a r X i v :a s t r o -p h /0401595v 1 28 J a n 2004WIYN Survey for Carbon Stars in the M 31and Cetus Dwarf Spheroidal
Galaxies:Evolutionary Implications
Daniel Harbeck
Department of Astronomy,University of Wisconsin,475North Charter Street,Madison,WI
53706
harbeck@https://www.doczj.com/doc/957086286.html, John S.Gallagher,III Department of Astronomy,University of Wisconsin,475North Charter Street,Madison,WI 53706jsg@https://www.doczj.com/doc/957086286.html, and Eva K.Grebel Astronomical Institute of the University of Basel,Venusstrasse 7,CH-4102Binningen,Switzerland grebel@astro.unibas.ch ABSTRACT We report results of a photometric survey with the WIYN telescope for carbon stars in the M 31dwarf spheroidal (dSph)companions And III,And V,And VI,and And VII,as well as in the relatively isolated Local Group dSph Cetus.We ?nd three carbon-star candidates in And VII and one carbon star in each And VI and https://www.doczj.com/doc/957086286.html,paring
the carbon star content with other Local Group dwarf galaxies,we argue against the presence of substantial intermediate-age stellar populations in the all of the galaxies surveyed with the exception of And VII.We discuss these results in the context of the origin of the Andromeda dSphs and conclude that these are ancient galaxies,most of which ceased star formation long before the main merger events in M 31.The M 31dSphs therefore show less diversity in star formation histories than the Galactic dSph companions,or the M 31dE companions,as illustrated by NGC 147which was surveyed as a calibration object.All of our dSph targets except And V have candidate carbon stars below the tip of the RGB,which resemble CH stars found in globular clusters.We estimate that 0.3%of stars in the dSphs are CH stars,presumably as a result of C pollution from a binary https://www.doczj.com/doc/957086286.html,parisons with CH star frequencies in globular clusters could constrain the impact of dense environments on the frequency of this form of binary star evolution.
Subject headings:Local Group—galaxies:dwarf—galaxies:stellar content—galax-
ies:evolution—stars:carbon—stars:statistics
1.Introduction
The two massive spiral galaxies of the Local group(LG),the Milky Way and Andromeda(M31) appear to have di?erent histories.While tidal streams associated with minor mergers orbit both spirals(e.g.,Ibata,Gilmore,&Irwin1995;Ibata et al.1997,2001;Ferguson et al.2002;Newberg et al.2002,2003;Majewski et al.2003;Yanny et al.2003),the di?ering levels of interactions in the histories of M31and the Milky Way may be re?ected in the mean metallicity of their halo stars. M31’s halo is more metal-rich than that of the Milky Way,suggesting that mergers have had a substantial impact on M31(see Durrell,Harris,&Pritchet2001;Brown et al.2003and references therein).
We also can ask to what degree the di?erent formation histories of M31and the Milky Way are re?ected in their systems of satellite galaxies.The dwarf spheroidal(dSph)galaxies of both systems are of special interest because these galaxies might be the unused basic building blocks in hierarchical galaxy formation scenarios(e.g.,Bullock,Kravtsov,&Weinberg2001),or,alterna-tively,what should have been larger systems whose structure and evolution was modifed by their proximity to giant spirals(e.g.,Mayer at al.2001).For a more detailed discussion of this subject, see Grebel,Gallagher,&Harbeck(2003).
While deep photometric studies over wide?elds for the Milky Way dSph satellites reach below the oldest main sequence turno?s(e.g.,Hurley-Keller,Mateo,&Grebel1999;Harbeck et al.2001; Carrera et al.2002;Monelli et al.2003;Lee et al.2003),allowing their star formation histories to be studied in detail,the distance of the M31dSph subsystem has so far limited existing ground-based photometric studies to the upper red giant branch level(e.g.,Armandro?et al.1993;Armandro?, Davies,&Jacoby1998;Grebel&Guhathakurta1999)and space-based photometric studies to the horizontal branch level(e.g.,Da Costa et al.2000;Da Costa,Armandro?,&Caldwell2002;Harbeck et al.2001;Karachentsev et al.2003).Thus,only indirect conclusions can be derived for their star formation history and mean age.Even at this level the M31dSphs appear to have unique properties in that Harbeck et al.(2001)found that the M31dSphs show a second parameter e?ect in their horizontal branch(HB)morphologies.After accounting for o?sets due to mean metallicities,the M31dSphs appear to have systematically redder HB morphologies than the Milky Way’s dSph companions.The origin of this second parameter e?ect is not clear,but explanations include a slightly(i.e.,2Gyr)younger age of the M31companions compared to their Galactic equivalents (see Da Costa et al.2000;Harbeck et al.2001).This has also been suggested for Cetus(Sarajedini et al.(2002)).
In this paper we study the stellar populations in the M31dSphs based on properties of stars on the extended asymptotic giant branch(EAGB)containing stars more luminous than the tip
of the red giant branch(RGB).These include classical EAGB carbon stars(C stars),which trace intermediate-age-to-old(1to10Gyr)stellar populations(Aaronson,Cook,&Norris1986).This class of C star results from thermal pulses and subsequent mixing of freshly synthesized C into the envelopes of the EAGB stars.The transition on the EAGB from an oxygen rich(M star)to C star therefore depends both on the evolution and initial abundances of the star;lower O abundances require less C to make C/O>1.
A second class of C star is present even in old globular cluster stellar populations with lumi-nosities below the tip of the RGB.These stars are products of mass transfer from a C star onto its main sequence binary companion,which subsquently evolves up the RGB(de Kool&Green 1995;Han et al.1995).The presence of C stars less luminous than the tip of the RG
B is evidence for binary evolution in a stellar population,and is not tied to the age of the population in any simple way.These are spectroscopically identi?ed as CH stars;for a review of CH and other types of carbon and related evolved stars,see McClure(1985).The CH stars in turn are likely to be evolved versions of dwarf carbon(dC)stars(de Kool&Green1995),and we discuss implications of the presence of CH stars in M31dSph companions in§3.4.
While C stars are useful stellar population diagnostics,no systematic wide-?eld survey for C stars in the M31dSph galaxies has been published so far.However,Aaronson et al.(1985)found two EAGB C star candidates in And II,which led them to suggest that And II sustained star formation as an irregular-like galaxy for an extended time.C?o t′e,Oke,&Cohen(1999)spectroscopically con?rmed an additional C star located below the RGB tip luminosity,which they interpreted as being a CH-like star,and probably a product of binary evolution of an undetermined age. However,their color-magnitude diagram(CMD)of And II con?rms the presence of an AGB and thus of an intermediate-age stellar population.It also provides a good example of the importance of spectroscopic con?rmation in these small galaxies with few EAGB star candidates(see their Fig.
4).In this paper we present a systematic photometric survey using the WIYN3.5-m telescope1 for C star candidates in the Andromeda dSph companions And III,And V,And VI,and And VII2, and in the comparatively isolated LG dSph galaxy Cetus.New data for NGC147as a calibrator for our survey technique will be presented as well.
2.Data and Reduction
We observed the Andromeda companions And III,And V,And VI,and And VII,as well as the Cetus dSph,with the MiniMo Mosaic CCD camera at the3.5m WIYN telescope located at Kitt Peak.We used Johnson V and I?lters to obtain temperature and luminosity information for stars in the galaxies in order to construct a color magnitude diagram(CMD),while observations in two narrow-band?lters centered on the TiO and CN feature at778nm and808nm,respectively, were used to identify cool giant stars with enhanced carbon abundance.The use of a CN-TiO ?lter combination is a well-established method for the reliable identi?cation of C stars(see Cook, Aaronson,&Norris1986;Albert,Demers,&Kunkel2000;Nowotny et al.2003).Most of the galaxies were observed during an observing campaign on2003September28to2003October1.
Since all galaxies are at a similar distance,the exposure times were chosen to be500s in each of the V and I?lter,and3×500s in each of the narrow band?lters.There are two exceptions: The exposure times in the V and I band?lters for And VII were split into2×300s to avoid CCD blooming of bright stars present in the?eld of view.The narrow band exposures for And VI were obtained during an earlier observing run at WIYN on2002October20;the exposure times are 2×500s per?lter.In addition we observed the dwarf elliptical galaxy NGC147to validate our ability to identify C stars.This galaxy is known to have a large number of C stars(approximately 146C stars have been found in the work of Nowotny et al.2003).
Although not always of photometric quality,the data are of superb quality in seeing.The typical seeing in the near infrared narrow-band?lters was0.5′′to0.6′′and better;the typical seeing in the broad band?lters was0.7′′,and never worse then0.8′′.MiniMo at WIYN consists of a mosaic of two CCD chips with a total?eld of view of9.6′×9.6′.The M31dSph satellites with typical core radii of order of1′to1.5′thus conveniently?t onto a single chip,and have been centered on chip#1of the mosaic.The more extended galaxies NGC147and Cetus were placed at the center of the?eld of view of MiniMo.
During the2003campaign there was a problem with the MiniMo CCD readout electronics, resulting in strong random variations of the CCD’s overscan level.Before correcting the raw CCD frames with daily zero calibrations frames,we subtracted the overscan on a line-by-line basis.The variations in the overscan did not completely vanish,leaving residual additional background noise with an RMS of order of5counts.Finally the images were corrected for illumination variations using dome?at?elds.
For each galaxy,all its images were registered to a common reference coordinate system.The three(or two in the case of And VI)exposures per narrow-band?lter were stacked and used for cosmic-ray rejection.In the case of And VII we also stacked the two V and I images.As an example we present a portion of the northern region of NGC147in Figure1.Point spread photometry was
performed in all?lters using the daophot implementation under IRAF3,resulting in photometric catalogs for each galaxy containing instrumental V,I,TiO,and CN?lter magnitudes.
Since the weather was non-photometric during parts of our observing run,we did not attempt to observe photometric standard stars,and all magnitudes cited in this paper are instrumental magnitudes.In order to identify C stars,we only need di?erential photometry.For clarity,however, we adopted I,and V?I zeropoints for each galaxy to match the magnitude and color of the blue side of the tip of the RGB with observed values(from Sarajedini et al.2002for Cetus,from Grebel &Guhathakurta1999for And VII and And VI,from Armandro?,Davies,&Jacoby1998and Armandro?et al.1993for And V and And III,respectively;NGC147is calibrated according to Nowotny et al.2003).We calibrated the zeropoint of the CN?TiO color using the assumption that blue stars(i.e.,bluer then the tip of the RGB)should have CN?TiO=0,since spectra of warmer stars are expected to featureless in this wavelength region(Brewer,Richer,&Crabtree 1995).
2.1.Identi?cation of Carbon stars
The color-magnitude diagram for our test case,NGC147,is shown in Fig.3(left).The intrin-sically broad red giant branch(RGB)features prominently as it does in the WFPC2observations of Han et al.(1997).We also?nd a prominent population of stars well above the tip of the RGB (TRGB).The right side of the same?gure demonstrates the selection of carbon stars from the two-color(V?I https://www.doczj.com/doc/957086286.html,?TiO)diagram:stars with high carbon content(and therefore low TiO but strong CN molecule band absorption)stand out in this plot and are selected according to the selection box(CN?TiO≥0.25).Stars in this plot with CN?TiO≥0.65mag are almost always false detections,and are rejected for NGC147(see discussion of false detections at the end of this section).Only stars with I≤21mag are plotted in our two-color diagram to limit this sample to objects with good photometry.Only stars with colors of the RGB and I≤20.7mag(Han et al. 1997)qualify as bona-?de C stars;stars fainter than the TRGB might be CH stars and thus are not intermediate age stellar population tracers.C stars selected this way are plotted in the CMD of NGC147with?lled circles.The substantial number of C star candidates(155)matches our expectation for this galaxy and compares well to the146C stars found by Nowotny et al.(2003).
In addition to the photometric selection,we construct the di?erence of the CCD images ob-served in the TiO and CN?lters to cross-identify the candidates on these images.An example of such a di?erence image is given in Fig.2,where we zoom into the boxed region of Fig.1.A visual inspection of the di?erence image of NGC147leads us to estimate a roughly10%incompleteness in our C star detections,which is compensated by roughly10%false detections.We did not cross-
identify each star in our NGC147catalog with the di?erence image,but will do so for the dSph galaxies and will accept only C stars that appear both in our photometric catalog and stand out as a clear detection in the di?erence images.The fact that we?nd a slightly larger number of C stars in NGC147than Nowotny et al.(2003)can be explained by our deeper photometry,better seeing conditions(by at least0.3′′in the narrow-band?lters),and a larger?eld coverage.A comparison between the catalog of C stars of Nowotny et al.(2003)indeed reveals that most of the stars are in common with our catalog,with both false detections and misses of order of10%in their as well as in our work.We thus increase the number of C stars in NGC147to approximately155,and conclude that our selection e?ciency of C star candidates is comparable to other surveys.
Due to the small absolute number and an improved crowding situation,we slightly loosen the photometric selection criterion for C stars in the dSphs,by requiring a CN?TiO color of ≥0.2mag and a luminosity of the C star candidates brighter than I=22mag.This selection will result in some false detections that we identi?ed and removed during the cross-correlation with the di?erence image.With the small number of C star candidates per galaxy we can a?ord to double-check each individual star.Reasons why stars might appear in the photometric catalog and not in the di?erence image turned out to be(and are indeed limited to):misidenti?cation of background galaxies,of cosmic ray trails(not all cosmic rays are actually removed),stars a?ected by stray light or blooming in the vicinity of bright stars in the?eld of view,blends of two stars, or CCD defects.C star candidates that turned out to be false detections have been marked with open circles in the diagrams.Stars that remain valid C star candidates after cross-identi?cation are plotted with?lled circles.
2.1.1.The Andromeda dSphs
The CMDs and two-color diagrams of the observed M31companions are presented in the same manner as for NGC147in Figs.4to7.The color of the RGB depends on the metallicity of the galaxies,and we carefully adjusted the V?I color boundary for the C star selection to avoid confusion with stars bluer than the tip of the RGB.The initial number of photometric detections of C star candidates that are not cross-identi?ed in the di?erence image is very di?erent for the four observed galaxies(as indicated by the number of open circles in the diagrams),and turned out to be clearly correlated with the number of(bright)?eld stars on the CCD frame.The larger the number of bright foreground stars,the larger the number of false detections.After comparing the initial photometric C star candidates with the di?erence images,we are left with a smaller set of reliable C star candidates in the galaxies.These are listed in Table1.
Depending on whether the bolometric luminosity of a C star candidate is brighter or clearly dimmer than the tip of the RGB,we classify it as a genuine C star(“C”in Table1)or as an evolved dC star(also called“CH”star),respectively.This selection criterion is unique for all but one star in And VII(see Figure7),which has almost the same luminosity as the TRGB.We classify this star as a C star candidate.This is justi?ed as technically AGB stars would have
at least the same bolometric luminosity as the tip of the RGB.If we apply a correction in the form B.C.=?0.246·(V?I)(Reid&Mould1984)this star would clearly satisfy the bolometric luminosity criterion.
The V-and I-band images and the TiO-and CN-band images of And VI were taken during two di?erent campaigns,and due to imperfect overlap of the two observations the total?eld covered of And VI is limited to a2.9′-wide stripe(more than twice the core radius of1.3′,Caldwell1999). The number of detected C stars for this galaxy therefore could be incomplete.
The lack of radial velocity information for the C star candidates prohibits prevents us from verifying their membership in the M31dSph companion galaxies.Owing to the large angular distance of these galaxies from M31,confusion with M31halo C stars seems unlikely.Indeed, all of our C star candidates are near the central regions of the dSphs,supporting the idea that younger(that is,intermediate-age)populations are primarily found in the central regions of dSphs (see Grebel1999,2000;Harbeck et al.2001).The centralized location of the C stars and their narrow band colors makes it unlikely that we are seeing misidenti?ed Galactic foreground dC stars or backgrund galaxies.In the remainder of this paper we will assume that the C star candidates are members of the M31dSph satellites.
2.1.2.Cetus
Cetus was placed on the center of the MiniMo?eld of view,so there is no photometry available for a central7′′wide stripe.The CMD and the two-color diagram of Cetus are shown in Figure8 and Fig.9for the MiniMo CCD chip1and chip2,respectively.We can identify three objects with enhanced carbon abundance.One of them is a likely C star candidate,while two of them appear to be CH stars or similar objects.However,due to the gap in the MiniMo image we might miss approximately one(1±1)C star in Cetus.In good agreement with earlier studies(Whiting,Hau, &Irwin1999;Sarajedini et al.2002)we do not?nd clear evidence for an EAGB in this galaxy.
3.Discussion
We successfully detected high probability candidates both for EAGB C stars and CH stars in four M31dSphs surveyed and the Cetus dSph.In his reviews of the C star content of Local Group galaxies,(Groenewegen1999,2002)plots absolute magnitude of LG galaxies versus the logarithm of the number of C stars,carefully corrected for area coverage.We expanded this plot with new data points as shown in Figure10using new results from the literature as summarized in Table2. Absolute V-band magnitudes were taken from Grebel,Gallagher,&Harbeck(2003).
We consider only LG galaxies where surveys for C star candidates using the CN-TiO narrow-band?lter technique are expected to be reasonably complete.While several C stars have been
found in Milky Way dSph galaxies(Aaronson&Mould1985;Groenewegen2002),in some cases these are likely to be CH-stars,and the surveys often have incomplete areal coverage.We therefore include only a few Milky Way dSph satellites in Figure10.For the SMC and LMC we adopt the DENIS infrared survey results for the number of C stars(Cioni&Habing2003).
The galaxies in Figure10show the well-known correlation between the absolute V-band lumi-nosity of a galaxy(i.e.,an approximate stellar mass)and the total number of C stars.A useful tool to study the C star content of a galaxy is N C,L=log(#C)+0.4·M V,which measures the number of C stars per unit luminosity,and thus is a measure for the deviation from the M V-log(#C)relation (Aaronson,Olszewski,&Hodge1983;Groenewegen1999).We plot N C,L vs.the mean metallicity of the galaxies in Fig.10(right).N C,L scatters between-3and-4.6for the galaxies,as previously illustrated by Groenewegen(1999,2002).There is no apparent trend with metallicity,consistent with the predictions of theoretical population models(Mouhcine&Lan?c on2003).These models show that for smoothly evolving stellar populations,N C,L is expected to drop substantially only for super-solar metallicities or systems where the stars are all ancient with ages≥9-10Gyr.
We divide the galaxies in this sample into three classes,motivated by their morphology and —where known—their star formation history:(i)“stellar fossil”dSphs,where star formation ceased at very early times,(ii)dwarf irregular galaxies,transition-type galaxies,and dSphs where the period of star formation extends over a substantial fraction of cosmic time,and(iii)the dE companions of M31.Of the Galactic dSphs included in Table2,a deep HST study of the stellar populations in Leo I revealed that this galaxy was actively forming stars until1Gyr ago,with slower ongoing star formation until～300Myr before the present(Caputo et al.1997;Gallart et al.1999). The situation is similar for Fornax,where star formation stopped only～100to200Myr in the past(Stetson,Hesser,&Smecker-Hane1998;Grebel&Stetson1999;for recent reviews of the star formation histories of Local Group dwarf galaxies,see Grebel1999,2000).These two Galactic dSphs are in our second star forming galaxy category.All of the M31dEs have large numbers of intermediate age stars,and low level star formation continues into the present in NGC185and NGC205(Lee,Freedman,&Madore1993;Grebel1997;Mart′?nez-Delgado,Aparicio,&Gallart 1999;Cappellari et al.1999;Davidge2003).We omit the compact elliptical M32from our discussion due to the lack of a published survey for C stars.
The di?erent symbols in Fig.10refer to the three classes of galaxies we just de?ned.We can extract a general trend from Fig.10(right panel):Quiescent dSph galaxies contain a small number of C stars per V-band luminosity(≤10?4.5),while those galaxies with active or recent star formation have a higher C star content(≈10?3.5).The recent star formation in the Fornax dSph makes this an outstanding galaxy in this plot.The normalized C star content of the three M31 dEs(NGC147,NGC205,and NGC185)scatters around N C,L=?4,consistent with their large intermediate-age stellar populations.
3.1.Star Formation Histories of the Andromeda dSphs
The CMDs derived from WFPC2imaging of And I,And II,And III,And V,And VI,and And VII do not extend much below the horizontal branch.They are therefore sensitive only to potential main sequence stars that have ages of≤1Gyr.None of these dSphs show evidence for star formation within this recent time frame(see,e.g.,Harbeck et al.2001;Karachentsev et al. 2003).Furthermore,the CMDs presented by Harbeck et al.(2001)show that red clumps,typical of intermediate age stars,are unlikely to be present in the M31dSphs,and that all the M31dSphs have pronounced horizontal branches.
3.2.The C/M ratio
Comparisons of the number of normal EAGB stars,seen as stars with spectral classes of M5 or later,to C stars also is a useful evolutionary diagnostic(see,e.g.,Blanco&McCarthy1983; Mouhcine&Lan?c on2003;Cioni&Habing2003).This ratio depends on both age and metallicity, with the relative number of C stars peaking for mean ages of≈1Gyr,and in all cases declining for ages greater than～10Gyr.Unfortunately,the relevant ratio of N C/N M5+is very di?cult to derive for the M31dSphs due to the very small number of C and M stars on the EAGB and the presence of substantial numbers of red Galactic foreground stars.
An approximate value of N C/N M5+can be obtained from our data by counting all stars redder than V?I≥2.0mag(to select M5+spectral classes;Richer,Pritchet,&Crabtree1985,Pritchet et al.1987)and I19.However,we avoid stars near to the saturation limit of the CCD,which are bright foreground stars,and objects whose peculiar colors indicate either that they are not stars or that a problem exists with the data.This approach is most e?ective when the density of EAGB stars relative to foreground?eld stars is>1, as in NGC147.
We counted all EAGB M5+stellar candidates in NGC147both in the full?eld of view(which will lead to an overestimation of N M5+due to?eld contamination),and within the central3′, which may cause us to slightly underestimate N M5+due to crowding e?ects.This approach yields
=0.19for the full?eld and the central region,respectively. N C/N M5+=159
575
Given the expected uncertainty in N C/N M5+of order of0.02we are in excellent agreement with the result of Nowotny et al.(2003),who found N C/N M5+=0.15for NGC147.
Since the M31dSphs cover a relatively small region of the WIYN MiniMo camera CCD chips, we counted all stars ful?lling the conditions de?ned above in strips above and below the dSph targets.The resulting estimate of the foreground Galactic star contamination at And VI is too large relative to any population of EAGB M5+stars to get a meaningful estimate for N M5+.Similarly, we?nd no M-star candidates in the Cetus dSph,where this method yields N M5+=?2±4.We also see that since And III and And V have no EAGB C stars,they must have N C/N M5+=0.
For And VII this method gives N M5+≈48.We derive a relative fraction of C stars of N C/N M5+=0.06or log(C/M)≈?1.2.For a galaxy with constant star formation we would expect log(C/M)≥1at[Fe/H]≈?1.5(e.g.,Fig.8in Mouhcine&Lan?c on2003).If we adopt a correction for the bolometric luminosity(as in Reid&Mould1984)to select M stars,we would slightly?nd38M5+stars despite the fact that we would include even redder stars with I-band luminosities fainter than the tip of the RGB by the selection,which mainly seems to re?ect the uncertainty in the background subtraction.Despite the considerable uncertainty in this ratio,we can say there is no indication for the presence of a signi?cant younger intermediate-age(<3Gyr) stellar population in And VII based on the models of Mouhcine&Lan?c on(2003).
The presence of only one carbon star in And VI and Cetus,where we?nd no signi?cant populations of EAGB M5+-stars might be interpreted as a high N C/N M5+ratio which would be unexpected for a small young stellar population.However,with only one candidate EAGB star in each galaxy,a range of possibilities existis,including the production of an EAGB C star via binary evolution.For example,C stars should be able to form from blue stragglers.Furthermore,with only one EAGB candidate per galaxy,spectroscopic con?rmation of membership is essential.
In summary,only And VII in our sample shows evidence for a substantial EAGB stellar pop-ulation.In this case the low value of the N C/N M5+ratio places these stars in the medium range of intermediate stellar ages,namely ages≥3-5Gyr.
3.3.On the origin of the Andromeda dwarf companion galaxies
We began this investigation with the objective of comparing the dSph companions of M31 with those of the Milky Way,and of investigating whether the dSphs might be linked to the merger history of M31.Our data are consistent with the M31dSphs having predominantly old stellar populations,where most star formation occurred at>10Gyr in the past.The only clear dSph exception are And II(from Aaronson et al.1985work),and And VII,where signi?cant star formation could have continued until3-5Gyr ago.Both the survey for EAGB stars presented here and the study of horizontal branch morphologies by Harbeck et al.(2001)are consistent with the view that the majority of M31’s dwarf satellites are old systems.In particular,we do not?nd examples of dSphs with recent star formation activity,like the Fornax or Carina dSph satellites of the Milky Way.
Any connections between the dSphs and stellar halo of M31remain tenuous.As Ferguson et al.(2002)emphasize,even though And I and And III lie in the projected vicinity of the main M31 southwestern stellar stream,their low metallicities make dSphs unlikely to have been dominant contributors to the more metal rich components of the M31halo.A further constraint comes from the Brown et al.(2003)analysis of their spectacularly deep HST CMD of the M31stellar halo.They?nd that the signi?cant metal-rich halo component of M31has an age of6-8Gyr, too young to be associated with any of the M31dSph companions with the possible exception of
the distant And VII dSph;see Grebel,Gallagher,&Harbeck(2003)for deprojected distances and mean metallicities of the M31dwarf companions.
In terms of their star-formation histories,M31’s dSphs resemble the ancient Galactic dSph companions as epitomized by the Draco and Ursa Minor dSphs.Of these two,Draco appears to be dark-matter dominated(e.g.,Odenkirchen et al.2001),whereas Ursa Minor may be undergoing tidal disruption(e.g.,Palma et al.2003),so Draco probably is the best comparison object.The M31dSph companions evidently formed as independent objects that are not directly associated with the recently uncovered indications of interactions with M31,which took place during the galactic“middle ages”some6–8Gyr in the past.
However,a possible environmental e?ect is seen in that only two M31dSphs evidently sup-ported extended periods of star formation,fewer than in the population of Galactic dSphs located at similar distances from their spiral host galaxy.That present-day environment cannot be the only agent becomes apparent when considering the similarly quiescent,isolated Cetus dSph(see Grebel,Gallagher,&Harbeck(2003)for a more extensive discussion).An independent constraint on the importance of dSphs for the accretion history of M31could be established by a study of the [α/Fe]abundances in both M31and its companions to see whether halo and dSphs exhibit similar di?erences as found for the Milky Way by,e.g.,Shetrone,C?o t′e,&Sargent(2001).Unfortunately, because of the distance of M31and its satellites only global[Fe/H]values can be measured spec-troscopically to date(C?o t′e,Oke,&Cohen1999;Guhathakurta,Reitzel,&Grebel2000;Reitzel& Guhathakurta2002).
3.4.On the frequency of dC/CH stars
The standard scenario of“extrinsic”C star formation implies that a main sequence star accretes material through Roche-lobe over?ow from its intrinsic EAGB C star binary companion.This mechanism also is responsible for CH-stars(see McClure&Woodsworth1990,Han et al.1995) and we can therefore consider the dC and CH-like stars to be tracers of similar e?ects of binary evolution.But what fraction of stars in a stellar population will su?er from pollution severe enough to turn them into C stars?This number depends both on the binary fraction,and the distribution of binary star semi-major axes,metallicity,and age(see,e.g.,de Kool&Green1995).A“hard”binary system with a orbital separation smaller then a typical AGB radius might disrupt the evolving AGB star before a third dredge-up is able to turn the AGB star into a C star.Binary-orbit shrinking due to close three-body encounters in dense globular clusters could reduce the speci?c frequency of dC stars(C?o t′e et al.1997).Thus the frequency of dC and CH stars is expected to depend also on the environment,and we should?nd relatively more dC/CH stars in low density dSph galaxies with old stellar populations than in globular clusters.
To estimate the relative number of CH-stars in the uncrowded dSph galaxies,we counted the number of RGB stars brighter than the I=22mag limit of our C star survey.The ratio between
numbers of CH-stars,which we approximate as evolved dC stars,and RGB stars is an approximate measure of the relative fraction of dC stars in the stellar populations of these galaxies.However, the small number statistics of the rare C-rich stars introduces substantial uncertainties into this ratio.In Table3we present the number of RGB stars and CH star candidates,as well as the estimated percentage of CH stars for the galaxies surveyed.We assume that all of our candidates are CH stars in the M31dSphs.Spectroscopic follow-up of these stars is essential to con?rm their membership by their radial velocities and verify that they are C-rich objects.
To improve the statistics,we simply sum up all of the RGB stars and CH stars to obtain a ?rst estimate of the dSph CH star frequency.We?nd～0.3%of the dSph’s stars to be CH stars that could have originated from dC stars which were contaminated during the evolution of a binary stellar system.The frequency of CH stars in globular clusters remains to be established since such stars are very rare(see C?o t′e et al.1997).
In NGC147we count CH stars in the same way as we did for the dSphs between the tip of the RGB and I≤22,and also count RGB stars in the same luminosity range.This way we derive a slightly higher CH stars frequency of0.8%,which might be unreliable since strong crowding might become important for the selection of fainter carbon-rich stars and confusion with genuine C stars at the bright end of the selection might lead to an overestimation of the number of CH stars.
4.Summary
We present results from a photometric survey for C stars and related carbon-rich stars in the And III,And V,And VI,And VII,and Cetus dSph galaxies carried out with the WIYN3.5-m telescope.Similar data also were obtained for the dE galaxy NGC147,previously surveyed for C stars by Nowotny et al.(2003),as a check on our technique.The small number of C stars found among the M31dSph satellite galaxies implies that they contain predominantly old stellar populations.Aside from And II and especially And VII,where star formation may have been active as recently as3-5Gyr in the past,the And III,And V,and And VI dSphs have not supported signi?cant star formation within the past～10Gyr.
The stellar populations of the M31dSphs both are older and more metal-poor than the intermediate-age M31stellar halo components.We conclude that the dSph satellites are an early legacy of the time before the prominent M31merger events that occurred about6-8Gyr in the past. The lack of a connection to the M31“middle ages”merger is further supported by the similarities in stellar populations between the M31satellites and relatively isolated Cetus dSph,as well as the Galactic dSphs with old populations,such as the Draco or UMi dSphs.
The frequency of C stars in the M31dE companion NGC147from our data and the recent study by Nowotny et al.(2003),places it at levels the actively star forming Magellanic Clouds and Fornax or Leo I,Galactic dSphs where star formation continued to within～1Gyr of the present. While the M31dEs structurally resemble scaled up dSph systems,they have very di?erent star
formation histories than most of the M31dSphs.This serves to emphasize the profound di?erences in stellar population characteristics among the M31dSph satellites.The low luminosity dSphs are predominantly stellar fossils,while the dEs made many of their stars5-10Gyr in the past.These dE galaxies therefore may be associated with some of the more pronounced merger features in M31, as others have suggested on the basis of their structures and mean stellar metallicities(Ferguson et al.2002).The And VII dSph is neither a dE-like object nor a collection of primarily ancient stars, and instead resembles Galactic dSphs which experienced star formation for more than～5Gyr after their formation.
We also found that roughly0.3%of the stars in dSphs to be candidate CH stars,products of binary evolution.Future investigations of dC/CH fractions in globular clusters will allow to investigate the impact of a dense environment on binary evolution.
These observations re?ect the dedicated e?orts of the WIYN Observatory sta?,and we thank them for their support.DH gratefully acknowledges support as a McKinney postdoctoral fellow and from the Graduate School at the University of Wisconsin-Madison.JSG acknowledges essential funding from NSF grant AST-9803018to the University of Wisconsin and expresses his appreciation to Andrew Cole,Ariane Lan?c on,and Mustapha Mouhcine for discussions regarding the properties and importance of E-AGB stars.EKG and JSG also thank the Swiss National Science Foundation for partial support,and all three authors express their appreciation to the Max-Planck-Gesellschaft for supporting stimulating workshops on dwarf galaxies.This research has made use of NASA’s Astrophysics Data System(ADS)and the NASA/IPAC Extragalactic Database(NED)which is operated by the Jet Propulsion Laboratory,California Institute of Technology,under contract with the National Aeronautics and Space Administration.
REFERENCES
Aaronson,M.,Olszewski,E.W.,Hodge,P.W.1983,ApJ,267,271
Aaronson,M.,Mould,J.1985,ApJ,290,191
Aaronson,M.,Olszewski,E.,Gordon,G.,Mould,J.,&Suntze?,N.1985,ApJ,296,L7 Aaronson,M.,Cook,K.H.,Norris,J.1986,in Spectral evolution of galaxies,ASSL Vol.122 (Dordrecht,Reidel),p.171
Albert,L.,Demers,S.,Kunkel,W.E.2000,AJ,119,2780
Armandro?,T.E.,Da Costa,G.S.,Caldwell,N.,&Seitzer,P.1993,AJ,106,986
Armandro?,T.E.,Davies,J.E.,&Jacoby,G.H.1998,AJ,116,2287
Armandro?,T.E.,Jacoby,G.H.,&Davies,J.E.1999,AJ,118,1220
Battinelli,P.&Demers,S.2000,AJ,120,1801
Blanco,V.M.&McCarthy,M.F.1983,AJ,88,1442
Brewer,J.P.,Richer,H.B.,&Crabtree,D.R.1995,AJ,109,2480
Brown,T.M.et al.2003,ApJ,529,L17
Bullock,J.S.,Kravtsov,A.V.,Weinberg.D.H.2001,ApJ,548,33
Caldwell,N.1999,AJ,118,1230
Cappellari,M.,Bertola,F.,Burstein,D.,Buson,L.M.,Greggio,L.,&Renzini,A.1999,ApJ,515, L17
Caputo,F.,Cassisi,S.,Castellani,M.,Marconi,G.,Santolamazza,P.1997,AJ,117,2199 Carrera,R.,Aparicio,A.,Mart′inez-Delgado,D.,Alonso-Garc′ia,J.2002,AJ,123,3199
Cioni,M.-R.L.&Habing,H.J.2003,A&A,402,133
Cook,K.H.,Aaronson,M.,Norris,J.1986,ApJ,305,634
C?o t′e,P.,Hanes,D.A.,McLaughlin,D.E.,Bridges,T.J.,Hesser,J.E.,&Harris,G.L.H.1997, ApJ,476,L15
C?o t′e,P.,Oke,J.B.,&Cohen,J.G.1999,AJ,118,1645
Davidge,T.J.2000,PASP,112,
Davidge,T.J.2003,ApJ,597,289
Da Costa,G.S.,Armandro?,T.E.,Caldwell,N.,&Seitzer,P.2000,AJ,119,705
Da Costa,G.S.,Armandro?,T.E.,&Caldwell,N.2002,AJ,124,332
Demers,S.&Battinelli,P.2002,AJ,123,238
Demers,S.,Battinelli,P.,&Letarte,B.2003,AJ,125,3037
Da Costa,G.S.,Armandro?,T.E.,Caldwell,N.,&Seitzer,P.2000,AJ,119,705
Durrell,P.R.,Harris,W.E.,Pritchet,C.J.2001,AJ,121,2557
Ferguson,A.M.N.,Irwin,M.J.,Ibata,R.A.,Lewis,G.F.,Tanvir,N.R.2002,AJ,124,1452 Gallart,C.,Freedman,W.L.,Aparicio,A.,Bertelli,G.,&Chiosi,C.1999,AJ,118,2245 Grebel,E.K.1997,Reviews of Modern Astronomy,10,29
Grebel,E.K.1999,in The Stellar Content of the Local Group,IAU Symposium192,eds.P.
Whitelock&R.Cannon(San Francisco:ASP),17
Grebel,E.K.2000,in Star Formation from the Small to the Large Scale,ESA SP-445,eds.F.
Favata,A.A.Kaas,&A.Wilson(Noordwijk:ESA),87
Grebel,E.K.&Guhathakurta,P.1999,ApJ,511,L101
Grebel,E.K.&Stetson,P.B.1999,in The Stellar Content of the Local Group,IAU Symposium 192,eds.P.Whitelock&R.Cannon(San Francisco:ASP),165
Grebel,E.K.,Gallagher,J.S.,&Harbeck,D.2003,AJ,125,1926
Groenewegen,M.A.T.1999,in Asymptotic Giant Branch Stars,IAU Symp.191,eds.T.Le Bertre,
A.L′e bre,&C.Waelkens(San Francisco:ASP),535
Groenewegen,M.A.T.2002,in Chemical Evolution of Dwarf Galaxies,Ringberg Workshop,astro-ph/0208449
de Kool,M.&Green,P.J.1995,ApJ,449,236
Guhathakurta,P.,Reitzel,D.B.,&Grebel,E.K.2000,Proc.SPIE,4005,168
Hane,Z.,Eggleton,P.P.,Podsiadowski,P.,Tout,C.A.1995,MNRAS,277,1443
Han,M.,Hoessel,J.G.,Gallagher,J.S.,Holtzman,J.,Stetson,P.B.1997,AJ,113,1001 Harbeck,D.et al.2001,AJ,122,3092
Hurley-Keller,D.,Mateo,M.,&Grebel,E.K.1999,ApJ,523,L25
Ibata,R.A.,Gilmore,G.,&Irwin,M.J.1995,MNRAS,277,781
Ibata,R.A.,Wyse,R.F.G.,Gilmore,G.,Irwin,M.J.,&Suntze?,N.B.1997,AJ,113,634 Ibata,R.Irwin,M.,Lewis,G.,Ferguson,A.M.N.,Tanvir,N.2001,Nature,412,49 Karachentsev,I.D.&Karachentseva,V.E.1999,A&A,341,355
Karachentsev,I.D.,Sharina,M.E.,Dolphin,A.E.,&Grebel,E.K.2003,A&A,408,111
Lee,M.G.,Freedman,W.L.,&Madore,B.F.1993,AJ,106,964
Lee,M.G.,et al.2003,AJ,126,2840
Majewski,S.R.,Skrutskie,M.F.,Weinberg,M.D.,&Ostheimer,J.C.2003,ApJ,599,1082 Margon,B.et al.2002,AJ,124,1651
Mart′?nez-Delgado,D.,Aparicio,A.,&Gallart,C.1999,AJ,118,2229
Mayer,L.et al.2001,ApJ,547,L123
McClure,R.D.1985,JRASC,79,277
McClure,R.D.,Woodsworth,A.W.1990,ApJ,352,709
Monelli,M.et al.2003,AJ,126,218
Mouhcine,M.&Lan?c on,A.2003,MNRAS,338,572
Newberg,H.J.et al.2002,ApJ,569,245
Newberg,H.J.et al.2003,ApJ,596,L191
Nowotny,W.,Kerschbaum,F.,Olofsson,H.,&Schwarz,H.E.2003,A&A,403,93 Odenkirchen,M.et al.2001,AJ,122,2538
Palma,C.,Majewski,S.R.,Siegel,M.H.,Patterson,R.J.,Ostheimer,J.C.,&Link,R.2003,AJ, 125,1352
Pritchet,C.J.,Schade,D.,Richer,H.B.,Crabtree,D.,&Yee,H.K.C.1987,ApJ,323,79 Reid,N.&Mould,J.1984,ApJ,284,98
Reitzel,D.B.&Guhathakurta,P.2002,AJ,124,234
Richer,H.B.,Pritchet,C.J.,&Crabtree,D.R.1985,ApJ,298,240
Sarajedini,A.et al.2002,ApJ,567,915
Shetrone,M.D.,C?o t′e,P.,&Sargent,W.L.W.2001,ApJ,548,592
Stetson,P.B.,Hesser,J.E.,&Smecker-Hane,T.A.1998,PASP,110,533 Whitelock,P.,Menzies,J.,Irwin,M.,&Feast,M.1999,IAU Symposium,192,136 Whiting,A.B.,Hau,G.K.T.,&Irwin,M.1999,AJ,118,2767
Yanny,B.et al.2003,ApJ,588,824
harbeck
harbeck
harbeck f04.jpg
Fig. 3.—Color-magnitude diagram(CMD;left)and two-color diagram(right)of NGC147;all magnitudes are instrumental,but zeropoint corrected as described in the text.The two-color plot shows the broad-band colors of stars in NGC147(i.e.,a temperature)versus the relative CN absorption strength as measured by the CN-TiO?lter colors;only stars brighter than I=22mag are plotted(indicated by a line in the CMD,left).Red stars with strong CN absorption falling into the selection box are identi?ed as Carbon stars and are clearly marked with?lled circles in both plots.
推进智慧城市建设，是上海加快实现创新驱动、转型发展的重要手段，深化实践“城市，让生活更美好”的重要举措，也是上海信息化新一轮加速发展的必然要求。上世纪90年代以来，上海把信息化作为覆盖现代化建设全局的战略举措，经过三个五年规划的持续推进，当前整体水平保持国内领先，部分指标达到发达国家先进水平，一批新兴技术创新成果在上海世博会上得到充分展示和示范应用，这些都奠定了建设智慧城市的基础。为继续合力推进智慧城市建设，依据《上海市国民经济和社会发展第十二个五年规划纲要》，制订本行动计划。 一、指导思想、推进原则、发展目标和任务概要 （一）指导思想。 高举中国特色社会主义伟大旗帜，以邓小平理论和“三个代表”重要思想为指导，深入贯彻落实科学发展观，围绕上海加快推进“四个率先”、加快建设“四个中心”和社会主义现代化国际大都市的战略目标，按照创新驱动、转型发展的总体要求，大力实施信息化领先发展和带动战略，以提升网络宽带化和应用智能化水平为主线，着力构建国际水平的信息基础设施体系、便捷高效的信息感知和智能应用体系、创新活跃的新一代信息技术产业体系、可信可靠的区域信息安全保障体系，充分发挥市场机制和企业主体作用，注重政府引导，完善市场监管，大力推进以数字化、网络化、智能化为主要特征的面向未来的智慧城市建设，全面提高城市现代化水平，让市民共享智慧城市建设成果。 （二）推进原则。 1、夯实基础，分步推进。把提升信息基础设施能级和夯实智慧应用基础放在突出位置，加强统筹规划、规范管理，加大投入和建设力度；通过分阶段发展，滚动推进实施计划，促进智慧城市建设持续深入发展。 2、创新发展，惠及民生。着眼于促进经济发展方式转变和市民生活改善，大力推进技术、应用、管理及体制机制的创新发展，探索新模式，培育新业态，不断提高城市运行效率和公共服务水平，促进经济社会协调发展，使广大市民、企业切实感受到智慧城市建设带来的实惠和便捷。 3、突出重点，聚焦项目。围绕经济建设、城市运行、社会管理、公共服务重点领域，突出针对性、实效性、可操作性，聚焦公共性、基础性、创新示范性、业务协同性项目，强化阶段目标和建设进度，加快信息技术在城市发展各领域的深入应用。 4、市区联动，示范带动。市和区县两级政府统筹协调推进，支持区县先行先试，加快重点领域、重点区域、重点项目的示范建设，增强辐射和带动作用，促进设施完善、应用渗透和产业发展。
我的老板黄光裕：揭开黄光裕鲜为人知的一面 黄光裕是我曾经的老板，这几年他深陷囫囵。虽然我远在非洲，却一直对案件保持着高度关注。现在案件审判完毕，一切尘埃落定，上帝的回归上帝，撒旦的还于撒旦。然而印象中的黄光裕在这个失眠的黎明时刻，轻轻地回到我的脑海中，并逐渐变得清晰起来。 黄光裕是潮汕人，偶像是他的老乡李嘉诚，作为生意人，把企业做大是他的终极目的。黄光裕的悲剧在于他没有把握好自己的角色，他应该知道自己是谁，适合做什么，不应该做什么。 我是谁?—这是一个困纠每个人的哲学问题，尼采认为自己是太阳，结果他疯了;黄光裕不是尼采，而他进了监狱。 他沉默地观察，犹如一只黑暗中的猎豹 十年前一个春天的早晨，位于北京(楼盘)东北四环霄云路鹏润大厦28搂那个宽大的办公室，我惴惴不安的站在门外。那时候鹏润大厦刚刚竣工，招租率不到50%，黄光裕刚从电器连锁行业涉足商业地产。 过五关斩六将之后，24岁的我带着简历，惴惴不安地推开门。黄光裕的办公室非常豪华，足有两百多平米，铺着厚厚的地毯，踩上去感觉自己的腿发软。黄光裕坐在紫檀红木的巨大的办公桌后面，一言不发地看着我。他的背后是巨大的书架，但只是稀稀拉拉放着几个文件夹，书架上面是一块大匾额，据说是启功手书的四个遒劲的大字—商者无域! 他沉默地观察，犹如一只猎豹在黑暗中蛰伏，等待着扑向猎物最好时机的到来。这种观察人与事物的方式成为黄光裕的特色。他等待商机，在等待的过程中思考、分析、判断、论证，当时机成熟时就毫不犹豫地纵身一跃，并直冲要害。 那天我感觉自己就是这个猎物，我带着伪装出的自信，向他亦步亦趋地走去。 其实我心里非常清楚，我能得到鹏润(中国)投资培训部部长的职位，先前那些过五关斩六将的经历完全可以忽略，关键就在于这20分钟，在于这位老板的首肯。
战神的挑战2——图?流程攻略 【游戏封?】 游戏名称：P u z z l e Q u e s t2 中?名称：战神的挑战2 游戏发?：N a m c o N e t w o r k s A m e r i c a,I n c. 游戏制作：I n?n i t e I n t e r a c t i v e 游戏语种：英? 游戏类型：R P G??扮演 发??期：2010年8?13?
%{p a g e-b r e a k|游戏介绍|p a g e-b r e a k}% 野蛮?的技能表(括号中学得该技能所需的等级)： 连捶(1)：战场上有多少红宝?，则造成1/2数量的伤害值，需要4的红魔法。 部落的标记(2)：消掉战场上所有的红宝?，每4颗红宝?增加1点头?伤害奖励，该效果?直持续。 狂怒(3)：在战场上随机位置?成14颗红宝?。 部落的守护(4)：消掉战场上所有的绿宝?，没颗绿宝?增加2点防御，效果?直持续。 猛击(5)：减少敌?每种颜?的魔法值各10。 头?粉碎者(6)：消掉所有头?，敌?损失的回合数为1+1/5消掉的头?数。 野蛮咆哮(7)：敌?防御减少75%，持续3回合，本回合未结束。 破坏狂(8)：消掉所有的绿宝?，增加相等数量的红魔法。 反冲(10)：使?后该回合内通过武器攻击造成的伤害增加50%。 战争狂嚎(12)：随机位置增加3颗红?头?，如果当前红魔法值不少于25则本回合未结束。 最后的反击(15)：使?后每损失25点?命值增加1点头?伤害，该技能
践踏(20)：选择?颗宝?，消掉周边3*3区域的宝?并获得所有这些宝?的效果，对敌?造成8的伤害。 残暴(25)：在后6回合内使头?伤害加倍。 猎头者(30)：消掉最上2?的宝?，获得它们的效果。对敌?造成10的伤害。 嗜?(35)：接下来的6个回合，对敌?造成伤害值的25%转化为??的?命值。 毁灭者(40)：增加50点武器攻击点数，本回合未结束。 迷幻之怒(50)：选择?种宝?，战场上所有该颜?的宝?转变为头?，红魔法不少于25则本回合未结束。 战?的?些分析：消宝?增加该颜?魔法，六个?格为装备的武器，拳头形状表?武器攻击点数，消掉战场中的拳头增加该点数，满?武器使?需求后点击武器?格可以释放，图中我?3、3的数值分别标?了?前的头?伤害加成值和防御值，前者增加消掉头?后对敌?的伤害值，后者标?有该数值%的机会使任何敌?对我?造成的伤害减半。左下?为现在装备的五个技能，注意战?中只能装备五个所以需要在战?前在技能选项中先选择好最有利于战?的技能。 野蛮?战?的?些?得： 消4个或以上的宝?能奖励?个回合，单回合连续消掉?批宝?会有更多奖励(?如稀有武器)。 消宝?时注意看看消去后是否会给对?造成机会，如果没有什么好的
智慧城市指标体系 1.0 智慧城市是指综合利用各类信息技术和产品，以“数字化、智能化、网络化、互动化、协同化、融合化”为主要特征，通过对城市内人与物及其行为的全面感知和互联互通，大幅优化并提升城市运行的效率和效益，实现生活更加便捷、环境更加友好、资源更加节约的可持续发展的城市。智慧城市是新一轮信息技术变革和知识经济进一步发展的产物，是工业化、城市化与信息化深度融合的必然趋势。建设智慧城市，实现以“智慧”引领城市发展模式变革，将进一步促进信息技术在公共行政、社会管理、经济发展等领域的广泛应用和聚合发展，推动形成更为先进的区域发展理念和城市管理模式。 因此，在前期研究的基础上，特制定《智慧城市指标体系1.0 》（以下简称“指标体系”）。 一、相关说明 《智慧城市指标体系1.0 》主要是基于城市“智慧化”发展理念，统筹考虑城市信息化水平、综合竞争力、绿色低碳、人文科技等方面的因素综合而成，目的主要是为了较为准确的衡量和反映智慧城市建设的主要进度和发展水平，为进一步提升城市竞争力、促进经济社会转型发展提供有益参考。 相关指标的确定主要本着以下原则：一是指标具有可采集性，历史和当前数据采集是可靠方便和科学的；二是指标具有代表性，可较全面反映某个方面的总体发展水平；三是具有可比性，不同城市间、城市不同历史阶段可根据指标进行科学比较；四是指标具有可扩展性，可根据实际发展情况对指标体系内
容进行增减和修改。 二、指标体系 根据以上的原则以及现阶段智慧城市建设的主要内容，“指标体系”主要可分为智慧城市基础设施、智慧城市公共管理和服务、智慧城市信息服务经济发展、智慧城市人文科学素养、智慧城市市民主观感知等5 个维度，包括19 个二级指标、64 个三级指标。 1、智慧城市基础设施指保障智慧城市各项功能通畅、安全、协同运作的相关基础设施。主要包括3 个二级指标，8 个三级指标。 1.1宽带网络覆盖水平。指各类有线和无线形式的宽带网络在城市中的覆盖比例。包括4 个三级指标。 1.1.1家庭光纤可接入率。光纤接入是指局端与用户之间完全以光纤作 为传输媒体。光纤接入覆盖率是反映了城市基础网络设施发展水 平核心指标之一。智慧城市的家庭光纤可接入覆盖率应在99%以 上。 1.1.2无线网络覆盖率。指通过各种无线传输技术实现的无线网络连接 在城市区域的覆盖率。智慧城市的无线网络覆盖率应在95%以 上。 1.1.3主要公共场所WLAf覆盖率。指大专院校、交通枢纽、商业集中 区、公共活动中心等主要公共场所WLAf覆盖率。智慧城市主要 公共场所WLAr应达99%以上。 1.1.4下一代广播电视网（NGB覆盖率。指电信网、计算机网和有线电 视网融合发展、互通互联以及相关衍生业务的发展水平。智慧城
他们已不在江湖——黑帮教父陈启礼 他们已不在江湖——黑帮教父陈启礼 作者: 文晔 2008-04-10 14:38:00 在台湾“大选”前一星期，拥有四十万成员的大帮派洪门举办大游行，呼吁拒领公投票，并力挺马英九。这一讲究忠义的神秘组织，从来就不曾缺席过政治广场——它曾经的会员“洪棍”孙中山，就借洪门之力，一举发动辛亥革命。 政治与帮派从来莫相分离，它们是一体两面，有时甚至是共生结构。去年年底，台湾竹联帮精神领袖陈启礼客死他乡，他的世纪葬礼，万人空巷，让人又忆及当年那举世震惊的江南命案，那一场政治与帮派共谋的历史。 政治、帮派有组织，无信仰。那些可歌可泣的英雄悲歌，也许只有融化在神道之路上，方能找到归宿。 竹联帮领袖陈启礼举行公祭，陈启礼义兄弟是最大的公祭团体，在前帮主黄少岑（左三）的带领下，约有五百人参与。图陈易辰 生于外省官宦之家，形成刚烈豪爽性格，他把竹联帮带上国际舞台，成为“天下第一帮派”，却因效命
政治，制造举世震惊的江南命案而入狱、出逃，最终客死他乡。 他为黑帮赋予了政治人格，却又卷入政治纷争。他的一生，堪称另一部杜月笙传奇。 2007年11月8日，台北飘着绵绵细雨，邻近基隆河畔的大直商圈，弥漫着诡异的氛围，九千多位穿着黑衣的台湾、香港与日本的黑帮代表，八百位刑警人手一台摄影机严格搜证盘查，另有十多台卫星新闻转播车，全都涌入了竹联帮精神领袖陈启礼的公祭现场。 警方为避免帮派借此造势滋事，竟破天荒地在公祭前三天举行全台大扫荡黑道，仍无法遏止这一场黑社会的“世纪丧礼”。 “全台湾也只有陈启礼有这样的实力，公祭可以 动员到台港日的黑道老大。”一位主跑社会新闻的记 者感叹。公祭当天，台湾的九个新闻电视频道全都被陈启礼的新闻所占据，转到哪一台都是在报导陈启礼的生平与公祭，就连晚上最热门的九点谈话节目，也全都在谈陈启礼。 台湾最大的外省挂（指1949年前后从中国大陆来台湾 的民众）帮派竹联帮第一代帮主陈启礼，并非出身草莽，而是家教甚严的外省官宦家庭。 陈启礼在柬埔寨（图伍崇韬）
《战神3》图文流程攻略Chapter 11 -奥林匹亚要塞 跟随赫尔墨斯的脚步，抵达木桥上，桥会被迎空飞来的火球砸断，并且背后会不断燃烧，被火追上便会坠崖而亡，中途桥会更改一起方向，不用搭理摇杆向上推一路按×注意面前的平民会阻挡你的道路，用攻击键杀死他们而不是圆圈，跨上平台，平台上有许多平民，抓住处决可以回血，他们的生杀大权就掌握在你的手中。 一路上连跑带揍也没能追上神使，不过最终这个罗嗦的家伙还是被逼在一个锁头上，去左边触发剧情，不用被赫尔墨斯所干扰，掌握自己的节奏一路上利用跳跃点抵达安全区域，上面拼命、小恶魔、狗仔龙蛇混杂，推荐使用太阳神的头颅△蓄力镇住他们，然后L ?清理。
接着向前走，赫尔墨斯把正门关了没办法，我们只能绕远路了，从门左边的楼梯左右开工跃上房顶，发现点赫尔墨斯已经跑到很远的地方等奎托斯了，无奈ing到圆台下方右侧拉动摇杆，腾出缺口跳上平台，拉动巨型投石车，利用QTE跟随巨石抵达赫尔墨斯所在的雅典娜巨像上，酷毙了～ 跟随赫尔墨斯的血迹到达与赫尔墨斯决战的平台，这家伙的速度非常快，天天跑路可不是 盖的，也许一开始会适应不来，用L ?来攻击命中率会比较大，或者直接重攻击的收尾重击的伤害非常大看准时机可以给予赫尔墨斯很大的伤害，途中会有QTE对抗，无外乎是正转或者是反转半圈摇杆，几下重击周后赫尔墨斯被击倒在地，显然他累了，这家伙临死之前还唧唧歪歪拿斯巴达人的荣耀来说事。
已经没有力气的赫尔墨斯坐在地上任你鱼肉，按下圈就开始华丽的表演，非常非常的血腥……未成年人绝对禁止观看…以上以及以下的图片纯属欣赏，完事之后获得“赫尔墨斯之靴”这件物品可以让你跑得飞快。
2020-2021上海上海外国语大学附属浦东外国语学校小学数学小升初第一次模 拟试卷附答案 一、选择题 1．加工一批零件，经检验有100个合格，不合格的有25个，这批零件的合格率是（）A. 25% B. 75% C. 80% D. 100% 2．下面得数不相等的一组是（）。 A. B. C. D. 3．若一个四位数6□8△，既是2的倍数，又是3和5的倍数，则这个数最大是（）. A. 6980 B. 6880 C. 6780 4．比的前项扩大3倍，比的后项不变，比值（） . A. 扩大3倍 B. 缩小3倍 C. 不变 5．某市规定每户每月用水量不超过6吨时，每吨价格为2.5元；当用水量超过6吨时，超过的部分每吨价格为3元。下图中能正确表示每月水费与用水量关系的是（）。 A. B. C. D.
6．下列描述正确的是（） A. 在图上可以找到-5、20、3.5三个数对应的点。 B. 上图中，直线上的数不是正数就是负数。 C. 在0和3之间的数只有1和2． 7．从6：00到9：00，时针（）。 A. 逆时针旋转90° B. 顺时针旋转90° C. 逆时针旋转180° D. 顺时针旋转180° 8．把正方体的表面展开，可能得到的展开图是（）。 A. B. C. D. 9．双十一，某件商品降价20%，降价前能买100件该商品的钱，降价后能买该商品（）A. 80件 B. 100件 C. 120件 D. 125件10．长沙地铁1号线和地铁2号线总里程约为50千米，2019年5月随着地铁4号线的开通，长沙地铁总里程增加了67%，地铁4号线开通后，长沙地铁总里程约为（） A. 67千米 B. 117.1千米 C. 33.5千米 D. 83.5千米11．学校有一块正方形草坪，正好能容纳100个小朋友做广播操。这块草坪的面积大约是（）。 A. 150平方米 B. 1500平方分米 C. 1500平方米 12．笑笑在班级里进行了一项调查，并把调查结果制成如右图所示的统计图。笑笑可能进行的调查内容是（）。
精心整理 中国十大顶级黑社会帮派排行榜 导读：NO10、竹联邦：竹联帮，是台湾着名也是国际性知名有组织性的广域黑社会团体，以台湾台北为主要据点。主要活动在台湾中部以北，全岛自北至南以及中、美、欧、澳皆有其据点。主要核心成员约2万人，一般 多，各堆份亦各自为政，更经常因争夺利益内讧，自己人打自己人。由於不团结关系，该帮会不少地盘已被新兴的“和胜和”、“和合图”及“新义安”等黑帮侵吞。据了解，原来总部设於广州西关宝华路十四号的洪门洪发山人马於四九年到港后，成立“14K”字头，在香港开发多个分堂发展地盘，及
后更开枝散叶。根据警方资料显示，“14K”目前共有四十五个分堆，不过，大部分分堆已没有活动，现时仍然活跃的有“实”、“孝”、“毅”、“义”、“德”、“信”、“梅”、“湃庐”、“胜”、“健”、“同”及“大圈”等。现时“德”字堆活跃於湾仔、铜锣湾、尖沙嘴、油麻地、旺角、黄大仙、观塘、葵涌、荃湾、元朗及大屿山等。 “和 “合桃” 设了代表处。十几年来，东星集团致力于娱乐和军火业，培育了颇受欢迎的“东星五虎”、“摇头宝”、“洗浴一卡通”、“酒吧保险”等知名品牌。2004年8月，交通银行引入战略投资者——潮州帮，并在盗车业务、酒店管理、洗钱管理及人身安全管理等领域开展了全面合作。2005年6月23日，东星集团在纳斯达克成功上市，成为中国社团境外上市第一股。截止2005
年末，东星集团的员工总数超过14万，首次超过洪兴社。装备质量和员工充足率居行业领先水平。东星集团曾先后多次被国际黑帮组织评为“中国最佳社团”。2006年列世界500家社团综合排名第65位，董事长骆驼先生与洪兴蒋天养先生共同荣获《教父》2006年度“中国最佳大佬”称号。有传言说，东星大佬是霍**。 “5T 党” 流域，声势和影响都很大的一个秘密结社组织。在四川的哥老会被称为袍哥。哥老会在湘军中影响巨大，对清朝末年的**有着巨大的影响。 NO1、洪门：洪门现在虽然很少有人知道，历史有是甚为悠久。但是也是客观事实的存在。洪门最初的出现在清朝，当时还不叫洪门，当时叫天地会。后来天地会覆灭以后，天地会的残余分子组建洪门出现。有传闻
【首发】PSP战神Ω奥林匹斯之链图文流程攻略! https://www.doczj.com/doc/957086286.html,-自由自在游戏社区奉献 《战神Ω奥林匹斯之链》（God of War:Chains of Olympus）是以PS2上大畅销的《战神》（God of War）系列为题材的PSP原创新作，本作由 Ready at Dawn研发，充分发挥PSP所具备的 3D处理性能，呈现出不亚于PS2版壮阔的游 戏场景以及细腻角色。此外，在日前SCEA旗下 工作室Ready at Dawn高级制作人Eric Koch也 通过官方博客PlayStation Blog对外确认，自 2007年起就备受注目的PSP游戏《战神Ω奥 林匹斯之链》已经顺利宣告完工，游戏已经交厂 压碟准备上市，现在这款PSP超级大作将于2008 年3月4日在北美地区发售。 游戏承袭相同的故事背景与游戏类型，玩家将再 度扮演斯巴达战士奎托斯，继续施展“浑沌双刃” 等致命武器，面对全新的难关、敌人与奥林匹斯 诸神的试炼，体验与不同于本传的原创故事剧 情。游戏承袭PS2系列作的特色，在PSP上 重现了广受欢迎的电影运镜式精采游戏画面与 刺激的动作战斗系统，并加入全新的招式、关卡、 机关与怪物，以及以希腊神话为基础的全新剧 情。玩家将扮演斯巴达战士奎托斯，从人间的雅 典一直到冥王哈帝斯的冥府之门，一路朝向地狱 的深渊迈进，体验希腊神话中黑暗且残暴的世 界，并对抗各种传说中的怪物以及强大的头目角 色。 游戏名称：战神Ω奥林匹斯之链/战神Ω奥林帕斯之链 英文名称：God of War:Chains of Olympus 代理发行：SCEA/Ready At Dawn Studios LLC.游戏类型：ACT-Action Game（动作游戏） 制作厂商：SCEA/Ready At Dawn Studios LLC.对应主机：Play Station Portable（PSP） 语言版本：英文（美版）发行日期：2008年03月04日 载体容量：UMD×1参考价格：$:39.99美元 介绍网站点击进入
上海外国语大学附属外国语学校是上海市乃至全中国知名的重点中学学校，是众多学生和家长为之向往的理想教育机构。 在上海经济建设日益繁荣、发展，国际大都市地位日益凸显的今天，作为全市仅有被批准可招收外籍学生并设立国际部四所中学之一，如何为在沪工作的外籍人子女提供良好的教育环境，从创办一流的国际学校方面进一步优化投资软环境，已成为政府相关职能部门和教育界有识之士共同关注的问题。上海外国语大学附属外国语学校立足自身教育基础与办学特色，高瞻远瞩地提出了“为社会培养国际化人才”的国际部教育理念，正是从实践出发积极探索和总结国内学校进行国际化教育、办学的经验与思路。 为了更好地实现这一教育理念和办学目标，“拓展生源市场、扩大办学规模”就成为上海外国语大学附属外国语学校国际部面临的当务之急。本方案即是从这一前提基础出发，按照市场经济的原理，同时遵循“教育产业化”的指导思想，就上海外国语大学附属外国语学校国际部如何走向市场进行项目行销策划。
1、拓展目标生源市场，扩大招生、办学规模； 2、树立上海外国语大学附属外国语学校国际部的品牌知名度与 美誉度； 3、综合提升上海外国语大学附属外国语学校的品牌价值，培育 “国际学校”的新品牌形象基础。
三、市场分析 1、潜力巨大的市场需求，尤以港澳台侨学生为主 据教育部门有关统计，目前在沪就读的境外人士子女人数已达5000余人：其中港澳台侨胞学生为4200余名，外籍人士子女近1000人；在港澳台侨胞学生中，台胞子女人数最多，约占50%；然后依次为香港同胞子女、侨胞子女和澳门同胞子女，分别约占35%、10%与5%。 随着上海城市经济建设的持续高速增长，外来投资比重的继续不断扩大，有关部门预计在未来几年内，境外人士子女在沪就读人数仍将保持近30%的高速增长态势，这将是一股巨大的市场需求。 2、单一外国模式的市场供给和本地现行教育体制无法满足不同 学生的个性需求 据上海教委公布的资料显示，上海共有22所国际学校可以为外籍人士及港澳台侨胞子女提供从幼儿园、小学、初中至高中的正规教育，而其中一半以上为外国人开办的学校，以招收本国学生或英语母语的学生为主。而港澳台侨胞学生更希望能在中国接受到更多的中文教育，因此他们愿意选择优秀的上海本地学校就读。目前上海有100余所学校可以接受港澳台侨胞子女入学就读，但上海实行的“就近入学”政策使得许多港澳台侨胞学生实际上无法进入优质、重点学校的。此外，澳台侨胞对于上海入学收费“一刀切”、子女入学不能单独编班等问题都表示不能理解。 因此，上海外国语大学附属外国语学校国际部优势显而易见，它可以在政策允许的范围内为澳台侨胞子女提供更多的入学选择。
《战神的挑战2》图文流程攻略 事情还没有结束，在更深的地下有人知道Laurella母亲的情况，打开通往下面的门离开地下墓穴的世界我们进入了地精实验室。 这扇巨大的金门在其他3个地方上锁了，分别拉下这3个地方的闸门。
石器时代的食人魔，有铁头功技能：造成20伤害并震晕一回合，附加当前对方蓝魔法数值的伤害。
来自希腊神话故事的人身牛头怪守卫第一道闸门的开关，战斗时你的武器会被替换成一件“斗牛士的披风”(需要8行动点数)，它的作用是防止被神牛冲倒。神牛的冲刺技能：造成10的伤害并击倒对方5个回合。另一个技能Gore：造成5的伤害，如果对方处于击倒状态则附加25点的伤害。 [pagesplitxx][pagetitle][/pagetitle] 这只枭守卫着南方闸门的开关，没有什么特殊的能力。
西方闸门开关由著名的美杜莎驻守，除了石化技能之外，它的毒武器造成14*8(回合)的伤害并给自己增加10的防御。其他生命和防御都较低，不难对付。拉下第三个开关，任务更新：逃离地精实验室。
看起来暴乱已经激怒了堕落的精灵，精灵boss和它的两个手下以及一个巨大的钢铁侠一起出现在这里。一番嘘寒问暖之后站在最前面的精灵族战士手持双刀前来切磋，解决掉开胃菜之后，对上身后那位女性战法师。她有一个Mirror Shield技能：将对方的防御值全部吸到自己身上，持续10+1/8自身蓝魔法的回合，而她初始防御就有47，所以使用该技能后基本上防御值超过100，注意使用减防技能。另一个Dark Blast技能如果紫色魔法多的话伤害也会很高，而且只消耗3的红色魔法。
上海外国语大学秀洲外国语学校 全新的校舍，蜿蜒的长廊、错落的石桌、雅致的凉亭、宽阔的操场、葱茏的绿意……在秀洲区育英路，在静静流淌的运河之畔，在静谧的居民社区之间，一处洋溢着诗情画意的校园让人流连忘返。她就是刚刚落成的上海外国语大学秀洲外国语学校。2012年8月31日，她终于在无数人的殷殷期盼中掀起了“盖头”。学校布局合理，设计别致，环境幽雅，是一所十二年一贯制公办学校。 2010年12月18日，嘉兴市秀洲区人民政府与上海外国语大学合作办学签约仪式在秀洲区会展中心隆重举行，标志着上外秀洲外国语学校正式落户秀洲新区。2011年9月1日，上外秀洲外国语学校“寄居”秀洲实验小学举行开学典礼，4个初中班共127名学生成为首批入学者。2012年8月31日，位于秀洲新区二期的新校舍一期正式揭牌。2012学年共设小学3个班和初中10个班。外国语、小班化、国际化、活动化——这些都是上外秀洲外国语学校最引以为豪的教育特色。作为秀洲新区学校的典型代表，该校实施小班化管理模式、尝试开展多国语言选修课、沿袭上外传统校园社团文化等特色，给秀洲区的孩子和家长一个又一个惊喜。
领导关怀篇：精神家园 从学校筹办到2011年9月开学至今，无论是前期校舍的筹建工作、师资力量的调配还是招生，学校的每一步发展都得到了各级领导的关心和支持，这让上外秀洲人倍受鼓舞，同时也深感责任重大。 筹办初期，上海外国语大学附属外国语学校校长崔德明先生等一行人来到我区，在陈明根局长、朱小观科长及洪福珍校长等的陪同下对学校筹办工作进行交流。崔校长就自己在上外附中实践多年的教育理念，对大到学校浓郁文化特色的锻造，小到教师梯队的合理设置、小语种的开设都提出了中肯的意见，言语间对新生婴儿般的秀洲外国语学校充满了美好的展望。 2011年9月开学典礼上，张国平副区长，陈明根局长，山陈云副局长、俞春明主任、朱小观科长、王尧忠科长、凌水良科长、金关明馆长等学校筹备小组领导出席了学校的开学典礼，与首届师生、家长共同见证和分享了这场盛典。 不日，祝亚伟书记、胡建丰主任、张国平副区长、陈明根局长等领导再次来到学校，实地参观教学环境。祝书记表示，社会关注、青睐上海外国语大学秀洲外国语学校，因此必将举全区之力将上外秀洲这篇文章做好；并希望学校能把上外附中自身的文化和嘉兴当地的特色相融合，从而将秀洲教育提升到一个新的台阶。 2012年5月，全国外国语学校工作研究会秘书长邢三多先生来到上外秀洲，结合上外附中成功考入哈佛等名校学子的学习历程，给全体师生作了的精彩讲座。不难看出，邢老师希望上海外国语大学秀洲外国语学校的学生能和上外附中的孩子一样出色，一样成功，这是一份怎样的期待和厚望！ 2012年8月31日，来自上外大及上外附中的领导和嘉兴市、秀洲区的重要领导也参加学校举行盛大的揭牌仪式，见证了上外秀洲的又一次蜕变。 领导们对学校发展的细节如此关注，不能不让我们深受感动，全体上外秀洲人也必将以此为起点和动力，将每一步都走得更踏实、更精彩！
[专题]旧上海黑社会老大杜月笙的经典语录 1、当你超过别人一点点，别人会嫉妒你;当你超过别人一大截，别人就会羡慕你。 2、如果你喜欢热闹，很可能是因为你灵魂感到寂寞，需要用喧嚣来填补心灵世界;如果你喜欢孤独，很可能是因为你内心世界充实丰富，并且不需要旁人介入。 3、同学聚会时，混得特别差和混得特别好的人一般都不会参加。前者或许是因为不好意思，后者则是实在太忙。 4、你被别人嫉妒，说明你卓越;你嫉妒别人，说明你无能。 5、恭维你的人越来越多，不一定是他们喜欢恭维人，而是因为你喜欢被恭维。 6、十十榴社区上看来的:喝酒时，想巴结你的人和想你出丑的人会一直找你干杯。 7、真正了解你的人，除了你的朋友外，就是你的对手。所以，请重视对手，因为他们能最早发现你的过失;请感谢对手，因为他们能使你不断改进自己的工作。 8、不管你爬到多么高的位置，掌握多么大的权力，永远不要在故友面前摆架子，那是不尊重自己的表现。 9、不管你对抽烟喝酒的态度是赞成、反感还是无所谓，它们都是把现代人情感拉近的最快方式。 10、不论你如何了解一个人，那都是片面的，不是全部。 11、名声是个很奇怪的东西:你不花精力去追求它，它会找上门来;你拼命去追求它，它倒摆起架子来了。
12、如果一个人什么生活嗜好都没有，那么他往往也没有好朋友。 13、男人最怕女人问他爱不爱她，如果答得太快，她会说他草率;答得太慢，她又会说他不坚定。 14、如果上帝和魔鬼同时去追求一个美丽的少女，那么最终赢得少女芳心的很可能是魔鬼。 15、看完贴不回帖的人有两种:一种是自以为是抱着无所谓的态度走马观花的，另一种是整天忙忙碌碌却又一事无成的人～ 】【做自己命运的主人】智慧和聪明是两回事。自古至今，聪明的人非常多，但伟人却很少。智慧不是一种才能，而是一种人生觉悟，是一种开阔的胸怀和眼光。一个人在社会上也许成功，也许失败，如果他是智慧的，那么他就不会把这些看得过于很重要，而能够站在人世间 一切成败之上，成为自己命运的主人。 【23】别让自己活得太累。应该学着想开、看淡，学着不强求，学着深藏。别让自己活得太累。适时放松自己，寻找宣泄，给疲惫的心灵解解压。人之所以会烦恼，就是记性太好，记住了那些不该记住的东西。所以，记住快乐的事，忘记令你悲伤的事. 24】昨天再美好，终究压缩成今天的回忆;我们再无奈，也阻挡不了时间匆忙的步履;今天再精彩，也会拼凑成明天的历史;我们再执着，也拒绝不了岁月赋予的伤痕。我们想念昨天，因为它融解了一切美好的向往，流逝了所有倾情的追求。过去已经定格，就让它尘封吧，努力书写今天，让明天的怀念多一些亮色～【12】【处理人际关系的十五条法则】1、学会换位思考;2、学会适应环 境;3、学会大方;4、学会低调;5、嘴要甜;6、有礼貌;7、言多必失;8、学会感恩;9、遵守时间;10、信守诺言;11、学会忍耐;12、有一颗平常心;13、学会赞扬别人;14、待上以敬，待下以宽;15、经常检讨自己。
Arboreth 死亡腾蔓 第1列的骷髅头向右移7次 第7列的紫星向左移6次 第3列的红宝石向下移 第6列的绿宝石向下移 Arkliche 大巫妖 第3列的绿宝石向右移 第6列的绿宝石向左移 第2列的紫星向右移 第7列的紫星向左移 第2列的骷髅头向上移 第7列的骷髅头向上移 Catapult 攻城机 第2列的黄宝石向左移 第7列的绿宝石向右移 第4列的蓝宝石向右移 第4列的紫星向右移 第3、6列的闪光骷髅头向上移 Centaur 半人马 第3列的蓝宝石向右移 第6列的蓝宝石向左移 第2列的红宝石向右移 第7列的红宝石向左移 第4列的骷髅头向左移 第5列的骷髅头向右移 Dark Dwarf 黑暗矮子 第8列的绿宝石向上移 第6列最上方的骷髅头向右移 第3列最上方的绿宝石向右移 第1列的绿宝石向上移 第3列的红宝石向上移 第6列的绿宝石向左移 第4列的红宝石向上移 第6列的金币向下移 Doom Knight 末日骑士 第２、４、６、８行最上方的骷髅头向下移 第１（最上方）、３（最下方）、５（最下方）、７（最下方）行的骷髅头向下移第３、７行的骷髅头向上移
Dragon Spider 龙蜘蛛 第２列的骷髅头向右移 第７列的骷髅头向左移 第４列最上方的黄宝石向上移 第５列最上方的黄宝石向上移 第４列最下方的红宝石向左移 第５列的红宝石向右移 Elven Guard 精灵守卫 第２列最下方的黄宝石向右移 第７列最下方的黄宝石向左移 第２列最下方的绿宝石向右移 第２列的绿宝石向右移 第２列的骷髅头向左移 第７列最上方的绿宝石向下移 第７列的骷髅头向右移 Fire Elemental 火元素 第５列最上方的骷髅头向下移 第３列最上方的骷髅头向下移 第６列最上方的骷髅头向下移 Fire Giant 火巨人 第８列的金币向左移 第２列的闪光骷髅头向右移 第５列的骷髅头向下移 第１列的金币向右移 第５列的红宝石向右移 Flame Dragon 火焰龙 第２、４列最下方的骷髅头向左移 第２列的骷髅头向下移２次 第４列的黄宝石向左移 第４列最下方的红宝石向上移 第６、８列最下方的骷髅头向左移 第６列的骷髅头向下移 第８列的骷髅头向左移 第６列的骷髅头向下移 第８列的黄宝石向左移 Frost Dragon 霜龙 第３列上方第２个骷髅头向右移 第６列最上方的骷髅头向左移
上海外国语大学中外合作办学（联合培养项目）管理办法（试行） 为进一步推进我校国际化教育的发展，加强对外合作与交流，规范中外合作办学（联合培养项目）的管理，实现学校整体发展目标，根据国务院《中华人民共和国中外合作办学条例》（以下简称《条例》）、教育部《中华人民共和国中外合作办学条例实施办法》（以下简称《实施办法》）及上海市教委的相关规定，结合我校实际情况，特制定本办法。 第一章总则 第一条本办法所称中外合作办学，是指以上海外国语大学的名义，同外国具有相应的办学资格的教育机构在中国境内合作举办或合作开展的，以中国公民为主要招生对象的教育机构或项目，实施教育、教学的活动。中外合作办学包括设立“中外合作办学机构”和举办“中外合作办学项目”。 第二条中外合作办学是我国教育对外开放的重要组成部分，必须遵守我国的宪法和有关法律、法规，维护国家的教育主权。中外合作办学应坚持我国的教育方针，符合中国教育事业发展的需要和人才培养的要求，保证教育质量，不得以盈利为目的，不得损害国家和社会公共利益。 第三条中外合作办学的宗旨是引进国外优质教育资源，借鉴国外先进办学经验，调整优化学科、专业结构和人才培养模式，增加教育的多样性和选择性，促进教育改革，努力培养国际化创新型人才。 第四条与我校进行中外合作办学的外国教育机构在其所在国家的教育水平或科研地位应高于或者相当于我校在国内的教育水平或科研地位。引进国外优质资源应立足于提高学校的教育、教学质量，着重发展我国急需的新兴、幼稚学科以及空白学科，但不得举办实施军事、警察、政治等特殊性质教育的机构，或者与外国宗教组织、宗教机构、宗教院校和宗教教职人员在国内从事合作办学活动。中外合作办学机构和项目不得进行宗教教育和开展宗教活动。 第五条上海外国语大学是对外签署合作协议、开展国际交流与合作活动和合作办学的主体。作为学校法人代表，校长对外行使协议签字权。各院（系、所）是中外合作办学的具体承办单位，可由校长授权的代表与外国教育机构签订协议。各院（系、所）未经校长授权，无权对外签署法律文件。 第六条本办法所称联合培养项目，是指除教育部批准设立或举办的中外合作办学机构或项目之外的，以联合培养、互认学分的方式与外国教育机构开展学生交流的活动，如3＋1、2＋2、1＋1、本硕连读、硕博连读等，其校内立项、申报程序和管理方法参照本办法执行。
黑社会性质组织犯罪是近年来比较突出的犯罪之一，也是2001年4月开始“严打”整治斗争的重点。为了打击日益猖獗的黑社会性质组织犯罪，1997年修订后的刑法第二百九十四条为打击黑社会性质组织犯罪提供了法律依据。在此，笔者对实践中反映较为突出的几个问题提出一些探讨意见。 一、黑社会性质组织的特征。 依照最高人民法院《关干审理黑社会性质组织犯罪的案件具体应用法律若干问题的解释》（2000年12月4日最高人民法院审判委员会第1148次会议通过）（以下简称《解释》）第一条规定，笔者认为，黑社会性质组织不同于一般共同犯罪，也不同于普通刑事犯罪集团，有其自身的特征，主要表现在组织结构、经济实力、非法保护、行为方式四个方面： （一）组织结构。黑社会性质组织的组织结构比较紧密，人数较多，有比较明确的组织者、领导者，骨干成员基本固定，有较为严格的组织纪律。关于“人数较多”的下限标准，从司法实践看，一般掌握有10人左右； （二）经济实力。黑社会性质组织，大都通过违法犯罪活动或者其他手段获取经济利益，聚敛不义之财，具有一定的经济实力； （三）非法保护。黑社会性质组织经常通过贿赂、威胁等手段向国家机关渗透，引诱、逼迫国家工作人员参加黑社会性质组织活动，或者为其提供非法保护，或者直接向国家机关安插成员； （四）行为方式。黑社会性质组织往往在一定区域诸如一个城市、一个县、一个乡镇、一个村街，或者在一定行业诸如建筑业、运输业、手工业等范围内，以暴力、威胁、滋扰等手段，大肆进行敲诈勒索、欺行霸市、聚众斗殴、寻衅滋事、故意伤害等违法犯罪活动，称王称霸，欺压残害群众，严重破坏经济、社会生活秩序。 具备上述四个方面的特征，就可以认定为黑社会性质的组织。 二、黑社会性质组织的组织结构。 《解释》第三条规定，组织、领导、参加黑社会性质的组织又有其他犯罪行为的，根据刑法第二百九十四条第三款的规定，依照数罪并罚的规定处罚；对于黑社会性质组织的组织者、领导者，应当按照其所组织、领导的黑社会性质组织所犯的全部罪行处罚；对于黑社会性质组织的参加者，应当按照其所参与的犯罪处罚。对于参加黑社会性质的组织，没有实施其他违法犯罪活动的，或者受蒙蔽、胁迫参加黑社会性质的组织，情节轻微的，可以不作为犯罪处理。 依照该《解释》，在司法实践中，对于黑社会性质组织的组织者、领导者，应当按照其所组织、领导的黑社会性质组织所犯的全部罪行处罚；对于不同层次、不同等级的组织者、领导者，应当按其直接组织、领导的层次和等级的黑社会性质组织所犯的全部罪行处罚。黑社会性质组织犯罪的一个非常重要的特点是组织者、领导者往往不亲自实施犯罪，而是逐级下达命令由最底层的小头目和一般成员实施具体犯罪，以逃避打击。因此，《解释》作出这样
《战神3》图文流程攻略 听完奎爷讲述一下自己在战神1以及战神2之后，玩家跟随奎托斯坠入冥河，顺着河流游，途中会被怨灵吸去生命/魔法以及武器能力，不用挣扎，这是剧情需要，上岸之后失去神力的奎爷疲倦不堪，拖着疲惫的步伐向前走吧，向前不用走多远便可以触发剧情，宙斯的姐姐-智慧女神雅 典娜，并且给失去光芒的混沌双刃注入了新的能力，变成了“流亡双刃”，拿起它，踏上冥界的征途。 向右走，通过跳跃点到达对面远处的平台，不要忘了下方有重要物品-两个红魂箱子以及一个装有“美杜莎之眼”的宝箱，拿完之后就可以上去继续征途了，一路向前解决一波杂兵，适应一下实力大不如前的奎托斯，抵达第三个存档点，此时有两条路，左边一条是通往蕴有四个红魂箱子的平台，右边则是继续流程。
喜欢搞基的-冥王哈迪斯在和你对话了，你明白不明白他话中的话呢……几句话之后获得新魔法“斯巴达军团”(怎么来的?有点莫名其妙～)接下来出现的一些敌人是给你练魔法的;面前有“地狱藤蔓”暂时还开不了，通过右方的锁链一路到对面，途中会有一些杂兵干扰，从锁链上下来之后补充一下生命以及魔法，继续赶路，跳下低处，别忘了背后有两个红魂箱子，然后向前推开大门，首先是一大堆被折磨的灵魂再被美杜莎虐待，上前解决掉两只美杜莎后大门便会打开，往左继续流程。 [pagesplitxx][pagetitle][/pagetitle]
一路向前到达“受折磨的皮尔埃托斯”处，开始一个小解谜，以皮尔埃托斯头上的平台为跳板，进入到里面的房间将“易燃的荆棘”推到对面地狱犬牢笼处，再回头跳上皮尔埃托斯头前方的平台，然后到达“易燃的荆棘”上方飞上上方的平台，触发机关放出地狱犬，几下攻击之后，触发QTE，骑上地狱犬自由的奔驰吧，清理掉路上的杂兵，驾驭地狱犬靠近皮尔埃托斯喷火，让他脱离苦海，随后处决胯下的地狱犬，去获取“阿波罗之弓”。 (使用方法是：按住L2锁定敌人，右摇杆切换目标，?射箭，按住?可以蓄力，带有穿透效果，杀伤力很可观。) 用阿波罗之弓燃烧掉场景中部上方的藤蔓，然后将“易燃的荆棘”推到如上图所示的位置，站在上面即可飞进地图中上方场景内奖励一个红魂箱子以及一个“凤凰羽毛”(增加魔法最大值物品)
智慧城市 上海市智慧城市建设情况 上海智慧城市建设第一轮三年行动计划自2011年9月发布以来，在社会各界的共同努力下，到2013年底已全面完成各项目标任务，在工信部组织的中国信息化发展水平评估中，上海以综合指数111.02排名全国第一，在网络就绪度、信息通信技术应用等两个二级指数排名全国第一。 上海信息基础设施服务能级显著提升，截至2013年底，光纤到户覆盖总量约800万户，是2010年的6.7倍，实现城镇化地区覆盖；家庭光纤宽带入户率和平均带宽分别达42%和17M；完成535万有线电视用户NGB网络改造，比2010年底增长4倍，基本覆盖中心城区和郊区部分城镇化地区；基于TD-SCDMA、WCDMA、CDMA2000三种制式的3G网络全市域覆盖，用户普及率达48%；全面启动基于TD-LTE、FDD-LTE两种制式的4G网络建设；WLAN覆盖场所达2.2万处（AP16万个），是2010年的3倍，456处公共场所开通i-Shanghai免费服务。 涵盖各领域的智能应用进一步深化，着力推动数字惠民、智慧城管、两化融合和电子政务行动，初步实现智慧城市建设应用领域全覆盖。卫生信息化工程实现市区及医联等多平台互联互通，动态采集维护3000多万份健康档案；建立统一的食品安全投诉举报热线，办理时间从30天缩减到19天；在43个社区试点开展以生活服务、智能家居等为重点的“智慧社区”建设；网格化管理模式从城市建设向综合管理拓展，有效推动大联动、大联勤；公共交通综合信息服务渠道向移动网络拓展，ETC建设基本覆盖全市主要道口；两化融合指数从2011年的75.5提高到2013年的80.4；2013年电子商务交易额达到1.06万亿元，是2010年的1.6倍；推动政府数据资源向社会开放，开通国内首个“政府数据服务网”；网上行政审批平台在内资企业设立、建设工程等领域实现并联审批；“12345”市民服务热线、法人数字证书“一证通用”等渠道整合不断深化。 新一代信息技术产业竞争力不断增强，高端软件取得快速发展，在操作系统、数据库、中间件等方面形成完整产业链；实施“云海计划”，金融云、中小企业服务云等示范项目进展顺利；物联网在水质监测、智能消防、环境监测、公共安全和智能照明等方面试点应用。截至2013年底，上海信息产业总规模达到1.09
2018-2019学年上外附中初二第一学期期中考试 Ⅱ. Choice10% 16. Which of the following DOESN’T belong to the same category as the others? A. Snow White and the Seven Dwarfs B. The Red Shoes C. The Little Red Riding Hood D. The Crafty Fo 17. --- There’s no chocolate mil left in the fridge. You _________ it all. --- Oh, I didn’t. It _________ somewhere else. Let me find it. A. must have drun; may be B. must drin; must be C. can drin; might be D. may have drun; can be 18. It too them about one month to _________ how to start the equipment. A. search for B. figure out C. chec out D. loo for 19. Joseph is the student who always ass the teachers _________ questions before they go. Which of the following CAN’T be used in the sentence? A. a few B. some C. an amount of D. a couple of 20. --- Do you thin robots will tae the place of human beings in the far future? --- _________ Which is NOT the correct response? A. I hope not. B. I thin not. C. It’s possible, but I really doubt it. D. I’m afraid not. 21. Regular eercise can help people _________ pressure and fatigue (疲劳). A. let go off B. catch hold of C. let go of D. beware of 22. Which of the following is CORRECT? A. Lily was annoyed with herself for being careless again. B. Mum always told a bedtime story and sang me to asleep when I was small. C. Jane put up her best smile and raised to greet her customer. D. Fanny is not a guest. She is supposed not to be here. 23. He doubt _________ he had seen was true. A. if that B.that what C. how that D. whether what 24. It’s too late to invite Tim. _________, you now how he hates parties. A. Besides B. It’s even worse C. By the way D. In other words 25. The two officers were etremely lucy to _________ serious injury. A. gallop B. chase C. escape D. miss