a r X i v :a s t r o -p h /0103055v 1 3 M a r 2001
Mon.Not.R.Astron.Soc.000,000–000(0000)Printed 1February 2008
(MN L A T E X style ?le v1.4)
A Survey of hard spectrum ROSAT sources 2:optical
identi?cation of hard sources
M.J.Page 1,J.P.D.Mittaz 1,F.J.Carrera 1,2
1Mullard Space Science Laboratory,University College London,Holmbury St Mary,Dorking,Surrey RH56NT,UK.2Instituto
de F′?sica de Cantabria (Consejo Superior de Investigaciones Cient′??cas–Universidad de Cantabria),39005Santander,Spain.
ABSTRACT
We have surveyed 188ROSAT PSPC ?elds for X–ray sources with hard spectra
(α<0.5);such sources must be major contributors to the X–ray background at faint ?uxes.In this paper we present optical identi?cations for 62of these sources:28AGN which show broad lines in their optical spectra (BLAGN),13narrow emission line galaxies (NELGs),5galaxies with no visible emission lines,8clusters and 8Galactic stars.
The BLAGN,NELGs and galaxies have similar distributions of X–ray ?ux and spectra.Their ROSAT spectra are consistent with their being AGN obscured by columns of 20.5 We propose that BLAGN are likely to constitute a signi?cant fraction of the faint,hard,0.5-2keV population and could be important to reproducing the shape of the X–ray background,because they are the most numerous type of object in our sample (comprising almost half the identi?ed sources),and because all our high redshift (z >1)identi?ed hard sources have broad lines. 1 INTRODUCTION The origin of most of the X–ray emission in the Uni-verse is still unknown because the sources that produce most of the >2keV X–ray background (XRB)are still to be resolved.ROSAT surveys have succeeded in resolv-ing ～80%of the 1-2keV XRB into individual sources (Hasinger et al.1998),and optical identi?cation and X–ray spectroscopy has been possible for brighter sources which produce ～40%of the 1-2keV background.The majority of these sources are broad line AGN (hereafter BLAGN),and at faint ?uxes narrow emission line galaxies (hereafter NELGs,McHardy et al.1998);Schmidt et al.(1998)argued that the NELGs are also AGN,but with low luminosity or obscured broad line regions.On aver-age,faint NELGs have harder X–ray spectra (f ν∝ν?αwith α～0.5,Romero-Colmenero et al.1996,Almaini et al.1996)than the broad line AGN which have mean α～1(Mittaz et al.1999,Ciliegi et al.1994). Despite the success of ROSAT surveys,the XRB can-not be synthesised by extrapolating the observed source populations to faint ?uxes,because the resultant spec-trum would be softer than that of the background;this discrepancy is present for all energy bands between 0.5and 40keV.This means that at faint ?uxes there must be a population of sources with spectra that are harder than the background.According to leading models,these hard sources (eg Fabian 1999,Gilli,Risaliti &Salvati 1999)are obscured AGN.However,the physical nature and observa-tional appearance of the XRB producing population is not yet known,and is the subject of some debate.For exam-ple,Gilli,Risaliti &Salvati (1999)examined a model in-tended to reproduce the XRB by extrapolating the X–ray emission of present epoch AGN to high redshift using the observed soft X–ray luminosity function.In contrast,the model of Fabian (1999)has a large fraction of the XRB due to a population of high redshift,heavily obscured,growing AGN,which are di?erent to anything observed in the local universe. In Page et al.(2000),hereafter paper 1,we presented a catalogue of 147serendipitous ROSAT sources which have spectra harder than that of the XRB.These sources have a steep N (S )relation down to the sensitivity limit of our survey (～10?14erg cm ?2s ?1),and are therefore likely to be the bright tail of the population of hard sources that c 0000RAS 2Page,Mittaz&Carrera dominate the source counts at faint?uxes.As such,they could o?er us a preview of the faint,hard and dominant, X-ray source population.We have therefore undertaken a programme of optical and infrared observations of our ROSAT hard source sample to?nd out what these sources are.In this paper we present the hard source identi?ca-tions obtained from our optical(spectroscopic)campaign together with those found in existing catalogues.Section2 details our method and observations,the results of which are given in Section3.These results are discussed in the context of absorbed AGN and the XRB in Section4.Fi-nally,we present our conclusions in Section5. Throughout this paper we de?ne power law spectral indexαsuch that fν∝ν?α. 2OPTICAL IDENTIFICATION 2.1Strategy To produce a systematic and e?cient optical identi?-cation programme,we divided the hard X-ray sources into two groups depending on the ease of optical iden-ti?cation.Sources which had one or two plausible candi-dates present in APM data and/or the DSS were consid-ered suitable for optical spectroscopy and make up the ‘spectroscopic sample’,while sources with no plausible candidates,or more than two,were considered unsuit-able for spectroscopy and became the‘imaging sample’. There are103sources in the spectroscopic sample and 44sources in the imaging sample.This paper will deal only with identi?ed sources from the spectroscopic sam-ple(except for two sources,RXJ005812.20-274217.8and RXJ101112.05+554451.3,which are fainter than our spec-troscopic sample limit but have catalogue identi?cations). The properties of sources in the imaging sample,and their relationship to the spectroscopic sample sources,will be discussed brie?y in Section3.2and in more detail in Car-rera et al.(in preparation)where we will present the re-sults of our optical and infrared imaging.The three sources of data for the identi?cation process were spectra taken on the William Herschel Telescope(WHT)and the Eu-ropean Southern Observatory3.6m Telescope(ESO3.6), and databases of existing catalogues.The optical spectra will be presented in Mittaz et al.(2001)along with a full description of the observations and data reduction. Catalogue identi?cations were obtained by search-ing the NASA Extragalactic Database(NED)and SIM-BAD around all the ROSAT hard source positions (not just the spectroscopic sample).One further source (RXJ043420.48-082136.7)was identi?ed from a WHT ISIS spectrum taken during the RIXOS programme,but was not part of the?nal RIXOS sample presented in Mason et al.(2000). 3RESULTS Table1contains the list of optical identi?cations.We have categorised our sources as follows.X-ray sources with an optical counterpart which is a Galactic star,of any type, have been classi?ed as stars,and X-ray sources which are clusters of galaxies have been classi?ed as clusters.X-ray Table2.Di?erent types of identi?ed hard sources and their mean properties.N is the number of sources, S is the mean ?tted?ux in units of10?14erg cm?2s?1, α is the mean ?tted spectral slope, z is the mean redshift and log L is the mean of the log of observed0.5-2keV luminosity in erg s?1,calculated as described in Section3.3.For comparison,the unidenti?ed sources from the spectroscopic sample are listed as No ID(S),while the unidenti?ed sources from the imaging sample are listed as‘No ID(I)’. N S α z log L offset BLAGN288.1-0.29 1.0043.71 6.1 NELGs1313.6-0.740.2542.687.2 galaxies5 4.0-0.430.1241.85 6.5 clusters819.90.210.2343.38-stars8 3.1-0.91--11.45 No ID(S)43 3.9-0.52--- No ID(I)42 3.2-0.54---sources with an extragalactic optical counterpart which has one or more broad emission lines,or a broad compo-nent(>2000km s?1)to an emission line,is classi?ed as a broad line AGN(BLAGN).X-ray sources with galaxy op-tical counterparts showing narrow emission lines(<2000 km s?1)but no broad emission lines are classed as narrow emission line galaxies(NELGs).Note that none of the nar-row line objects in this survey would be classi?ed as nar-row line Seyfert1s(eg by the criteria given in Goodrich 1989).Galaxies with no discernable emission lines were classed as galaxies.The numbers of objects in each cate-gory,and their mean properties are given in Table2.The sample is dominated by extragalactic sources,and of these over half are broad line AGN. The distributions of o?sets between the X-ray posi-tions and the optical counterparts for the di?erent classes of hard source are shown in Fig.1.The mean o?sets for each source type are given in Table2and are6–7arc-seconds for all source types except for the Galactic stars, which have a mean o?set of12arcseconds and a?at dis-tribution of o?sets(Fig.1);this suggests that the‘star’identi?cations are less secure than the others. We have systematically checked the redshifts of the extragalactic hard sources for similarity to the redshifts of the targets of the PSPC observations in which they were detected.Only two sources,RXJ111926.34+210646.1and RXJ120403.79+280711.2,both clusters of galaxies,have redshifts similar to the observation targets. 3.1X-ray slopes and?uxes The?tted X-ray spectral slopes and?uxes of the di?erent types of sources are shown in Fig.2,and their mean slopes and?uxes are given in Table2.A noticeable feature of Fig. 2is that the clusters of galaxies are concentrated towards the top right(soft spectrum,high?ux)corner compared to the other sources.This trend is con?rmed by a two dimensional Kolmogorov Smirnov(2DKS)test(Fasano& Franceschini1987):the cluster distribution of(α,S)is dif-ferent to that for any(or all)of the other source types with >99%con?dence.Because they are not particularly hard, and because they are predominantly bright and therefore do not have as steep an N(S)relation as the rest of the hard sources,the clusters are unlikely to be important contributors to the faint hard source population. c 0000RAS,MNRAS000,000–000 A Survey of hard spectrum ROSAT sources2:optical identi?cation of hard sources3 Table1.Hard source optical counterparts Source optical position origin type z cat name notes RA dec RXJ001144.43-362638.0001144.54-362639.0EFOSC BLAGN0.900 RXJ004651.98-204329.0004651.83-204328.6cat BLAGN0.380[HB89]0044-209 RXJ005734.78-272827.4005734.94-272828.0EFOSC BLAGN 2.185 RXJ005736.81-273305.9005736.75-273304.6cat NELG0.213GSGP4X:069 RXJ005746.75-273000.8005746.83-273000.9cat galaxy0.019ESO411-G034 RXJ005801.64-275308.6005801.32-275310.2EFOSC NELG0.416GSGP4X:091 RXJ005812.20-274217.8005813.57-274211.4cat NELG0.597GSGP4X:100 RXJ013555.47-183210.2013555.71-183224.9EFOSC star0.000 RXJ013707.63-183846.4013707.75-183849.9EFOSC star0.000Unlikely to be X-ray source RXJ013721.47-182558.3013721.94-182603.0EFOSC NELG0.336 RXJ014159.22-543037.0014159.81-543039.6EFOSC BLAGN0.168 RXJ031456.58-552006.8031456.30-552006.1cat galaxy0.387[GZd97]1.4GHz38 RXJ033340.22-391833.4033339.54-391841.4EFOSC BLAGN 1.436 RXJ033402.54-390048.7033403.26-390036.9EFOSC galaxy0.061PKS0332-39W AT radio source RXJ034119.02-441033.3034119.23-441029.9cat BLAGN0.505QSF3X:51 RXJ043420.48-082136.7043420.19-082131.3cat BLAGN0.155 RXJ045558.99-753229.1045558.82-753228.0cat NELG0.018ESO033-G002 RXJ052839.93-325148.5052839.83-325144.7cat cluster0.273[VMF98]042 RXJ082640.20+263112.3082640.52+263114.1ISIS NELG0.182 RXJ085340.52+134924.9085341.01+134919.7cat NELG0.190MS0850.8+1401Uncertain ID RXJ085851.49+141150.7085850.75+141154.5ISIS NELG0.453 RXJ090518.27+335006.0090517.94-335016.1ISIS NELG0.425 RXJ090923.64+423629.2090923.82+423623.3ISIS BLAGN0.177 RXJ091908.27+745305.6091910.56+745311.2ISIS galaxy0.073 RXJ094144.51+385434.8094144.61+385439.1ISIS BLAGN 1.819 RXJ095340.67+074426.1095340.12+074412.3cat BLAGN0.760RIXOS F218 001 RXJ111926.34+210646.1111925.93+210647.4cat cluster0.176 RXJ111942.16+211518.1111942.13+211516.6cat BLAGN 1.288 RXJ112056.87+132726.2112057.48+132708.0ISIS star0.000Unlikely to be X-ray source RXJ114621.27+285320.6114619.93+285306.6cat cluster0.170part of[VMF98]107 RXJ115952.10+553212.1115952.28+553206.1cat cluster0.081MS1157.3+5548 RXJ120403.79+280711.2120403.55+280701.3cat cluster0.167MS1201.5+2824 RXJ121017.25+391822.6121016.61+391816.6ISIS NELG0.022 RXJ121115.30+391146.8121115.67+391154.2cat cluster0.340MS1208.7+3928 RXJ121803.82+470854.612184.54+470851.0ISIS BLAGN 1.743 RXJ124913.86-055906.2124913.85-055919.4cat BLAGN 2.212[HB89]1246-057BALQSO RXJ131635.62+285942.7131634.72+285929.3cat BLAGN0.277RIXOS F224 026 RXJ133152.51+111643.5133152.25+111649.6cat BLAGN0.090RIXOS F278 011 RXJ140134.94+542029.2140134.59+542031.1ISIS galaxy0.069 RXJ140416.61+541618.2140416.79+541614.6ISIS BLAGN 1.405 RXJ142754.71+330007.0142754.51+325959.8cat BLAGN0.420RIXOS F110 4Page,Mittaz& Carrera Figure1.Histogram of o?sets,in bins of2arcseconds,between the X–ray positions and optical counterparts for the di?erent classes of identi?ed sources. Note that the very hard mean spectral index of the Galactic stars(see Table2)is due to the three objects with best?tα with best?tα=?1.65and RXJ133146.37+111420.4with best?tα=?1.472)are unlikely to be correct identi?ca- tions(see Section3.6). The other three types of sources(BLAGN,NELGs and galaxies)have distributions of(α,S)which are indis- tinguishable from one another according to the2DKS test; any(or all)could be signi?cant contributors to the faint, hard population. For comparison Figure2also shows the unidenti?ed sources.Unidenti?ed objects in the spectroscopic sample are found with similar spectral slopes and?uxes to the identi?ed sources(except the clusters which are softer and brighter).The sources in the imaging sample are more concentrated toward faint?uxes and comprise most of the faintest(S～10?14erg cm?2s?1)hard sources. 3.2The unidenti?ed sources We now consider brie?y how fair a subsample the identi- ?ed sources are of the whole ROSAT hard source sample. Starting with the spectroscopic sample,candidates were chosen for identi?cation on our WHT and ESO3.6m ob- serving runs without regard to their optical magnitudes and morphologies,(except to exclude sources with an ex- isting catalogue identi?cation)and are hence an unbi- ased subsample of the spectroscopic sample.The catalogue identi?cations,although including a few optically bright galaxies,are mostly from previous?ux limited X–ray sur- veys.They therefore tend to have higher X–ray?uxes than the spectroscopic sample as a whole,but are otherwise a fair subsample.This means that except for a bias towards higher X–ray?uxes,the identi?ed sources are a fair sub- sample of the spectroscopic sample. The spectroscopic sample is a signi?cant fraction of the whole ROSAT hard source sample(103of147sources), but it cannot be considered a fair subsample because it ex- cludes the optically faint sources which form the imaging sample.Without spectroscopically identifying the imaging sample(which is currently impractical)it is not possible to determine whether or not the imaging sample is actually made up of the same mix of sources as the spectroscopic sample.However we can examine whether it is possible,by assuming that similar types of sources will have similar X– ray to optical?ux ratios.Figure3shows the X–ray?ux against the APM red(E or R)magnitude for the identi?ed sources with available APM data.BLAGN,NELGs and galaxies are found with similar ranges of X–ray to opti- cal ratio.The optical counterparts to the imaging sample sources are presumed to be fainter than the plate limit, which we take to be20.5and21.0for sources with APM data available for E and R plates respectively.The imag- ing sample sources are plotted in Fig.3with these lower limits except for two sources RXJ031956.76-663938.5and RXJ101031.05+503458.6,which are in the imaging sam- ple because there are too many potential counterparts for practical spectroscopic follow up.The dashed line corre- sponds to an X–ray to optical?ux ratio which is similar to that of RXJ111750.51+075712.8,which has the high- est X–ray to optical?ux ratio of the identi?ed spectro- scopic sample sources excluding the clusters.Only six of the imaging sample sources lie above the dashed line,and therefore de?nitely have X–ray to optical?ux ratios di?er- ent to those of the identi?ed sources.Therefore the limits on the optical to X–ray ratios are consistent with the iden- ti?ed sources being the same types of objects as constitute almost the whole ROSAT hard source sample. 3.3Redshifts and luminosities Fig.4shows the redshifts and0.5-2keV luminosities for the extragalactic hard sources.Luminosities were calcu- lated from the?tted?uxes,K corrected using the best?t spectral slopes,and assuming H0=50km s?1Mpc?3, q0=0.The majority of the BLAGN have higher lumi- nosities and redshifts than the NELGs and galaxies;all the high redshift(z>1)sources are BLAGN.This may imply that either hard spectrum narrow line sources do not exist at high luminosity/redshift or our spectroscopic c 0000RAS,MNRAS000,000–000 A Survey of hard spectrum ROSAT sources2:optical identi?cation of hard sources 5 Figure2.X-ray spectral slopes and?uxes of the di?erent types of hard source.For comparison the unidenti?ed sources are shown in the last panel:the spectroscopic sample as?lled dots and the imaging sample as crosses(see Section2for de?nitions of the two samples). sample is not deep enough(in X–ray or optical?ux)to ?nd them. 3.4X–ray-optical-radio?ux ratios It is common to parameterise the X–ray to optical and optical to radio?ux ratios of AGN asαOX andαOR,where αOX is the slope of the power law which(in the object’s rest frame)would connect the?ux density(Fν)at2500?A with the X–ray?ux density at2keV,andαOR is the slope of the power law which would connect the?ux density at 2500?A with the?ux density at5GHz. For all sources we have estimated the rest frame2500 ?A?ux density using B photometry(taken from Carrera et al.in preparation)and assuming a power law optical-UV spectrum with slopeα=0.5,and using the B magnitude to?ux conversion given by Wilkes et al.(1994).The B magnitudes have been corrected for Galactic reddening using the expression for E(B?V)in Bohlin,Savage& Drake(1978)and assuming A B=4E(B V). To estimate the rest frame5GHz?uxes we have searched for potential radio counterparts to our X–ray sources in the catalogues of radio sources in the VLA1.4 GHz FIRST(White et al.1997)and NVSS(Condon et al. 1998)surveys and the5GHz Parkes-MIT-NRAO(PMN, Gri?th&Wright1993)survey.Additionally,radio images from these surveys were searched by eye to ensure that any extended radio sources associated with our X–ray sources were not missed,and to ensure that there were no spuri- ous radio counterparts associated with other extended ra- dio sources.The uncertainty in radio source position from these three surveys ranges from～better than1arcsecond (FIRST)to around10arcseconds(PMN).The sky den- sity of radio sources is su?ciently low(reaching around 100deg?2at the～1mJy completeness limit of FIRST) that it is unlikely that there are any chance coincidences. Where no suitable radio source appears in a survey cat- alogue,we have taken the catalogue completeness limit as the upper limit to the radio?ux of the X–ray source. We took the best measurement(or upper limit)available from the three surveys and assume a radio spectral slope ofα=0.7. The2keV?ux density has been estimated from the c 0000RAS,MNRAS000,000–000 6Page,Mittaz & Carrera Figure 3.Optical magnitudes against X–ray ?uxes for the identi?ed sources inthe spectroscopic sample (symbols)and the sources in the imaging sample (lower limits).The gradient of the dashed line corresponds to a constant ratio of X–ray to optical ?ux. ?tted 0.5-2keV ?uxes and assuming an X–ray spectral slope of α=0. We then computed αOX =0.384log[f ν(2500?A )/f ν(2keV)]and αOR =?0.186log[f ν(2500?A )/f ν (5GHz)] αOX and αOR are shown in Fig.5for all the hard sources identi?ed as BLAGN,NELGs and galaxies.The horizontal dashed line marks αOR =0.35which is com-monly used to di?erentiate radio loud and radio quiet objects (Zamorani et al.1981).Seven hard sources (four BLAGN,2galaxies and 1NELG)lie above this line,and are therefore radio loud.This is a large radio loud fraction (15+7?5%where errors are the Poission 68%con?dence in-terval,Gehrels 1986)of the BLAGN,NELGs and galaxies compared to the fraction found in normal ROSAT surveys without spectral selection,eg Cilliegi et al.(1995)?nd that only two of the eighty CRSS AGN and NELGs (2.5+3.3 ?1.6%)are radio loud.On the other hand,the distribution of αOX of the hard sources is quite similar to that found in other AGN surveys (eg Ciliegi et al.1995,Wilkes et al.1994),with the majority of sources having 1<αOX <1.8.3.5 X–ray absorption The leading hypothesis to explain the majority of faint hard sources which contribute substantially to the XRB Figure 4.Redshifts and observed 0.5-2keV luminosities for the di?erent extragalactic source types is that they are intrinsically absorbed AGN (eg Fabian &Iwasawa 1999,Setti &Woltjer 1989).This is also a likely hypothesis for our hard sources,because the optical spec-tra and colours of a signi?cant fraction of our BLAGN and NELGs suggest absorption (Mittaz et al.2001and Carrera et al.2001).Assuming that our BLAGN,NELGs and galaxies have hard spectra because of absorption,we have estimated their column densities from their 3colour ROSAT PSPC spectra.We assume that before absorp-tion they have power law X–ray spectra with energy in-dex α=1(typical for X-ray selected AGN,eg Mittaz et al.1999,Maccacaro et al.1988)and ?t their intrinsic cold gas column.The ?tting procedure was identical to that described in paper 1except that the free parameters in the ?t are intrinsic column and power law normalisa-tion rather than power law slope and normalisation.The results of these ?ts are given in Table 3. The BLAGN,NELG and galaxies’?tted absorbing columns and luminosities (before absorption)are shown in Fig.6.Most of the high luminosity sources (near the top of Fig.6)are BLAGN,while most of the galaxies are found with low luminosities;the mean log L (in erg s ?1,0.5-2keV)for the BLAGN,NELGs and galaxies are 44.4,43.2and 42.2respectively.We note that the trend in Fig.6for the most absorbed sources to have the highest luminosity is probably a selection e?ect due to the shifting of the rest frame emitted passband to higher energy with increasing redshift.This means that sources detectable in the PSPC and satisfying our spectral selection criterion c 0000RAS,MNRAS 000,000–000 A Survey of hard spectrum ROSAT sources2:optical identi?cation of hard sources7 Table3.Hard sourceαOX,αOR and?tted columns Source———X–ray———B mag A B————radio————αOXαOR—X–ray column?t—?ux aαlog L b?uxνsurvey N H norm c (mJy)(GHz)(cm?2) RXJ001144.43-362638.0 4.19+0.60 ?0.56-0.14+0.27 ?0.35 43.97+0.06 ?0.06 20.38±0.120.08<2.50 1.4NVSS 1.32+0.04 ?0.04 <0.3321.34+0.43 ?0.29 2.32+0.52 ?0.39 RXJ004651.98-204329.019.37+1.95 ?1.560.32+0.13 ?0.11 44.05+0.04 ?0.04 18.60±0.300.11<2.50 1.4NVSS 1.30+0.06 ?0.06 <0.2120.72+0.08 ?0.09 9.91+0.89 ?0.92 RXJ005734.78-272827.4 1.15+0.31 ?0.20-0.34+0.56 ?0.99 43.91+0.10 ?0.08 18.62±0.160.13<2.50 1.4NVSS 1.84+0.06 ?0.06 <0.2122.60+0.26 ?0.48 0.90+0.33 ?0.27 RXJ005736.81-273305.9 1.25+0.23 ?0.250.00+0.36 ?0.64 42.34+0.07 ?0.10 20.72±0.300.13<2.50 1.4NVSS 1.42+0.08 ?0.07 <0.3621.07+0.40 ?0.46 0.79+0.22 ?0.18 RXJ005746.75-273000.8 1.75+0.26 ?0.280.08+0.34 ?0.32 40.42+0.06 ?0.08 13.53±0.100.13 3.80±0.70 1.4NVSS 2.45+0.04 ?0.04 -0.16+0.02 ?0.02 20.80+0.29 ?0.28 1.02+0.21 ?0.18 RXJ005801.64-275308.6 5.09+0.50 ?0.52-0.35+0.31 ?0.29 43.45+0.04 ?0.05 21.43±0.150.13<2.50 1.4NVSS 1.09+0.04 ?0.04 <0.4121.55+0.17 ?0.25 3.31+0.71 ?0.54 RXJ005812.20-274217.80.90+0.24 ?0.22-0.30+0.58 ?1.02 42.97+0.10 ?0.12 22.63±0.300.13<2.50 1.4NVSS 1.21+0.09 ?0.09 <0.5121.75+0.29 ?0.57 0.65+0.29 ?0.17 RXJ013721.47-182558.3 3.91+0.57 ?0.460.03+0.19 ?0.27 43.22+0.06 ?0.05 20.87±0.110.07<2.50 1.4NVSS 1.23+0.04 ?0.04 <0.3620.84+0.17 ?0.15 2.02+0.30 ?0.26 RXJ014159.22-543037.08.81+1.51 ?1.51-0.22+0.41 ?0.57 42.98+0.07 ?0.08 17.38±0.100.17<37.00 5.0PMN 1.60+0.05 ?0.04 <0.3921.37+0.20 ?0.46 5.98+1.77 ?1.54 RXJ031456.58-552006.8 3.45+0.54 ?0.48-1.66+0.70 ?0.85 43.04+0.06 ?0.06 21.72±0.130.18 1.25±0.11 1.4FIRST 1.10+0.05 ?0.04 0.37+0.02 ?0.02 22.12+0.10 ?0.15 4.42+1.18 ?1.03 RXJ033340.22-391833.4 3.37+0.70 ?0.75-0.24+0.71 ?0.77 44.17+0.08 ?0.11 19.42±0.120.10<2.50 1.4NVSS 1.52+0.06 ?0.05 <0.2622.48+0.19 ?0.37 3.01+1.19 ?0.97 RXJ033402.54-390048.77.22+0.99 ?0.87-0.06+0.30 ?0.23 42.05+0.06 ?0.06 16.03±0.300.101567.10±52.60 1.4NVSS 1.84+0.07 ?0.07 0.51+0.03 ?0.03 20.74+0.29 ?0.22 3.97+0.69 ?0.58 RXJ034119.02-441033.3 2.60+0.41 ?0.400.06+0.34 ?0.34 43.37+0.06 ?0.07 21.55±0.110.10<45.00 5.0PMN 1.19+0.04 ?0.04 <0.7221.10+0.38 ?0.31 1.48+0.34 ?0.25 RXJ043420.48-082136.711.51+2.69 ?1.82-1.17+1.21 ?0.95 42.97+0.09 ?0.07 18.68±0.130.42 3.70±0.60 1.4NVSS 1.32+0.05 ?0.05 0.24+0.02 ?0.02 21.95+0.11 ?0.22 14.67+5.80 ?4.18 RXJ045558.99-753229.190.78+4.93 ?3.88-2.43+0.26 ?0.26 42.08+0.02 ?0.02 16.05±0.070.59<20.00 5.0PMN 1.34+0.02 ?0.02 <0.2721.89+0.04 ?0.04 135.47+13.96 ?12.08 RXJ082640.20+263112.3 3.81+0.83 ?0.87-1.27+0.93 ?1.06 42.61+0.09 ?0.11 20.34±0.140.25<0.91 1.4FIRST 1.27+0.06 ?0.05 <0.2521.93+0.15 ?0.22 4.57+2.06 ?1.38 RXJ085340.52+134924.912.00+0.98 ?1.16-0.19+0.23 ?0.34 43.22+0.03 ?0.04 19.21±0.090.2523.20±1.50 1.4NVSS 1.26+0.03 ?0.03 0.42+0.01 ?0.01 21.38+0.15 ?0.25 7.80+1.52 ?1.22 RXJ085851.49+141150.7 4.05+0.81 ?0.65-1.32+0.82 ?0.84 43.26+0.08 ?0.08 20.82±0.300.29<2.50 1.4NVSS 1.20+0.08 ?0.08 <0.3922.11+0.13 ?0.18 4.81+1.51 ?1.37 RXJ090518.27+335006.07.58+2.29 ?1.33-2.43+1.80 ?1.09 43.32+0.11 ?0.08 20.45±0.090.16<0.97 1.4FIRST 1.17+0.05 ?0.06 <0.2522.41+0.08 ?0.18 15.65+6.87 ?4.00 RXJ090923.64+423629.27.40+0.97 ?0.870.22+0.20 ?0.22 42.98+0.05 ?0.05 18.25±0.090.11<2.50 1.4NVSS 1.50+0.04 ?0.03 <0.1620.69+0.17 ?0.18 3.86+0.51 ?0.50 RXJ091908.27+745305.6 4.73+1.01 ?0.92-0.35+0.54 ?0.82 42.01+0.08 ?0.09 17.82±0.090.14<2.50 1.4NVSS 1.63+0.05 ?0.05 <0.1321.57+0.27 ?0.42 4.01+2.69 ?1.61 RXJ094144.51+385434.8 2.11+0.51 ?0.53-0.12+0.57 ?0.58 44.17+0.09 ?0.13 21.11±0.140.10<1.01 1.4FIRST 1.35+0.07 ?0.06 <0.3221.92+0.46 ?0.43 1.34+0.41 ?0.37 RXJ095340.67+074426.1 4.32+1.25 ?1.09-0.38+0.52 ?0.94 43.81+0.11 ?0.13 20.01±0.090.19<2.50 1.4NVSS 1.35+0.06 ?0.06 <0.3121.77+0.34 ?0.45 3.06+1.44 ?0.95 RXJ101112.05+554451.3 6.95+0.90 ?0.88-0.43+0.29 ?0.29 44.32+0.05 ?0.06 22.02±1.000.05161.50±0.15 1.4FIRST 1.00+0.18 ?0.17 0.78+0.07 ?0.07 21.62+0.43 ?0.17 4.01+0.91 ?0.57 RXJ101123.17+524912.4 3.34+0.96 ?0.87-1.41+0.93 ?1.22 43.58+0.11 ?0.13 20.86±0.090.05<0.96 1.4FIRST 1.29+0.06 ?0.06 <0.2822.51+0.16 ?0.28 3.91+1.96 ?1.21 RXJ101147.48+505002.2 4.56+1.01 ?0.82-0.09+0.44 ?0.47 42.07+0.09 ?0.09 16.74±0.220.06<0.96 1.4FIRST 1.82+0.07 ?0.07 <-0.0220.65+0.73 ?0.28 2.75+0.95 ?0.55 RXJ104723.37+540412.6 1.71+0.70 ?0.61-0.56+0.90 ?1.09 43.78+0.15 ?0.19 20.09±0.110.06<0.96 1.4FIRST 1.54+0.09 ?0.07 <0.2322.22+0.42 ?0.61 1.31+0.78 ?0.45 RXJ110742.05+723236.08.11+1.22 ?1.100.12+0.37 ?0.45 44.97+0.06 ?0.06 19.07±0.080.21370.60±11.10 1.4NVSS 1.43+0.04 ?0.04 0.64+0.01 ?0.01 21.58+0.82 ?0.38 4.75+1.11 ?0.75 RXJ111750.51+075712.816.55+1.57 ?1.40-0.15+0.23 ?0.29 44.38+0.04 ?0.04 20.67±0.090.24<2.50 1.4NVSS 1.01+0.03 ?0.03 <0.3621.57+0.18 ?0.20 9.94+1.60 ?1.26 RXJ111942.16+211518.1 3.44+0.62 ?0.480.13+0.30 ?0.30 44.24+0.07 ?0.07 19.91±0.090.09<0.93 1.4FIRST 1.44+0.04 ?0.04 <0.2121.42+0.36 ?0.28 1.89+0.37 ?0.30 RXJ121017.25+391822.6 4.62+0.68 ?0.67-0.02+0.35 ?0.49 40.98+0.06 ?0.07 17.18±0.500.14<0.98 1.4FIRST 1.73+0.10 ?0.10 <0.0421.10+0.22 ?0.49 2.88+0.78 ?0.51 RXJ121803.82+470854.6 1.51+0.44 ?0.42-0.52+0.60 ?1.07 43.82+0.11 ?0.14 21.04±0.090.08<0.98 1.4FIRST 1.42+0.07 ?0.06 <0.3122.30+0.34 ?0.69 1.07+0.53 ?0.30 RXJ124913.86-055906.2 2.38+0.47 ?0.36-0.09+0.57 ?0.55 44.36+0.08 ?0.07 17.26±0.300.15<2.50 1.4NVSS 1.92+0.07 ?0.08 <0.1222.23+0.36 ?0.57 1.53+0.39 ?0.38 RXJ131635.62+285942.713.74+0.98 ?1.000.35+0.10 ?0.08 43.64+0.03 ?0.03 20.32±0.300.08<0.93 1.4FIRST 1.10+0.06 ?0.06 <0.2520.53+0.07 ?0.07 6.55+0.50 ?0.47 RXJ133152.51+111643.556.99+4.09 ?3.88-1.72+0.27 ?0.33 43.22+0.03 ?0.03 18.16±0.100.138.00±1.00 1.4NVSS 1.17+0.03 ?0.03 0.24+0.02 ?0.02 21.80+0.06 ?0.06 64.44+9.09 ?7.69 RXJ135105.69+601538.5 3.83+0.44 ?0.45-0.12+0.33 ?0.27 43.07+0.05 ?0.05 20.53±0.090.12<2.50 1.4NVSS 1.27+0.03 ?0.03 <0.3321.17+0.23 ?0.25 2.22+0.42 ?0.31 RXJ135529.59+182413.6 3.63+0.86 ?0.89-0.41+0.84 ?0.94 44.02+0.09 ?0.12 20.61±0.090.14<2.50 1.4NVSS 1.31+0.06 ?0.05 <0.3522.25+0.25 ?0.50 2.82+1.29 ?0.78 RXJ140134.94+542029.2 2.94+0.58 ?0.57-0.13+0.46 ?0.59 41.76+0.08 ?0.09 18.42±0.090.08<1.00 1.4FIRST 1.63+0.05 ?0.04 <0.1021.02+0.39 ?0.46 1.89+0.64 ?0.39 RXJ140416.61+541618.2 2.79+0.62 ?0.48-0.08+0.34 ?0.56 44.14+0.09 ?0.08 21.16±0.200.08<0.99 1.4FIRST 1.28+0.06 ?0.06 <0.3221.69+0.40 ?0.38 1.70+0.45 ?0.35 RXJ142754.71+330007.0 3.00+0.51 ?0.460.21+0.27 ?0.39 43.31+0.07 ?0.07 19.66±0.080.07<0.83 1.4FIRST 1.46+0.04 ?0.04 <0.1820.81+0.38 ?0.35 1.57+0.29 ?0.27 RXJ163054.25+781105.18.96+0.74 ?0.87-0.01+0.37 ?0.29 43.62+0.03 ?0.04 20.54±0.140.28<2.50 1.4NVSS 1.11+0.04 ?0.04 <0.3521.52+0.17 ?0.31 5.81+1.22 ?1.06 RXJ163308.57+570258.7 1.89+0.32 ?0.33-0.11+0.42 ?0.69 44.40+0.07 ?0.08 20.06±0.120.1317.20±0.15 1.4FIRST 1.55+0.05 ?0.04 0.47+0.01 ?0.01 22.48+0.31 ?0.54 1.20+0.33 ?0.26 RXJ204640.48-363147.5 6.29+0.68 ?0.71-0.14+0.45 ?0.36 44.31+0.04 ?0.05 18.76±0.070.2823.70±0.90 1.4NVSS 1.48+0.03 ?0.03 0.40+0.01 ?0.01 21.89+0.17 ?0.22 3.92+0.65 ?0.57 RXJ204716.74-364715.19.13+0.86 ?0.91-0.64+0.35 ?0.53 41.97+0.04 ?0.05 17.57±0.080.28 4.60±0.50 1.4NVSS 1.54+0.03 ?0.03 0.16+0.01 ?0.01 21.53+0.12 ?0.15 7.88+1.65 ?1.37 RXJ213807.61-423614.316.71+5.05 ?3.62-1.10+0.92 ?1.06 41.40+0.11 ?0.11 16.15±0.070.18<47.00 5.0PMN 1.67+0.05 ?0.05 <0.3221.74+0.17 ?0.27 19.00+9.30 ?6.98 RXJ235113.89+201347.330.31+3.16 ?3.06-0.55+0.29 ?0.44 42.37+0.04 ?0.05 16.94±0.130.30 5.90±0.50 1.4NVSS 1.43+0.04 ?0.04 0.14+0.02 ?0.02 21.44+0.12 ?0.18 23.84+5.35 ?4.08 a Units of erg cm?2s?1 b See Section3.3 c Units of erg cm?2s?1keV?1 (see paper1)will have larger columns at higher redshift (and hence at higher luminosity). 3.6Notes on individual sources RXJ004651.98-204329.0The hard ROSAT spectrum of this active galaxy was the subject of Elvis et al.(1997) who proposed that absorption in material associated with NGC247may be responsible. RXJ005801.64-275308.6A second,slightly fainter NELG at J2000position00h58m1.69s?27o53′16.80′′has the same redshift(z=0.086)as,and is within10arcsec-onds of,the NELG identi?ed as the X–ray source. RXJ013707.63-183846.4The star has an unremarkable G type spectrum,and the X–ray source is coincident with a bright radio source(MRC0134-188)and hence the star is unlikely to be the correct optical counterpart.The real optical counterpart is too faint to be seen on POSS. RXJ031456.58-552006.8This radio galaxy has ex-tended double lobe structure;see Gruppioni,Mignoli& Zamorani(1999). RXJ033402.54-390048.7This source is a wide angle c 0000RAS,MNRAS000,000–000 8Page,Mittaz & Carrera Figure 5.αOX and αOR for the hard sources tail radio source in the galaxy cluster Abell 3135.A mag-nitude V ～16Galactic star is also close to the X-ray source position but is unlikely to be related. RXJ043420.48-082136.7The identi?cation spectrum of this object was taken on the WHT as part of RIXOS,but the source was not part of the ?nal RIXOS sample and is not included in the ?nal catalogue (Mason et al.2000). RXJ085340.52+134924.9This RIXOS identi?cation is uncertain because there is another optical counterpart closer to the centre of the X–ray error circle that was not observed.Note also that the position of the optical counterpart is incorrect in Mason et al.(2000),which should be the same as that in Table 1,i.e.08h 53m 41.01s +13o 49′19.7′′(J2000). RXJ095340.67+074426.1The RIXOS identi?cation and redshift of this source are based on a relatively poor optical spectrum and therefore may be incorrect. RXJ101112.05+554451.3This source was identi?ed as an obscured radio loud AGN by Barcons et al.(1998).It has strong narrow emission lines but Mg II λ2798is broad,and hence we have classi?ed it as a BLAGN. RXJ101147.48+505002.2This X–ray source was iden-ti?ed with a NELG with z =0.067by Carballo et al.(1995),but we identify the source with a BLAGN with z =0.079,which is brighter and closer to the X–ray source.Notably,the z =0.079BLAGN showed only narrow lines in the optical spectrum of Carballo et al.(1995);the H αline pro?le appears genuinely to have changed between 1994and 1998. Figure 6.Fitted columns and unabsorbed 0.5-2keV luminosi-ties for the di?erent types of hard sources. RXJ111926.34+210646.1This galaxy cluster and the target of the PSPC observation (PG 1116+215)in which it was found have very similar redshifts (0.0176and 0.1765respectively)and therefore this source is not strictly serendipitous. RXJ112056.87+132726.2The X–ray source is coin-cident with the symmetric double radio source 87GB 111822.7+134349,and hence the star is unlikely to be the correct identi?cation for the X–ray source. RXJ120403.79+280711.2This galaxy cluster and the target of the PSPC observation (PG 1202+281)in which it was found have similar redshifts (0.0167and 0.1653re-spectively)and therefore this source may not be strictly serendipitous. RXJ124913.86-055906.2This broad absorption line (BAL)QSO was the only bona-?de BALQSO in sample of Green &Mathur (1996)to be detected as a PSPC source.RXJ133146.37+111420.4This X–ray source is coinci-dent with the radio source 87GB 132918.1+112918,and hence the star is unlikely to be the correct optical coun-terpart. RXJ142754.71+330007.0The RIXOS identi?cation and redshift of this source are based on a relatively poor optical spectrum and therefore may be incorrect. 4DISCUSSION Excluding the clusters,which are unlikely to be an impor-tant part of the faint,hard X–ray source population (see c 0000RAS,MNRAS 000,000–000 A Survey of hard spectrum ROSAT sources2:optical identi?cation of hard sources9 Section3.1),we have identi?ed3types of extragalactic hard source:BLAGN,NELGs and galaxies.At?rst sight the identi?cation content of the sample appears similar to that of other PSPC surveys with similar?ux limits but without any spectral selection,eg BLAGN being the most numerous source.However,in two respects the identi?ca-tion content of this survey is signi?cantly di?erent. The?rst di?erence is that there is a higher proportion of radio loud objects(15+7?5%)in this survey(see Section 3.4).There are two possible reasons why this should be so.One is that the intrinsic X–ray emission of radio loud sources may be harder than that of radio quiet sources (Reeves et al.1997)because the radio loud sources have an additional,hard spectrum X–ray emission component from the inner parts of radio jets.The other possibility is that our radio loud sources are absorbed,and because they are intrinsically more X–ray luminous than radio quiet sources they are relatively numerous in a relatively bright survey of hard spectrum sources.This would be analo-gous to the high proportion of(presumably unabsorbed) radio loud sources present in bright soft X–ray surveys(eg 11±2%in the EMSS,Della Ceca et al.1994)compared to fainter soft X–ray surveys(eg2.5+3.3 ?1.6 %in the CRSS, Ciliegi et al.1995). The second di?erence is that there are nearly half as many NELGs as BLAGN(see Table1)compared to ratios of～1:13NELGS to AGN in RIXOS(Mason et al.2000) and～1:6in the CCRS(Boyle,Wilkes&Elvis1997). This implies that the fraction of sources with hard spectra is larger in the NELG population than in the BLAGN population.This is consistent with the?ndings that the NELGs in faint X–ray surveys have,on average,harder X–ray spectra than BLAGN(Romero-Colmenero et al.1996, Almaini et al.1996),and with the hypothesis that most X–ray selected NELGs are absorbed AGN(Schmidt et al. 1998,Lehmann et al.2000). Hence the hypothesis that most of the sources have hard X–ray spectra because they are absorbed could ac-count for both the high radio loud and NELG content of this survey.It is also consistent with the preliminary anal-yses of the optical spectra and optical colours of the hard sources(Mittaz et al.2001and Carrera et al.2001). Related to the absorption hypothesis,an important ?nding is that the distributions of X–ray spectral slopes and?uxes of the BLAGN,NELGs and galaxies are in-distinguishable within the current sample,but the three groups have di?erent ranges of luminosities.The galax-ies are found at low luminosity while the high luminosity sources are BLAGN(see?gures4and6).The absence of high luminosity,absorbed narrow line AGN has also been noted by Akiyama et al.(2000)in the ASCA Large Sky survey.These results are consistent with all three source types having the same mechanism for their X–ray spec-tra(an absorbed active nucleus)but optical emission line properties which depend on luminosity.For this reason we point out that the high redshift,high luminosity,absorbed QSOs expected to produce a large fraction of the X–ray background are not neccessarily narrow line objects(the proposed“QSO2s”)like Seyfert2s,their low luminosity counterparts.5CONCLUSIONS We have performed a survey of ROSAT?elds for serendip-itous sources with hard spectra(α<0.5);such sources must be a major contributor to the X–ray background at faint?uxes.In this paper we have presented optical identi?cations for62of these sources.Almost half(28)of these sources are BLAGN,while12are NELGs and5are galaxies without visible emission lines.We have also found 8clusters of galaxies among the hard spectrum sources. However,these are predominantly bright sources and are not particularly hard(their best?t spectral indices all lie in the range0.0<α<0.5),and hence clusters are un-likely to be an important component of the hard,faint population. The hard spectrum BLAGN have a distribution of X–ray to optical ratios which is similar to that found for AGN from other soft X–ray surveys(1<αOX<2).However,a relatively large proportion(15%)of the BLAGN,NELGs and galaxies are radio loud.This could be because the radio jets in these objects produce intrinsically hard X–ray emission,or if they are absorbed,it could be because radio loud objects are more X–ray luminous than radio quiet objects. The BLAGN,NELGs and galaxies have indistinguish-able distributions of X–ray?ux and spectra,hence any or all may be important to the hard,faint population required to solve the XRB spectral paradox.The ma-jority of the galaxies are low luminosity sources,while the highest luminosity objects,and all the high redshift (z>1)sources,are BLAGN.Their ROSAT spectra are consistent with their being AGN obscured by columns of 20.5 FJC thanks the DGES for partial?nancial support,un-der project PB95-0122.This research was based on obser-vations collected at the European Southern Observatory, Chile,ESO No.62.O-0659,and on observations made at the William Herschel Telescope which is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astro?sica de Canarias.This research has made use of data obtained from the Leicester Database and Archive Service at the Department of Physics and Astronomy,Leicester University,UK.This research has made use of the SIMBAD database,operated at CDS, Strasbourg,France,and of the NASA/IPAC Extragalac-tic Database(NED)which is operated by the Jet Propul-sion Laboratory,California Institute of Technology,under contract with the National Aeronautics and Space Admin-istration. 7REFERENCES Akiyama M.,et al.,2000,ApJ,in press(astro-ph/0001289) Almaini O.,Shanks T.,Boyle B.J.,Gri?ths R.E.,Roche c 0000RAS,MNRAS000,000–000 10Page,Mittaz&Carrera N.,Stewart G.C.,Georgantopoulos I.,1996,MN- RAS,282,295 Barcons X.,Carballo R.,Ceballos M.T.,Warwick R.S., Gonzalez-Serrano,1998,MNRAS,301,L25 Bohlin R.C.,Savage B.D.,Drake J.F.,1978,ApJ,224,132 Boyle B.J.,Wilkes B.J.&Elvis M.,1997,MNRAS,285, 511 Carballo R.,et al.,1995,MNRAS,277,1312 Carrera F.J.,Mittaz J.P.D.,Page M.J.,2001,proceed- ings of“X–ray astronomy’999:Stellar End- points,AGN and the Di?use Background”,eds G.Malaguti,G.Palumbo&N.White,in press Ciliegi P.,Elvis M.,Wilkes B.J.,Boyle B.J.,McMahon R.G.,Maccacaro T.,1995,MNRAS,277,1463 Condon J.J.,Cotton W.D.,Greisen E.W.,Yin Q.F.,Per- ley R.A.,Taylor G.B.,&Broderick J.J.,1998, AJ,115,1693 Della Ceca R.,Zamorani G.,Maccacaro T.,Wolter A., Gri?ths R.,Stocke J.T.,Setti G.,1994,ApJ,430, 533 Elvis M.,Fiore F.,Giommi P.,&Padovani P.,1997,MN- RAS,291,L49 Fabian A.C.,1999,MNRAS in press Fabian A.C.,Iwasawa K.,1999,MNRAS,303,L34 Gehrels N.,1986,ApJ,303,336 Gilli R.,Risaliti G.,&Salvati M.,1999,A&A,347,424 Goodrich R.W.,1989,ApJ,342,224 Gri?th M.R.&Wright A.E.,1993,AJ,105,1666 Gruppioni C.,Mignoli M.,&Zamorani G.,1999,MNRAS, 304,199 Lehmann I.,et al.,2000,A&A,in press Maccacaro T.,Gioia I.M.,Wolter A.,Zamorani G.,Stocke J.T.,1988,ApJ,326,680 Mason K.O.,et al.,2000,MNRAS,311,456 McHardy I.M.,et al.,1998,MNRAS,295,641 Mittaz J.P.D.,Page M.J.,Carrera F.J.,2001,proceed- ings of“X–ray astronomy’999:Stellar End- points,AGN and the Di?use Background”,eds G.Malaguti,G.Palumbo&N.White,in press Mittaz et al.,1999,MNRAS,308,233 Page M.J.,Mittaz J.P.D.&Carrera F.J.,2000,‘paper1’, MNRAS,318,1073 Reeves,J.N.,Turner M.J.L.,Ohashi T.,Kii T.,1997, MNRAS,292,468 Romero Colmenero E.,Branduardi-Raymont G.,Carrera F.J.,Jones L.R.,Mason K.O.,McHardy I.M., Mittaz J.P.D.,1996,MNRAS,282,94 Schmidt M.,Hasinger G.,Gunn J.,Schneider D.,Burg R., Giacconi R.,Lehmann I.,MacKenty J.,Tr¨u mper J.,Zamorani G.,1998,A&A,329,495 Setti G.,Woltjer L.,1989,A&A,224,L21 White R.L.,Becker R.H.,Helfand D.J.,&Gregg M.D., 1997,ApJ,475,479 Wilkes B.J.,et al.1994,ApJS,92,53 Zamorani G.,et al.1981,ApJ,245,357 c 0000RAS,MNRAS000,000–000 从实践的角度探讨在日语教学中多媒体课件的应用 在今天中国的许多大学，为适应现代化，信息化的要求，建立了设备完善的适应多媒体教学的教室。许多学科的研究者及现场教员也积极致力于多媒体软件的开发和利用。在大学日语专业的教学工作中，教科书、磁带、粉笔为主流的传统教学方式差不多悄然向先进的教学手段而进展。 一、多媒体课件和精品课程的进展现状 然而，目前在专业日语教学中能够利用的教学软件并不多见。比如在中国大学日语的专业、第二外語用教科书常见的有《新编日语》（上海外语教育出版社）、《中日交流标准日本語》（初级、中级）（人民教育出版社）、《新编基础日语（初級、高級）》（上海译文出版社）、《大学日本语》（四川大学出版社）、《初级日语》《中级日语》（北京大学出版社）、《新世纪大学日语》（外语教学与研究出版社）、《综合日语》（北京大学出版社）、《新编日语教程》（华东理工大学出版社）《新编初级（中级）日本语》（吉林教育出版社）、《新大学日本语》（大连理工大学出版社）、《新大学日语》（高等教育出版社）、《现代日本语》（上海外语教育出版社）、《基础日语》（复旦大学出版社）等等。配套教材以录音磁带、教学参考、习题集为主。只有《中日交流標準日本語（初級上）》、《初級日语》、《新编日语教程》等少数教科书配备了多媒体DVD视听教材。 然而这些试听教材，有的内容为日语普及读物，并不适合专业外语课堂教学。比如《新版中日交流标准日本语（初级上）》，有的尽管DVD视听教材中有丰富的动画画面和语音练习。然而，课堂操作则花费时刻长，不利于教师重点指导，更加适合学生的课余练习。比如北京大学的《初级日语》等。在这种情形下，许多大学的日语专业致力于教材的自主开发。 其中，有些大学的还推出精品课程，取得了专门大成绩。比如天津外国语学院的《新编日语》多媒体精品课程为2007年被评为“国家级精品课”。目前已被南开大学外国语学院、成都理工大学日语系等全国40余所大学推广使用。 Unit1 Americans believe no one stands still. If you are not moving ahead, you are falling behind. This attitude results in a nation of people committed to researching, experimenting and exploring. Time is one of the two elements that Americans save carefully, the other being labor. "We are slaves to nothing but the clock,” it has been said. Time is treated as if it were something almost real. We budget it, save it, waste it, steal it, kill it, cut it, account for it; we also charge for it. It is a precious resource. Many people have a rather acute sense of the shortness of each lifetime. Once the sands have run out of a person’s hourglass, they cannot be replaced. We want every minute to count. A foreigner’s first impression of the U.S. is li kely to be that everyone is in a rush -- often under pressure. City people always appear to be hurrying to get where they are going, restlessly seeking attention in a store, or elbowing others as they try to complete their shopping. Racing through daytime meals is part of the pace こんにちは。（kon ni qi wa） 你好。 こんばんは。（kon ban wa） 晚上好。 おはようございます。（o ha you go za i mas） 早上好。 お休(やす)みなさい。（o ya su mi na sai） 晚安。 お元気(げんき)ですか。（o gen ki de s ka？） 您还好吧，相当于英语的“How are you”，一种打招呼的方式。 いくらですか。（i ku la de s ka？） 多少钱？ すみません。（su mi ma sen） 不好意思，麻烦你…。相当于英语的“Excuse me”。用于向别人开口时。 ごめんなさい。（go men na sai） 对不起。 どういうことですか。（dou iu ko to de su ka?） 什么意思呢？ 山田さんは中国語(ちゅうごくご)が上手(じょうず)ですね。 （ya ma da san wa jiu go ku ko ga zyou zu de su ne） 山田的中国话说的真好。 まだまだです。（ma da ma da de s） 没什么。没什么。（自谦） どうしたの。（dou si ta no） どうしたんですか。（dou si tan de su ka？） 发生了什么事啊。 なんでもない。（nan de mo nai） 没什么事。 ちょっと待ってください。（jou to ma te ku da sai，可以简单地表达为：jou to）请稍等一下。 約束(やくそく)します。（ya ku so ko si ma s） 就这么说定了。 これでいいですか。（korede idesuka ？） 这样可以吗？ けっこうです。（ke kou de s） もういいです。（mou i i de s） 不用了。 どうして。（dou si de） なぜ（na ze） 为什么啊？ いただきます（i ta da ki ma s） 那我开动了。（吃饭动筷子前） ごちそうさまでした。（ko ji sou sa ma de si ta） 我吃饱了。（吃完后） ありがとうございます。（a li ga to go za i ma s） 谢谢。 どういたしまして。（dou i ta si ma si de） 别客气。 本当(ほんとう)ですか。（hon dou de su ka？） 真的？ うれしい。（so ne si i） 我好高兴。（女性用语） よし。いくぞ。（yo si。i ku zo） 好！出发（行动）。（男性用语） 新视野三版读写B2U4Text A College sweethearts 1I smile at my two lovely daughters and they seem so much more mature than we,their parents,when we were college sweethearts.Linda,who's21,had a boyfriend in her freshman year she thought she would marry,but they're not together anymore.Melissa,who's19,hasn't had a steady boyfriend yet.My daughters wonder when they will meet"The One",their great love.They think their father and I had a classic fairy-tale romance heading for marriage from the outset.Perhaps,they're right but it didn't seem so at the time.In a way, love just happens when you least expect it.Who would have thought that Butch and I would end up getting married to each other?He became my boyfriend because of my shallow agenda:I wanted a cute boyfriend! 2We met through my college roommate at the university cafeteria.That fateful night,I was merely curious,but for him I think it was love at first sight."You have beautiful eyes",he said as he gazed at my face.He kept staring at me all night long.I really wasn't that interested for two reasons.First,he looked like he was a really wild boy,maybe even dangerous.Second,although he was very cute,he seemed a little weird. 3Riding on his bicycle,he'd ride past my dorm as if"by accident"and pretend to be surprised to see me.I liked the attention but was cautious about his wild,dynamic personality.He had a charming way with words which would charm any girl.Fear came over me when I started to fall in love.His exciting"bad boy image"was just too tempting to resist.What was it that attracted me?I always had an excellent reputation.My concentration was solely on my studies to get superior grades.But for what?College is supposed to be a time of great learning and also some fun.I had nearly achieved a great education,and graduation was just one semester away.But I hadn't had any fun;my life was stale with no component of fun!I needed a boyfriend.Not just any boyfriend.He had to be cute.My goal that semester became: Be ambitious and grab the cutest boyfriend I can find. 4I worried what he'd think of me.True,we lived in a time when a dramatic shift in sexual attitudes was taking place,but I was a traditional girl who wasn't ready for the new ways that seemed common on campus.Butch looked superb!I was not immune to his personality,but I was scared.The night when he announced to the world that I was his girlfriend,I went along 日语常用会话100句 1 、はじめまして。初次见面。 2 、どうぞよろしく。请多关照。 3 、よろしくお愿（ねが）いします。请多关照。 4 、こちらこそよろしくお愿（ねが）いします。也请您多关照。 5 、自己（じこ）绍介（しょうかい）いたします。我来自我介绍一下。 6 、これはわたしの名刺（めいし）です。这是我的名片。 7 、わたしは李（り）と申（もう）します。我姓李。 8 、山田（やまだ）さんでいらっしゃいますね。您是山田先生吧！ 9 、私（わたし）は山田（やまだ）です。我是山田。 10 、あのかたはどなたですか。那位是谁？ 11 、こちらは社长（しゃちょう）の松本（まつもと）です。这是我们总经理松本。 12 、彼（かれ）は中国人（ちゅうごくじん）ではありませんか。他不是中国人吗？ 13 、彼（かれ）は中国人（ちゅうごくじん）ではありません。他不是中国人。 14 、彼（かれ）は日本人（にほんじん）です。他是日本人。 15 、あなたも日本人（にほんじん）ですか。你也是日本人吗？ 16 、そうですか。是吗？ 17 、はい。是的。 18 、そうです。是那样的（是的）。 19 、いいえ。不对（不是）。 ?? 20 、そうではありません。不是那样的（不是）。 21 、いいえ、ちがいます。不，不对（不是）。 22 、よくいらっしゃいました。欢迎，欢迎。 23 、お迎（むか）えにきました。来欢迎您了。 24 、出迎（でむか）えに参（まい）りました。来欢迎您了。 25 、お疲（つか）れでしょう。路上辛苦了。 26 、ちっとも疲（つか）れていません。一点也不累。（っ是促音） 27 、それはなによりです。那太好了。 28 、途中（とちゅう）はどうでしたか。旅途顺利吗？ 29 、とても顺调（じゅんちょう）でした。很顺利。 30 、いつ上海（しゃんはい）をたちましたか。什么时候离开上海的？ 31 、日本（にほん）は始（はじ）めてですか。是第一次来日本吗？ 32 、皆（みな）さんのご来访（らいほう）をお待（ま）ちしておりました。我们在等待着各位的光临。 33 、わざわざお出迎（でむか）えしていただき、ありがとうございます。承蒙特意来接，深表谢意！ 34 、お忙（いそが）しいところをありがとうございます。百忙中特意来接，非常感谢！ 35 、日本（にほん）に来（き）た目的（もくてき）は？来日本的目的是什么？ Unit 1 1学习外语是我一生中最艰苦也是最有意义的经历之一。虽然时常遭遇挫折，但却非常有价值。 2我学外语的经历始于初中的第一堂英语课。老师很慈祥耐心，时常表扬学生。由于这种积极的教学方法，我踊跃回答各种问题，从不怕答错。两年中，我的成绩一直名列前茅。 3到了高中后，我渴望继续学习英语。然而，高中时的经历与以前大不相同。以前，老师对所有的学生都很耐心，而新老师则总是惩罚答错的学生。每当有谁回答错了，她就会用长教鞭指着我们，上下挥舞大喊：“错！错！错！”没有多久，我便不再渴望回答问题了。我不仅失去了回答问题的乐趣，而且根本就不想再用英语说半个字。 4好在这种情况没持续多久。到了大学，我了解到所有学生必须上英语课。与高中老师不。大学英语老师非常耐心和蔼，而且从来不带教鞭！不过情况却远不尽如人意。由于班大，每堂课能轮到我回答的问题寥寥无几。上了几周课后，我还发现许多同学的英语说得比我要好得多。我开始产生一种畏惧感。虽然原因与高中时不同，但我却又一次不敢开口了。看来我的英语水平要永远停步不前了。 5直到几年后我有机会参加远程英语课程，情况才有所改善。这种课程的媒介是一台电脑、一条电话线和一个调制解调器。我很快配齐了必要的设备并跟一个朋友学会了电脑操作技术，于是我每周用5到7天在网上的虚拟课堂里学习英语。 6网上学习并不比普通的课堂学习容易。它需要花许多的时间，需要学习者专心自律，以跟上课程进度。我尽力达到课程的最低要求，并按时完成作业。 7我随时随地都在学习。不管去哪里，我都随身携带一本袖珍字典和笔记本，笔记本上记着我遇到的生词。我学习中出过许多错，有时是令人尴尬的错误。有时我会因挫折而哭泣，有时甚至想放弃。但我从未因别的同学英语说得比我快而感到畏惧，因为在电脑屏幕上作出回答之前，我可以根据自己的需要花时间去琢磨自己的想法。突然有一天我发现自己什么都懂了，更重要的是，我说起英语来灵活自如。尽管我还是常常出错，还有很多东西要学，但我已尝到了刻苦学习的甜头。 8学习外语对我来说是非常艰辛的经历，但它又无比珍贵。它不仅使我懂得了艰苦努力的意义，而且让我了解了不同的文化，让我以一种全新的思维去看待事物。学习一门外语最令人兴奋的收获是我能与更多的人交流。与人交谈是我最喜欢的一项活动，新的语言使我能与陌生人交往，参与他们的谈话，并建立新的难以忘怀的友谊。由于我已能说英语，别人讲英语时我不再茫然不解了。我能够参与其中，并结交朋友。我能与人交流，并能够弥合我所说的语言和所处的文化与他们的语言和文化之间的鸿沟。 III. 1. rewarding 2. communicate 3. access 4. embarrassing 5. positive 6. commitment 7. virtual 8. benefits 9. minimum 10. opportunities IV. 1. up 2. into 3. from 4. with 5. to 6. up 7. of 8. in 9. for 10.with V. 1.G 2.B 3.E 4.I 5.H 6.K 7.M 8.O 9.F 10.C Sentence Structure VI. 1. Universities in the east are better equipped, while those in the west are relatively poor. 2. Allan Clark kept talking the price up, while Wilkinson kept knocking it down. 3. The husband spent all his money drinking, while his wife saved all hers for the family. 4. Some guests spoke pleasantly and behaved politely, while others wee insulting and impolite. 5. Outwardly Sara was friendly towards all those concerned, while inwardly she was angry. VII. 1. Not only did Mr. Smith learn the Chinese language, but he also bridged the gap between his culture and ours. 2. Not only did we learn the technology through the online course, but we also learned to communicate with friends in English. 3. Not only did we lose all our money, but we also came close to losing our lives. ?第1课 “对不起” ---------------------------------------------------------------------------------------------------------------------- ～在成田机场①～ ?みか：あのう、すみません。 ?美香：对不起 パスポートが落お ちましたよ （你的）护照掉了。 ?レオ：えっ！ ?莱奥：什么？ ---------------------------------------------------------------------------------------------------------------------- ?重点语句 #1 「あのう、すみません」 「あのう、すみません」是和陌生人打招呼时的说法。「あのう」可以唤起对方的注意，以便开始对话。「すみません」是“对不起”的意思。 ?第2课 “谢谢” ---------------------------------------------------------------------------------------------------------------------- ～在成田机场②～ ?みか：あのう、すみません。 ?美香：对不起 パスポートが落お ちましたよ （你的）护照掉了。 ?レオ：えっ！ ?莱奥：什么？ ああ、どうもありがとうございます。 啊，谢谢。 ?みか：どういたしまして。 ?美香：不客气。 ---------------------------------------------------------------------------------------------------------------------- ?重点语句 #2 「どうもありがとうございます」 「どうもありがとうございます」时表示感谢的较为郑重的说法。「ありがとう」是“谢谢”的意思，在它的前面和后面分别加上「どうも」和「ございます」，语气就变得格外郑重了。当有人向你表示感谢时，你可以回答说「どういたしまして」。 ?第3课 “请多关照” ---------------------------------------------------------------------------------------------------------------------- ～在成田机场③～ ?レオ：あのう、ぼくはレオ…。あなたは？ ?莱奥：嗯，我叫莱奥…… 你呢？ ?みか：私わたしはみか、岡田おかだ みかです。 ?美香：我叫美香，冈田美香。 どうぞよろしく。 请多关照。 ?レオ：こちらこそ、どうぞよろしく。 ?莱奥：也请你多多关照。 ---------------------------------------------------------------------------------------------------------------------- ?重点语句 #3 「どうぞよろしく」 「どうぞよろしく」是和初次见面的人寒暄时使用的比较简略的说法，一般是在说完自己的姓名之后，再说「どうぞよろしく」。 ?第4课 “我第一次来日本” ---------------------------------------------------------------------------------------------------------------------- ～在成田机场④～ 附件1 2020年1月广东省自学考试各专业开考课程考试时间安排表 专业代码/名称学历层次专业建设主考学校 （专业课程组） 1月4日1月5日 上午9:00-11:30下午14:30-17:00上午9:00-11:30下午14:30-17:00代码课程名称代码课程名称代码课程名称代码课程名称 020202 税收学（本科）广东财经大学 00069国际税收03403国有资产管理00062税收管理00999政府预算管理 11389财税史00068外国财政 020301K 金融学（本科）深圳大学 （金融） 00079保险学原理 020301K 金融学（本科） 深圳大学 （金融管理） 11743企业组织与经营环境11742商务沟通方法与技能11741市场与市场营销11745战略管理与伦理 11744会计原理与实务11752管理数量方法与分析11750国际商务金融11751企业成本管理会计 11753金融管理综合应用 1 专业代码/名称学历层次专业建设主考学校 （专业课程组） 1月4日1月5日 上午9:00-11:30下午14:30-17:00上午9:00-11:30下午14:30-17:00代码课程名称代码课程名称代码课程名称代码课程名称 020301K 金融学 （本科） 广东金融学院00079保险学原理 020301K 金融学（本科） 华南理工大学 华南农业大学 暨南大学 广东外语外贸大学 华南师范大学 广东财经大学 11743企业组织与经营环境11742商务沟通方法与技能11741市场与市场营销11745战略管理与伦理 11744会计原理与实务11752管理数量方法与分析11750国际商务金融11751企业成本管理会计 11753金融管理综合应用 020304 投资学（本科）广东工业大学 05175税收筹划04762金融学概论08592房地产投资08591金融营销 12326金融理财分析技术与技巧07250投资学原理12327金融理财规划 020401 国际经济与贸易（本科）广东外语外贸大学 广东工业大学 广东财经大学 深圳大学 11465现代公司管理07788国际结算 030101K 法学（本科） 暨南大学 广东财经大学 华南师范大学 （法律） 00229证据法学 2 新大学日语简明教程课文翻译 第21课 一、我的留学生活 我从去年12月开始学习日语。已经3个月了。每天大约学30个新单词。每天学15个左右的新汉字，但总记不住。假名已经基本记住了。 简单的会话还可以，但较难的还说不了。还不能用日语发表自己的意见。既不能很好地回答老师的提问，也看不懂日语的文章。短小、简单的信写得了，但长的信写不了。 来日本不久就迎来了新年。新年时，日本的少女们穿着美丽的和服，看上去就像新娘。非常冷的时候，还是有女孩子穿着裙子和袜子走在大街上。 我在日本的第一个新年过得很愉快，因此很开心。 现在学习忙，没什么时间玩，但周末常常运动，或骑车去公园玩。有时也邀朋友一起去。虽然我有国际驾照，但没钱，买不起车。没办法，需要的时候就向朋友借车。有几个朋友愿意借车给我。 二、一个房间变成三个 从前一直认为睡在褥子上的是日本人，美国人都睡床铺，可是听说近来纽约等大都市的年轻人不睡床铺，而是睡在褥子上，是不是突然讨厌起床铺了？ 日本人自古以来就睡在褥子上，那自有它的原因。人们都说日本人的房子小，从前，很少有人在自己的房间，一家人住在一个小房间里是常有的是，今天仍然有人过着这样的生活。 在仅有的一个房间哩，如果要摆下全家人的床铺，就不能在那里吃饭了。这一点，褥子很方便。早晨，不需要褥子的时候，可以收起来。在没有了褥子的房间放上桌子，当作饭厅吃早饭。来客人的话，就在那里喝茶；孩子放学回到家里，那房间就成了书房。而后，傍晚又成为饭厅。然后收起桌子，铺上褥子，又成为了全家人睡觉的地方。 如果是床铺的话，除了睡觉的房间，还需要吃饭的房间和书房等，但如果使用褥子，一个房间就可以有各种用途。 据说从前，在纽约等大都市的大学学习的学生也租得起很大的房间。但现在房租太贵，租不起了。只能住更便宜、更小的房间。因此，似乎开始使用睡觉时作床，白天折小能成为椅子的、方便的褥子。 新视野大学英语第一册Unit 1课文翻译 学习外语是我一生中最艰苦也是最有意义的经历之一。 虽然时常遭遇挫折，但却非常有价值。 我学外语的经历始于初中的第一堂英语课。 老师很慈祥耐心，时常表扬学生。 由于这种积极的教学方法，我踊跃回答各种问题，从不怕答错。 两年中，我的成绩一直名列前茅。 到了高中后，我渴望继续学习英语。然而，高中时的经历与以前大不相同。 以前，老师对所有的学生都很耐心，而新老师则总是惩罚答错的学生。 每当有谁回答错了，她就会用长教鞭指着我们，上下挥舞大喊：“错！错！错！” 没有多久，我便不再渴望回答问题了。 我不仅失去了回答问题的乐趣，而且根本就不想再用英语说半个字。 好在这种情况没持续多久。 到了大学，我了解到所有学生必须上英语课。 与高中老师不同，大学英语老师非常耐心和蔼，而且从来不带教鞭！ 不过情况却远不尽如人意。 由于班大，每堂课能轮到我回答的问题寥寥无几。 上了几周课后，我还发现许多同学的英语说得比我要好得多。 我开始产生一种畏惧感。 虽然原因与高中时不同，但我却又一次不敢开口了。 看来我的英语水平要永远停步不前了。 直到几年后我有机会参加远程英语课程，情况才有所改善。 这种课程的媒介是一台电脑、一条电话线和一个调制解调器。 我很快配齐了必要的设备并跟一个朋友学会了电脑操作技术，于是我每周用5到7天在网上的虚拟课堂里学习英语。 网上学习并不比普通的课堂学习容易。 它需要花许多的时间，需要学习者专心自律，以跟上课程进度。 我尽力达到课程的最低要求，并按时完成作业。 我随时随地都在学习。 不管去哪里，我都随身携带一本袖珍字典和笔记本，笔记本上记着我遇到的生词。 我学习中出过许多错，有时是令人尴尬的错误。 有时我会因挫折而哭泣，有时甚至想放弃。 但我从未因别的同学英语说得比我快而感到畏惧，因为在电脑屏幕上作出回答之前，我可以根据自己的需要花时间去琢磨自己的想法。 突然有一天我发现自己什么都懂了，更重要的是，我说起英语来灵活自如。 尽管我还是常常出错，还有很多东西要学，但我已尝到了刻苦学习的甜头。 学习外语对我来说是非常艰辛的经历，但它又无比珍贵。 它不仅使我懂得了艰苦努力的意义，而且让我了解了不同的文化，让我以一种全新的思维去看待事物。 学习一门外语最令人兴奋的收获是我能与更多的人交流。 与人交谈是我最喜欢的一项活动，新的语言使我能与陌生人交往，参与他们的谈话，并建立新的难以忘怀的友谊。 由于我已能说英语，别人讲英语时我不再茫然不解了。 我能够参与其中，并结交朋友。 逝者如斯分享日志日语最基本的100句对话 9月29日 12:47 日语最基本的100句对话 作者： er.已被分享1次评论(0)复制链接 日语最基本的100句对话···会说了，基本上可以应付基本礼仪··· こんにちは。（kon ni chi wa） 你好。 こんばんは。（kon ban wa） 晚上好。 おはようございます。（o ha you go za i mas） 早上好。 お休(やす)みなさい。（o ya su mi na sai） 晚安。 お元気(げんき)ですか。（o gen ki de s ka？） 您还好吧，相当于英语的“How are you”，一种打招呼的方式。 いくらですか。（i ku la de s ka？） 多少钱？ すみません。（su mi ma sen） 不好意思，麻烦你…。相当于英语的“Excuse me”。用于向别人开口时。 ごめんなさい。（go men na sai） 对不起。 どういうことですか。（dou iu ko to de su ka?） 什么意思呢？ 田中さんは中国語(ちゅうごくご)が上手(じょうず)ですね。 （ta na ka san wa jiu go ku ko ga zyou zu de su ne） 田中的中国话说的真好。 まだまだです。（ma da ma da de s） 没什么。没什么。（自谦） どうしたの。（dou si ta no） どうしたんですか。（dou si tan de su ka？） 发生了什么事啊。 なんでもない。（nan de mo nai） 没什么事。 ちょっと待ってください。（jou to ma te ku da sai，可以简单地表达为：jou to） 请稍等一下。 約束(やくそく)します。（ya ku so ko si ma s） 就这么说定了。 これでいいですか。（ko na de i i de su ka？） 这样可以吗？ けっこうです。（ke kou de s） もういいです。（mou i i de s） 不用了。 どうして。（dou si de） なぜ（na ze） 为什么啊？ いただきます（i ta da ki ma s） 那我开动了。（吃饭动筷子前） ごちそうさまでした。（ko ji sou sa ma de si ta） 我吃饱了。（吃完后） ありがとうございます。（a li ga to go za i ma s） 谢谢。 どういたしまして。（dou i ta si ma si de） 习惯与礼仪 我是个漫画家，对旁人细微的动作、不起眼的举止等抱有好奇。所以，我在国外只要做错一点什么，立刻会比旁人更为敏锐地感觉到那个国家的人们对此作出的反应。 譬如我多次看到过，欧美人和中国人见到我们日本人吸溜吸溜地出声喝汤而面露厌恶之色。过去，日本人坐在塌塌米上，在一张低矮的食案上用餐，餐具离嘴较远。所以，养成了把碗端至嘴边吸食的习惯。喝羹匙里的东西也象吸似的，声声作响。这并非哪一方文化高或低，只是各国的习惯、礼仪不同而已。 日本人坐在椅子上围桌用餐是1960年之后的事情。当时，还没有礼仪规矩，甚至有人盘着腿吃饭。外国人看见此景大概会一脸厌恶吧。 韩国女性就座时，单腿翘起。我认为这种姿势很美，但习惯于双膝跪坐的日本女性大概不以为然，而韩国女性恐怕也不认为跪坐为好。 日本等多数亚洲国家，常有人习惯在路上蹲着。欧美人会联想起狗排便的姿势而一脸厌恶。 日本人常常把手放在小孩的头上说“好可爱啊！”，而大部分外国人会不愿意。 如果向回教国家的人们劝食猪肉和酒，或用左手握手、递东西，会不受欢迎的。当然，饭菜也用右手抓着吃。只有从公用大盘往自己的小盘里分食用的公勺是用左手拿。一旦搞错，用黏糊糊的右手去拿， 会遭人厌恶。 在欧美，对不受欢迎的客人不说“请脱下外套”，所以电视剧中的侦探哥隆波总是穿着外套。访问日本家庭时，要在门厅外脱掉外套后进屋。穿到屋里会不受欢迎的。 这些习惯只要了解就不会出问题，如果因为不知道而遭厌恶、憎恨，实在心里难受。 过去，我曾用色彩图画和简短的文字画了一本《关键时刻的礼仪》（新潮文库）。如今越发希望用各国语言翻译这本书。以便能对在日本的外国人有所帮助。同时希望有朝一日以漫画的形式画一本“世界各国的习惯与礼仪”。 练习答案 ５、 （１）止める並んでいる見ているなる着色した （２）拾った入っていた行ったしまった始まっていた 新视野大学英语第三版第二册读写课文翻译 Unit 1 Text A 一堂难忘的英语课 1 如果我是唯一一个还在纠正小孩英语的家长，那么我儿子也许是对的。对他而言，我是一个乏味的怪物：一个他不得不听其教诲的父亲，一个还沉湎于语法规则的人，对此我儿子似乎颇为反感。 2 我觉得我是在最近偶遇我以前的一位学生时，才开始对这个问题认真起来的。这个学生刚从欧洲旅游回来。我满怀着诚挚期待问她：“欧洲之行如何？” 3 她点了三四下头，绞尽脑汁，苦苦寻找恰当的词语，然后惊呼：“真是，哇！” 4 没了。所有希腊文明和罗马建筑的辉煌居然囊括于一个浓缩的、不完整的语句之中！我的学生以“哇！”来表示她的惊叹，我只能以摇头表达比之更强烈的忧虑。 5 关于正确使用英语能力下降的问题，有许多不同的故事。学生的确本应该能够区分诸如their/there/they're之间的不同，或区别complimentary 跟complementary之间显而易见的差异。由于这些知识缺陷，他们承受着大部分不该承受的批评和指责，因为舆论认为他们应该学得更好。 6 学生并不笨，他们只是被周围所看到和听到的语言误导了。举例来说，杂货店的指示牌会把他们引向stationary（静止处），虽然便笺本、相册、和笔记本等真正的stationery（文具用品）并没有被钉在那儿。朋友和亲人常宣称They've just ate。实际上，他们应该说They've just eaten。因此，批评学生不合乎情理。 7 对这种缺乏语言功底而引起的负面指责应归咎于我们的学校。学校应对英语熟练程度制定出更高的标准。可相反，学校只教零星的语法，高级词汇更是少之又少。还有就是，学校的年轻教师显然缺乏这些重要的语言结构方面的知识，因为他们过去也没接触过。学校有责任教会年轻人进行有效的语言沟通，可他们并没把语言的基本框架——准确的语法和恰当的词汇——充分地传授给学生。 新视野大学英语1课文翻译 1下午好！作为校长，我非常自豪地欢迎你们来到这所大学。你们所取得的成就是你们自己多年努力的结果，也是你们的父母和老师们多年努力的结果。在这所大学里，我们承诺将使你们学有所成。 2在欢迎你们到来的这一刻，我想起自己高中毕业时的情景，还有妈妈为我和爸爸拍的合影。妈妈吩咐我们：“姿势自然点。”“等一等,”爸爸说，“把我递给他闹钟的情景拍下来。”在大学期间，那个闹钟每天早晨叫醒我。至今它还放在我办公室的桌子上。 3让我来告诉你们一些你们未必预料得到的事情。你们将会怀念以前的生活习惯，怀念父母曾经提醒你们要刻苦学习、取得佳绩。你们可能因为高中生活终于结束而喜极而泣，你们的父母也可能因为终于不用再给你们洗衣服而喜极而泣！但是要记住：未来是建立在过去扎实的基础上的。 4对你们而言，接下来的四年将会是无与伦比的一段时光。在这里，你们拥有丰富的资源：有来自全国各地的有趣的学生，有学识渊博又充满爱心的老师，有综合性图书馆，有完备的运动设施，还有针对不同兴趣的学生社团——从文科社团到理科社团、到社区服务等等。你们将自由地探索、学习新科目。你们要学着习惯点灯熬油，学着结交充满魅力的人，学着去追求新的爱好。我想鼓励你们充分利用这一特殊的经历，并用你们的干劲和热情去收获这一机会所带来的丰硕成果。 5有这么多课程可供选择，你可能会不知所措。你不可能选修所有的课程，但是要尽可能体验更多的课程！大学里有很多事情可做可学，每件事情都会为你提供不同视角来审视世界。如果我只能给你们一条选课建议的话，那就是：挑战自己！不要认为你早就了解自己对什么样的领域最感兴趣。选择一些你从未接触过的领域的课程。这样，你不仅会变得更加博学，而且更有可能发现一个你未曾想到的、能成就你未来的爱好。一个绝佳的例子就是时装设计师王薇薇，她最初学的是艺术史。随着时间的推移，王薇薇把艺术史研究和对时装的热爱结合起来，并将其转化为对设计的热情，从而使她成为全球闻名的设计师。 6在大学里，一下子拥有这么多新鲜体验可能不会总是令人愉快的。在你的宿舍楼里，住在你隔壁寝室的同学可能会反复播放同一首歌，令你头痛欲裂！你可能喜欢早起，而你的室友却是个夜猫子！尽管如此，你和你的室友仍然可能成 日语最基本的100句对话 こんにちは。（kon ni ji wa） 你好。 こんばんは。（kon ban wa） 晚上好。 おはようございます。（o ha you go za i mas） 早上好。 お休(やす)みなさい。（o ya su mi na sai） 晚安。 お元気(げんき)ですか。（o gen ki de s ka？） 您还好吧，相当于英语的“How are you”，一种打招呼的方式。 いくらですか。（i ku la de s ka？） 多少钱？ すみません。（su mi ma sen） 不好意思，麻烦你…。相当于英语的“Excuse me”。用于向别人开口时。 ごめんなさい。（go men na sai） 对不起。 どういうことですか。（dou iu ko to de su ka?） 什么意思呢？ 山田さんは中国語(ちゅうごくご)が上手(じょうず)ですね。 （ta na ka san wa jiu go ku ko ga zyou zu de su ne） 山田的中国话说的真好。 まだまだです。（ma da ma da de s） 没什么。没什么。（自谦） どうしたの。（dou si ta no） どうしたんですか。（dou si tan de su ka？） 发生了什么事啊。 なんでもない。（nan de mo nai） 没什么事。 ちょっと待ってください。（jou to ma te ku da sai，可以简单地表达为：jou to） 请稍等一下。 約束(やくそく)します。（ya ku so ko si ma s） 就这么说定了。 これでいいですか。（ko na de i i de su ka？） 这样可以吗？ けっこうです。（ke kou de s） もういいです。（mou i i de s） 不用了。 どうして。（dou si de） なぜ（na ze） 为什么啊？ いただきます（i ta da ki ma s） 那我开动了。（吃饭动筷子前） ごちそうさまでした。（ko ji sou sa ma de si ta） 我吃饱了。（吃完后） ありがとうございます。（a li ga to go za i ma s） 谢谢。 どういたしまして。（dou i ta si ma si de） 别客气。 本当(ほんとう)ですか。（hon dou de su ka？） 真的？ うれしい。（so ne si i） 我好高兴。（女性用语） よし。いくぞ。（yo si。i ku zo） 好！出发（行动）。（男性用语） いってきます。（i te ki ma s） 我走了。（离开某地对别人说的话） いってらしゃい。（i te la si yai） 您好走。（对要离开的人说的话） 新视野大学英语2课文翻译（Unit1-Unit7） Unit 1 Section A 时间观念强的美国人 Para. 1 美国人认为没有人能停止不前。如果你不求进取，你就会落伍。这种态度造就了一个投身于研究、实验和探索的民族。时间是美国人注意节约的两个要素之一，另一个是劳力。 Para. 2 人们一直说：“只有时间才能支配我们。”人们似乎是把时间当作一个差不多是实实在在的东西来对待的。我们安排时间、节约时间、浪费时间、挤抢时间、消磨时间、缩减时间、对时间的利用作出解释；我们还要因付出时间而收取费用。时间是一种宝贵的资源，许多人都深感人生的短暂。时光一去不复返。我们应当让每一分钟都过得有意义。 Para. 3 外国人对美国的第一印象很可能是：每个人都匆匆忙忙——常常处于压力之下。城里人看上去总是在匆匆地赶往他们要去的地方，在商店里他们焦躁不安地指望店员能马上来为他们服务，或者为了赶快买完东西，用肘来推搡他人。白天吃饭时人们也都匆匆忙忙，这部分地反映出这个国家的生活节奏。工作时间被认为是宝贵的。Para. 3b 在公共用餐场所，人们都等着别人吃完后用餐，以便按时赶回去工作。你还会发现司机开车很鲁莽，人们推搡着在你身边过去。你会怀念微笑、简短的交谈以及与陌生人的随意闲聊。不要觉得这是针对你个人的，这是因为人们非常珍惜时间，而且也不喜欢他人“浪费”时间到不恰当的地步。 Para. 4 许多刚到美国的人会怀念诸如商务拜访等场合开始时的寒暄。他们也会怀念那种一边喝茶或咖啡一边进行的礼节性交流，这也许是他们自己国家的一种习俗。他们也许还会怀念在饭店或咖啡馆里谈生意时的那种轻松悠闲的交谈。一般说来，美国人是不会在如此轻松的环境里通过长时间的闲聊来评价他们的客人的，更不用说会在增进相互间信任的过程中带他们出去吃饭，或带他们去打高尔夫球。既然我们通常是通过工作而不是社交来评估和了解他人，我们就开门见山地谈正事。因此，时间老是在我们心中的耳朵里滴滴答答地响着。 Para. 5 因此，我们千方百计地节约时间。我们发明了一系列节省劳力的装置；我们通过发传真、打电话或发电子邮件与他人迅速地进行交流，而不是通过直接接触。虽然面对面接触令人愉快，但却要花更多的时间, 尤其是在马路上交通拥挤的时候。因此，我们把大多数个人拜访安排在下班以后的时间里或周末的社交聚会上。 Para. 6 就我们而言，电子交流的缺乏人情味与我们手头上事情的重要性之间很少有或完全没有关系。在有些国家, 如果没有目光接触，就做不成大生意，这需要面对面的交谈。在美国，最后协议通常也需要本人签字。然而现在人们越来越多地在电视屏幕上见面，开远程会议不仅能解决本国的问题，而且还能通过卫星解决国际问题。从实践的角度探讨在日语教学中多媒体课件的应用
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