correc-tion for completeness to be adjusted to thefields aroundNGC1399.The result gave361objects on59.0square ar-cmin in the backgroundfield down to V=24mag,or abackground density of6.1±0.3objects per square arcminas background value for the counts in bothfields aroundNGC1399.Table8shows the densities computed in in-10Globular cluster systems in Fornaxcreasing elliptical rings22.7′′(100pix)wide,plotted inFig.10.Table8.The density profile of globular clusters around NGC1399.Column one list the mean ring radii,column2and3show the density of objects found in the NE and NWfield57′′89.7±18.783.4±8.680′′49.7±10.134.5±5.8102′′43.8±7.940.2±5.7125′′38.5±6.443.1±5.4147′′32.0±5.326.8±4.0170′′24.5±4.225.2±3.6193′′20.6±3.619.7±3.0216′′14.2±2.814.0±2.4238′′22.3±3.312.4±2.2261′′15.3±2.611.4±2.0284′′16.0±2.513.5±2.1307′′12.1±2.110.2±1.8329′′12.2±2.011.5±1.8352′′10.7±1.811.3±1.8375′′11.2±1.88.1±1.4397′′13.2±1.98.2±1.4420′′9.3±1.68.0±1.4443′′8.8±1.58.8±1.4465′′9.7±1.58.4±1.7488′′6.7±1.36.0±1.7511′′6.5±1.59.5±2.4534′′5.9±1.66.9±2.3Galaxy name density slope gal.light slope bkg density 556′′4.8±1.68.6±3.0light profile due to the large cD envelope of the galaxy(e.g.Schombert1986).For the four normal galaxies,the values found are verysimilar to results of previous studies of globular clustersystems around normal early-type galaxies(e.g.Kissler–Patig et al.1996and references therein).6.DiscussionThe previous sections demonstrate that while the globularcluster systems of our faint early-type galaxies have verysimilar properties,the globular clusters in NGC1399,thecentral giant elliptical cD galaxy,are much more numerousand have a different color distribution as well as aflatterdensity profile.While it is true for NGC1399that globular clustersappear in a much larger number than in spirals,it is notfor our fainter galaxies.Harris&Harris(1996)compiledGlobular cluster systems in Fornax11all the globular cluster systems investigated to date.If we select from their list all the S0,Sa,and Sb galaxies (excluding the two outstanding galaxies with M V<−22), we get for the ten remaining galaxies an average number of globular clusters of345±185per galaxy,for an average luminosity of M V=−21.1.The three ellipticals and the S0galaxy that we investigated here have a mean of406±81 globular clusters and therefore do not have more globular clusters in absolute numbers than do these spirals.Comparing the specific frequencies of spirals to that of ellipticals is very difficult,if it makes sense at all.First because ideally it should relate the number of globular clusters to the mass of the galaxy by assuming a con-stant M/L ratio,which is a reasonable assumption when comparing ellipticals among each other but not when com-paring spirals with ellipticals.Second because even when reducing this discrepancy by normalizing the number of globular clusters to the spheroid luminosity,it is unclear which fraction of the globular clusters in spirals are associ-ated with the halo and the bulge,while elliptical galaxies are most probably bulge dominated.Thus it is not clear if we compare comparable values.However,as a comparison, the sample of spirals mentioned above has an average S of 1.3±0.8,and would S be computed for the spheroid lumi-nosities,it would increase by about1(e.g.Harris1991). The value for spirals does therefore not deviate that much from the values derived in Sect.3.2.Similarity seems to exist further in the color distribu-tion of the globular clusters in our faint galaxies and in spirals.They are slightly redder(i.e.probably more metal-rich),but show a similar dispersion around the median to that in the Milky Way,and cover a similar range of colors. Here again dominating bulge clusters,in contrast to the halo dominated Milky Way system,could possibly explain the small color differences.Finally we conclude that for our faint elliptical galax-ies there is no strong need to a different globular cluster formation or evolution scenario,as well as no need for any increase of the number of globular clusters during a hypothetic merger event.On the contrary,for NGC1399these conclusions are not true.NGC1399has far more globular clusters,and a much higher specific frequency than the spiral galaxies. The surface density profile is muchflatter and the globu-lar clusters cover rather homogeneously the full range of colors,and show signs of several populations.As pointed out by several authors before,the formation of the glob-ular cluster system in NGC1399must have undergone a different history,similar to other central giant ellipticals (e.g.Harris1991).Note that the globular cluster system of NGC1399confirms all the predictions that Ashman& Zepf(1992)made for a globular cluster system that ex-perienced a merger:it has a broad(multi–modal?)color distribution,aflat surface density profile,and an increased number of globular clusters.However,NGC1399is one of the galaxies with an outstanding specific frequency,even for a possible enrichment by a merger.While the forma-tion of a large number of globular clusters in coolingflows seems to be ruled out(Bridges et al.1996),it was specu-lated that NGC1399’s position in the center of the Fornax cluster favored the huge number of globular clusters also observed in other galaxies lying at the center of galaxy clusters(e.g.Harris1991).One possibility would be the increased number of merger events at early times,since we showed that the multi–modal color distribution does not exclude several components to have formed the globu-lar cluster system of NGC1399.Another hypothesis could be that the large number of globular clusters is related to the large number of dwarf galaxies whose density Hilker et al.(1995)reported to increase significantly towards the center of the Fornax cluster.One could speculate that ac-creted while still gaseous,the dwarf galaxies formed with high efficiency globular clusters in the dense environment of NGC1399.The high specific frequency would then be a consequence of a Searle&Zinn(1978)scenario combined with the dense environment of NGC1399.However,no more than speculations could be made to date to explain the high specific frequencies of central galaxies.Finally we note the constancy of the specific frequen-cies in all our faint galaxies.The mean for our faint early–type galaxies in Fornax is4.2with a dispersion of1.0.We can add NGC1404,another probable member of Fornax from a study of Richtler et al.(1992,however note their possible argument against a membership of the galaxy to the cluster),and assume a similar distance modulus of 31.0±0.2.We then get a absolute magnitude of−21.0±0.2, and a specific frequency of3.5±0.8.The effectiveness in globular cluster formation within the normal galaxies of the Fornax galaxy cluster must have been very similar and might hint to similar formation histories of the galaxies in the cluster.Acknowledgements.We wish to thank the staffof the Las Cam-panas observatory for the friendly atmosphere and their valu-able help during the observing run.Thanks also to Bill Har-ris for providing a electronic copy of his globular cluster sys-tem compilation,and later for his comments as referee that helped to improve the paper.MKP aknowledges a studentfel-lowship at the European Southern Observatory,SK and MH were supported by the DFG project Ri418/5-1,LI would like to acknowledge support from Proyecto FONDECYT# 1960414.This research made use of the NASA/IPAC extra-galactic database(NED)which is operated by the Jet Propul-sion Laboratory,Caltech,under contract with the National Aeronautics and Space Administration.ReferencesAguilar L.,Hut P.,Ostriker J.,1988,ApJ335,720Ashman K.M.,&Zepf S.E.,1992,ApJ384,50Ashman K.M.,Bird C.M.,Zepf S.E.,1994,AJ108,2348 Bridges T.J.,Hanes D.A.,Harris W.E.,1991,AJ101,469 Bridges T.J.,Carter D.,Harris W.E.,Pritchet C.J.,1996,MN-RAS in press12Globular cluster systems in Fornax Burstein D.,Heiles C.,1982,AJ87,1165Conti P.S.,Vacca W.D.,1994ApJ423,L97Couture J,Harris W.E.,Allwright J.W.B.,1990,ApJS73,671Couture J,Harris W.E.,Allwright J.W.B.,1991,ApJ372,97Geisler D.,Forte J.C.,1990,ApJ350,L5Geisler D.,Lee M.G.,Kim E.,1996,AJ111,1529Goudfrooij P.,Hansen,L.,Jorgensen H.E.,et al.,1994,A&AS104,179Hanes 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星团星团并不是星辰在天界中的偶尔聚集，而是很有秩序地在天空中运行的星群，主要分为两类：一类是“疏散星团”（open cluster），或者称为“银河星团”（galactic cluster），因为它们都位于银河系中；另一类则是“球状星团”（globular cluster）。

在距离我们比较近的几个星团中，肉眼可以看见其中最明亮的恒星，如昴星团，又叫“七姐妹”。

在秋冬季的夜空中，这是7颗肉眼能够观测到的、呈短把勺子形的恒星。

如果观测者仔细观察的话，甚至能够从这个星团中看出九颗或十颗星星，通过望远镜观测到的就更多了。

昴星团的南边又有一个显著的疏散星团，属于金牛座，那就是毕宿星团。

这个星团可以引领我们找到天牛的头部V形，其中还有明亮的红色星毕宿五，尽管这颗亮星还没有被确定为这个星团的成员。

疏散星团中的成员在空间中的运动都具有一致性，有些星团的距离比较近，所以容易观测到它们的运动，这一类星团又被称为“移动星团”（moving cluster），毕宿星团就是一个典型。

这个V形星群（毕宿五除外）及其附近的星都在一致地向东运动，它们的运动路线虽然不是完全平行的，但远远望去也好像是在沿着许多条道路向远方汇聚，这表明它们还在退后。

约在一百万年前，这个星团与我们的距离大约是65光年，而现在的距离已经增加了一倍。

或许亿年之后，这个星团会距离我们更远，直到成为望远镜中的一个暗淡天体，去到距离猎户座中的红星参宿四比较近的位置。

我们现在也正被移动星团包围，但太阳并不是其中的成员。

这个星团中的一部分出现在北天，形成北斗，但需要去掉勺柄末端的一颗星和指极星上方的一颗星。

南天中是天狼星，还有一些散布得比较远的亮星，它们都是这个移动星团中的成员。

经过很长一段时间之后，它们会将我们远远甩在后面，成为平常状况的疏散星团。

有些疏散星团，用我们肉眼看起来像是一块雾斑，被称为“蜂巢”的鬼宿星团便是一个典型的例子。

鬼宿星团属于黄道带中的巨蟹座，在狮子座中的镰刀形附近。

天文词汇Ggalactic cannibalism 星系相食宇宙中，大型星系并吞小型星系的现象。

galactic corona 银冕银晕外面物质密度更低的区域，延伸的距离可能是星系可见直径的数倍。

galaxy seeds 星系种子初期宇宙中，小型的重力引力中心。

这些星系种子进一步吸引更多物质，形成星系群、丝状结构和长城结构。

Galilean satellites 伽利略卫星木星的四颗卫星，因为是伽利略在十七世纪发现，因而得名。

gas tail (type I ) 气尾、气体尾受太阳风的吹袭，而落在彗星后方的游离化气体喷陷，颜色偏蓝。

参见尘尾 (dust tail) 。

Gauss (G) 高斯量测磁场强度的单位，一高斯是一特斯拉的一万分之一。

geocentric universe 地心宇宙模型认为地球是宇宙中心的宇宙模型，例如：托勒密宇宙模型。

geosynchronous orbit 地球同步轨道一种绕行地球的卫星轨道，周期为24小时而且是由西向东运行，卫星永远驻留在地球表面同一点的上方。

giant molecular clouds 巨大分子云星际空间，低温、巨大且致密的分子云，新恒星的诞生处。

giant stars 巨星恒星演化离开主序带后，体积膨胀、表面温度降低、变得非常明亮，因为这类恒星大约是太阳的10至100倍，所以被称为巨星。

巨星位在赫罗图的右上角。

glacial period 冰河期冰棚覆盖大范围地球表面的时期。

glitch 频率突变波霎 (旋转中子星) 的自转周期，突然发生改变的现象。

globular cluster 球状星团外观上，恒星的分布是球形的星团。

球状星团通常含有五万到一百万颗恒星，星团大小约有75光年，通常出现在星系的球状部份。

球状星团内的恒星，金属的含量低，年龄大。

graben rille 条状纹脉行星表面，因为断层运动或表壳陷落，所形成的直线形纹脉。

grand unified theories (GUTs) 大统一理论把电磁力、弱作用力和强作用力，纳入同一种理论架构的理论。

天文学专业词汇CAMC, Carlsberg Automatic Meridian 卡尔斯伯格自动子午环Circlecannibalism 吞食cannibalized galaxy 被吞星系cannibalizing galaxy 吞食星系cannibalizing of galaxies 星系吞食carbon dwarf 碳矮星Cassegrain spectrograph 卡焦摄谱仪Cassini 〈卡西尼〉土星探测器Cat's Eye nebula （ NGC 6543 ）猫眼星云CCD astronomy CCD 天文学CCD camera CCD 照相机CCD photometry CCD 测光CCD spectrograph CCD 摄谱仪CCD spectrum CCD 光谱celestial clock 天体钟celestial mechanician 天体力学家celestial thermal background 天空热背景辐射celestial thermal background radiation 天空热背景辐射central overlap technique 中心重迭法Centaurus arm 半人马臂Cepheid distance 造父距离CFHT, Canada-Franch-Hawaii Telecope 〈CFHT〉望远镜CGRO, Compton Gamma-Ray Observatory 〈康普顿〉γ射线天文台chaos 混沌chaotic dynamics 混沌动力学chaotic layer 混沌层chaotic region 混沌区chemically peculiar star 化学特殊星Christmas Tree cluster （ NGC 2264 ）圣诞树星团chromosphere-corona transition zone 色球-日冕过渡层chromospheric activity 色球活动chromospherically active banary 色球活动双星chromospherically active star 色球活动星chromospheric line 色球谱线chromospheric matirial 色球物质chromospheric spectrum 色球光谱CID, charge injected device CID、电荷注入器件circular solution 圆轨解circumnuclear star-formation 核周产星circumscribed halo 外接日晕circumstellar dust disk 星周尘盘circumstellar material 星周物质circumsystem material 双星周物质classical Algol system 经典大陵双星classical quasar 经典类星体classical R Coronae Borealis star 经典北冕 R 型星classical T Tauri star 经典金牛 T 型星Clementine 〈克莱芒蒂娜〉环月测绘飞行器closure phase imaging 锁相成象cluster centre 团中心cluster galaxy 团星系COBE, Cosmic Background Explorer 宇宙背景探测器coded mask imaging 编码掩模成象coded mask telescope 编码掩模望远镜collapsing cloud 坍缩云cometary burst 彗暴cometary dynamics 彗星动力学cometary flare 彗耀cometary H Ⅱ region 彗状电离氢区cometary outburst 彗爆发cometary proplyd 彗状原行星盘comet shower 彗星雨common proper-motion binary 共自行双星common proper-motion pair 共自行星对compact binary galaxy 致密双重星系天文学专业词汇compact cluster 致密星团; 致密星系团compact flare 致密耀斑composite diagram method 复合图法composite spectrum binary 复谱双星computational astrophysics 计算天体物理computational celestial mechanics 计算天体力学contact copying 接触复制contraction age 收缩年龄convective envelope 对流包层cooling flow 冷却流co-orbital satellite 共轨卫星coplanar orbits 共面轨道Copernicus 〈哥白尼〉卫星coprocessor 协处理器Cordelia 天卫六core-dominated quasar （ CDQ ）核占优类星体coronal abundance 冕区丰度coronal activity 星冕活动、日冕活动coronal dividing line 冕区分界线coronal gas 星冕气体、日冕气体coronal green line 星冕绿线、日冕绿线coronal helmet 冕盔coronal magnetic energy 冕区磁能coronal red line 星冕红线、日冕红线cosmic abundance 宇宙丰度cosmic string 宇宙弦cosmic void 宇宙巨洞COSMOS 〈COSMOS〉底片自动测量仪C-O white dwarf 碳氧白矮星Cowling approximation 柯林近似Cowling mechnism 柯林机制Crescent nebula （ NGC 6888 ）蛾眉月星云Cressida 天卫九critical equipotential lobe 临界等位瓣cross-correlation method 交叉相关法cross-correlation technique 交叉相关法cross disperser prism 横向色散棱镜crustal dynamics 星壳动力学cryogenic camera 致冷照相机cushion distortion 枕形畸变cut-off error 截断误差Cyclops project 〈独眼神〉计划D abundance 氘丰度Dactyl 艾卫dark halo 暗晕data acquisition 数据采集decline phase 下降阶段deep-field observation 深天区观测density arm 密度臂density profile 密度轮廓dereddening 红化改正Desdemona 天卫十destabiliizing effect 去稳效应dew shield 露罩diagonal mirror 对角镜diagnostic diagram 诊断图differential reddening 较差红化diffuse density 漫射密度diffuse dwarf 弥漫矮星系diffuse X-ray 弥漫 X 射线diffusion approximation 扩散近似digital optical sky survey 数字光学巡天digital sky survey 数字巡天disappearance 掩始cisconnection event 断尾事件dish 碟形天线disk globular cluster 盘族球状星团dispersion measure 频散量度dissector 析象管distance estimator 估距关系distribution parameter 分布参数disturbed galaxy 受扰星系disturbing galaxy 扰动星系Dobsonian mounting 多布森装置Dobsonian reflector 多布森反射望远镜Dobsonian telescope 多布森望远镜dominant galaxy 主星系double-mode cepheid 双模造父变星double-mode pulsator 双模脉动星double-mode RR Lyrae star 双模天琴 RR 型星double-ring galaxy 双环星系DQ Herculis star 武仙 DQ 型星dredge-up 上翻drift scanning 漂移扫描driving system 驱动系统dumbbell radio galaxy 哑铃状射电星系Du Pont Telescope 杜邦望远镜dust ring 尘环dwarf carbon star 碳矮星dwarf spheroidal 矮球状星系dwarf spheroidal galaxy 矮球状星系dwarf spiral 矮旋涡星系dwarf spiral galaxy 矮旋涡星系dynamical age 动力学年龄dynamical astronomy 动力天文dynamical evolution 动力学演化。

用于岩屑描述的标准缩略词整理人：黄灵军录井二分公司2001年2月20日用于岩屑描述的标准缩略词英文词中文词义缩略词about 大约abtabove 在上ab , abv absent 不存在、缺失abs abundant 丰富abd, abnd accumulation 累计accum acicular 针状acicafter 在---之后aft agglomerate 集块岩Aglm aggregate 集合体Aggalgae , algal 藻类Alg , alg allochem 异化颗粒Allo altered 改变的、蚀变的alt alternation 交变的、交互的altgamber 琥珀色amb ammonite 菊石Amm amorphous 无定形的、非结晶的amor amount 总数Amtand 和、及& andesite 安山岩Andes angular 棱角的ang anhedral 他形的、劣形的ahd anhydrite 硬石膏Anhy,anhy anthracite 无烟煤Anthr aphanitic 隐晶质的aph apparent 表观apr appears 出现ap ,aprs approximate 近似的、大约的apprx, aprox aragonite 霰石（文石）Arag arenaceous 砂质的arenargillaceous 泥质的arg argillite 泥板岩argl arkose (-ic) 长石砂岩（的）Ark , ark as above 同上 a.a. asphalt (-ic) 沥青、地沥青（的）Asph , asph assemblage 组合、集合Assem associated 联合的、伴生的assocat 在--- @ authigenic 自生的authg average 平均值、平均的Av , avband (-ed) 带、夹层Bnd , bnd barite 重晶石Bar basalt (-ic) 玄武岩Bas , bas basement 基础、基底Bm become (-ing) 变成bcmbed (-ed) 层Bd , bdd bedding 层理、层面、分层Bdg Belemnites 箭石属（头足类）Belm bentonite (-ic) 斑脱岩的、膨润土（的）Bent , bent bitumen (-inous) 沥青（的）Bit , bit bioclastic 生物碎屑的biocl ,bioc bioherm (-al) 生物礁岩、生物丘Bioh , bioh biomicrite 生物微晶灰岩Biomi biosparite 生物亮晶灰岩Biosp biostrom (-al) 生物层Biost , biost biotite 黑云母Biot birdseye 鸟眼Bdeye black (-ish) 黑（的）、暗淡的blk , blksh blade (- ed) 刀片、刀片状的Bld , bld bleeding 析水bldg bloacky 块状的、断块的blkyblue (-ish) 兰色bl , blsh bored (-ing) 钻孔的Bor , bor bottom 底、底部Btm ，Bbotryoid (-al) 葡萄状的Bot , bot , btry boulder 漂砾、巨砾Bld , Bldr boundstone 粘结碳酸岩Bdst brachiopod 腕足动物Brach , Brac brackish 稍咸的brak branching 分叉的、分支的brhgbreak 断裂、破裂、层缺Brk , brk breccia (-ted) 角砾岩Brec , brec bright 明亮的brt , bri brittle 脆性的britbrown 褐色、棕色brn bryozoa 苔藓动物Brybubble 泡Bublbuff 浅黄色bu , bf burrow (-ed) 掘穴遗迹Bur , burcalcarenite 钙屑灰岩、灰屑岩Clcar calcilutite 泥屑石灰岩Clclt calcirudite 砾屑石灰岩Clcrd calcisiltite 粉砂屑石灰岩Clslt calcisphere 钙球石Clcsp calcite (-ic) 方解石（的）Calc, calctc calcareous 钙质的calccaliche 钙质壳、钙结层、生硝cche carbonaceous 碳的、碳质的、含碳的carb carbonized 炭化cbcasing 套管、下套管csgcavern (-ous) 洞穴、洞穴状的Cav ,cav caving 塌落物、井壁坍塌Cvg , Cav cament (-ed,-ing) 胶结、胶结物Cmt , cmt center 中心cntr cephalopod 头足类Ceph chalcedony 玉髓Chal , chal chalk (-y) 白垩、燧石（的）Chk , chky charophyte 轮藻类Charchert (-y) 燧石（的）Cht , chtchitin (-ous) 几丁质（的）Chit , chit chlorite (-ic) 绿泥石Chlor , chlor , chl chocolate 赭色choccone-in-cone 叠锥c-in-c circulate (-ion) 循环Circ , circ clastic 碎屑状的、碎屑岩clasclay (-ey) 粘土（粘土质的）Cl , cl ,cly claystone 粘土岩Clst, clyst clean 干净的clnclear 清晰的clrcleavage 解理、劈理Clvgcluster 星团、束、族、群Cluscoal 煤C，coal coarse 粗的、粗粒的crs , c , cse coated (-ing) 表层、外壳cotd , Cotg , cotg coated grains 包粒cotd gncobble 中砾Cblcolor (-ed) 颜色Col , col common 普通的、常见的comcompact 致密的cpctcompare 比较、对照cfconcentric 同心的cncn, cncnc conchoidal 贝壳状的conchconcretion (-ary) 固结作用、结核Conc , conc conglomerate (-ic) 砾岩、砾岩的Cgl , cgl conodont 牙形刺、牙形石Cono considerable 大量的、值得考虑的cons consolidated 固结的consol conspicuous 明显的、显著的conspiccontact 接触Ctc ，cont contamination (-ed) 污染Contam , contam,contm content 含量、容量、内容Contcontorted 扭曲、cntrt,contrtcoquina (-iod) 贝壳灰岩Coq , coqidcoral , coralline 珊瑚的Cor , corln core 岩心、核心 Ccorrect 校正corr coring 取心crg covered 覆盖（着的）cov cream 奶油色、米色crm creams 钻井用特级金刚石Crm crenulated 褶皱的cren crevice 裂隙crev crinkled 成波纹的crnk crinoid (-al) 海百合Crin , crinal cross 十字形的、交叉的xcross-bedded 交错层x-bd , xbdd cross-laminated 交错纹理x-lam , xlam cross-stratified 交错层理的x-strat , xstrat cryptograined 隐粒的crpgr cryptocrystalline 隐晶质的crpxl crumpled 揉皱的crpld crystocrystalline 结晶的、晶质的crpxln crystal (-line) 晶体Xl , xln cube , cubic 立方体的Cub , cub cuttings 岩屑Ctgs cypridospsis 介形类Cypdark (-er) 暗的dk , dkr dead 死的、静的dddebris 碎屑、岩屑Deb decrease (-ing) 减少、减小Decr , decr degree 度degrdense 致密的、密集的dns depauperate 发育不全的depau description 描述、说明Descr determine 确定、决定dtrm detrital 碎屑的detr , dtrl devitrified 失去玻璃光泽的devitdiabase 辉绿岩Db diagenesis (-etic) 成岩作用Diagn , diagn diameter 直径Diadiatoms 硅藻Diat difference 差别Dif disseminated 散布、浸染dissem dism distillate 蒸馏Distditto 同上的、同前的do , dto dolomite (-ic) 白云石、白云岩Dol , dol dolocast 白云石晶模dolc dolomold 白云石穴dolmd dolostone 白云岩Dolst dominant (-ly) 占优势的、支配的domdrill collar 钻铤Dcdrilling 钻井drlg drillpipe 钻杆Dpdrill stem test 钻杆测试DSTdrusy 晶簇状druearthy 土状的ea , ethyeast 东、东方、东部 Eechinoid 海胆ech elevation 高程、高度、海拔Elev elliptical 椭圆的elip elongate 延伸、伸长elong , elg embedded 埋入的、嵌入的embd ,embdd enlarged 扩大、放大enlrgequant 相eqnt equivalent 相等的、相当的Equiv estimated 估计的est euhedral 全形的、自形的euhd , euhed euxinic 静海（相）的eux evaporite (-itic) 蒸发盐（岩）Evap , evap excellent 卓越的、优良的exexposed 暴露的expextraclast (-ic) 外来碎屑Exclas , exclas extremely 极端的extrextrusion 挤压extrextrusive rock, extrusive 喷出岩Exv , exvfacet (-ed) 刻面Fac , facfaint 不明显的fntfair 中等的frfault (-ed) 断层Flt , fltfauna 动物（群）Faufeet 英尺（复数）Ftfeldspar (-athic) 长石Fspr , fspr , fld fenestra (-al) 窗、模孔、透明斑点Fen，fen ferruginous 含铁的ferr，fefinal flowing pressure 最终流动压力FFPfinal hydrosfatic pressure最终流体静压力FHPfinal shut-in pressure 最终关井压力FSIPfibrous 纤维状的fibr，fibfigure 形状figfill 充满flfine (-ly) 细的、细粒状的 f , fnlyfissile 易剥裂的fisflaggy 板层、薄层flgflake , flaky 薄片、片状、鳞片状Flk , flkflat 平的、平坦的flflesh 一切生物flsflint 电石、黑燧石flntfloating 漂浮的fltgflora 植物群、植物区系Flo fluorescence (-ent) 荧光Fluor , fluor ，flor foliated 叶片状folfoot 英尺Ftforaminifer , foraminiferal 有孔虫（的）Foram , foram formation 地层Fmfossil (-iferous) 化石（含化石的）Foss , foss ，fosfracture (-d) 裂隙、破裂Frac , frac fragment (-al) 碎片Frag , frag frequent 频繁的freqfresh 新鲜的、淡的frsfriable 易碎的、脆的frifringe (-ing) 边缘、条纹Frg , frgfrosted 结水、霜状条纹frosfrosted quartz grains 霜状表面石英颗粒 F.Q.G.fucoid (-al) 树枝状Fuc , fuc fusulinid 纺锤蜓Fusgabbro 辉长石Gabgastropod 腕足类Gastgas 天然气Ggenerally 一般地gengeopetal 向地性geptgilsonite 硬沥青Gilglass (-y) 玻璃（的）Glas , glas , gl glauconite (-itic) 海绿石Glauc , glauc , glau globigerina (-inal) 抱球虫属Glob , glob globular 球状glblrgloss (-y) 光泽（的）Glos , glos gneiss (-y) 片麻岩的Gns , gnsgood 好的gd , ggrade 等级grdgrading 粒级变化、分选gradgrain (-s , -ed) 粒、颗粒Gr , grgraiu 颗粒grgrainstone 粒状灰岩Grstgranite 花岗岩Grt , grnt granite wash 花岗砂岩G.W.granule (-ar) 粒状（的）Gran , gran ，grnl grapestone 葡萄状灰岩grapst graptolite 笔石Grapgravel 砾石、沙砾Grv , gvlgray , grey (-ish) 灰色的gry , grysh ,gy greywacke 灰瓦岩、杂砂岩、硬砂岩Gwke , gywk greasy 油脂的gsy , grsy green (-ish) 绿色（的）gn , gnshgrit (-ty) 粗砂岩Gt , gt , grty gypsum (-iferous) 石膏Gyp , gyphackly 锯齿状hklhalite (-iferous) 石盐（的）Hal , hal hard 硬的hdheavy 重的hvy hematite (-ic) 赤铁矿Hem , hem heterostegina 异盖虫属Het heterogeneous 非均质hetr hexagonal 六角形的hexhigh (-ly) 高hi homogeneous 均质的hom horizontal 水平的hor , hrznl hydrocarbon 烃Hydcigneous rock (igneous) 火成的Ig , ig impregnated 浸泽的imprg impression 印膜、痕迹、影响Impinitial hydrostatic pressure 初始流体静压力IHPinch 英寸In inclusion (-ded) 包体、包括Incl , incl increasing 增加incr indistinct 不清楚的indst indurated 固结的ind inoceramus 叠瓦蛤属Inocin part 在某种程度上的I.P. insoluble 不溶的insl interbedded 互层的intbd , intbdd intercalatey 夹层、插入层intercal interclast 层间碎屑intclintercrystalline 晶间的intxln , intxl interfragmantal 碎片间的intfrag intergranular 粒间的intgran intergrown 共生的、交互生长的intgn interlaminated 层间的intrlam interpartical 粒间的intpar interpretation 解释intpt intersticies (-itial) 间隙的Intst , intst interval 间隔、层段Intvl , intv interaclast (-ic) 内碎屑Intclas , intclas intraparticle 粒内的intrapar intrusion 侵入作用intrIntrusive rock , intrusive 侵入岩Intr , intr invertebrate 无脊椎的Invtb , Invrtb iridescent 彩虹的、闪光色的iridiron 铁Fe ironstone 富铁岩石、铁石Fe-st irregular (-ly) 不规则的、紊乱的irr , ireg isopachous 等厚的isojasper 碧玉Jaspjoint (-ed,-ing) 节理、接头、连接Jt , jtkaolin (-itic) 高龄土Kao , kao kelly bushing 方补心KB kerogen 干酪根Kerkick off 初始造斜KOlacustrine 湖成的laclamina (-tions , -ated) 薄的、薄层Lam , lam large 大（量）的lge , lrg laterite (-itic) 砖红壤Lat , lat lavender 淡紫色lavlayer 层Lyr leached 过滤的lchd , lchlens , lenticular 透镜状的Len , lentlight 光、淡色的、浅色的ltlignite (-itic) 褐煤Lig , lig limestone 灰岩Lslimonite (-itic) 褐铁矿Lim , lim , lmn limy 石灰质的lmylithic 石质的、岩性的lit , ltc lithographic 石印的、致密晶质的lithgr ,lith lithology (-ic) 岩性学Lith , lithlittle 小、少Ltl , ltllittoral 滨海的littlocal 局部的loclong 长的lgloose 松散的lselower 下部的、早期的、较低的l , lowlumpy 块状的lmpyluster , luster 光泽Lstrlutite 泥质岩、细屑岩Lutmacrofossil 大化石Macrofos ,macfos magnetite , magnetic 磁铁矿、磁性的Mag , mag manganese , manganiferous 锰、含锰的Mn , mn marble 大理石（岩）Mblmarl (-y) 泥灰岩（含泥灰质的）Mrl , mrl marlstone 泥灰岩Mrlstmarine 海的marnmaroon 栗色、紫酱色marmassive 块状的mass , mas material 物质Matmatrix 基质Mtrx , mtx maximum 最大的maxmedium 中等的、介质m , med member 段、成员Mbr meniscus 新月形的men metamorphic rock 变质岩Metametamorphic (-osed) 变质的meta , metaph metasomaticous 交代msmmica (-ceous) 云母Mic , mica micrite (-ic) 微晶灰岩Micr , micr microcrystalline 微晶质microxln , micxl microfossil (-iferous) 微体化石Microfos , microfos ,micfos micrograined 微粒的micgrmicro-oolite 微鲕状灰岩Microol micropore (-osity) 微孔隙Micropor , micropor microspar 微亮晶Microspr microstylolite 微缝合线Microstyl middle 中部、中间Midmiliolid 小栗虫目Milidmilky 乳状的mkymineral (-ized) 矿物Min , min , mnrl minimum 最小minminor 较小的、次要的mnrminute 分钟mnut moderate 中等的modmold (-ic) 模、印膜Mol , mol mollusc 软体动物Moll , mol mosaic 镶嵌mosmottled 斑点、杂色mott , mot mud (-dy) 泥、泥浆的md , mdy mudstone 泥岩Mdst muscovite 白云母Muscnacreous 珍珠的nacno 不、无nnodules (-ar) 结核Nod , nod north 北、北部Nno sample 无样品n.s.no show 无显示n/snovaculite 致密石英岩Novacno visible porosity 无可见孔隙N.V.P.numerous 许多的numobject 目的obj occasional 偶见的occochre 赭石ochodor 气味odoil 石油O , oiloil source rock 生油岩OSRolive 橄榄色、茶青色olvooid (-al) 鲕石、鲕粒Oo , oo oolicast (-ic) 空鲕粒Ooc , ooc oolite (-itic) 鲕状岩、鲕状的Ool , ool oomold (-ic) 鲕状模Oomol , oomol ,oom oncolite (-oidal) 核形石Onc , onc opaque 不透明的op , opqopen hole 裸眼井OHopposite 对应的opporange (-ish) 橙色or , orsh , orng orbitolina 园笠虫Orbitorganic 有机的orgorigin 起点orig orthoclase 正长石Orth orthoquartzite 正石英岩O-Qtz ostracod 介形亚纲Ostr , Ost overgrowth 增生、次生加大ovgth oxidized 氧化oxoyster 牡蛎Oystpacker 封隔器pkr packstone 泥砾状灰岩Pkstpaper (-y) 纸状的Pap , pap part (-ly) 部分的Pt , pt particle 颗粒Par , par parting 裂缝、断口Ptgparts per milliom 百万分之一PPMpatch (-y) 斑点、斑纹Pch , pch , pchy pearly 珍珠状、碎片状prlypebble (-ly) 细砾、卵石Pbl , pbl pelecypod 瓣鳃纲Pelec , plcy pellet (-al) 球粒、团粒Pel , pel pelletoid (-al) 似球粒Peld , peld perforate 射孔perf permeability (-able) 渗透率Perm , K , perm pendular (-ous) 悬垂的Pend , pend petroleum,petroliferous 石油Pet , pet phlogopite 金云母Phlog phosphate (-atic) 磷酸盐Phos , phos phyllite , phyllitic 千枚岩Phyl , phyl phreatic 潜水的、蒸汽喷发的phrpink 粉红的pkpinkish 粉红的pkishpin-point (porosity) 极微小的p.p.pisoid (-al) 豆状的Piso , piso pisolite , pisolitic 豆状岩Pisol , pisol pitted 多坑的pit plagioclase 斜长石Plagplant 植物pltplastic 塑性的plasplaty 片状的pltyplugged & abandoned 填井P&A plugged back 回堵PBpolish , polished 抛光Pol , pol pollen 花粉Poln polygonal 多边形的polypoor 劣质的p porcelaneous 瓷质的porcel , porc porosity , porous 孔隙、孔隙度、孔隙的Por , por , Φpossible (-ly) 可能的poss , pos predominant (-ly) 占优势的pred preserved 保存的prespresent depth 现深度PDprimary 原生的、主要的prim probable (-ly) 大概的、可能的prob production 生产、产量Prod prominent 突起的、显著的prom pseudo- 假-- ps , psdo pseudo oolite (-ic) 假鲕Psool , psool pumice-stone 浮石岩Pstpurple 紫红色purppyrite (-itized , -itic) 黄铁矿Pyr , pyr pyrobitumen 焦沥青Pybit , pyrbit pyroclastic 火山碎屑岩pyrcl , pyrclasquartz (-ose) 石英（质）Qtz , qtz quartzite (-ic) 石英岩的Qtzt , qtztradial (-ating) 放射状的Rad ,rad random 随机的randrange 范围rngrare 稀少的r , rr recemented 再胶结的recem recovery (-ered) 回收Rec , rec recrystallized 重结晶的rexlzdred (-ish) 红的rd , rdsh , r reef (-oid) 礁Rf , rf reguler 正规的reg remains 遗体、残留物Rem , rmn reaming 划眼、扩眼rmg replaced (-ment) 交代、置换Repl , rep residue (-ual) 残余物Res , res , resd resinous 树脂的rsnsrhomb (-ic) 菱形的Rhb , rhb , rhmb ripple 波纹、波痕Rplrock 岩石Rkround (-ed) 圆的rnd , rnddrubble (-bly) 碎石Rbl , rblsacks 袋、包sxsalt (-y) 盐Sa , sasalt water 盐水S.W.same as above 同上 a.a. sample 样品Spl , smpl sand (-y) 砂（质）Sd , sdy sandstone 砂岩sst , Ss saturation (-ated) 饱和Sat , sat scales 尺度、比例scscarce 稀有的scs scattered 散布的scatschist (-ose) 片岩、片状岩Sch , sch secondary 次生的sec sediment (-ary) 沉积物（的）Sed , sed shadow 阴影shadshale (-ly) 页岩Sh , sh shell 贝壳Shlshow 显示Shw siderite (-itic) 菱铁矿Sid , sid sidewall core 井壁取心S.W.C. silica (-iceous) 二氧化硅Sil , sil silky 丝一样的slkysilt (-y) 粉砂Slt , slty siltstone 粉砂岩sltst similar 相似的simsize 大小、尺寸szskeletal 骨骼的skelslabby 板状的slbslate (-y) 板岩Sl , sl slickenside (-d) 擦痕面Slick , slick,sks slight (-ly) 轻微的sli , slily , sl slow 慢的slosmall 小的sml , ssmooth 光滑的，平滑的smsoft 软的sft solution , soluble 溶解，可溶解的Sol , sol , solb somewhat 有点，轻微的smwt sorted (-ing) 分选srt , srtg south 南，南部Sspar (-ry) 晶石，粘土细脉Spr , spr sparse (-ly) 稀疏的sps , spsly speck (-led) 斑点Spk , spk , spec sphalerite 闪锌矿Sphal spherule (-itic) 球粒（状的）Spher ,spher , sph spicule (-ar) 针状的Spic , spic splintery 裂片状的Splin , splty sponge 海绵Spgspore 孢子Spo, spr spot 点、滴spspotted (-y) 斑点（状）sptd , spty squeeze 挤压squstain (-ed,-ing ) 色斑、浸染、着色Stn , stn stalactitic 钟乳石Stalstrata (-ified) 地层、成层的Strat , strat streak (-ed) 条痕Strk , strk striae (-ted) 擦痕、条痕Stri , stri stringer 沉积薄层strgr , strg stromatolite (-itic) 叠层石Stromlt , stromlt stromatoporoid 层孔虫属Strom structure 构造Str , struc stylolite (-itic) 缝合线Styl , styl subangular 次棱角状sbang sublithic 次石质的sblit subrounded 次圆状的sbrndd sucrosic 糖粒状sucsulphur , sulphurous 硫、多硫的Su , su , s superficial oolite (-ic) 表层的、鲕表Spfool , spfool surface 表面Surfswab 抽吸swb syntaxial 共轴的syntabular (-ate) 板、横隔、表格式的tabtan 棕黄色tn terrininous 陆源的、陆生的tertesting 测试tstg texture (-d) 结构Tex , tex think 厚的、粗大的thkthin 薄的、细小的thnthin-bedded 薄层的t.b.thin section 薄片T.s. throughout 遍及thrutight 致密的ti , tttop 顶、盖层Tptop of 顶部T/total depth 总深度TD tough 坚韧的tghtrace 痕迹、痕量、记录道Tr translucent 半透明的trnsl transparent 透明的trnsp trilobite 三叶虫tril , Trilo tripoli (-itic) 硅藻土Trip , trip tube (-ular) 管Tub , tub tuff (-aceous) 凝灰岩Tf , tf , tuf true vertical depth 实际垂直深度TVD type (-ical) 类型Typ , typunconformity 不整合Unconf unconsolidated 未固结的uncons underclay 底粘土层Uc underlying 下伏的undly uniform 一致的、均匀的uni upper 上部的、上面的u , upvadose 渗流Vad , vad variation (-able) 变种、变化Var , var variegated 杂色的、班驳的vgt varicolored 杂色的varic , vcol varved 纹泥、季候泥vrvdvein (-ing , -ed) 脉、岩脉Vn , vn veinlet 细脉Vnlet vermillon 朱红石榴石verm vertebrate 脊椎动物门vrbt vertical 垂直的vert , vrt very 十分vvery poor sample 质量极差样品V.P.S vesicular 多孔状、多泡状ves violet 紫色vi vitreous 玻璃质、透明的vit volcanic 火山岩volcvug 晶洞vugwaiting on 等候wo water 水wtr water cushion 水垫w/c wavy 波状wvy waxy 蜡的wxy weak 弱的wk weather 气候wthr well 井wwhite 白色whwith 同w/ yellow 黄色yelzeolite 氟石zeo zone 带zn备注：1、名词性缩略词均以大写字母开始。