A median redshift of 2.4 for galaxies bright at submillimetre wavelengths

a r X i v :a s t r o -p h /0304235v 1 13 A p r 2003———————————————————————–

Version:2Febuary 2008,C07037LS/ks

A signi?cant fraction of the energy emitted in the early Universe came from very luminous galaxies that are largely hidden at optical wavelengths (because of interstellar dust grains);this energy now forms part of the cosmic back-ground radiation at wavelengths near 1mm.1These submillimetre (submm)galaxies were resolved from the background in 1997,2but have been di?cult to identify and study due to the poor spatial resolution of submm instruments.3This has impeded the determination of their distances (or redshifts,z ),a cru-cial element in understanding their nature and evolution.4Here we report spectroscopic redshifts for ten representative submm galaxies that we identi-

?ed reliably using high resolution radio observations.5,6,7The median redshift for our sample is 2.4,with a quartile range of z =1.9–2.8.The submm popu-lation therefore coexists with the peak activity of quasars,which are thought to be massive black holes in the process of accreting matter,suggesting a close relationship between the growth of massive black holes and luminous dusty galaxies.8The space density of submm galaxies at z >2is about 1000times greater than that of similarly luminous galaxies in the present-day Universe,so they represent an important component of star formation at high redshifts.

The?rst real insight in the origin of the far-IR/submm background came with the commissioning of the SCUBA submm camera on the JCMT.Almost100%of the submm background has been resolved with the deepest SCUBA maps,which exploit a sensitivity boost from gravitational lenses.2,3,9However,the near-IR/optical faintness of the submm galaxy population conspires with the modest positional precision available from the large (15′′)SCUBA beam and the large surface density of unrelated optically-faint galaxies to render positional coincidence alone inadequate to identify counterparts.3,5This problem is compounded by the small?eld of view of SCUBA:compiling large samples of submm galaxies is slow,with roughly one detected every night.Because of these di?culties, robust spectroscopic redshifts have been published for only a handful of submm sources, all atypically bright at optical wavelengths.10,11,12,3

Here,we have overcome these problems by taking advantage of1.4-GHz radio data from the Very Large Array(VLA)radio telescope(Hubble Deep Field13,SSA13?eld14, ElaisN2and Lockman?elds7).These deep images have?ne(1–2′′)spatial resolution and a large(30′FWHM)?eld of view.The radio data was exploited to followup SCUBA submm data in the Hubble Deep Field(12hr RA)and SSA13(13hr RA)?elds15,5,16,and the Lockman(10hr RA)and ElaisN2(16hr RA)?elds17.The radio data are sensitive to the synchrotron radio emission from cosmic-ray electrons accelerated in the supernovae explosions of the same high-mass stars that heat the dust and generate the far-IR/submm emission.Hence a deep radio image should be an e?cient route to pinpoint the positions of many submm galaxies.This is con?rmed in?elds with both submm and radio observa-tions:radio counterparts brighter than30μJy can be found for60–70%of submm galaxies brighter than5mJy at850μm(which have a surface density of450deg?2,3and contribute about20%of the submm background).7,16Moreover,the accurate radio positions mean that SCUBA’s e?cient‘photometry’mode can be used to search for submm galaxies,5,6,18 raising the detection rate to around ten per night.

Although submm galaxies have faint optical continuum emission,3the radio-detected samples are su?ciently large to allow e?cient,multi-object optical spectroscopy using10-m telescopes.Slit positions can be assigned accurately,as the radio/submm emission can be

located on optical images to within0.3–0.8′′.7Using this approach we targetted34radio-detected submm galaxies mostly brighter than5mJy at850μm with optical magnitudes in the range I=22.2–26.4using the ESI and LRIS spectrographs on the Keck telescopes (Fig.1).We measured redshifts for ten submm galaxies,representative of the blank-?eld population.We have doubled the number of optically bright(I<23.5)submm galaxies with accurate redshifts.Our six redshifts for I>23.5submm galaxies represent the?rst redshifts for this class of submm galaxy.The redshifts span the range z=0.8–3.7,with a median of2.4and an interquartile range of1.9–2.8(Fig.2).These redshifts allow dust temperatures T d and bolometric luminosities to be determined(see Table1),assuming that the tight correlation between far-IR and radio emission observed at low redshifts19 remains valid.Typical values are of order35K and several1012L⊙respectively.Note that relativistic electrons accelerated in shocks close to an active galactic nucleus(AGN) should boost the radio?ux density above that expected from the standard correlation. If the radio emission is boosted by an AGN then both temperature and luminosity are overestimated.There are no obvious cases in the present sample in this category.

The redshifts impose robust limits to the space densities of submm galaxies in the redshift ranges0.5–1.2,1.8–2.8and2.8–4(the gap at z=1.2–1.8is the spectroscopic desert in which no strong restframe UV lines are redshifted into the optical window):we calculateρ=(3.3±2.3)×10?6Mpc?3,(6.5±2.5)×10?6Mpc?3and(2.4±1.2)×10?6 Mpc?3,respectively,assuming a?atΛ=0.7Universe with H0=65km s?1Mpc?1.This compares to a space density of～10?8Mpc?3for low-redshift galaxies with comparable bolometric luminosities greater than5×1012L⊙,comparable to the luminosities of our spectroscopically targeted galaxies at any redshift greater than one.The volume density of very luminous galaxies thus increases almost a thousandfold from z～0to2.

The relationship between di?erent classes of high-redshift galaxy is critical for our understanding of galaxy evolution.Our spectroscopy shows that the submm galaxies are coeval with the important populations of star-forming galaxies and quasars detected at z= 2–3using optical and X-ray techniques.8,20,21,22We can use their relative space densities to compare and relate these populations.In a1000Mpc3box at z～2.5,there are10Lyman-

break galaxies with R AB<25.5(～0.2×L?1500)and1submm galaxy from our sample(with 850μm?ux>5mJy),but the single submm galaxy produces a comparable luminosity to the10Lyman-break galaxies.(Here R AB is the?ux normalized magnitude near6900?A; L?1500is the characteristic luminosity at restframe1500?A,denoting a change in slope in the luminosity function.)Equally,the volume density of submm galaxies is similar to that of narrow-line Type-II AGN selected at these redshifts,from both X-ray and optical surveys, and an order of magnitude greater than that of bright optical quasars with M B>?25.8 However,the links between the di?erent classes of sources all depend critically on whether the activity is intermittent or continuous.

To quantify the whole submm population using this survey we must account for several selection e?ects.In particular,requiring a radio identi?cation prior to spectroscopy limits the maximum redshift.Studies of galaxies at low and moderate redshifts suggest that changes in the dust properties,especially the dust temperature T d,modify the relative strength of the emission in the submm and radio wavebands.23The detectability of distant submm galaxies(at a?xed850-μm?ux)in the radio waveband thus depends on the dust temperature:warmer galaxies are detectable at z≥3,while the radio emission from cooler sources falls below the?ux limit at lower redshifts.18About30%of submm galaxies that are brighter than5mJy at850μm are not detected in the radio:these galaxies would be lost from our catalogue at z～2.5for the coldest plausible T d～25K,and at z>3for the typical T d?35K that we?nd.Hence,we can only place a lower limit on the space density in the highest redshift interval.The density derived at z=2should be una?ected by the need for the galaxies to be detected at radio wavelengths.

We must also consider the completeness of our spectroscopic observations.While our redshift completeness is relatively high(～30%),we failed to?nd convincing redshifts for 24galaxies.However,nine of of these have strong single emission line detections which could plausibly be identi?ed as Lyman-α.Some of the remainder without emission lines could lie in the spectroscopic desert,making redshifts di?cult to identify.The absence of sources at z～1.5in Table1suggests that this e?ect is probably responsible for some of the incompleteness.Our targets generally have faint UV continua,and so there is a bias

towards identifying redshifts for galaxies with strong emission lines.If the missing galaxies lie outside of the desert,but lack strong emission lines,then their radio detection suggests they probably lie in the same z=1–4range spanned by the spectroscopically identi?ed sources.

On the basis of bolometric luminosities estimated from our radio and submm mea-surements and redshifts(Table1),assuming the far-IR–radio correlation,we calculate the following luminosity densities from our survey:ρL(0.5

)×107L⊙Mpc?3.ρL(1.8

?5

To translate these values into star-formation densities we must subtract any contribution to the luminosities of these galaxies from the heating of dust by an active galactic nucleus (AGN).The proportion of the submm population detected in deep Chandra and XMM-Newton X-ray surveys,which are sensitive to even dust-obscured AGN,7,20at?ux densities signi?cantly greater than that expected from star formation alone is at most30%.Hence, we assume conservatively that the far-IR luminosity is derived from star formation in the remaining70%.Luminosity-density measurements can be translated into a star-formation density using the standard calibration of1.6–2.2×109L⊙(M⊙yr?1)?1.24 The bright radio-detected submm galaxies presented here represent just20%of the 850-μm background,yet their estimated star-formation densities at redshifts of2and3 are comparable with those inferred from optical observations.21Both of these estimates require corrections,in the case of the optical surveys an increase of a factor of5is needed to account for dust obscuration,25while our submm estimate needs to be corrected by a similar factor to account for spectroscopic incompleteness and sources below our submm ?ux limit.We?nd that the submm and Lyman-break populations encompass all of the star formation activity needed to reproduce the star formation history inferred from models of the background radiation and submm counts.4Hence,our substantially complete redshift survey provides the strongest evidence for a rapid increase in the volume density of dusty, very luminous galaxies in the distant Universe.Their density peaks at a redshift z?2.4 at a value about1000times greater than that at the present epoch.Thus we conclude that the balance between the star-formation density in the most luminous dust-obscured versus

unobscured galaxies has altered radically over the last80%of the history of the Universe.

References.

1.Fixsen,D.J.,Dwek,E.,Mather,J.C.,Bennett,C.L.,Shafer,R.A.The spectrum

of the extragalactic far-infrared background from the COBE FIRAS observations.

Astrophys.J.508,123–128(1998).

2.Smail,I.,Ivison,R.J.,&Blain,A.W.A deep submillimeter survey of lensing clusters:

a new window on galaxy formation and evolution.Astrophys.J.490,L5–L8(1997).

3.Smail,I.,Ivison R.J.,Blain,A.W.,&Kneib,J.-P.The nature of faint submillimetre-

selected galaxies.Mon.Not.R.Astron.Soc.331,495–520(2002).

4.Blain,A.W.,Smail,I.,Ivison,R.J.,Kneib,J.-P.The history of star-formation in

dusty galaxies.Mon.Not.R.Astron.Soc.302,632–648(1999).

5.Barger,A.J.,Cowie,L.L.,Richards,E.A.Mapping the evolution of high-redshift

dusty galaxies with submillimeter observations of a radio-selected sample.Astron.J.

119,2092–2109(2000).

6.Chapman,S.C.,Richards,E.A.,Lewis,G.F.,Wilson,G.,Barger,A.J.The nature

of the bright submillimeter galaxy population.Astrophys.J.548,L147–L151(2001).

7.Ivison,R.J.,Greve,T.,Smail,I.,Dunlop,J.,Roche,N.,Scott,S.,Page M.,Stevens,

J.,Almaini,O.,Blain,A.,Willott,C.,Fox,M.,Gilbank,D.,Serjeant,S.,&Hughes D.

Deep radio imaging of the SCUBA8-mJy survey?elds:submm source identi?cations and redshift distribution.Mon.Not.R.Astron.Soc.337,1(2002).

8.Boyle,B.J.,Shanks,T.,Croom,S.M.,Smith,R.J.,Miller,L.,Loaring,N.,Heymans,

C.The2dF QSO redshift survey–I.The optical luminosity function of quasi-stellar

objects.Mon.Not.R.Astron.Soc.317,1014–1022(2000).

9.Cowie,L.L.,Barger,A.J.,Kneib,J.-P.Faint Submillimeter Counts from Deep850

Micron Observations of the Lensing Clusters A370,A851,and A2390.Astron.J.

123,2197–2205(2002).

10.Ivison,R.J.,Smail,I.,Le Borgne,J.-F.,Blain,A.W.,Kneib,J.-P.,Bezecourt,J.,

Kerr,T.H.,&Davies,J.K.A hyperluminous galaxy at z=2.8found in a deep submillimetre survey.Mon.Not.R.Astron.Soc.298,583–593(1998).

11.Barger,A.J.,Cowie,L.L.,Smail,I.,Ivison,R.J.,Blain,A.W.,&Kneib,J.-P.

Redshift distribution of the faint submillimeter galaxy population.Astron.J.117, 2656–2665(1999).

12.Ivison,R.J.,Smail,I,Barger,A.J.,Kneib,J.-P.,Blain,A.W.,Owen,F.N.,Kerr,T.

H.,&Cowie,L.L.The diversity of SCUBA-selected galaxies Mon.Not.R.Astron.

Soc.315,209–221(2000).

13.Richards,E.A.The Nature of Radio Emission from Distant Galaxies:The1.4GHZ

Observations.Astrophys.J.533,611–630(2000).

14.Fomalont,E.B.,Kellermann,K.I.,Partridge,R.B.,Windhorst,R.A.,Richards,E.

A.The Microjansky Sky at8.4GHz.Astron.J.123,2402–2416(2002).

15.Barger,A.J.,Cowie,L.L.,Sanders,D.,Fulton,E.,Taniguchi,Y.,Sato,Y.,Kawara,

K.,Okuda,H.Submillimetre-wavelength detection of dusty star-forming galaxies at high redshift.Nature394,248–251(1998).

16.Chapman,S.C.,Barger,A.,Cowie,L.,Borys,C.,Capak,P.,Fomalont,E.,Lewis,

G.,Richards, E.,Scott,D.,Ste?en,A.,Wilson,G.,Yun,M.,The properties of

microjansky radio sources in the HDF-N,SSA13,and SSA22Fields.Astrophys.J.

585,57(2003).

17.Scott,S.E.,Fox,M.J.,Dunlop,J.S.,Serjeant,S.,Peacock,J.A.,Ivison,R.J.,Oliver,

S.,Mann,R.G.,Lawrence,A.,Efstathiou,A.,Rowan-Robinson,M.,Hughes,D.H., Archibald,E.N.,Blain,A.,Longair,M.The SCUBA8-mJy survey-I.Submillimetre maps,sources and number counts.Mon.Not.R.Astron.Soc.331,817–837(2002).

18.Chapman,S.C.,Lewis,G.F.,Scott,D.,Borys,C.,Richards,E.A.,Understanding the

nature of the optically faint radio sources and their connection to the submillimeter population.Astrophys.J.570,557–570(2002).

19.Condon,J.Radio emission from ordinary galaxies.Annu.Rev.Astron.Astrophy.

30,575–611(1992).

20.Barger,A.J.,Cowie,L.L.,Brandt,W.N.,Capak,P.,Garmire,G.P.,Hornschemier,

A.E.,Ste?en,A.T.,Wehner,E.H.X-ray,optical and infrared imaging and spectral

properties of the1-Ms Chandra Deep Field North sources.Astron.J.124,1839 (2002).

21.Steidel,C.C.,Adelberger,K.L.,Giavalisco,M.,Dickinson,M.&Pettini,M.Lyman-

break galaxies at z>4and the evolution of the ultraviolet luminosity density at high redshift.Astrophys.J.519,1–17(1999).

22.Steidel,C.,Hunt,M.,Shapley,A.,Adelberger,K.,Pettini,M.,Dickinson,M.&

Giavalisco,M.The population of faint optically-selected AGN at z～3.Astrophys.

J.in the press;also available as prerint astro-ph/0205142at https://www.360docs.net/doc/d96349117.html, (2002).

23.Blain,A.W.,Smail,I.,Ivison,R.J.,Kneib,J.-P.,Frayer,D.T.Submillimeter galax-

ies.Physics Reports369,111–196;also available as preprint astro-ph/0202228at https://www.360docs.net/doc/d96349117.html,(2002).

24.Kennicutt,R.C.Star formation in galaxies along the Hubble sequence.Annu.Rev.

Astron.Astrophys.36,189–232(1998).

25.Pettini,M.,Shapley,A.E.,Steidel,C.C.,Cuby,J.-G.,Dickinson,M.,Moorwood,A.

F.M.,Adelberger,K.L.,&Giavalisco,M.The rest-frame optical spectra of Lyman-

break galaxies:star formation,extinction,abundances and kinematics.Astrophys.J.

554,981–1000(2001).

26.Chapman,S.C.,Helou,G.,Lewis,G.F.,Dale,D.,The bi-variate luminosity-color dis-

tribution of IRAS galaxies,and impications for the high redshift Universe.Astrophys.

J.in the press;also available as preprint astro-ph/0301233at https://www.360docs.net/doc/d96349117.html, (2002).

27.Chapman,S.C.,Smail,I.,Ivison,R.,Blain,A.,The e?ect of lensing on the identi?-

cation of SCUBA galaxies,Mon.Not.R.Astron.Soc.335,17–21(2002).

28.Oke,J.B.,Cohen,J.G.,Carr,M.,Cromer,J.,Dingizian,A.,Harris,F.H.,Labrecque,

S.,Lucinio,R.,&Schaal,W.The Keck low-resolution imaging spectrometer.Publ.

Astron.Soc.Pac.107,375–385(1995).

29.Sheinis,A.I.,Bolte,M.,Epps,H.W.,Kibrick,R.I.,Miller,J.S.,Radovan,M.V.,

Bigelow,B.C.,&Sutin B.M.ESI,a new Keck Observatory echellette spectrograph and imager.Publ.Astron.Soc.Pac.114,851–865(2002).

30.Smail,I.,et al.,A vigorous starburst in the SCUBA galaxy N2-850.4.Mon.Not.

R.Astron.Soc.(in the press);preprint available at https://www.360docs.net/doc/d96349117.html,/astro-ph/0303128(2003).

Acknowledgments.

We are grateful to Chuck Steidel,Alice Shapley and Tim Heckman for insightful discus-sions.SCC acknowledges support from NASA.IRS acknowledges support from the Royal Society and a Philip Leverhulme Prize Fellowship.NRAO is operated by Associated Uni-versities Inc.,under a cooperative agreement with the US National Science Foundation. Data presented herein were obtained using the W.M.Keck Observatory,which is oper-ated as a scienti?c partnership among Caltech,the University of California and NASA. The Observatory was made possible by the generous?nancial support of the W.M.Keck Foundation.

The authors declare that they have no competing?nancial interests.

Correspondence and requests for materials should be addressed to Scott Chapman(schap-man@https://www.360docs.net/doc/d96349117.html,).

Table 1.

Positions of submm galaxies with redshifts from our survey,along with their measured red-shifts,submm ?uxes and optical magnitudes,infered dust temperatures T d and bolometric luminosities L bol .T d and L bol were calculated,based on the redshift,submm and radio ?ux densities,assuming that the far-IR–radio correlation applies.Sources are in order of decreasing ?ux density,as in Figure 1.(SMM163704.3+410530was previously published in 27.)Submm ?uxes for sources in the Lockman (10hr RA)and ElaisN2(16hr RA)?elds are from 17while ?uxes for other sources were measured ourselves.Six out of 10galaxies have I -band magnitudes fainter than 23.5,consistent with the optical ?ux distribution of blank-?eld submm galaxies presented elsewhere,16and con?rming that our sample is representative of the population.Galaxies with hotter inferred dust temperatures could have their radio ?ux densities enhanced by contribution from an active galactic nucleus.Understanding the relationship between submm galaxies and other high-redshift populations will be helped by comparing the strength of the clustering,both within and between the di?erent classes.This will require substantially larger samples than are currently available.

RA dec redshift

S 850μm (mJy)I -mag T d (K)L bol (1012 L ⊙)SMM105224.6+572119 2.429

11.7±3.425.921±5 3.0+2.0?0.7SMM163704.3+4105300.840

11.2±1.621.516+4.1?2.20.58+.32?.34SMM105230.6+572212 2.610

11.0±2.623.029±6 6.9+5.9?3.3SMM163650.0+405733 2.376

8.2±1.722.254+11?745+53?19SMM123600.2+621047 1.998

7.9±2.423.637+8?410+11?4SMM131201.2+424208 3.419

6.2±1.223.548+10?720+18?7SMM10520

7.7+571907 2.698

6.2±1.626.036+7?4

7.8+7.1?2.3SMM131212.7+424423 2.811

5.6±1.92

6.454+19?1030+60?16SMM163658.8+405733 1.189

5.1±1.422.425+5?91.5±1.2SMM105155.7+572312 3.699 4.5±1.324.259+26

?1630+82

?20

Figure Legends.

Figure1.The ten spectra from Table1with identi?ed redshifts(smoothed to the instrumental reso-lution)from the sample of34submm galaxies observed,spanning the I=22.2–26.4range.(Note that SMM163704.3+410530was previously published in27.)Pilot observations,using Keck’s ESI29spectro-graph on2001July16in the ELAIS-N217?eld yielded three spectra with strong emission lines.Multi-object Keck observations of31submm galaxies using LRIS28were made on2002March18–19in light cirrus conditions(with good0.8′′seeing)in the HDF&SSA13?elds5,16,and the Lockman Hole and ELAIS-N2?elds17.All the spectra probe the observed wavelength range from0.3–1μm.Exposures times were1.5–4.5hr,split into30-min integrations.Data reduction followed standard techniques using custom IRAF scripts.One-dimensional spectra were extracted and compared with template spectra and emission-line catalogues to identify redshifts.All identi?cations are based on multiple lines,most prominently the Lyαline which varies tremendously in both?ux(ranging from1to60μJy)and rest-frame equivalent width(3to>100?A).Weaker stellar/interstellar/AGN features and/or continuum breaks were detected in the spectra,strengthening the redshift identi?cations.Two galaxies at the same redshifts were identi?ed in the vicinity of the10robust submm sources,as shown for the companions SMMJ105155.7+572312-a(one of the few submm galaxies showing Lyman-αin absorption)and SMMJ105155.7+572312-b.The highest S/N spectrum(SMMJ163650.0+405733–30)includes features indicative of both strong starburst activity (P-Cygni wind absorption pro?les,stellar/interstellar absorption lines)and a weak AGN,a mix typical of hybrid starburst/Seyfert-2galaxies.None of our spectra have broad lines like Type-I AGN.Narrow-line Type-II AGN with enhanced N V and/or C IV emission are consistent with half of our spectra.Despite this evidence for AGN in these galaxies,they appear to be relatively weak in energetic terms as compared to those identi?ed in X-ray or optical surveys.

Figure2.The redshift histogram of our submm galaxy sample.We describe the selection e?ects using an evolving model of the local far-IR luminosity function,in which the dusty galaxies are represented by a range of template spectral energy distributions.The model has been tuned to?t the statistical properties of the submm-radio galaxy population(surface density on the sky and submm–radio colours).26 As a range of spectral energy distributions are represented at each galaxy luminosity,a broader redshift distribution results than if the luminosity was tied one-to-one with the dust temperature.23We plot the predicted redshift distributions for submm galaxies with?ux densities S850μm>5mJy(solid line)and

radio sources with30μJy

的、地、得的用法和区别

“的、地、得”的用法和区别 导入（进入美妙的世界啦~） “的、地、得”口诀儿歌 的地得，不一样，用法分别记心上， 左边白，右边勺，名词跟在后面跑。 美丽的花儿绽笑脸，青青的草儿弯下腰， 清清的河水向东流，蓝蓝的天上白云飘， 暖暖的风儿轻轻吹，绿绿的树叶把头摇， 小小的鱼儿水中游，红红的太阳当空照， 左边土，右边也，地字站在动词前， 认真地做操不马虎，专心地上课不大意， 大声地朗读不害羞，从容地走路不着急， 痛快地玩耍来放松，用心地思考解难题， 勤奋地学习要积极，辛勤地劳动花力气， 左边两人双人得，形容词前要用得， 兔子兔子跑得快，乌龟乌龟爬得慢， 青青竹子长得快，参天大树长得慢， 清晨锻炼起得早，加班加点睡得晚， 欢乐时光过得快，考试题目出得难。 知识典例（注意咯，下面可是黄金部分！） 的、地、得 “的”、“地”、“得”的用法区别本是中小学语文教学中最基本的常识，但在使用中也最容易发生混淆，再加上一段时间里，中学课本中曾将这三个词的用法统一为“的”，因此造成了很多人对它们的用法含混不清进而乱用一通的现象。

一、“的、地、得”的基本概念 1、“的、地、得”的相同之处。 “的、地、得”是现代汉语中高频度使用的三个结构助词，都起着连接作用；它们在普通话中都读轻声“de”，没有语音上的区别。 2、“的、地、得”的不同之处。 吕叔湘、朱德熙所著《语法修辞讲话》认为“的”兼职过多，负担过重，而力主“的、地、得”严格分工。50 年代以来的诸多现代汉语论著和教材，一般也持这一主张。从书面语中的使用情况看，“的”与“地”、“得”的分工日趋明确，特别是在逻辑性很强的论述性、说明性语言中，如法律条款、学术论著、外文译著、教科书等，更是将“的”与“地”、“得”分用。 “的、地、得”在普通话里都读轻声“de”，但在书面语中有必要写成三个不同的字：在定语后面写作“的”，在状语后面写作“地”，在补语前写作“得”。这样做的好处，就是可使书面语言精确化。 二、“的、地、得”的用法 1、的——定语的标记，一般用在主语和宾语的前面。“的”前面的词语一般用来修饰、限制“的”后面的事物，说明“的”后面的事物怎么样。结构形式一般为：形容词、名词（代词）+的+名词。如： ①颐和园(名词)的湖光山色（主语）美不胜收。 ②她是一位性格开朗的女子(名词，宾语)。 2、地——状语的标记，一般用在谓语（动词、形容词）前面。“地”前面的词语一般用来形容“地”后面的动作，说明“地”后面的动作怎么样。结构方式一般为：形容词（副词）+地+动词（形容词）。如： ③她愉快(形容词)地接受(动词，谓语)了这件礼物。 ④天渐渐(时间副词)地冷(形容词，谓语)起来。 3、得——补语的标记，一般用在谓语后面。“得”后面的词语一般用来补充说明“得”前面的动作怎么样，结构形式一般为：动词（形容词）+得+副词。如： ⑤他们玩(动词，谓语)得真痛快(补语)。

of与for的用法以及区别

of与for的用法以及区别 for 表原因、目的 of 表从属关系 介词of的用法 （1）所有关系 this is a picture of a classroom （2）部分关系 a piece of paper a cup of tea a glass of water a bottle of milk what kind of football，American of soccer？ （3）描写关系 a man of thirty 三十岁的人 a man of shanghai 上海人 （4）承受动作 the exploitation of man by man．人对人的剥削。 （5）同位关系 It was a cold spring morning in the city of London in England． （6）关于，对于 What do you think of Chinese food？ 你觉得中国食品怎么样？ 介词 for 的用法小结 1. 表示“当作、作为”。如: I like some bread and milk for breakfast. 我喜欢把面包和牛奶作为早餐。What will we have for supper? 我们晚餐吃什么?

2. 表示理由或原因,意为“因为、由于”。如: Thank you for helping me with my English. 谢谢你帮我学习英语。 Thank you for your last letter. 谢谢你上次的来信。 Thank you for teaching us so well. 感谢你如此尽心地教我们。 3. 表示动作的对象或接受者,意为“给……”、“对…… (而言)”。如: Let me pick it up for you. 让我为你捡起来。 Watching TV too much is bad for your health. 看电视太多有害于你的健康。 4. 表示时间、距离,意为“计、达”。如: I usually do the running for an hour in the morning. 我早晨通常跑步一小时。We will stay there for two days. 我们将在那里逗留两天。 5. 表示去向、目的,意为“向、往、取、买”等。如: let’s go for a walk. 我们出去散步吧。 I came here for my schoolbag.我来这儿取书包。 I paid twenty yuan for the dictionary. 我花了20元买这本词典。 6. 表示所属关系或用途,意为“为、适于……的”。如: It’s time for school. 到上学的时间了。 Here is a letter for you. 这儿有你的一封信。 7. 表示“支持、赞成”。如: Are you for this plan or against it? 你是支持还是反对这个计划? 8. 用于一些固定搭配中。如: Who are you waiting for? 你在等谁? For example, Mr Green is a kind teacher. 比如,格林先生是一位心地善良的老师。

to与for的用法和区别

to与for的用法和区别 一般情况下, to后面常接对象; for后面表示原因与目的为多。 Thank you for helping me. Thanks to all of you. to sb.表示对某人有直接影响比如，食物对某人好或者不好就用to; for表示从意义、价值等间接角度来说，例如对某人而言是重要的，就用for. for和to这两个介词，意义丰富，用法复杂。这里仅就它们主要用法进行比较。 1. 表示各种“目的” 1. What do you study English for? 你为什么要学英语？ 2. She went to france for holiday. 她到法国度假去了。 3. These books are written for pupils. 这些书是为学生些的。 4. hope for the best, prepare for the worst. 作最好的打算，作最坏的准备。 2．对于 1．She has a liking for painting. 她爱好绘画。 2．She had a natural gift for teaching. 她对教学有天赋/ 3．表示赞成同情，用for不用to. 1. Are you for the idea or against it? 你是支持还是反对这个想法？ 2. He expresses sympathy for the common people.. 他表现了对普通老百姓的同情。 3. I felt deeply sorry for my friend who was very ill. 4 for表示因为，由于（常有较活译法） 1 Thank you for coming. 谢谢你来。 2. France is famous for its wines. 法国因酒而出名。 5．当事人对某事的主观看法，对于（某人），对…来说（多和形容词连用）用介词to，不用for.. He said that money was not important to him. 他说钱对他并不重要。 To her it was rather unusual. 对她来说这是相当不寻常的。 They are cruel to animals. 他们对动物很残忍。 6．for和fit, good, bad, useful, suitable 等形容词连用，表示适宜，适合。 Some training will make them fit for the job. 经过一段训练，他们会胜任这项工作的。 Exercises are good for health. 锻炼有益于健康。 Smoking and drinking are bad for health. 抽烟喝酒对健康有害。 You are not suited for the kind of work you are doing. 7. for表示不定式逻辑上的主语，可以用在主语、表语、状语、定语中。 1．It would be best for you to write to him. 2．The simple thing is for him to resign at once. 3．There was nowhere else for me to go. 4．He opened a door and stood aside for her to pass.

“的、地、得”的用法和区别

的、地、得的用法和区别 的、地、得的用法和区别老班教育 一、的、地、得的基本概念 1、的、地、得的相同之处。 的、地、得是现代汉语中高频度使用的三个结构助词，都起着连接作用；它们在普通话中都读轻声de，没有语音上的区别。 2、的、地、得的不同之处。 吕叔湘、朱德熙所著《语法修辞讲话》认为的兼职过多，负担过重，而力主的、地、得严格分工。50 年代以来的诸多现代汉语论著和教材，一般也持这一主张。从书面语中的使用情况看，的与地、得的分工日趋明确，特别是在逻辑性很强的论述性、说明性语言中，如法律条款、学术论著、外文译著、教科书等，更是将的与地、得分用。 的、地、得在普通话里都读轻声de，但在书面语中有必要写成三个不同的字：在定语后面写作的，在状语后面写作地，在补语前写作得。这样做的好处，就是可使书面语言精确化。 二、的、地、得的用法 （一）、用法 1、的——定语的标记，一般用在主语和宾语的前面。的前面的词语一般用来修饰、限制的后面的事物，说明的后面的事物怎么样。 结构形式一般为：形容词、名词（代词）+的+名词。如： 颐和园(名词)的湖光山色（主语）美不胜收。 她是一位性格开朗的女子(名词，宾语)。 2、地——状语的标记，一般用在谓语（动词、形容词）前面。地前面的词语一般用来形容地后面的动作，说明地后面的动作怎么样。 结构方式一般为：形容词（副词）+地+动词（形容词）。如： 她愉快(形容词)地接受(动词，谓语)了这件礼物。 天渐渐(时间副词)地冷(形容词，谓语)起来。 3、得——补语的标记，一般用在谓语后面。得后面的词语一般用来补充说明得前面的动作怎么样。 结构形式一般为：动词（形容词）+得+副词。如： 他们玩(动词，谓语)得真痛快(补语)。 她红(形容词，谓语)得发紫(补语)。 （二）、例说 的，一般用在名词和形容词的后面，用在描述或限制人物、事物时，形容的词语与被形容的词语之间，表示一种描述的结果。如：漂亮的衣服、辽阔的土地、高大的山脉。结构一般为名词（代词或形容词）+的+名词。如，我的书、你的衣服、他的孩子，美丽的景色、动听的歌曲、灿烂的笑容。 地，用法简单些，用在描述或限制一种运动性质、状态时，形容的词语与被形容的词语之间。结构通常是形容词+地+动词。前面的词语一般用来形容后面的动作。一般地的后面只跟动词。比如高兴地跳、兴奋地叫喊、温和地说、飞快地跑；匆匆地离开；慢慢地移动......... 得，用在说明动作的情况或结果的程度时，说明的词语与被说明的词语之间，后面的词语一般用来补充和说明前面的情况。比如。跑得飞快、跳得很高、显得高雅、显得很壮、馋得直流口水、跑得快、飞得高、走得慢、红得很……得通常用在动词和形容词（动词之间）。

常用介词用法(for to with of)

For的用法 1. 表示“当作、作为”。如: I like some bread and milk for breakfast. 我喜欢把面包和牛奶作为早餐。 What will we have for supper? 我们晚餐吃什么? 2. 表示理由或原因,意为“因为、由于”。如: Thank you for helping me with my English. 谢谢你帮我学习英语。 3. 表示动作的对象或接受者,意为“给……”、“对…… (而言)”。如: Let me pick it up for you. 让我为你捡起来。 Watching TV too much is bad for your health. 看电视太多有害于你的健康。 4. 表示时间、距离,意为“计、达”。如: I usually do the running for an hour in the morning. 我早晨通常跑步一小时。 We will stay there for two days. 我们将在那里逗留两天。 5. 表示去向、目的,意为“向、往、取、买”等。如: Let’s go for a walk. 我们出去散步吧。 I came here for my schoolbag.我来这儿取书包。 I paid twenty yuan for the dictionary. 我花了20元买这本词典。 6. 表示所属关系或用途,意为“为、适于……的”。如: It’s time for school. 到上学的时间了。 Here is a letter for you. 这儿有你的一封信。 7. 表示“支持、赞成”。如: Are you for this plan or against it? 你是支持还是反对这个计划? 8. 用于一些固定搭配中。如: Who are you waiting for? 你在等谁? For example, Mr Green is a kind teacher. 比如,格林先生是一位心地善良的老师。 尽管for 的用法较多，但记住常用的几个就可以了。 to的用法: 一：表示相对，针对 be strange (common, new, familiar, peculiar) to This injection will make you immune to infection. 二：表示对比，比较 1：以-ior结尾的形容词，后接介词to表示比较，如：superior ,inferior,prior,senior,junior 2: 一些本身就含有比较或比拟意思的形容词，如equal，similar，equivalent，analogous A is similar to B in many ways.

(完整版)介词for用法归纳

介词for用法归纳 用法1：(表目的)为了。如： They went out for a walk. 他们出去散步了。 What did you do that for? 你干吗这样做？ That’s what we’re here for. 这正是我们来的目的。 What’s she gone for this time? 她这次去干什么去了？ He was waiting for the bus. 他在等公共汽车。 【用法说明】在通常情况下，英语不用for doing sth 来表示目的。如： 他去那儿看他叔叔。 误：He went there for seeing his uncle. 正：He went there to see his uncle. 但是，若一个动名词已名词化，则可与for 连用表目的。如： He went there for swimming. 他去那儿游泳。(swimming 已名词化) 注意：若不是表目的，而是表原因、用途等，则其后可接动名词。(见下面的有关用法) 用法2：(表利益)为，为了。如： What can I do for you? 你想要我什么？ We study hard for our motherland. 我们为祖国努力学习。 Would you please carry this for me? 请你替我提这个东西好吗？ Do more exercise for the good of your health. 为了健康你要多运动。 【用法说明】(1) 有些后接双宾语的动词(如buy, choose, cook, fetch, find, get, order, prepare, sing, spare 等)，当双宾语易位时，通常用for 来引出间接宾语，表示间接宾语为受益者。如： She made her daughter a dress. / She made a dress for her daughter. 她为她女儿做了件连衣裙。 He cooked us some potatoes. / He cooked some potatoes for us. 他为我们煮了些土豆。 注意，类似下面这样的句子必须用for： He bought a new chair for the office. 他为办公室买了张新办公椅。 (2) 注意不要按汉语字面意思，在一些及物动词后误加介词for： 他们决定在电视上为他们的新产品打广告。 误：They decided to advertise for their new product on TV. 正：They decided to advertise their new product on TV. 注：advertise 可用作及物或不及物动词，但含义不同：advertise sth＝为卖出某物而打广告；advertise for sth＝为寻找某物而打广告。如：advertise for a job=登广告求职。由于受汉语“为”的影响，而此处误加了介词for。类似地，汉语中的“为人民服务”，说成英语是serve the people，而不是serve for the people，“为某人的死报仇”，说成英语是avenge sb’s death，而不是avenge for sb’s death，等等。用法3：(表用途)用于，用来。如： Knives are used for cutting things. 小刀是用来切东西的。 This knife is for cutting bread. 这把小刀是用于切面包的。 It’s a machine for slicing bread. 这是切面包的机器。 The doctor gave her some medicine for her cold. 医生给了她一些感冒药。 用法4：为得到，为拿到，为取得。如： He went home for his book. 他回家拿书。 He went to his friend for advice. 他去向朋友请教。 She often asked her parents for money. 她经常向父母要钱。

的地得的用法和区分

《“的、地、得”的用法》语文微课教案 一、教学背景 在语言文字规范化大背景下，帮助学生解决应用“的地得”的疑惑与困难。 二、设计思路 针对学生对于“的地得”的误用与忽视展开教学，规范结构助词“的地得”的使用。按照“问题的提出、问题的分析、问题的解决”的思路展开教学，总结归纳优化的方式方法。 三、教学目标 1、知道“怎么样的什么、怎么样地干什么、干得怎么样”三种固定搭配。 2、掌握“的、地、得”的区别与联系。 3、运用小儿歌“动前土、名前白、行动后面双人来”的口诀帮助正确使用“的、地、得”。 四、教学重难点 1、知道“的、地、得”的区别。 2、在实际情境中正确运用“的、地、得”。 五、教学时间 8分钟微课堂 六、教学适用对象 义务教育九年制内的学生 七、教学准备

多媒体课件、录屏软件 八、教学设计与过程 开场白： 同学们好！今天我们一起来学习“的、地、得”的正确用法。首先我们来了解一下它们的区别。 1、相同之处：原来它们都是念轻声“de”，都是结构助词，起连接作用。 2、不同之处：在书面语中要写成三个不同的字，而且它们的搭配及用法也各不相同。 （1）怎么样的什么 （2）怎样样地干什么 （3）干得怎么样 下面我们就来学习一下它们的正确用法。 白勺“的”的结构是用“形容词或名词或代词+的+名词”来表示，而我们最常见，用得最多的还是“形容词+的+名词”的结构。 而土也“地”的用法可以用“形容词+地+动词”的结构来表示。 双人“得”是用“动词+得+形容词”的结构来表示 3、练习巩固 （1）形近区分 静静（的）河面静静（地）写字欢乐（的）山谷

欢乐（地）歌唱满意（地）点头满意（的）作品 （2）类别区分 1）跑（得）飞快飞快（地）跑 2）愉快（的）旅行旅行（得）愉快 3）强烈（的）渴望强烈（地）渴望 （3）综合杂糅 小雏鹰飞到大树的上方，高兴地喊起来：“我真的会飞啦！而且飞（得）很高呢！” 小结：能填对这个句子的你肯定就已经学会它们的用法了！ 4、特殊情况 质疑：假如遇到特殊情况怎么办呢？ 我从书包里拿出书交给她们，她们高兴得．围着我跳起舞来。（出自二年级上册《日记两则》） （1）质疑：为什么这里要使用“得”呢？ （2）释疑：原来这里强调的是心情，动词在后，形容词在前，相当于后置，“得”修饰“跳舞”而非“围”。现在你明白了吧？ 5、小结归纳： 怎么样，你们学会了吗？为了让同学们能够更快的记住它们的用法，老师送给大家一首口诀来帮助你们熟记三个“的”的正确使用方法：动前土、名前白、行动后面双人来。

of和for的用法

of 1....的,属于 One of the legs of the table is broken. 桌子的一条腿坏了。 Mr.Brown is a friend of mine. 布朗先生是我的朋友。 2.用...做成的;由...制成 The house is of stone. 这房子是石建的。 3.含有...的;装有...的 4....之中的;...的成员 Of all the students in this class,Tom is the best. 在这个班级中,汤姆是最优秀的。 5.(表示同位) He came to New York at the age of ten. 他在十岁时来到纽约。 6.(表示宾格关系) He gave a lecture on the use of solar energy. 他就太阳能的利用作了一场讲演。 7.(表示主格关系) We waited for the arrival of the next bus. 我们等待下一班汽车的到来。

I have the complete works of Shakespeare. 我有莎士比亚全集。 8.来自...的;出自 He was a graduate of the University of Hawaii. 他是夏威夷大学的毕业生。 9.因为 Her son died of hepatitis. 她儿子因患肝炎而死。 10.在...方面 My aunt is hard of hearing. 我姑妈耳朵有点聋。 11.【美】(时间)在...之前 12.(表示具有某种性质) It is a matter of importance. 这是一件重要的事。 For 1.为,为了 They fought for national independence. 他们为民族独立而战。 This letter is for you. 这是你的信。

双宾语 to for的用法

1.两者都可以引出间接宾语，但要根据不同的动词分别选用介词to 或for：(1) 在give, pass, hand, lend, send, tell, bring, show, pay, read, return, write, offer, teach, throw 等之后接介词to。 如： 请把那本字典递给我。 正：Please hand me that dictionary. 正：Please hand that dictionary to me. 她去年教我们的音乐。 正：She taught us music last year. 正：She taught music to us last year. (2) 在buy, make, get, order, cook, sing, fetch, play, find, paint, choose,prepare, spare 等之后用介词for 。如： 他为我们唱了首英语歌。 正：He sang us an English song. 正：He sang an English song for us. 请帮我把钥匙找到。 正：Please find me the keys. 正：Please find the keys for me. 能耽搁你几分钟吗(即你能为我抽出几分钟吗)? 正：Can you spare me a few minutes? 正：Can you spare a few minutes for me? 注：有的动词由于搭配和含义的不同，用介词to 或for 都是可能的。如：do sb a favour＝do a favour for sb 帮某人的忙 do sb harm＝do harm to sb 对某人有害

的地得的用法教案

“的、地、得”的用法教案 教学目标： 1.能通过看视频知道“的、地、得”的用法区别。 2.能在小组合作中正确掌握“的、地、得”的用法。 3.能正确熟练地运用“的、地、得”。 教学重点：通过看视频知道“的、地、得”的用法区别。 教学难点：正确熟练地运用“的、地、得”。 教学过程： 一、导入（板书课题：“的、地、得”的用法“的、地、得”） 这三个字认识吧！虽然它们都有一个相同的读音de，但用法却不一样，可不能把他们用错了。究竟他们的用法有什么不同，我们来听听他们的故事吧！ 二、看微视频，学习“的、地、得”的用法区别。 三、小结： 1.孩子们，刚才看了视频知道他们是谁吗？（白勺的，土也地，双人得。） （1）白勺的是个杂货铺老板，她的店里都有什么？（彩色的毛巾美味的汉堡结实的帐篷舒适的儿童车捕捉风的网会唱歌的小树开个没完的花朵优美动听的歌曲飘来飘去的云……）还可能有什么？ 你们一定会发现，白勺的的用法有什么特点？（后面是名词。）板书：名词 （2）土也地是个运动男孩，他喜欢？（悠闲地散步欢快地跳舞兴奋地跳跃开心地捕蝴蝶看图书踢球骑自行洗澡吃冰淇淋……）他还可能喜欢干什么呢？你发现了吗？土也地的用法特点？（后面是动词。）板书：动词 （3）双人得呢？她是个总喜欢评价别人的小妹妹。（球踢得真棒舞跳得精彩长得好高呀……） 她可能还怎么评价别人？（歌唱得动听饭吃得很饱人长得漂亮）你们会发现，双人得的前面通常都是——动词。板书：动词 2.小结：所以，他们的用法也很简单，区别就在这里。 （白勺的用在名词前面；土也地用在动词前面；双人得用在动词后面。）你明白了吗？ 四、我来考考你们，看哪一组完成得又对又快！ 1.菜鸟级练习 2.老鸟级练习 3.大虾级练习 五、总结

for和of的用法

for的用法： 1. 表示“当作、作为”。如: I like some bread and milk for breakfast. 我喜欢把面包和牛奶作为早餐。 What will we have for supper? 我们晚餐吃什么? 2. 表示理由或原因,意为“因为、由于”。如: Thank you for helping me with my English. 谢谢你帮我学习英语。 Thank you for your last letter. 谢谢你上次的来信。 Thank you for teaching us so well. 感谢你如此尽心地教我们。 3. 表示动作的对象或接受者,意为“给……”、“对…… (而言)”。如: Let me pick it up for you. 让我为你捡起来。 Watching TV too much is bad for your health. 看电视太多有害于你的健康。 4. 表示时间、距离,意为“计、达”。如:

I usually do the running for an hour in the morning. 我早晨通常跑步一小时。 We will stay there for two days. 我们将在那里逗留两天。 5. 表示去向、目的,意为“向、往、取、买”等。如: Let’s go for a walk. 我们出去散步吧。 I came here for my schoolbag.我来这儿取书包。 I paid twenty yuan for the dictionary. 我花了20元买这本词典。 6. 表示所属关系或用途,意为“为、适于……的”。如: It’s time for school. 到上学的时间了。 Here is a letter for you. 这儿有你的一封信。 7. 表示“支持、赞成”。如: Are you for this plan or against it? 你是支持还是反对这个计划? 8. 用于一些固定搭配中。如:

for和to区别

1.表示各种“目的”，用for （1）What do you study English for 你为什么要学英语？ （2）went to france for holiday. 她到法国度假去了。 （3）These books are written for pupils. 这些书是为学生些的。 （4）hope for the best, prepare for the worst. 作最好的打算，作最坏的准备。 2．“对于”用for （1）She has a liking for painting. 她爱好绘画。 （2）She had a natural gift for teaching. 她对教学有天赋/ 3．表示“赞成、同情”，用for （1）Are you for the idea or against it 你是支持还是反对这个想法？ （2）He expresses sympathy for the common people.. 他表现了对普通老百姓的同情。 （3）I felt deeply sorry for my friend who was very ill. 4. 表示“因为，由于”（常有较活译法），用for （1）Thank you for coming. 谢谢你来。

（2）France is famous for its wines. 法国因酒而出名。 5．当事人对某事的主观看法，“对于（某人），对…来说”，（多和形容词连用），用介词to，不用for. （1）He said that money was not important to him. 他说钱对他并不重要。 （2）To her it was rather unusual. 对她来说这是相当不寻常的。 （3）They are cruel to animals. 他们对动物很残忍。 6．和fit, good, bad, useful, suitable 等形容词连用，表示“适宜，适合”，用for。（1）Some training will make them fit for the job. 经过一段训练，他们会胜任这项工作的。 （2）Exercises are good for health. 锻炼有益于健康。 （3）Smoking and drinking are bad for health. 抽烟喝酒对健康有害。 （4）You are not suited for the kind of work you are doing. 7. 表示不定式逻辑上的主语，可以用在主语、表语、状语、定语中。 （1）It would be best for you to write to him. （2） The simple thing is for him to resign at once.

英语形容词和of for 的用法

加入收藏夹 主题： 介词试题It’s + 形容词 + of sb. to do sth.和It’s + 形容词 + for sb. to do sth.的用法区别。 内容： It's very nice___pictures for me. A.of you to draw B.for you to draw C.for you drawing C.of you drawing 提交人：杨天若时间：1/23/2008 20:5:54 主题：for 与of 的辨别 内容：It's very nice___pictures for me. A.of you to draw B.for you to draw C.for you drawing C.of you drawing 答：选A 解析：该题考查的句型It’s + 形容词+ of sb. to do sth.和It’s +形容词+ for sb. to do sth.的用法区别。 “It’s + 形容词+ to do sth.”中常用of或for引出不定式的行为者，究竟用of sb.还是用for sb.，取决于前面的形容词。 1) 若形容词是描述不定式行为者的性格、品质的，如kind，good，nice，right，wrong，clever，careless，polite，foolish等，用of sb. 例： It’s very kind of you to help me. 你能帮我，真好。 It’s clever of you to work out the maths problem. 你真聪明，解出了这道数学题。 2) 若形容词仅仅是描述事物，不是对不定式行为者的品格进行评价，用for sb.，这类形容词有difficult，easy，hard，important，dangerous，（im）possible等。例： It’s very dangerous for children to cross the busy street. 对孩子们来说，穿过繁忙的街道很危险。 It’s difficult for u s to finish the work. 对我们来说，完成这项工作很困难。 for 与of 的辨别方法： 用介词后面的代词作主语，用介词前边的形容词作表语，造个句子。如果道理上通顺用of，不通则用for. 如： You are nice.(通顺，所以应用of)。 He is hard.(人是困难的，不通，因此应用for.) 由此可知，该题的正确答案应该为A项。 提交人：f7_liyf 时间：1/24/2008 11:18:42

双宾语tofor的用法

1. 两者都可以引出间接宾语，但要根据不同的动词分别选用介词to 或for： (1) 在give, pass, hand, lend, send, tell, bring, show, pay, read, return, write, offer, teach, throw 等之后接介词to。 如： 请把那本字典递给我。 正：Please hand me that dictionary. 正：Please hand that dictionary to me. 她去年教我们的音乐。 正：She taught us music last year. 正：She taught music to us last year. (2) 在buy, make, get, order, cook, sing, fetch, play, find, paint, choose,prepare, spare 等之后用介词for 。如： 他为我们唱了首英语歌。 正：He sang us an English song. 正：He sang an English song for us. 请帮我把钥匙找到。 正：Please find me the keys. 正：Please find the keys for me. 能耽搁你几分钟吗(即你能为我抽出几分钟吗)? 正：Can you spare me a few minutes? 正：Can you spare a few minutes for me? 注：有的动词由于搭配和含义的不同，用介词to 或for 都是可能的。如： do sb a favou r do a favour for sb 帮某人的忙 do sb harnn= do harm to sb 对某人有害

的 地 得 用法辨析

的、得、地的用法：动词前提土旁、动词后双人旁、一动不动白字旁 （一） 的地得，不一样，用法分别记心上， 左边白，右边勺，名词跟在后面跑。 美丽的花儿绽笑脸，青青的草儿弯下腰， 清清的河水向东流，蓝蓝的天上白云飘， 暖暖的风儿轻轻吹，绿绿的树叶把头摇， 小小的鱼儿水中游，红红的太阳当空照， 左边土，右边也，地字站在动词前， 认真地做操不马虎，专心地上课不大意， 大声地朗读不害羞，从容地走路不着急， 痛快地玩耍来放松，用心地思考解难题， 勤奋地学习要积极，辛勤地劳动花力气， 左边两人就使得，形容词前要用得， 兔子兔子跑得快，乌龟乌龟爬得慢， 青青竹子长得快，参天大树长得慢， 清晨锻炼起得早，加班加点睡得晚， 欢乐时光过得快，考试题目出得难。 （二）“的、地、得”快板 的地得、的地得，用作助词都读de. 作文写话用不准，朗读往往会念错。 有趣的活动、绿的树，活动是事，树是物。 事物前面用的字，小朋友们都记着。 认真地想、快快地跑，想跑看摸是动作。 动作前面用地字，位置千万不要挪。 看得清，记得准，唱得好，飞得高。 动作后面用得字，补充说明要记牢。 （三）“的、地、得”用法简要口诀 名词前面“白勺”“的”， 动词前面“土也”“地”， 形容动后“双人”“得”， 当作助词都读“de”。 二、“的、地、得”用法小析 “的”后面跟的都是表示事物名称的词或词语，如：敬爱的总理、慈祥的老人、戴帽子的男孩、珍贵的教科书、鸟的天堂、伟大的祖国、有趣的情节、优雅的环境、可疑的情况、团结友爱的集体、他的妈妈、可爱的花儿、谁的橡皮、清清的河水...... “地”后面跟的都是表示动作的词或词语，如：高声地喊、愉快地唱、拼命地逃、疯狂地咒骂、严密地注视、一次又一次地握手、迅速地包围、沙沙地直响、斩钉截铁地说、从容不迫地申述、用力地踢、仔细地看、开心地笑笑......” “得”前面跟的多数是表示动作的词或词语，后面跟的都是形容事物状态的词或词语，表示怎么怎么样的，如：走得很快、踩得稀烂、疼得直叫唤、瘦得皮包骨头、红得发紫、气得双脚直跳、理解得十分深刻、乐得合不拢嘴、惊讶得目瞪口呆、大得很、扫得真干净、笑得多甜啊...... 三、“的、地、得”的用法补充说明：

to和for的用法有什么不同(一)

to和for的用法有什么不同（一） 一、引出间接宾语时的区别 两者都可以引出间接宾语，但要根据不同的动词分别选用介词to 或for，具体应注意以下三种情况： 1. 在give, pass, hand, lend, send, tell, bring, show, pay, read, return, write, offer, teach, throw 等之后接介词to。如： 请把那本字典递给我。 正：Please hand me that dictionary. 正：Please hand that dictionary to me. 她去年教我们的音乐。 正：She taught us music last year. 正：She taught music to us last year. 2. 在buy, make, get, order, cook, sing, fetch, play, find, paint, choose, prepare, spare 等之后用介词for 。如： 他为我们唱了首英语歌。 正：He sang us an English song. 正：He sang an English song for us. 请帮我把钥匙找到。 正：Please find me the keys. 正：Please find the keys for me. 能耽搁你几分钟吗(即你能为我抽出几分钟吗)? 正：Can you spare me a few minutes?

正：Can you spare a few minutes for me? 3. 有的动词由于用法和含义不同，用介词to 或for 都是可能的。如： do sb a favor＝do a favor for sb 帮某人的忙 do sb harm＝do harm to sb 对某人有害 在有的情况下，可能既不用for 也不用to，而用其他的介词。如： play sb a trick＝play a trick on sb 作弄某人 请比较： play sb some folk songs＝play some folk songs for sb 给某人演奏民歌 有时同一个动词，由于用法不同，所搭配的介词也可能不同，如leave sbsth 这一结构，若表示一般意义的为某人留下某物，则用介词for 引出间接宾语，即说leave sth for sb；若表示某人死后遗留下某物，则用介词to 引出间接宾语，即说leave sth to sb。如： Would you like to leave him a message? / Would you like to leave a message for him? 你要不要给他留个话？ Her father left her a large fortune. / Her father left a large fortune to her. 她父亲死后给她留下了一大笔财产。 二、表示目标或方向的区别 两者均可表示目标、目的地、方向等，此时也要根据不同动词分别对待。如： 1. 在come, go, walk, move, fly, ride, drive, march, return 等动词之后通常用介词to 表示目标或目的地。如： He has gone to Shanghai. 他到上海去了。 They walked to a river. 他们走到一条河边。