a r X i v :a s t r o -p h /0511498v 1 16 N o v 2005
Draft version February 5,2008
Preprint typeset using L A T E X style emulateapj
Spectroscopy of GRB 050505at z =4.275:A log N (HI)=22.1DLA Host
Galaxy and the Nature of the Progenitor
E.Berger 1,2,3,B.E.Penprase 4,S.B.Cenko 5,S.R.Kulkarni 6,D.B.Fox 7,
C.C.Steidel 6,and N.A.Reddy 6
Draft version February 5,2008
ABSTRACT
We present the discovery of the optical afterglow of GRB 050505and an optical absorption spectrum obtained with the Keck I 10-m telescope.The spectrum exhibits three redshifted absorption systems with the highest,at z =4.2748,arising in the GRB host galaxy.The host absorption system is marked by a damped Ly α(DLA)feature with a neutral hydrogen column density of log N (HI)=22.05±0.10,higher than that of any QSO-DLA detected to date,but similar to several other recent measurements from GRB spectra.In addition,we detect absorption lines from both low-and high-ionization species from which we deduce a metallicity,Z ≈0.06Z ⊙,with a depletion pattern that is roughly similar to that of the Galactic warm halo,warm disk,or disk+halo.More importantly,we detect strong absorption
from Si II *indicating a dense environment,n H ～>102cm ?3
,in the vicinity of the burst,with a size of ～4pc.In addition,the C IV absorption system spans a velocity range of about 103km s ?1,which is not detected in any other absorption feature.We show that the most likely interpretation for this wide velocity range is absorption in the wind from the progenitor star.In this context,the lack of corresponding Si IV absorption indicates that the progenitor had a mass of ～<25M ⊙and a metallicity ～<0.1Z ⊙,and therefore required a binary companion to eject its hydrogen envelope prior to the GRB explosion.Finally,by extending the GRB-DLA sample to z ≈4.3we show that these objects appear to follow a similar metallicity-redshift relation as in QSO-DLAs,but with systematically higher metallicities.It remains to be seen whether this trend is simply due to the higher neutral hydrogen columns in GRB-DLAs,or if it is a manifestation of di?erent star formation properties in GRB-DLAs.Thus,GRBs hold the potential to probe all scales relevant to our understanding of the star formation process and its relation to metal production.
Subject headings:gamma-rays:bursts —ISM:abundances —ISM:kinematics —stars:mass loss —
stars:Wolf-Rayet
1.INTRODUCTION
The study of star formation and the associated pro-duction and enrichment of the interstellar medium (ISM)and intergalactic medium (IGM)by metals is focused on two observational approaches:large galaxy surveys based on rest-frame UV,optical,near-infrared and far-infrared emission,and the use of high redshift quasars as probes of the ISM/IGM.The former provides a view of the star for-mation activity from high redshift to the present,as well as the possible enrichment of the IGM through galactic-scale winds.In the context of quasar absorption studies the highest column density absorbers,the so-called damped Lyman alpha (DLA)systems (N (HI)≥2×1020cm ?2)are of particular interest.This is because of the similarity of their column densities to those in local luminous galax-ies,the fact that at these columns the hydrogen is mainly neutral and may form stars,and the conclusion that the
bulk of the neutral gas in the range z ～0?5is in DLAs (for a recent review see Wolfe et al.2005and references therein).
The connection between luminous star-forming galaxies and DLAs remains an open question.This is primarily due to observational limitations inherent in both approaches.First,surveys of star-forming galaxies at z ～>2are limited to relatively bright object,L ～>0.3L ?(e.g.,Steidel et al.2003).Furthermore,with the exception of the brightest galaxies,the continuum emission is typically too faint to observe absorption from interstellar gas and therefore to tie together the star formation and ISM properties.On the other hand,the use of quasar sight lines to probe the disks of high redshift galaxies is limited by a cross-section selec-tion e?ect to large impact parameters (～>10kpc).More-over,in the case of DLAs the small impact parameters severely limit the identi?cation of the DLA counterparts against the bright background quasar.Thus,while some
1Observatories of the Carnegie Institution of Washington,813Santa Barbara Street,Pasadena,CA 911012Princeton
University Observatory,Peyton Hall,Ivy Lane,Princeton,NJ 08544
3Hubble Fellow
4Pomona College Department of Physics and Astronomy,610N.College Avenue,Claremont,CA 5Space Radiation Laboratory,MS 220-47,California Institute of Technology,Pasadena,CA 91125
6Division of Physics,Mathematics and Astronomy,105-24,California Institute of Technology,Pasadena,CA 91125
7Department of Astronomy and Astrophysics,Pennsylvania State University,525Davey Laboratory,University Park,PA 16802
1
2
DLA counterparts have been identi?ed,primarily at z～<1 (e.g.,Chen&Lanzetta2003),a de?nitive association with star-forming systems or LBGs remains elusive.
Despite the observational challenges,the various galaxy surveys have provided evidence for near solar metallici-ties in at least some of the bright high redshift galaxies (Shapley et al.2004;Swinbank et al.2004).Typical star formation rates in the bright galaxies are in the range of ～10?102M⊙yr?1(Shapley et al.2001;F¨o rster Schreiber et al.2004;Swinbank et al.2004).On the other hand, DLAs appear to be metal poor,with a typical Z～0.03 Z⊙(Prochaska et al.2003),and while they exhibit evi-dence for star formation in a few cases,the rates typically appear to be lower than in the LBGs(Bunker et al.1999). An alternative approach to probing intervening gas in galaxies and the IGM is to use the afterglows of gamma-ray bursts(GRBs).In the context of the relation to star formation and the nature of DLAs,GRBs o?er several ad-vantages over quasar studies.First,GRBs are embedded in star forming galaxies with typical o?sets of a few kpc or less(Bloom et al.2002).They therefore not only pro-vide a direct link to star formation,but also probe the re-gions of most intense star formation,and hence production and dispersal of metals.Second,since the GRB afterglow emission fades away on a timescale of days to weeks,the host galaxy and any intervening DLAs can be subsequently studied directly(e.g.,Vreeswijk et al.2004).
Third,and perhaps most important,since GRBs are likely to be located in star forming regions(e.g.,molecular clouds)within their host galaxies,this approach provides the only systematic way to directly probe the small-scale environment and conditions of star formation at high red-shift;the probability of intersecting an individual molec-ular cloud in a quasar sight line is vanishingly small.In the same vein,GRBs can probe the circumstellar environ-ment of the progenitor star itself and provide a unique view of the mass loss history and properties of the progenitor (e.g.,metallicity,mass,binarity).With a large statistical sample,this is the only way to compare the properties of massive stars and individual star forming regions at high redshift to those in the Milky Way and the local universe. Over the past several years,a few absorption spectra of GRB afterglows have been obtained,revealing rela-tively large neutral hydrogen column densities(most in the DLA category;e.g.,Vreeswijk et al.2004).The metal-licity,inferred in only a few cases,appears to be sub-solar (Z～0.01?0.1Z⊙;Vreeswijk et al.2004;Chen et al.2005; Starling et al.2005a),but with a dust-to-gas ratio that is larger than that in QSO-DLAs(Savaglio et al.2003).In addition,some spectra reveal complex velocity structure, interpreted to arise from ordered galactic rotation(Castro et al.2003),and in one case appearing to arise in the com-plex wind environment of the progenitor star(e.g.,M¨o ller et al.2002).These results already suggest that GRBs probe environments that are likely missed in the quasar surveys.
With the advent of the Swift satellite,we can now start to utilize GRBs as probes of the high redshift universe in a systematic manner.Swift’s sensitivity and ability to rapidly and accurately localize a large number of GRBs has resulted in a redshift distribution spanning nearly uni-formly from z～0.5to～>6(Berger et al.2005;Jakobsson et al.2005b;Kawai et al.2005;Haislip et al.2005).This sample is therefore well-matched to the star formation his-tory of the universe,and over time will allow us to address the redshift evolution of star forming environments and perhaps individual massive stars.
Along these lines,we present here an absorption spec-trum of GRB050505,which reveals a DLA with a col-umn density log N(HI)=22.05±0.10at a redshift of z=4.2748.This system is currently the highest redshift GRB host for which detailed information is available.The spectrum probes not only the interstellar medium of the host galaxy,but also provides information on the local environment of the burst,likely including the wind of the progenitor star from which we are able to draw conclusions about the nature of the star that exploded.
2.OBSERVATIONS
GRB050505was detected by Swift on2005May5.974 UT.The duration and?uence of the burst are60s and (4.1±0.4)×10?6erg cm?2,respectively(Hullinger et al. 2005).Observations with the Swift X-ray telescope(XRT) started47min after the burst,and revealed an uncata-logued source atα=09h27m03.2s,δ=+30?16′21.5′′(J2000) with an uncertainty of about6′′and a?ux of～2×10?11 erg cm?2s?1(Kennea et al.2005).No object was de-tected by the Swift UV/optical telescope(UVOT)in the ?rst8hours to a limit of V>20.35mag and B>21.04 mag,at a mean time of2.49and2.59hr,respectively (Rosen et al.2005).
We initiated observations of GRB050505with the Low Resolution Imaging Spectrometer(LRIS)mounted on the Keck I10-m telescope about6.4hr after the burst.We obtained simultaneous g-and I-band observations and de-tected an object close to the center of the XRT error cir-cle atα=09h27m03.3s,δ=+30?16′23.7′′(J2000),with a brightness I=20.51±0.05mag and g=23.67±0.12mag (Figure1).The spectral slope between the two bands, Fν∝ν?4.9±0.3,is too sharp for host galaxy extinction, and instead suggests a redshift z～4?5.5.Contempora-neous observations with UKIRT revealed a near-IR coun-terpart with a brightness of K=18.1±0.2mag(Rol et al. 2005).
Following the identi?cation of the afterglow we used LRIS to obtain two900-s spectra with a1′′wide slit. The spectra were reduced using standard IRAF routines, while recti?cation and sky subtraction were performed us-ing the method of Kelson(2003).Wavelength calibra-tion was performed using HgArNeZnCd arc lamps and air-to-vacuum and heliocentric corrections were applied. The resulting dispersion scales are1.86?A/pix for the red side and0.61?A/pix for the blue side,with an rms wave-length uncertainty of about0.2?A.Finally,?ux calibra-tion was performed using the spectrophotometric standard BD+284211,with a correction for the small amount of Galactic extinction,E(B?V)=0.021mag(Schlegel et al. 1998).Convolution of the spectrum with the I?lter band-pass results in a?ux density of15.8±1.5μJy(20.5±0.1 mag),in very good agreement with the measured I-band
3 magnitude.This indicates that slit losses were minimal.
We identify three redshift systems in the extracted spec-
trum,z1=4.2748±0.0008,z2=2.2650±0.0008,and
z3=1.6948±0.0003.We associate the redshift system z1
with the host galaxy of GRB050505given the nature of the
absorption lines(see§3)and the lack of Lyαforest absorp-
tion redward of the damped Lyαfeature at the redshift z1.
At this redshift,using the standard cosmology(H0=71
km s?1Mpc?1,?m=0.27and?Λ=0.73),the isotropic-
equivalentγ-ray energy release is Eγ,iso≈8.9×1053erg,
while the X-ray luminosity extrapolated to t=10hr(as-
suming the typical Fν∝t?1.3)is L X,iso≈2.3×1046erg
s?1(Nousek et al.2005).Both values are at the high end
of the distribution for previous GRBs(Berger et al.2003;
Bloom et al.2003).
3.THE HOST GALAXY ABSORPTION SYSTEM
The spectrum of GRB050505is dominated by a broad
absorption feature centered on an observed wavelength of
about6400?A,which we identify as Lyα.A Voigt pro?le?t
to the Lyαabsorption feature results in a column density
of neutral hydrogen,log N(HI)=22.05±0.10,indicating
that the absorber is a DLA,with one of the highest column
densities measured to date in either QSO or GRB sight
lines(Curran et al.2002;Vreeswijk et al.2004).We note
that the actual column density may be somewhat higher
since,unlike in the case of quasars,the GRB is embedded
in the host galaxy(Vreeswijk et al.2004).The average
?ux decrement between Lyαand Lyβis about0.55,which
is in good agreement with the values measured in quasar
sight lines at the same redshift(Cristiani et al.1993).
Blueward of the damped Lyαfeature we detect absorp-
tion from the Lyαforest,likely mixed with metal absorp-
tion features of oxygen,silicon,nitrogen,sulfur,carbon,
and iron.Due to the low resolution of our spectrum we
cannot disentangle the contribution of the metals from the
forest.We also detect Lyβabsorption,and at a wavelength
of about4880?A we detect the Lyman limit.
Redward of the Lyαabsorption feature we detect a wide
range of metal lines.The identi?cations,observed wave-
lengths,and equivalent widths(EWs)of these lines are
listed in Table1.We note that in some cases these lines
are blended with absorption features from the lower red-
shift system at z2=2.265.Most of the lines detected in
the spectrum appear to be saturated.We can obtain a
lower limit on the column density assuming the optically
thin case
N=m e c2
fλ2
=1.13×1020cm?2
(Wλ/?A)
c
(2)
where the line center’s optical depth is given by
τ0=
π1/2e2fλN
(b/km s?1)
(3)
and the function
F(τ0)= ∞0[1?exp(?τ0e?x2)]d x.(4)
We assume that all species share the same value of the
Doppler parameter,b,and we?t iteratively for b and the
column density of each species(e.g.,Savaglio et al.2003).
The resulting best-?t COG is shown in Figure3,and the
column densities are listed in Table2.We?nd that lines
of C I and Ni II are well-described by the linear part of the
COG,lines of S II are mildly saturated,and most other
species lie on the?at portion of the COG.We stress that
given the assumption of a single b value,as well as the low
resolution of our spectrum,the derived column densities
of the strongly saturated lines should still be considered
as rough lower limits.
With this caveat in mind we derive the following abun-
dances from the COG analysis.The column density of
S II is log N≈16.1,leading to an abundance relative to
the solar value of[S/H]≈?1.2;here we use the compila-
tion of solar abundances of Asplund et al.(2005).Sulfur
is a non-refractory element and its gas-phase abundance
therefore closely matches the gas metallicity.The derived
value is roughly similar to those of both QSO-and GRB-
DLAs.The Fe II column density of log N≈15.5indi-
cates an abundance of[Fe/H]≈?2.0,which is similar to
the mean value for QSO-DLAs at a similar redshift range
(e.g.,Prochaska et al.2003).The ratio of sulfur to iron,
[S/Fe]≈0.8,however,is at the high end of values mea-
sured for QSO-DLAs,which at[Fe/H]≈?2.0range from
about0.1to1(Lopez&Ellison2003).Since iron is a
strongly depleted element,the large value of[S/Fe]sug-
gests a high dust content,similar to the inference made in
several other GRB-DLAs(Savaglio et al.2003;Savaglio&
Fall2004;Watson et al.2005).
Inspecting the abundances of other ions we?nd that
[Si/H]≈?1.6,when we sum the contributions of Si II and
Si IV.The ratio compared to iron is[Si/Fe]≈0.4,which
is in excellent agreement with the median value of about
0.4for QSO-DLAs(Wolfe et al.2005).
Using the abundances of sulfur,silicon,and iron we pro-
vide a comparison to the Milky Way depletion patterns in
Figure4.We consider the four typical patterns of warm
halo(WH),warm disk+halo(WDH),warm disk(WD),
and cool disk(CD)clouds(Savage&Sembach1996),and
follow the method of Savaglio et al.(2003)to determine
the metallicity and dust-to-gas ratio in each case.We?nd
that the?rst three depletion patterns provide an adequate
representation of the data with a metallicity Z≈0.06Z⊙
and dust-to-gas ratios of1.1(WH),0.95(WDH),and0.85
(WD).The cool disk depletion pattern does not provide
an adequate?t since it underestimates the silicon abun-
dance and over-estimates the iron abundance.Given the
inferred metallicities and dust-to-gas ratios we calculate a
rest-frame V-band extinction of about0.3±0.1mag.
4
3.1.A C IV Out?ow
The most prominent metal absorption feature in the spectrum of GRB050505,with a total rest-frame equiva-lent width of about11.6?A,is a blend of C IVλλ1548,1550. The overall velocity spread of this feature is about950km s?1,extending blueward of the systemic redshift of the host galaxy,as de?ned by other metal absorption features (Figure5).The wide velocity spread is not observed in any of the other low-or high-ionization features;for ex-ample the limit on blue-shifted Si IV is log N<13.5,at least a factor of thirty below the C IV column density.It is not clear from the low resolution spectrum if the veloc-ity structure is due to a set of discrete absorbers or to a relatively uniform distribution of C IV.
Regardless of this distinction,the observed velocity range is much larger than the typical values associated with the rotation or velocity dispersion of individual galax-ies,including those observed in past GRB absorption spec-tra(e.g.,GRB000926with v≈170km s?1;Castro et al.2003).Similarly,blueshifted absorption by inter-stellar low-and high-ionization gas has been detected in the stacked spectra of Lyman break galaxies(LBGs),but with a typical velocity shift relative to the nebular emis-sion lines of only～?150km s?1(Adelberger et al.2003). On the other hand,Frye et al.(2002)?nd evidence for out?ows in z～>4lensed galaxies which approach800km s?1,but these out?ows are evident in low-ionization lines of O I,Si II,and C II.In local bright starburst galax-ies out?ow velocities are typically～<300km s?1(Heck-man et al.2000).Therefore,unless the wind from the host galaxy of GRB050505is unusually fast,we consider this interpretation unlikely.This would particularly be the case if the host of GRB050505is similar to those of other GRBs,which tend to have relatively low masses(Chris-tensen et al.2004)and would therefore have escape veloc-ities much smaller than103km s?1.
The C IV absorption may be alternatively related to an extended large-scale structure along the line of sight. Adelberger et al.(2003)?nd a strong correlation between the location of C IV absorbers in quasar sight lines and the location of LBGs.In particular,for a C IV column density of>1014cm?2(as observed in the spectrum of GRB050505)about80%of the absorbers lie within600km s?1and?θ=35′′of an LBG.While this velocity range is similar to the one observed here,it has been argued that the actual out?ow velocities are～<400km s?1(Songaila 2005),and that the extent of the C IV bubbles may be a re?ection of pre-galactic enrichment at z～10by slower winds from dwarf galaxies(Porciani&Madau2005).Since here we directly detect an out?ow with v～103km s?1it is unlikely to be related to the C IV bubbles discussed in Adelberger et al.(2003)and Songaila(2005).
Another possibility in the context of an extended struc-ture is that the C IV absorption arises from an overlapping structure of galactic halos,perhaps stretched out along a dark matter?lament.This hypothesis is di?cult to assess with a single absorption spectrum.However,if such struc-tures are ubiquitous they should be observed in a large fraction of GRB absorption spectra,as well as in quasar absorption spectra.Studies of C IV systems in quasar spectra suggest that these systems are strongly clustered for velocity shifts of～<200km s?1and are essentially un-correlated for v～>500km s?1(Rauch et al.1996;Pichon et al.2003).Thus,we conclude that the observed C IV ve-locity structure is not due to a galactic-scale phenomenon. In the context of a massive star progenitor,an attrac-tive alternative is that the C IV velocity structure is the signature of a fast wind.A similar inference was made in the case of GRB021004,which exhibited a complex ve-locity structure extending from about140to3000km s?1 (M¨o ller et al.2002;Mirabal et al.2003;Schaefer et al. 2003;Fiore et al.2005;Starling et al.2005b).The pres-ence of such a fast out?ow led to the general conclusion that the progenitor was a Wolf-Rayet star.However,un-like in the case presented here,the velocity structure in the spectrum of GRB021004was evident in both low-and high-ionization lines,including H I.This raised the di?-culty of explaining the presence of both types of species in the highly-ionized burst environment,as well as the pres-ence of a large column of hydrogen in a Wolf-Rayet wind. While these di?culties prevented a de?nitive explana-tion of the high-velocity absorbers,two main possibilities have been discussed.Mirabal et al.(2003)argue that to reach the observed expansion velocities,radiative accelera-tion of the pre-existing fragmented shell nebula is required. In this model the interaction of the fast Wolf-Rayet wind with the slower winds of earlier mass loss episodes results in a fragmented structure due to Rayleigh-Taylor instabil-ities.The radiation pressure produced by the GRB and afterglow emission then accelerates the fragmented shell nebula to velocities of hundreds to thousands of km s?1. van Marle et al.(2005),on the other hand,produce hy-drodynamic numerical simulations of the interactions of various mass-loss phases(fast main sequence wind,slow red supergiant wind,and a fast wolf-Rayet wind),and conclude that these interactions lead to a clumpy struc-ture with a velocity range in excess of2000km s?1.The fragmented and clumpy structure of the wind is a common theme in both scenarios,and is used to explain the similar kinematic structure in both the low-and high-ionization lines.
In the case of GRB050505the velocity structure is only apparent in C IV,suggesting that a more uniform wind structure is allowed.Still,the e?ect of the ioniz-ing radiation of the GRB has to be taken into account. Since the recombination timescale is expected to be sig-ni?cantly longer than the lifetime of the GRB(unless the density is～>106cm?3;Perna&Loeb1998),we can estimate the size of the ionized region roughly as r～
5
Thus,the observations require a fast-moving(～103km s?1)wind,enriched in carbon and de?cient in silicon,and with a radius of at least a few parsec.These requirements can be naturally satis?ed in the case of a Wolf-Rayet wind for which typical velocities can easily exceed103km s?1 and extend out to a distance of～20pc(Abbott1978;van Marle et al.2005).
The lack of silicon absorption,with a column density that is at least a factor of thirty lower than that of C IV, provides interesting constraints on the nature of the pro-genitor.Calculations of theoretical pro?les of C IV and Si IV in the winds from a range of massive stars suggest that while strong C IV absorption is nearly always present, the presence of Si IV lines depends sensitively on a star’s mass and metallicity(Leitherer&Lamers1991).Thus, the wind from progenitors with a low mass and metallicity will have negligible Si IV absorption.For example,in the case of a wind from a25M⊙star at the end of core hydro-gen burning the ratio of Si IV to C IV matches the observed limit of EW(SiIV)/EW(CIV)<0.1for Z～<0.1Z⊙,while for a60M⊙star the theoretical ratio is～0.5even for Z=0.03Z⊙.These considerations indicate that the pro-genitor of GRB050505was most likely a carbon-rich(WC) Wolf-Rayet star with a relatively low mass(～<25M⊙)and metallicity(Z～<0.1Z⊙).
However,radiatively-driven winds follow a mass loss rate metallicity relation,˙M∝Z0.5?0.7(Maeder&Meynet 1988;Leitherer&Lamers1991)and therefore single stars reach the Wolf-Rayet phase at a higher mass when their metallicity is low;in the Galaxy M WR,min≈25M⊙,while in the SMC M WR,min≈45M⊙(Maeder1998;Maeder &Meynet2000).With a metallicity of～<0.1Z⊙and a mass of only～25M⊙,it appears that the progenitor of GRB050505was not su?ciently massive to have become a Wolf-Rayet star.It is therefore likely that the progenitor required a companion star in order to eject the hydrogen envelope.
3.2.Si II*
Another interesting feature of the spectrum of GRB050505is the detection of strong?ne-structure ab-sorption from Si II*.Since these transitions have not been convincingly detected in QSO-DLAs(e.g.,Howk et al. 2005)and since they are most likely excited by collisions with electrons(for T～<105K;Silva&Viegas2002),we conclude that the Si II*absorber is coincident with the local,high density environment of the GRB.In Figure6 we show the three detected Si II and Si II*transitions. We note that the Si IIλ1304and Si II*λ1309pair is lo-cated in the atmospheric B-band,therefore precluding a clear measurement of the equivalent widths.In addition, due to the low spectral resolution,the Si IIλ1260transi-tion is blended with S IIλ1259and Fe IIλ1260,although given the large oscillator strength of the Si II transition, it likely dominates the measured equivalent width.Our estimate of the column density is thus based primarily on Si IIλ1527and on Si II*λλ1264,1533(Figure6).
The absorption lines of both species are saturated and the ratio of column densities is therefore somewhat un-certain,although it is clear that the column of Si II*is fairly large;using the weakest,unblended line of Si II* under the assumption of the optically thin case we?nd log N(SiII?)≈14.7.This value is somewhat higher than those found in two previous GRB spectra:log N≈14.2 (GRB030323;Vreeswijk et al.2004)and log N≈14.3 (GRB020813;Savaglio&Fall2004),but the rough sim-ilarity may re?ect comparable physical conditions in the local environments of GRBs.
Using the COG analysis we?nd that the ratio of column densities is
N Si II?
1015.7
≈0.2.(5)
With this value,and using the calculations of Silva&Vie-gas(2002),we estimate that for a temperature of103K (i.e.,a neutral medium),the implied volume density of H I is n H I～102cm?3if the electron fraction is n e=0.1n H I. If the electron fraction is n e<10?4n H I,as may be ex-pected for a neutral medium in which the electrons pri-marily come from low-ionization species with an abun-dance relative to hydrogen of～10?4(Silva&Viegas 2002;Vreeswijk et al.2004),the density is n H I～104 cm?3.In this framework,the size of the absorbing region is?～1022.05/103～3.5pc assuming that the hydrogen is co-located with the Si II*absorber.The inferred mass of the absorbing region is M=m p N(H I)?2～103M⊙. Naturally,if only a fraction of the H I column is associ-ated with the Si II*absorber,then the derived mass and size are in fact upper limits.The inferred compact size of the absorber explains the non-detection of Si II*in the QSO-DLAs,since the probability of intersecting a region of only a few parsec in size is vanishingly small.
We note that there are two di?culties with this interpre-tation if we insist that the compact Si II*absorber has to be placed around the GRB.First,in order to survive the burst of ionizing radiation from the GRB(which a?ects the environment on a scale of～10pc)the Si II absorber has to be shielded.Second,as discussed in the previous section,the wind from the progenitor star appears to be de?cient in silicon,and another source for the Si II may be required.These arguments suggest that the Si II is located in the vicinity of the GRB,but is probably not directly associated with the progenitor star itself,and is instead a signature of the dense environment in the star forming region.
3.3.Limits on the H2Column Density Absorption lines of molecular hydrogen may be detected in the spectrum of GRB050505if the burst occurred in a dense molecular cloud.Unfortunately,at the low resolu-tion of our spectrum it is essentially impossible to discern H2absorption lines from the Lyαforest and transitions due to metals.We note that in general the molecular fraction in DLAs is～<10?4,and only a small number of DLAs exhibit detectable fractions of H2(Ledoux et al. 2003).The explanation for this trend is a combination of a low dust content and fairly intense far-UV radiation?eld, which combine to reduce the formation rate of H2and increase the photodissociation rate,respectively(Wolfe et al.2005).However,if GRBs tend to occur in molec-ular clouds,GRB-DLAs may exhibit preferentially higher
6
fractions of molecular hydrogen,particularly in light of the fairly large dust-to-gas ratios in comparison to QSO-DLAs (Savaglio et al.2003).
On the other hand,as discussed in detail by Draine& Hao(2002),the optical/UV radiation from the GRB itself is expected to photoionize and dissociate H2molecules to a distance of a few parsec.If the cloud hosting the GRB progenitor is smaller than this size,or if the burst is lo-cated near the edge of the cloud we expect that no H2 absorption features will be detected even if the molecular fraction was initially high.
If the cloud is su?ciently large,the UV radiation ?eld is expected to also excite H2into vibrational levels which will produce observable absorption features at rest-wavelengths of1110?1705?A(Draine&Hao2002).The strongest features are atλ=1254.8?A andλ=1277.3?A. While we detect an absorption feature coincident with the 1277.3?A line,we interpret this feature as C Iλ1277.2whose equivalent width is in good agreement with other C I lines. The non-detection of vibrational H2absorption,under the assumption that the cloud size is su?ciently large,places a limit of log N(H?2)～<18cm?2(Draine&Hao2002),and hence f(H2)～<10?4.
3.4.Limits on LyαEmission
We do not detect Lyαin emission with a3σlimit of F<2.1×10?17erg cm?2s?1.At the redshift of the burst this limit translates to an upper limit on the line luminosity of L<3.9×1042erg s?https://www.doczj.com/doc/7b10269280.html,ing the conversion of Kennicutt(1998)and assuming case B recombination, the limit on the star formation rate implied by the non-detection of Lyαemission is SFR=9.1×10?43L Lyα<3.5 M⊙yr?1.
The limit on the inferred star formation rate is about a factor of three higher than the value inferred for GRB030323at z=3.372(Vreeswijk et al.2004),but it is signi?cantly lower than the value measured for GRB021004,≈11M⊙yr?1,based on Lyαemission(e.g., Fynbo et al.2005).In fact,nearly every GRB host in which Lyαemission can be detected has been detected (Jakobsson et al.2005a),while the fraction of LBGs with Lyαequivalent widths similar to those in GRB hosts is only～1/3(Shapley et al.2003).
We note that the lack of Lyαemission may still accom-modate a star formation rate higher than our formal limit since the Lyαphotons are easily destroyed by resonant scattering in the presence of dust.Thus,even for a fairly low dust content it is possible that the star formation rate is in fact higher than the limit provided above.A bet-ter assessment of the star formation rate requires near-IR spectroscopy of the host galaxy for detection of Hαat3.46μm and/or[O II]λ3727at1.97μm.
4.INTERVENING SYSTEMS
We detect two intervening systems at z2=2.265and z3=1.695.The latter is detected only in Mg II with a rest-frame equivalent width of1.98?A(λ2796.35)and0.94?A (λ2803.53).These values match the expected2:1ratio in the optically thin case,suggesting that the lines are not saturated.The derived column density is about5×1013 cm?2.A comparison to the sample of Steidel&Sargent (1992)reveals that～10%of quasar sight lines reveal sys-tems with similarly large equivalent widths.However,un-like the observed doublet ratio of about two measured here, the range of doublet ratios for the quasar Mg II systems with EW～>2?A is typically1?1.3,indicative of strong sat-uration.We?nally note that for a magnesium abundance of about10%the solar value,the inferred column density in the z3system suggests an associated neutral hydrogen column density of log N(HI)～18.5cm?2.
The z2redshift system exhibits a wider range of ab-sorption features,but unfortunately,some of these lines are blended with features from the host galaxy.Still,sev-eral Fe II lines,as well as the Mg II doublet,and a sin-gle Mn II line are not blended,allowing us to estimate the column density of some metals in the z2system.A COG?t to the three Fe II lines indicates b≈60km s?1 and log N(FeII)≈15.0.The Mg II ratio of about0.85 indicates strong saturation,and a lower limit on the col-umn density of log N(MgII)≈14.6,assuming the same Doppler parameter as for the Fe II lines.Finally,assum-ing that the single Mn II line is optically thin we esti-mate log N(MnII)≈13.7.Thus,the relative abundance is[Fe/Mn]～>?0.7,while in DLAs it is typically～0. This suggests that we may be underestimating the Fe II by about0.7dex.
We also note that both iron and manganese are strongly depleted in the Galaxy,while elements such as zinc are rel-atively undepleted(Savage&Sembach1996).In our case, the Zn IIλ2062.66line is blended with C I from the host galaxy system.However,using the measured equivalent width as an upper limit and assuming the optically thin case,we?nd log N(ZnII)<13.4.Thus,[Mn/Zn]>?0.5 and[Fe/Zn]>?1.2are in agreement with the typical values measured for DLAs of about?0.5and?0.4,re-spectively,particularly if the abundance of Fe II is in fact underestimated as suggested above.
5.DISCUSSION AND CONCLUSIONS
The absorption spectrum of GRB050505exhibits a DLA with a column density of log N(HI)≈22.05associ-ated with the host galaxy.The measured column is higher than that of any QSO-DLA studied to date,but is similar to those measured for several GRB-DLAs,albeit at the highest redshift to date8.In Figure7we provide a sum-mary of the column densities measured from both quasars and GRBs to date.As already noted in Vreeswijk et al. (2004),these distributions di?er signi?cantly,presumably as a result of the smaller impact parameters in the case of GRB-DLAs and the possibility that they probe individual dense star forming regions.The metallicity we infer for GRB050505,Z≈0.06Z⊙,is within the range of values measured for QSO-DLAs at a similar redshift(Prochaska et al.2003),but is a factor of several higher than the mean metallicity of about0.01Z⊙.
This,along with the metallicities inferred for?ve addi-
8An absorption spectrum of GRB050904at z=6.29has been obtained by Kawai et al.(2005),but the column density and metallicity have not been published so far.
7
tional GRB-DLAs,is shown in Figure8.In the top panel we plot the metallicity as determined from various indica-tors as a function of redshift in comparison to QSO-DLAs. For the QSO sample,Prochaska et al.(2003)noted an ap-parent trend of increased metallicity with lower redshift.
A similar trend appears in the admittedly small GRB-DLA sample which spans from z≈2to4.3.However, it is also clear that the GRB-DLAs have systematically higher metallicities compared to QSO-DLAs.In the bot-tom panel of Figure8we plot the metallicity as a function of hydrogen column density.No clear trend is evident,per-haps suggesting that the higher metallicities in GRB-DLAs may not be simply a function of the column density,but may re?ect a di?erence in the star formation properties, rates,or history of GRB-selected host galaxies compared to QSO-DLAs.
We highlight two aspects of the spectrum,which provide insight into scales and conditions that are not typically probed in quasar sight lines:A C IV out?ow that is most likely associated with the wind of the progenitor star,and strong absorption from?ne-structure Si II*that is associ-ated with a dense region in the vicinity of the burst.The latter suggests that the GRB progenitor lived in an envi-ronment typical of a molecular cloud.The C IV out?ow,taken in association with the lack of corresponding Si IV absorption suggests that the progenitor star had a rela-tively low mass and metallicity,M～25M⊙and Z～<0.1 Z⊙.The combination of these properties suggests that the progenitor was part of a binary system,with the compan-ion responsible for stripping the hydrogen envelope.
The continued detection of high-velocity features in GRB absorption spectra may thus hold the only key to a detailed understanding of the distribution of progenitor properties(mass,metallicity,binarity),as well as the abil-ity to probe the properties of individual molecular clouds at high redshift.Coupled with information on the galac-tic scale properties of the ISM,GRBs can probe all the scales relevant to our understanding of the star formation process and its relation to metal production,as well as the relation between DLAs and star forming galaxies.
We thank Michael Rauch for helpful discussions and comments,and Allard-Jan van Marle for information on Wolf-Rayet winds.EB is supported is supported by NASA through Hubble Fellowship grant HST-01171.01awarded by the Space Telescope Science Institute,which is operated by AURA,Inc.,for NASA under contract NAS5-26555.
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10
Table1
Line Identification
λobs Line f ij z W0log N
(?A)(?A)(?A)(cm?2) Note.—Absorption features identi?ed in the spectrum of GRB050505.We do not include metal lines
blueward of the Lyαabsorption since at the low resolution of our spectrum these lines are blended with
Lyαforest features.The columns are(left to right):(i)Observed wavelength,(ii)line identi?cation,
(iii)oscillator strength(Prochaska et al.2003),(iv)redshift of the line,(v)rest-frame equivalent width,
and(vi)logarithm of the column density assuming the optically-thin case(Equation1);in most cases
this is a lower limit since the lines are genearlly saturated.In the case of blended features we derive
the column density by assuming that the total equivalent width is due to the highest redshift feature
(typically the host galaxy).a Absorption features are located in the atmospheric B band;b Absorption
features are located in the atmospheric A band.
11
Table2
Column Densities of Ions in z1
Ion log N[X/H]
(cm?3)
Note.—Ionic column densities and abun-
dances relative to the Solar values as de-
rived from the curve-of-growth analysis
(Figure3).These values are lower limits
in most cases given the low spectral resolu-
tion and the location of most lines on the
?at portion of the COG.Thus,the metallic-
ity as inferred from the sulfur abundance is
>0.06Z⊙.
～
12
Fig.1.—Discovery image of the optical afterglow of GRB050505obtained with LRIS on the Keck I10-m telescope.The inset is a combined g+I?ux-calibrated color image clearly showing the red color of the afterglow which is due to the damped Lyαabsorption,the Lyαforest,and the Lyman limit absorption atλ～<4900?A(see Figure2).
Fig.
are given in§2.Metal absorption features from all three systems are shown,including lines that are blends from both z1 and z2.We note that absorption features blueward of the damped Lyman alpha feature are strongly blended with the Lyman alpha forest at the resolution of our spectrum and their position is shown only for completeness.The inset shows a zoom-in of the Lyman alpha absorption.The solid line is the best?t with log N(HI)=22.05,and the dashed lines
designate the1σuncertainty of0.1dex.
14
Fig. 3.—Curve of growth(COG)for the host galaxy system of GRB050505.We constructed the COG by iteratively ?tting for the column densities of individual ions and the Doppler parameter,b,which we assumed to have a single value. Transitions in the linear part of the COG lead to well-determined columns(modulo the low resolution of our spectrum). Transitions on the?at portion of the COG are sensitive to the value of b and should be considered as lower limits.
15
Fig. 4.—Depletion pattern for the host galaxy of GRB050505using the inferred columns of sulfur,silicon,and iron relative to hydrogen.The lines represent the depletion patterns expected for various phases of the interstellar medium based on observations in the Milky Way(Savage&Sembach1996),with the dust-to-gas(κ)and metallicity left as free parameters.We?nd that a cool disk interpretation is unlikely.
?1, z1B3). This scenario provides an adequate?t to the data,and indicates that the velocity structure is most likely due to a fast
wind from the progenitor star.
17
Fig.the ratio in the
18
Fig.7.—Fractional distribution of neutral hydrogen column densities from quasar(Curran et al.2002)and GRB observations(Jakobsson et al.2004;Vreeswijk et al.2004;Chen et al.2005;Prochaska et al.2005b,a;Starling et al.2005a; Vreeswijk et al.2005;Watson et al.2005).The GRB-DLAs exhibit higher column densities with about a third exceeding the values measured in any QSO-DLA.
19
Fig.(black; Savaglio et al. 2005);The trend of increased metallicity with lower redshift,noted for QSO-DLAs by Prochaska et al.(2003),is also apparent in the GRB-DLA sample,albeit at an overall higher metallicity.This suggests that GRBs select more metal-enriched systems, but it is not clear at the present if this is related to the higher column densities.
中文颜色名称颜色对照表 鸨色#f7acbc 赤白橡 #deab8a 油色 #817936 绀桔梗 #444693 踯躅色#ef5b9c 肌色 #fedcbd 伽罗色 #7f7522 花色 #2b4490 桜色#feeeed 橙色 #f47920 青丹 #80752c 瑠璃色 #2a5caa 蔷薇色#f05b72 灰茶 #905a3d 莺色 #87843b 琉璃绀 #224b8f 韩红#f15b6c 茶色 #8f4b2e 利久色 #726930 绀色 #003a6c 珊瑚色#f8aba6 桦茶色 #87481f 媚茶 #454926 青蓝 #102b6a 红梅色#f69c9f 枯茶 #5f3c23 蓝海松茶 #2e3a1f 杜若色 #426ab3 桃色#f58f98 焦茶 #6b473c 青钝 #4d4f36 胜色 #46485f 薄柿#ca8687 柑子色 #faa755 抹茶色 #b7ba6b 群青色 #4e72b8 薄红梅#f391a9 杏色 #fab27b 黄绿 #b2d235 铁绀 #181d4b
曙色#bd6758 蜜柑色 #f58220 苔色 #5c7a29 蓝铁 #1a2933 红色#d71345 褐色 #843900 若草色 #bed742 青褐 #121a2a 赤丹#d64f44 路考茶 #905d1d 若绿 #7fb80e 褐返 #0c212b 红赤#d93a49 饴色 #8a5d19 萌黄 #a3cf62 藤纳戸 #6a6da9 胭脂色#b3424a 丁子色 #8c531b 苗色 #769149 桔梗色 #585eaa 真赭#c76968 丁子茶 #826858 草色 #6d8346 绀蓝 #494e8f 今様色#bb505d 黄栌 #64492b 柳色 #78a355 藤色 #afb4db 梅染#987165 土器色 #ae6642 若草色 #abc88b 藤紫 #9b95c9 退红色#ac6767 黄枯茶 #56452d 松叶色 #74905d 青紫 #6950a1 苏芳#973c3f 狐色 #96582a 白绿 #cde6c7 堇色 #6f60aa 茜色#b22c46 黄橡 #705628 薄绿 #1d953f 鸠羽色 #867892
感官动词和使役动词 默认分类2010-05-28 23:14:26 阅读46 评论0 字号：大中小订阅 使役动词，比如let make have就是3个比较重要的 have sb to do 没有这个用法的 只有have sb doing.听凭某人做某事 have sb do 让某人做某事 have sth done 让某事被完成（就是让别人做） 另外： 使役动词 1.使役动词是表示使、令、让、帮、叫等意义的不完全及物动词,主要有make(使,令), let(让), help(帮助), have(叫)等。 2.使役动词后接受词,再接原形不定词作受词补语。 He made me laugh. 他使我发笑。 I let him go. 我让他走开。 I helped him repair the car. 我帮他修理汽车。 Please have him come here. 请叫他到这里来。 3.使役动词还可以接过去分词作受词补语。 I have my hair cut every month. 我每个月理发。 4.使役动词的被动语态的受词补语用不定词,不用原形不定词。 (主)He made me laugh. 他使我笑了。 (被)I was made to laugh by him. 我被他逗笑了。 使役动词有以下用法： a. have somebody do sth让某人去做某事 ??i had him arrange for a car. b. have somebody doing sth.让某人持续做某事。 ??he had us laughing all through lunch. 注意：用于否定名时，表示“允许” i won't have you running around in the house. 我不允许你在家里到处乱跑。 ******** 小议“使役动词”的用法 1. have sb do 让某人干某事 e.g:What would you have me do? have sb/sth doing 让某人或某事处于某种状态，听任 e.g: I won't have women working in our company. The two cheats had the light burning all night long. have sth done 让别人干某事，遭受到 e.g:you 'd better have your teeth pulled out. He had his pocket picked. notes: "done"这个动作不是主语发出来的。 2.make sb do sth 让某人干某事 e.g:They made me repeat the story. What makes the grass grow?
#FF8C00#FF83FA#FF82AB#FF8247 #FF7F50#FF7F24#FF7F00#FF7256 #FF6EB4#FF6A6A#FF69B4#FF6347 建议收藏下载本文，以便随时学习！ #FF4500#FF4040#FF3E96#FF34B3 #FF3030#FF1493#FF00FF#FF0000 #FDF5E6#FCFCFC#FAFAFA#FAFAD2 #FAF0E6#FAEBD7#FA8072#F8F8FF #F7F7F7#F5FFFA#F5F5F5#F5F5DC #F5DEB3#F4F4F4#F4A460#F2F2F2 #F0FFFF#F0FFF0#F0F8FF#F0F0F0 #F0E68C#F08080#EEEEE0#EEEED1 #EEEE00#EEE9E9#EEE9BF#EEE8CD #EEE8AA#EEE685#EEE5DE#EEE0E5 #EEDFCC#EEDC82#EED8AE#EED5D2 #EED5B7#EED2EE#EECFA1#EECBAD #EEC900#EEC591#EEB4B4#EEB422 #EEAEEE#EEAD0E#EEA9B8#EEA2AD #EE9A49#EE9A00#EE9572#EE82EE #EE8262#EE7AE9#EE799F#EE7942 #EE7621#EE7600#EE6AA7#EE6A50 #EE6363#EE5C42#EE4000#EE3B3B #EE3A8C#EE30A7#EE2C2C#EE1289 #EE00EE#EE0000#EDEDED#EBEBEB #EAEAEA#E9967A#E8E8E8#E6E6FA #E5E5E5#E3E3E3#E0FFFF#E0EEEE #E0EEE0#E0E0E0#E066FF#DEDEDE #DEB887#DDA0DD#DCDCDC#DC143C #DBDBDB#DB7093#DAA520#DA70D6 #D9D9D9#D8BFD8#D6D6D6#D4D4D4
感官动词 1.see, hear, listen to, watch, notice等词，后接宾语，再接省略to的动词不定式或ing形式。前者表全过程，后者表正在进行。句中有频率词时，以上的词也常跟动词原形。 注释:省略to的动词不定式--to do是动词不定式，省略了to,剩下do，其形式和动词原形是一样的，但说法不同。 see sb do sth 看到某人做了某事 see sb doing sth 看到某人在做某事 hear sb do sth 听到某人做了某事 hear sb doing sth 听到某人在做某事 以此类推... I heard someone knocking at the door when I fell asleep. (我入睡时有人正敲门,强调当时正在敲门) I heard someone knock at the door three times. (听到有人敲门的全过程) I often watch my classmates play volleyball after school. (此处有频率词often) （了解）若以上词用于被动语态，须将省略的to还原： see sb do sth----sb be seen to do sth hear sb do sth----sb be seen to do sth 以此类推... We saw him go into the restaurant. → He was seen to go into the restaurant. I hear the boy cry every day. → The boy is heard to cry every day. 2.感官动词look, sound, smell, taste, feel可当系动词，后接形容词。 He looks angry. His explanation sounds reasonable. The cakes smell nice.
英语中感官动词的用法 一、感官动词 1、感官动词(及物动词)有：see/notice/look at/watch/observe/listen to/hear/feel(Vt)/taste(Vt)/smell(Vt) 2、连缀动词(含感官不及物动词) be/get/become/feel/look/sound/smell/taste/keep/stay/seem/ appear/grow/turn/prove/remain/go/run 二、具体用法： 1、see, hear, smell, taste, feel,这五个动词均可作连系动词，后面接形容词作表语，说明主语所处的状态。其意思分别为"看/听/闻/尝/摸起来……"。除look之外，其它几个动词的主语往往是物，而不是人。 例如：These flowers smell very sweet.这些花闻起来很香。 The tomatoes feel very soft.这些西红柿摸起来很软。 2、这些动词后面也可接介词like短语，like后面常用名词。 例如：Her idea sounds like fun.她的主意听起来很有趣。 3、这五个感官动词也可作实义动词,除look(当"看起来……"讲时)只能作不及物动词外,其余四个既可作及物动词也可作不及物动词,此时作为实义动词讲时其主语一般为人。 例如:She smelt the meat.她闻了闻那块肉。 I felt in my pocket for cigarettes.我用手在口袋里摸香烟。 4、taste, smell作不及物动词时,可用于"t aste / smell + of +名词"结构,意为"有……味道/气味"。 例如:The air in the room smells of earth.房间里的空气有股泥土味。 5、它们(sound除外)可以直接作名词,与have或take构成短语。 例如：May I have a taste of the mooncakes?我可以尝一口这月饼吗？taste有品位、味道的意思。 例如：I don’t like the taste of the garlic.我不喜欢大蒜的味道。 She dresses in poor taste.她穿着没有品位。 look有外观，特色的意思，例：The place has a European look.此地具有欧洲特色。 feel有感觉，感受的意思，watch有手表，观察的意思。例：My watch is expensive.我的手表很贵。 6、其中look, sound, feel还能构成"look / sound / feel + as if +从句"结构，意为"看起来/听起来/感觉好像……"。 例如：It looks as if our class is going to win.看来我们班好像要获胜了。 7、感官动词+do与+doing的区别： see, watch, observe, notice, look at, hear, listen to, smell, taste, feel + do表示动作的完整性，真实性；+doing 表示动作的连续性，进行性。 I saw him work in the garden yesterday.昨天我看见他在花园里干活了。(强调"我看见了"
颜色RGB对照表（颜色大全） ■RGB(255,192,203) ■★●◆pink（粉红） ■RGB(220,20,60) ■★●◆crimson（腥红） ■RGB(255,240,245) ■★●◆lavenderblush（苍白的紫罗兰红） ■RGB(219,112,147) ■★●◆palevioletred（脸红的淡紫红） ■RGB(255,105,180) ■★●◆hotpink（热情的粉红） ■RGB(199,21,133) ■★●◆mediumvioletred（适中的紫罗兰红） ■RGB(218,112,214) ■★●◆orchid（兰花紫） ■RGB(216,191,216) ■★●◆thistle（苍紫） ■RGB(221,160,221) ■★●◆plum（轻紫） ■RGB(238,130,238) ■★●◆violet（紫罗兰） ■RGB(255,0,255) ■★●◆magenta（洋紫) ■RGB(255,0,255) ■★●◆fuchsia（紫红） ■RGB(139,0,139) ■★●◆darkmagenta（深洋紫） ■RGB(128,0,128) ■★●◆purple（紫） ■RGB(186,85,211) ■★●◆mediumorchid（适中的兰花紫） ■RGB(148,0,211) ■★●◆darkviolet（深紫罗兰） ■RGB(75,0,130) ■★●◆indigo（靓青） ■RGB(138,43,226) ■★●◆blueviolet（蓝紫罗兰） ■RGB(147,112,219) ■★●◆mediumpurple（适中的紫） ■RGB(123,104,238) ■★●◆mediumslateblue（适中的的板岩蓝） ■RGB(106,90,205) ■★●◆slateblue（板岩蓝） ■RGB(72,61,139) ■★●◆darkslateblue（深板岩蓝） ■RGB(230,230,250) ■★●◆lavender（熏衣草花的淡紫） ■RGB(248,248,255) ■★●◆ghostwhite（幽灵白） ■RGB(0,0,255) ■★●◆blue（蓝） ■RGB(0,0,205) ■★●◆mediumblue（适中的蓝） ■RGB(25,25,112) ■★●◆midnightblue（午夜蓝） ■RGB(0,0,139) ■★●◆darkblue（深蓝） ■RGB(0,0,128) ■★●◆navy（海军蓝） ■RGB(65,105,225) ■★●◆royalblue（皇家蓝） ■RGB(100,149,237) ■★●◆cornflowerblue（矢车菊蓝） ■RGB(176,196,222) ■★●◆lightsteelblue（淡钢蓝） ■RGB(119,136,153) ■★●◆lightslategray（浅石板灰） ■RGB(112,128,144) ■★●◆slategray（石板灰） ■RGB(30,144,255) ■★●◆dodgerblue（道奇蓝） ■RGB(240,248,255) ■★●◆aliceblue（爱丽丝蓝） ■RGB(70,130,180) ■★●◆steelblue（钢蓝） ■RGB(135,206,250) ■★●◆lightskyblue（淡天蓝） ■RGB(135,206,235) ■★●◆skyblue（天蓝） ■RGB(0,191,255) ■★●◆deepskyblue（深天蓝） ■RGB(173,216,230) ■★●◆lightblue（淡蓝） ■RGB(176,224,230) ■★●◆powderblue（火药蓝）
颜色代码大全 AA 指定透明度。 00 是完全透明。 FF 是完全不透明。超出取值范围的值将被恢复为默 认值。 ffff00 ffff33 ffff66 ffff99 ffffcc ffffff ffcc00 ffcc33 ffcc66 ffcc99 ffcccc ffccff ff9900 ff9933 ff9966 ff9999 ff99cc ff99ff ff6600 ff6633 ff6666 ff6699 ff66cc ff66ff ff3300 ff3333 ff3366 ff3399 ff33cc ff33ff ff0000 ff0033 ff0066 ff0099 ff00cc ff00ff ccff00 ccff33 ccff66 ccff99 ccffcc ccffff cccc00 cccc33 cccc66 cccc99 cccccc ccccff cc9900 cc9933 cc9966 cc9999 cc99cc cc99ff cc6600 cc6633 cc6666 cc6699 cc66cc cc66ff cc3300 cc3333 cc3366 cc3399 cc33cc cc33ff cc0000 cc0033 cc0066 cc0099 cc00cc cc00ff 99ff00 99ff33 99ff66 99ff99 99ffcc 99ffff 99cc00 99cc33 99cc66 99cc99 99cccc 99ccff 999900 999933 999966 999999 9999cc 9999ff 996600 996633 996666 996699 9966cc 9966ff 993300 993333 993366 993399 9933cc 9933ff 990000 990033 990066 990099 9900cc 9900ff 66ff00 66ff33 66ff66 66ff99 66ffcc 66ffff 66cc00 66cc33 66cc66 66cc99 66cccc 66ccff 669900 669933 669966 669999 6699cc 6699ff 666600 666633 666666 666699 6666cc 6666ff 663300 6633336633666633996633cc 6633ff 660000 660033 660066 660099 6600cc 6600ff 33ff00 33ff33 33ff66 33ff99 33ffcc 33ffff 33cc00 33cc33 33cc66 33cc99 33cccc 33ccff 339900 339933 339966 339999 3399cc 3399ff 336600 336633 336666 336699 3366cc 3366ff 333300 333333 333366 3333993333cc 3333ff 330000 330033 330066 330099 3300cc 3300ff
中文颜色名称颜色对照表 1鸨色 #f7acbc 赤白橡 #deab8a 油色 #817936 绀桔梗 #444693 2踯躅色 #ef5b9c 肌色 #fedcbd 伽罗色 #7f7522 花色 #2b4490 3桜色 #feeeed 橙色 #f47920 青丹 #80752c 瑠璃色 #2a5caa 4蔷薇色 #f05b72 灰茶 #905a3d 莺色 #87843b 琉璃绀 #224b8f 5韩红 #f15b6c 茶色 #8f4b2e 利久色 #726930 绀色 #003a6c 6珊瑚色 #f8aba6 桦茶色 #87481f 媚茶 #454926 青蓝 #102b6a 7红梅色 #f69c9f 枯茶 #5f3c23 蓝海松茶 #2e3a1f 杜若色 #426ab3 8桃色 #f58f98 焦茶 #6b473c 青钝 #4d4f36 胜色 #46485f 9薄柿 #ca8687 柑子色 #faa755 抹茶色 #b7ba6b 群青色 #4e72b8 10薄红梅 #f391a9 杏色 #fab27b 黄緑 #b2d235 铁绀 #181d4b 11曙色 #bd6758 蜜柑色 #f58220 苔色 #5c7a29 蓝铁 #1a2933 12红色 #d71345 褐色 #843900 若草色 #bed742 青褐 #121a2a 13赤丹 #d64f44 路考茶 #905d1d 若緑 #7fb80e 褐返 #0c212b 14红赤 #d93a49 饴色 #8a5d19 萌黄 #a3cf62 藤纳戸 #6a6da9 15臙脂色 #b3424a 丁子色 #8c531b 苗色 #769149 桔梗色 #585eaa 16真赭丁子茶草色绀蓝
1.感官动词用法之一：see, hear, listen to, watch, notice等词，后接宾语，再接动词原形或ing形式。前者表全过程，后者表正在进行。句中有频率词时，以上的词也常跟动词原形。 I heard someone knocking at the door when I fell asleep. (我入睡时有人正敲门) I heard someone knock at the door three times. (听的是全过程) I often watch my classmates play volleyball after school.(此处有频率词often) 若以上词用于被动语态，后面原有动词原形改为带to不定式： We saw him go into the restaurant. →He was seen to go into the restaurant. I hear the boy cry every day. →The boy is heard to cry every day. 2.感官动词用法之二：look, sound, smell, taste, feel可当系动词，后接形容词： He looks angry. It sounds good. The flowers smell beautiful. The sweets taste sweet. The silk feels soft. I felt tired. They all looked tired. 这些动词都不用于被动语态。如：The sweets are tasted sweet.是个病句。注意：如果加介词like,则后不可接形容词，而接名词或代词：
#FF0033 #990033 #CC6699 #FF3399#FF9999 #9933FF #663399#3333FF #33CCCC #00CC99 #66FFCC #66FF66 #66CCFF #0099FF#CCCCFF #FFFF33 #CC9933 #996600#CC6633 #FF33CC#FFCCFF #33CCFF#9999FF #009933 #006600 #99CC66 #669933 #FF6666#FFCC33 Aqua #FF0000Yellow #0000FF #FF0000, #FFFF33 , #0000FF, #3333FF, #FFFFF, #00CC99, #33CCFF, #6633CC, #009933,#990033,#66FF66, #33CCCC, #66FFCC, #9933FF, #FFCC33, #CC6699, #669933, #FF9999, #6699FF, #CCC33, #6600FF, #99CC66, #CCCCC, #999999
#CCFF33, #CC6666,#333333,#666666, #AAAAAA,#DDDDDD,#BBBBBB,#222222,#444444,#555555,#77777,#888888,#EEEEE E 红色和粉红色，以及它们的16进制代码。 #9900 33 #CC66 99 #FF669 9 #FF33 66 #9933 66 #CC00 66 #CC00 33 #FF00 66 #FF00 33 ..#CC3399 .. #FF33 99#FF99 99 #FF99C C #FF00 99 #CC33 66 #FF66 CC #FF33 CC #FFCC FF #FF99 FF #FF00CC 紫红色，以及它们的16进制代码。 #FF66 FF #CC33 CC #CC00F F #FF33 FF #CC99 FF #9900 CC #FF00 FF #CC66 FF #9900 99 #CC0099 #CC33 FF #CC99 CC #99006 6 #9933 99 #CC66 CC #CC00 CC #6633 66 蓝色，以及它们的16进制代码。 #6600 99 #666F F #000CC #9933 CC #6666 99 #6600 66 #3333 66 #0066 CC #9900 FF #333399 #99CC FF #9933 FF #33009 9 #6699 FF #9966 CC #3300 CC #0033 66 #3300 33 #3300 FF #6699CC #6633 99#3333 FF #00669 9 #6633 CC #3333 CC #3399 CC #6600 CC #0066 FF #0099 CC #9966FF #0033 FF #66CC FF #33006 6 #3366 FF #3399 FF #6600 FF #3366 CC #0033 99 #6633 FF #000066 #0099 FF #CCCC FF #00003 3 #33CC FF #9999 FF #0000 FF #00CC FF #9999 CC #0000 99 #6666CC #0033 CC 黄色、褐色、玫瑰色和橙色，以及它们的16进制代码。 #FFFF CC #FFCC 00 #CC990 90 #6633 00 #FF66 00 #6633 33 #CC66 66 #FF66 66 #FF00 00 #FFFF99 #FFCC 66#FF99 00 #FF996 6 #CC33 00 #9966 66 #FFCC CC #6600 00 #FF33 00 #FF66 66 #FFCC33 #CC66 00#FF66 33 #99663 3 #CC99 99 #FF33 33 #9900 00 #CC99 66 #FFFF 33 #CC99 33 #993300 #FF99 33#3300 00 #99333 3 #CC33 33 #CC00 00 #FFCC 99 #FFFF 00 #9966 00 #CC66 33 绿色，以及它们的16进制代码。 #99FF FF #33CC CC #00CC9 9 #99FF 99 #0099 66 #33FF 33 #33FF 00 #99CC 33 #CCC3 3 #66FFFF #66CC#66FF#66FF6#0099#00CC#66FF#3366#3330#33FF#339999
劳尔色卡色号，中英文颜色名称对照列表
赤白橡#deab8a 油色 #817936 绀桔梗 #444693 肌色 #fedcbd 伽罗色 #7f7522 花色 #2b4490 橙色 #f47920青丹 #80752c 瑠璃色 #2a5caa 灰茶莺色琉璃绀
#905a3d#87843b#224b8f 茶色 #8f4b2e 利久色 #726930 绀色 #003a6c 桦茶色#87481f 媚茶 #454926 青蓝 #102b6a 枯茶 #5f3c23蓝海松茶 #2e3a1f 杜若色 #426ab3 焦茶 #6b473c 青钝 #4d4f36 胜色 #46485f 柑子色#faa755抹茶色 #b7ba6b 群青色 #4e72b8 杏色 #fab27b 黄緑 #b2d235 铁绀 #181d4b 蜜柑色#f58220苔色 #5c7a29 蓝铁 #1a2933 褐色 #843900若草色 #bed742 青褐 #121a2a 路考茶#905d1d 若緑 #7fb80e 褐返 #0c212b 饴色 #8a5d19萌黄 #a3cf62 藤纳戸 #6a6da9 丁子色#8c531b 苗色 #769149 桔梗色 #585eaa 丁子茶#826858草色 #6d8346 绀蓝 #494e8f 黄栌 #64492b 柳色 #78a355 藤色 #afb4db 土器色#ae6642若草色 #abc88b 藤紫 #9b95c9 黄枯茶#56452d 松叶色 #74905d 青紫 #6950a1 狐色 #96582a 白緑 #cde6c7 菫色 #6f60aa 黄橡 #705628薄緑 #1d953f 鸠羽色 #867892
感官动词的概念和相关考点 1、什么是感官动词？ 听觉：listen to、hear 视觉：look at、seem、watch 嗅觉：smell 触觉：feel、touch 味觉：taste 2、感官动词如何正确使用？ Tom drove his car away. →I saw him drive away. (全过程) 用法一：somebody did sth + I saw this I saw somebody do something. Tom was waiting for the bus. →I saw Tom waiting for the bus. (看不到全过程) 用法二：somebody was doing sth + I saw this I saw somebody doing something 练习： 一、句子翻译 1. I didn,t hear you come in. 2. I suddenly felt sth touch me on the shoulder. 3. I could hear it raining. 4. Listen to the birds singing. 5. Can you smell sth burning? 6. I found Sue in my room reading my letters. 二、灵活运用 1. I saw Ann waiting for the bus. 2. I saw Dave and Helen playing tenins. 3. I saw Clair having her meal. 三、选择最佳选项 1. Did anybody see the accident (happen/happening)? 2. We listen to the old man (tell/telling) his story from beginning to the end. 3. Listen! Can you hear a baby (cry/crying)? 4.—Why did you turn around suddenly? — I heard someone (call/calling) my name. 5. We watched the two men (open/opening) a window and (climb/climbing) through it into house. 6. When we got there, we found our cat (sleep/sleeping) on the table. 四、感官动词的被动语态 Oh，the milk is tasted strange.
颜色代码对照表 颜色代码大全
#FFFFFF #FFFFF0 #FFFFE0 #FFFF00 #FFFAFA #FFFAF0 #FFFACD #FFF8DC #FFF68F #FFF5EE #FFF0F5 #FFEFDB #FFEFD5 #FFEC8B #FFEBCD #FFE7BA #FFE4E1 #FFE4C4 #FFE4B5 #FFE1FF #FFDAB9 #FFD700 #FFD39B #FFC1C1 #FFC125 #FFC0CB #FFBBFF #FFB90F #FFB6C1 #FFB5C5 #FFAEB9 #FFA54F #FFA500 #FFA07A #FF8C69 #FF8C00 #FF83FA #FF82AB #FF8247 #FF7F50 #FF7F24 #FF7F00 #FF7256 #FF6EB4 #FF6A6A #FF69B4 #FF6347 #FF4500 #FF4040 #FF3E96 #FF34B3 #FF3030 #FF1493 #FF00FF #FF0000 #FDF5E6 #FAFAFA #FAFAD2 #FAF0E6 #FAEBD7 #FA8072 #F8F8FF #F7F7F7 #F5FFFA #F5F5F5 #F5F5DC
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我们学过了五个与人的感觉有关的动词，它们是look，sound，smel l，taste，feel，我们可称之为“感官”动词。它们的用法有着许多相同点，但也有不同之处，现就此作一小结。 一、这五个动词均可作连系动词，后面接形容词作表语，说明主语所处的状态。其意思分别为“看/听/闻/尝/摸起来……”。除loo k之外，其它几个动词的主语往往是物，而不是人。例如：These flowers smell very sweet. 这些花闻起来很香。 The tomatoes feel very soft. 这些西红柿摸起来很软。 The music sounds beautiful. 二、这些动词后面也可接介词like短语，like后面常用名词。例如： Her idea sounds like fun. 她的主意听起来很有趣。 He looks like his father. 三、这五个感官动词也可作实义动词，除look（当“看起来……”讲时）只能作不及物动词外，其余四个既可作及物动词也可作不及物动词，其主语通常是人。例如： She smelt the meat. 她闻了闻那块肉。
I felt in my pocket for cigarettes. 我用手在口袋里摸香烟。 He tasted the soup and added some salt. Miss Wang asked us to look at the blackboard. 四、taste，smell作不及物动词时，可用于“taste / smell + of + 名词”结构，意为“有……味道 / 气味”。例如： The air in the room smells of earth. 房间里的空气有股泥土味。 The bread taste of sugar. 五、它们（sound除外）可以直接作名词，与have或take构成短语。例如： May I have a taste of the mooncakes？我可以尝一口这月饼吗？ May I have a look at your photo? 六、其中look，sound，feel还能构成“look / sound / feel + as if +从句”结构，意为“看起来/听起来/ 感觉好像……”。例如：
■RGB(220,20■,★60●◆) crimso（n 腥红） ■RGB(255,240,■2★4●5◆)lavenderb（l us苍h白的紫罗兰 红） ■RGB(219,112■,1★4●7◆)paleviolet（re脸d 红的淡紫红） ■RGB(255,105,■1★8●0◆)hotpin（k热情的粉红） ■RGB(199,21,■1★3●3◆) mediumviole（tr适e d中的紫罗兰 红） ■RGB(218,112■,2★1●4◆)orch（i d 兰花紫） ■RGB(216,191,■2★1●6◆)thistl（e 苍紫） ■RGB(221,160,■2★2●1◆)plum（轻紫） ■RGB(238,130,■2★3●8◆)viole（t 紫罗兰） ■RGB(255,0,2■★55●◆) magen（ta洋紫) ■RGB(255,0,2■★55●◆) fuchs（ia紫红） ■RGB(139,0,1■★39●◆) darkmage（nt深a 洋紫） ■RGB(128,0,1■★28●◆) purpl（e 紫） ■RGB(186,85,■2★1●1◆) m ediumor（c h适id中的兰花紫） ■RGB(148,0,2■★1●1◆) darkvio（let深紫罗兰） ■RGB(75,0,1■3★0●)◆indig（o 靓青） ■RGB(138,43,■2★2●6◆) bluevio（let蓝紫罗兰） ■RGB(147,112■,2★1●9◆)mediumpu（rp适le中的紫） ■RGB(123,104,■2★3●8◆)mediumslate（bl适ue中的的板岩蓝）■RGB(106,90,■2★0●5◆) slatebl（u e板岩蓝） ■RGB(72,61,1■★39●◆) darkslateb（lu深e 板岩蓝） ■RGB(230,230,■2★5●0◆)lavend（er熏衣草花的淡紫） ■RGB(248,248,■2★5●5◆)ghostwh（ite幽灵白） ■RGB(0,0,2■5★5●)◆blue（蓝） ■RGB(0,0,2■0★5●)◆mediumb（lu适e中的蓝） ■RGB(25,25,1■★1●2◆) midnightb（l u午e 夜蓝） ■RGB(0,0,1■3★9●)◆darkbl（u e深蓝） ■RGB(0,0,1■2★8●)◆nav（y 海军蓝） ■RGB(65,105,■2★2●5◆) royalbl（u e皇家蓝） ■RGB(100,149,■2★3●7◆)cornflower（b lu矢e车菊蓝） ■RGB(176,196,■2★2●2◆)lightsteelb（lu淡e 钢蓝） ■RGB(119,136■,1★5●3◆)lightslateg（ra浅y 石板灰） ■RGB(112,128■,1★4●4◆)slategr（ay石板灰） ■RGB(30,144,■2★5●5◆) dodgerb（lue道奇蓝） ■RGB(240,248,■2★5●5◆)alicebl（u e爱丽丝蓝） ■RGB(70,130,■1★8●0◆) steelbl（u e钢蓝） e天蓝） ■RGB(135,206,■2★5●0◆)lightskyb（lu淡 ■RGB(135,206,■2★3●5◆)skyblu（e天蓝） ■RGB(0,191,2■★55●◆) deepskyb（l u深e 天蓝） ■RGB(173,216,■2★3●0◆)lightblu（e淡蓝） ■RGB(176,224,■2★3●0◆)powderb（lue火药蓝） ■RGB(95,158,■1★6●0◆) cadetbl（ue军校蓝）
颜色代码表：以下样色显示您可能觉得不够精确，这和电脑显示器有直接关系。您可查看html字体的颜 色代码，绝对正确，绝无重复。
QQ空间代码 欢迎您使用RGB颜色查询对照表 当你要给你的网页添加颜色时，有时，你能够直接使用该颜色的名称，但是大多情况下，你只能使用十六进制代码来使用这些字体颜色。（浏览器能够理解这些代码。） 为了方便你去使用这些代码，我们制作了这个列表，右边是颜色，左边是十六进制代码。 Hex Code Color #FFFFFF #FFFFCC #FFFF99 #FFFF66 #FFFF33 #FFFF00 #FFCCFF #FFCCCC #FFCC99 #FFCC66 #FFCC33 #FFCC00 #FF99FF #FF99CC #FF9999 #FF9966 #FF9933 #FF9900 #FF66FF #FF66CC #FF6699 #FF6666 #FF6633 #FF6600 #FF33FF #FF33CC #FF3399 #FF3366Hex Code Color #CCFFFF #CCFFCC #CCFF99 #CCFF66 #CCFF33 #CCFF00 #CCCCFF #CCCCCC #CCCC99 #CCCC66 #CCCC33 #CCCC00 #CC99FF #CC99CC #CC9999 #CC9966 #CC9933 #CC9900 #CC66FF #CC66CC #CC6699 #CC6666 #CC6633 #CC6600 #CC33FF #CC33CC #CC3399 #CC3366 Hex Code Color #99FFFF #99FFCC #99FF99 #99FF66 #99FF33 #99FF00 #99CCFF #99CCCC #99CC99 #99CC66 #99CC33 #99CC00 #9999FF #9999CC #999999 #999966 #999933 #999900 #9966FF #9966CC #996699 #996666 #996633 #996600 #9933FF #9933CC #993399 #993366