Spectral Evidence for Widespread Galaxy Outflows at z4

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Spectral Evidence for Widespread Galaxy Out?ows at z >4Brenda Frye 1Department of Astrophysical Sciences,Princeton University,Peyton Hall,Princeton,NJ 08544Tom Broadhurst Racah Institute of Physics,The Hebrew University,Jerusalem,Israel 91904and Narciso Ben′?tez Department of Physics and Astronomy,Johns Hopkins University,3400N.Charles Street,Baltimore,MD 21218-2686ABSTRACT We present discovery spectra of a sample of eight lensed galaxies at high redshift,3.7

We also ?nd a trend of increasing equivalent width of Ly-αemission with redshift,which may be a genuine evolutionary e?ect towards younger stellar populations at high redshift with less developed stellar continua.No obvious emission is de-tected below the Lyman limit in any of our spectra,nor in deep U or B -band images.The UV continua are reproduced well by early B-stars,although some dust absorption would allow a ?t to hotter stars.If B-stars dominate,then their relatively prominent stellar absorption lines should separate in wavelength from those of the out?owing gas,requiring more detailed spectroscopy.After correct-ing for the lensing,we derive small physical sizes for our objects,～0.5-5kpc

h?1for a?at cosmology with?m=0.3,?Λ=0.7.The lensed images are only

marginally resolved in good seeing despite their close proximity to the critical

curve,where large arcs are visible and hence high magni?cations of up to～20×

are inferred.Two objects show a clear spatial extension of the Ly-αemission

relative to the continuum starlight,indicating a“breakout”of the gas.The sizes

of our galaxies together with their large gas motion suggests that out?ows of gas

are common at high redshift and associated with galaxy formation.

Subject headings:cosmology:gravitational lensing—cosmology:observations

—galaxies:clusters:individual(Abell2390,2219,1689,AC114)—galaxies:

distances and redshifts

1.Introduction

The photometric selection of high redshift galaxies by their Lyman-limit break has proven to be a successful means of obtaining galaxy redshifts in the range2.5

Only a handful of higher redshift galaxies are known,the best examples being serendipi-tous discoveries boosted by lensing(Warren et al.1996;Franx et al.1997;Trager et al.1997; Frye&Broadhurst1998).Others are identi?ed primarily on the basis of an asymmetric emission line taken to be Ly-α(Dey et al.1998),or by virtue only of a relatively large lower limit for the equivalent width of single emission lines(Weymann et al.1998;Hu et al.1998; Hu et al.1999;Stern et al.2000a;Rhoads et al.2000;Manning et al.2000).In principle, high quality photometry alone is su?cient for z>4.5candidates because the strength of the Lyman-series forest depression(Madau1995)can be established from bright QSO spectra (Schneider et al.1989;Storrie-Lombardi et al.1996),yielding precise predictions about the galaxy colors at those redshifts.This continuum suppression feature has led to convincing claims of z>5for the very reddest objects in the Hubble Deep Field(Lanzetta et al.1996; Spinrad et al.1998),and more recently,to the successful selection of high redshift QSOs

by Stern et al.(2000b)and the Sloan Digital Sky Survey collaboration(Fan et al.2000; Anderson et al.2001,and references therein).

Here we make use of this established high redshift Lyman-series depression to color select galaxies for spectroscopy near the critical curves of some of the most massive lensing clusters.This approach provides a viable way of obtaining useful spectroscopy of high-z galaxies,under favorable circumstances,where lensing is compounded by a massive cluster galaxy lying close to the critical curve of a cluster(Franx et al.1997;Frye&Broadhurst 1998).

The galaxies presented here form part of a systematic redshift survey of red-selected galaxies behind massive lensing clusters.Most galaxies selected in this way are early type lying at modest redshift behind the cluster.We present the full redshift survey,and measurements of cluster masses by magni?cation,in a di?erent paper(Frye et al.2001). Here we show only the most distant galaxies discovered in our survey as a by-product of the red selection,and whose optical colors place them in the range3.5

This paper is organized as follows.In§2we describe the target selection and in§3we outline the photometric and spectroscopic observations and data analysis techniques.This is followed by a presentation of the photometric and spectroscopic results in§4,an examination of the agreement with photometric redshift results in§5,and an analysis of gas motion and the equivalent width of the Ly-αemission line in§6.We close in§7with a discussion of our main results.

2.Target Selection

The lensing clusters were chosen to have the largest possible critical radii and to lie at relatively low redshift so as to maximize the number of background galaxies redder than the cluster early type sequence.Most of our color-selected galaxies have modest redshifts, 0.4

Target selection for spectroscopy is based on color and not on elongated morphologies. This is because in general relatively circular mass substructure can create apparently undis-

torted images(e.g.Trager et al.(1997)).Also,in the case of intrinsically small sources, the elongation by lensing may still leave an object poorly resolved even with Hubble Space Telescope(HST)resolution(for this reason lensed QSOs do not appear arc shaped).This is demonstrated,for example,in Fig5,which shows the galaxy at z=4.868along with its ground based UBV IJ images.The object lies close to a giant arc and is therefore highly magni?ed,by～10×,but is only marginally resolved spatially due to its intrinsically small size.

The minimum color for our selection is set by the upper envelope of early type cluster members,which is sharply de?ned and varies between clusters as a result of the k-correction (Kaiser et al.1995).At z>4,Ly-αfalls longward of the V band so that a color di?erence between V and I will be apparent.At z=4.5the continuum depression amounts to～2 magnitudes in V(Fig.1).

3.Observations

3.1.Imaging and Photometry

The magnitudes quoted here are SExtractor MAGBEST magnitudes(Bertin&Arnouts 1996),or for the very compact objects,aperture magnitudes corrected to‘total’magni-tudes using stellar aperture corrections.We used the following imaging data for making our photometric measurements and target selections.

3.1.1.A2219

We have obtained deep observations on Keck I with the Low Resolution Imaging Spec-trometer(LRIS)in July,1996in good seeing～0.′′7(Oke et al.1995),totalling20min in V and10min in I(Fig.8).Two giant arcs frame the very large cluster member just below and west of center,with many other arclets seen about the bright central galaxies.

3.1.2.A1689

We obtained deep V and I band observations at the European Space Observatory(ESO) New Technology Telescope(NTT)in1995.In1999we obtained new deep V,R,I,and Z data taken in average seeing of0.′′8with LRIS at Keck II.The largest arc is shown in Fig3,subtending30degrees around the cluster center.Many other giant arcs are visible at

this radius,following a contour encompassing the bright central galaxies.The photometric redshift analysis presented in§5is based on these data plus additional U band observations with the Du Pont telescope at Las Campanas,B band observations with the Nordic Optical Telescope at La Palma,and deep J,H,K imaging taken at ESO NTT with the Son of ISAAC (SOFI)IR imaging spectrograph.The reduction and analysis of these UBV RIZJHK data will be presented in an upcoming paper(Ben′?tez&Broadhurst2002).

3.1.3.A2390

The imaging data were taken at the Canada France Hawaii Telescope in V and I,and for the core region,archival HST images were analyzed in V and I(Squires et al.1996;Frye &Broadhurst1998).The righthand panel in Fig.7and the color plate in Frye&Broadhurst (1998)show the arcs at z=4.04and other giant arcs in the center of this cluster.

3.1.

4.AC114

The imaging data were taken at the Anglo Australian Telescope,consisting of approx-imately3hours of imaging in the B and I bands.For this cluster,the color selection was based only on these two bands.

3.2.Spectroscopy

3.2.1.A1689

Some of the spectroscopic observations were carried out with LRIS on the Keck I tele-scope in June1997,totalling2h43min through a1.′′0slit and in seeing of0.′′6-0.′′8.The 300line/mm grating was used blazed at5000?A,resulting in a resolution of12?A at6000?A, determined from unblended sky lines.Adequate relative spectrophotometry is obtained by taking the spectrum of an early type cluster member at z=0.187,observed simultaneously through the multislit mask,and comparing it to the standard empirical E/SO spectrum of Kennicutt(1992).These observations resulted in the detection of three high redshift galaxies at z=3.77,z=4.87,and z=5.12,shown in Figs.4,5,and??respectively.

More spectroscopic observations of these and other red selected galaxies behind A1689 were made with LRIS on Keck II in March and April1999,totalling2h20min and2h 05min respectively,through a1.′′0slit,and in good seeing of～0.′′8on both occasions.The

400line/mm grating was used blazed at6700?A,resulting in a resolution of10?A at6000?A, determined from unblended sky lines.Relative spectrophotometry for the z=4.868galaxy is obtained using the same?uxing curve established for the June1997data.Although fairly rough,the?uxing curve is found to be smooth across the throughput,leaving the spectral features una?ected and therefore adequate for the purposes of our redshift survey.This set of observations resulted in additional observations for the objects at z=3.770and z=5.120.

In total,three high-z galaxies were discovered behind A1689,with exposure times of3h 40min(z=5.12),4h40min(z=4.87)and2h20min and3h40min(z=3.77).

3.2.2.A2219

The spectroscopy for the three high-z galaxies behind A2219was taken with LRIS on Keck II in August1998in5h40min of exposure with the400line grating(Figs.9,10,11). The slit width was1′′,resulting in a resolution of10?A and a dispersion of1.8?A/pix.We observed the spectrophotometric standard G24-9under photometric conditions,providing a relative?ux calibration.

3.2.3.A2390

The spectroscopy for the one dimensional spectrum for the z=4.039galaxy behind A2390 (Fig.7)was taken with LRIS on Keck I in June1997in2hr50min of exposure,and is described in a previous paper(Frye&Broadhurst1998).Further longslit spectroscopy at higher spectral resolution was also obtained with Keck I in June1997,whose two dimensional spectrum is shown in the lower panel of Fig7.

3.2.

4.AC114

The spectroscopy for the high-z galaxy at z=4.248behind AC114was taken with LRIS on Keck II in August1997in2hr8min of exposure with the300line grating blazed at5000?A. The slit width was1′′,resulting in a resolution of12?A at the blazing angle,determined from unblended sky lines.

3.3.Reductions

We developed our own IDL reduction software to handle the large number of spectra e?ciently(～40targets per multislit mask with3-6exposures per mask),and to address issues relating to pronounced?exure and other spectral image artifacts(see§3.3.2and§3.3.3 below).Our aim is to maximize the signal-to-noise without resampling the data,so that groups of pixels carrying faint continuum signal have every chance of being detected as a coherent pattern in the?nal reduced image.Although purpose built,the code is general and can be applied to single and multislit data.It is also fast and convenient,processing the raw ?ts?les directly.

3.3.1.Reduction Procedure

The reduction procedure begins by?attening the data via dome or super?ats,as avail-able.White light dispersed?at?elds or‘object?ats’are used to take out the wavelength dependent e?ects of the pixel response.Cosmic ray events are removed byσ-clipping above a suitable threshold which depends mainly on the number of independent exposures.Fringing changes between the exposures,and therefore is not removed completely by the dome?at,re-quiring dithering the spectra along the slit to average away this problem at long wavelengths (>7500?A).

Spatial curvature corrections are important for tracking the object plus background accurately,amounting to up to5pixels from center to end of a slitmask(see§3.3.2).Its proper characterization allows for the detection of the faintest objects,where the continuum signal is not readily identi?ed before one dimensional extraction but can be located blindly with knowledge of the spatial curvature plus the known device coordinates of the mask and targets.We identify cosmic rays incident on the data frames by?agging the hottest members in each spatial column with the median,and then by?tting low order polynomials and applying iterativeσ-clipping.The mean value of the good background pixels is then subtracted from the image.

The spectra typically have a relatively limited coverage of sky,with on average only 10-40pixels in a given spatial column with which to determine the best estimate.In these cases,and on account of the spectral tilt,sky subtraction is achieved by correcting for a gradient in the spatial direction of the sky values(see§3.3.2below).This distortion results in a slowly changing gradient in sky values in the spatial direction which we?t with a low order polynomial.We?nd that since many more independent sky pixels are averaged over in this way than in the standard procedure for sky subtraction this leads to a more accurate

correction,eliminates the need for rebinning,and produces higher signal-to-noise results.

The wavelength calibration is obtained accurately from the many bright sky lines in the red,and the choice of lines is interactively improved on with a cursor connection.The1d spectra are then extracted without resampling,and following the spatial curvature.Cosmic rays on the object are?agged in one dimension,byσ-clipping relative to the local continuum, and then removed across a stack of exposures by interactiveσ-clipping.Thresholds are set for acceptable number of cosmic‘hits’per pixel stack,to avoid removal of real spectral features.

3.3.2.Curvature Correction

Following the Curvature

The data are distorted in the spatial direction with respect to the2d detector frame.We?nd that we can remove this2d curvature without repixelization by following the curvature of the initially straight slit boundaries which lie between the multislit spectra on the slitmask.At each boundary the pixel values abruptly drop from the sky value of typically～200counts per pixel down to zero,providing a well de?ned curvature.We?t it with a low order polynomial and then shift the solution onto the object spectrum.We then sum up the object signal in the dispersion direction,shifting the entire pixel stack along spatially by on average3-5 pixels from center to end of the mask,as determined by the polynomial.In this way we avoid rectifying the2d image or introducing noise into the background-limited data.Note for its ability to follow background-limited objects over the full dispersion range,we advise this approach over the conventional one of following the curvature of the object itself.

Spectral Tilt

While good?at?elding may average out the background sky,it does not account for a slow wavelength variation in the spatial direction.This type of curvature imposes a tilt on the spectrum which is most pronounced on the edges of the bright sky lines.Here the large change in signal from the background value to emission peak introduces an increment-decrement pattern,resulting in an arti?cial P-Cygni type pro?le that depends slowly on wavelength.In between the sky lines this e?ect can be traced well with a slowly varying polynomial.Operationally,we?t a linear slope in the spatial direction to each spatial pixel stack which is determined by smoothing over a running boxcar along the dispersion direction to get a good local estimate.This procedure of treating the sky as a smoothly varying2D surface is found to improve the signal-to-noise of the data considerably for sections lying

between the sky lines.

For bright sky lines,however,the slope in the spatial direction is determined for each column and then subtracted,since the gradient of the sky values is very steep and depends sensitively on where the sky line lies with respect to the?xed pixel grid.Although only one column is used at a time,this estimate is a fair one because the sky lines are relatively bright.Note that this process does not require rebinning of the data,unlike the conventional approach of rectifying the entire2D frame with arc-lamp calibrations.

3.3.3.Artifacts

Both punched and milled masks produce physical defects along the slits,imprinting dark and bright spatially-dependent striations into the data.The resulting artifacts of this nonuniform illumination typically a?ect the background by3-5%,enough to lose background-limited spectra completely for an unlucky alignment where an object falls into a trough. The e?ect is much worse for the punched masks,which were used in about one third of the experimental runs.The e?ect can be corrected for,to?rst order,by dividing the object?ats into the data,but,as with the fringing correction,small time dependent changes occur that limit the usefulness of the?at?eld.

The spatial pro?le of the slit,or slit function,is complex,varying on subpixel scales. The sampling of the slit function in the spatial direction varies along the spectrum due to the curvature,and therefore o?ers in principle the opportunity to de?ne this function over di?erent pixel phases.In this way one potentially can piece together a well sampled function and apply it to the data.Although this algorithm is not part of the standard reduction code, it has been used in some of the more gross examples of non-uniform illumination.

4.Results

A total of eight high redshift galaxies were discovered as a consequence of our V?I color selection and these are listed in Table1,2.details.Table1gives the imaging details in?ve columns:cluster name;position in J2000coordinates;I A

B magnitude and its1σerror;(V?I)AB color;and lensing corrected size,in kpc h?1for a?at cosmology with ?m=0.3,?Λ=0.7.Table2gives the spectral details in six columns:cluster name,redshift (not heliocentric corrected);rest equivalent width of Ly-α;summed rest equivalent width of OIλ1302+SiIIλ1304;summed rest equivalent width of SiIIλ1260+OIλ1302+SiIIλ1304 +CIIλ1336;and velocity shift between the centroid position of Ly-αand the absorption

lines.

The apparent magnitudes of these objects are relatively bright owing to the large mag-ni?cations,23

The results are organized as follows.In§4.1we describe the continuum models generated for comparison with the data,in§4.2we give the error estimation,in§4.3we give the prescription for estimating the magni?cation,and in§4.4we present the spectra and images.

4.1.Continuum Modelling

Stellar continuum?ts are compared with the?uxed spectra.The model is composed of a single stellar spectral type,which we?nd is su?cient for estimating the continuum shapes and determining the relative line velocities.Continuum light in the UV sampled at high redshift is of course dominated by the hottest stars for any reasonable initial mass function (IMF),given the steep dependence of luminosity on temperature for opaque material(de Mello et al.2000).A more detailed?t to our data,using spectral synthesis models,will be presented elsewhere.Kurucz models with solar metallicities were used to estimate the temperature of the dominant contribution to the UV at restframe～1000?A,where we sample their spectra(Kurucz1993).Reddening is expected to be important at short wavelengths, as is underscored by the presence of metal lines in all of the high redshift galaxies in our sample.The e?ects of reddening and/or age variations on the colors and continuum shapes may be constrained with the help of infrared information.

We include sources of opacity into the models as necessary.The requisite Lyman-series opacity,as de?ned by Haardt&Madau(1996),is found to match the data well(Fig.5).Our highest signal-to-noise data also require an HI opacity at the source,with column densities of HI between logN=21.1and logN=21.5(Figs.9,10,11).

The hot B-stars which typically give good?ts to the continuum also show an intrinsic Ly-αabsorption which can dilute an otherwise strong Ly-αemission.This becomes increasingly more pronounced for late B-stars,where the absorption increases strongly with decreasing temperature.Fig.11shows one of our model?ts to the data.Here we?t a simple two component model consisting of a B3star plus Lyman-series opacity.Continuum?tting in this detail has not been possible for comparably high redshift galaxies(Dey et al.1998;Hu

et al.1998),for which the continuum is only marginally detected at best,or in the case of the z=4.92lensed galaxy of Franx et al.(1997),its continuum is contaminated by light from

a nearby cluster member.

4.2.Error Estimation

Error estimates on the equivalent width of Ly-αemission and its wavelength centroid are made with respect to the above continuum models,in an attempt to deal with a potentially large gradient in the continuum light pro?le under this line,due to HI absorption local to the galaxy and potentially from stellar atmospheres.Hence,there is most likely a sizable systematic uncertainty in the equivalent width of this line and also some smaller error on the central velocity.The uncertainty in the model then is the main source of error,which we have included in Table2.

As the equivalent width is measured with respect to the best?t model,the errors we quote on it are based on the uncertainty in the normalization of the best?t model.A1σestimate of the continuum height is determined simply by the absolute value of the dispersion of the continuum in each wavelength bin about the mean continuum level,excluding sky pixels and the ends of the spectrum.This dispersion measure is then corrected downward by a factor representing the square-root of the number of useful wavelength bins over which the continuum?t is made.The equivalent width is then remeasured,shifting the normalization up and down by this error in normalization.For the absorption lines,the continuum height is better determined locally,as the continuum gradient is rather?at in general for these lines and so the standard manual technique of continuum and line selected spectral regions is adopted and the error again is assumed to be dominated by the uncertainty on the continuum ?t.

The centroid velocity is less sensitive to the choice of model and is determined simply from an intensity weighted?rst moment of the wavelength integrated over a restricted range of wavelength which is somewhat subjectively determined by the quality of the data but covering typically not much more than about twice the spectral resolution of～10?A.In most cases the emission line is not evidently well resolved and hence the central wavelength largely re?ects the instrumental resolution and over sampling of our data by a factor of about 6for each wavelength bin relative to the resolution for the400-line grating.

For the absorption lines,the centroid velocity is determined using a local?t to the continuum height and,in the usual way,the?ux-weighted wavelength centroid is determined relative to the local continuum level.The error on the velocity centroid is close to the

sampling limit of1.8?A or≈70km s?1for the best de?ned lines.A purely empirically determined estimate can also be obtained by comparing the redshifts from the di?erent absorption lines.In this case the dispersion is somewhat larger than the sampling,≈110km s?1,on average,providing an average internal estimate.The larger of these two numbers we quote for?V in Table2,where the dispersion is determined for each spectrum individually in the case where more than one absorption line redshift can be measured.

4.3.Magni?cation Estimation

The main uncertainty in estimating the magni?cation of an image is the gradient of the lensing mass pro?le.The?atter the pro?le,for a?xed Einstein ring radiusθE,the greater the magni?cation.For a power law mass density pro?leΣ∝θ?p,where p is the power law index,we may expect the slope to lie in the range0.5

It is relatively straightforward to obtain a useful expression for the magni?cation at angular positionθ,μ(θ),in terms ofθE/θ:

μ(θ)?1= 1? θEθ p

For highly magni?ed images close to the Einstein radius(θe≈θ),this reduces to

μ(θ)≈1

(1?θE/θ)

In terms of the magni?cation by a singular isothermal lens,it becomesμ(θ)≈1

μt(θ)?1= 1? θE

p

1

p μiso t.Hence,this

correction is inversely dependent on the slope of the mass pro?le for images close to the Einstein ring.

In the following section we provide?uxes corrected for lensing by the factorμ(θ),and intrinsic sizes corrected for lensing by the factorμt(θ),covering what we assume to be the range of plausible central slopes of0.5

4.4.Individual High-z Detections

Each high-z detection will be discussed in turn below.In the main panel of each?gure we show the signal versus observed wavelength on the lower axis and restframe wavelength on the upper axis.Continuum models are compared with the data,where relevant(see§4.1). The sky spectrum is included at the bottom of the panel in order to evaluate the reliability of the spectrum more clearly.It varies markedly with wavelength due to the presence of many bright sky lines and fringing in the red.We attach a postage stamp image of each object in two or more of the UBV IJ bands,and center the object in the overlayed circle. Magni?cations are computed and used to estimate the unlensed?ux and intrinsic size(see §4.3).Note that the objects are typically only marginally resolved,resulting in upper limits on the sizes and lower limits on the magnitudes.We measure sizes for a?at cosmology with ?m=0.3,?Λ=0.7.

4.4.1.A1689

z=3.770

The image and spectrum for this multiply lensed object are shown in Figs.3,and4re-spectively.A shallower,blue spectrum appears in the lefthand panel and a deeper,higher resolution one on the right.The spectrum shows very weak or absent Ly-αemission,for which we quote an upper limit on the equivalent width of～3?A.Both the Ly-αand Ly-βbreaks are detected,and several metal lines are clearly identi?ed as SiIIλ1260,OI and SiII atλ1302andλ1304respectively,CIIλ1336,and SiIVλ1398andλ1402,from which we determined the redshift.

This object is obviously elongated by lensing(see image in righthand panels),forming a tangential arc of angular size2.2′′.The object lies about15′′outside the Einstein ring, resulting in a tangential magni?cation of6-12and a?ux magni?cation of6-24for the un-certain slope in the range0.5

z=4.868

The image of our brightest object,I AB=23.3,is shown in Fig.3,and its?uxed spectrum in Fig.5.From the emission line,readily identi?ed as Ly-α,a distinctive break on the blueward side and the clear presence of an absorption line at7396?A,identi?ed as SiIIλ1260, we determined the redshift.Ly-αis redshifted by360±70km s?1from the metal line,and is obviously asymmetric with a more extended wing on the red side.Such a pro?le shape is now established as a common property of all high-z galaxies where Ly-αis seen and the data are of su?cient quality(Franx et al.1997;Frye&Broadhurst1998;Dey et al.1998; Pettini&et al2001).

A distinctive wedge-like step shortward of Ly-βis observed,as predicted at high red-shift(Madau1995),and caused by the increasing opacity of the Lyman-series forest for wavelengths greater than that of Ly-βat the emission redshift.A good continuum?t is found to a late type B0star(see§4.1).This is considerably bluer than the B3and B5best ?ts to our other high-z spectra(Figs.9,10,11,and Fig.2in Frye&Broadhurst(1998)).

No signi?cant?ux is seen in the spectrum below the Lyman limit and no emission is detected in the U and B bands down to our2σlimiting magnitudes of U AB=27.3and B AB=26.7(see also Fig.5),indicating that no signi?cant?ux has escaped below the Lyman limit,at least along our line of sight.A more detailed determination of the escape fraction will be published elsewhere.A de?cit of continuum?ux below the Lyman limit is

not unexpected for any galaxy in which star formation is centrally concentrated.Of course in addition,any modest column lower redshift intervening forest cloud in the range z>4.3 could also lead to a non-detection in the U and B bands.

This is the reddest object measured in the?eld,(V?I)AB>3.2,and almost redder than a passively evolving elliptical is expected to reach at maximum,near z=1(See Fig.1). Our deep ground based image resolves the object in I in seeing of0.′′8,and detects it at the 3σlevel in J.

The intrinsic size of the object can be determined roughly by its position relative to the Einstein radius,which we take to beθE=50′′given by the main arc(Fig.3).The lensed image lies～20′′outside this radius,resulting in a tangential stretch factor of3-7and a?ux magni?cation of3-14for a slope in the range0.5

z=5.120

The highest redshift object in our sample lies at z=5.120(Fig.3)and its spectrum is shown in Fig.6.From the strong asymmetric emission line detected at7430?A(see inset),and a distinctive break on the blueward side we determined the redshift.The line has an obviously asymmetric pro?le and the largest observed equivalent width of our sample,Wα～30?A. Identi?ed as Ly-α,we tentatively?nd absorption at the expected position of SiIIλ1260at the ～2.5σlevel.Our deep imaging provides a lower limit of(V?I)AB>1.5,with I AB=25.2 and a2σupper limit of V AB>26.5.Below the galaxy and sky spectrum are the images in U,B,V,I,and J.The object appears clearly only in the I band,where it is faint and unresolved.No?ux is seen in the spectrum below the Lyman limit.

The magni?cation of this object is hard to determine with any precision because it lies so close to the critical curve,within5′′,where the magni?cation diverges.It is interesting that despite the very large magni?cation,which must be in excess ofμ>10,the object is at best only marginally spatially resolved,meaning that its luminous part is intrinsically very small,of order0.′′7/μor<0.5kpc h?1for the?at case.We estimate an unlensed apparent magnitude of I AB>27.5.

4.5.A2390

z=4.039

The image and?uxed spectrum for this multiply lensed object is shown in Fig.7and is discussed in detail in a previous paper(Frye&Broadhurst1998).The prominent features detected are the Lyman-series and Ly-βbreaks,and an asymmetric Ly-αemission line which is redshifted by420km s?1with respect to the clearly detected interstellar absorption lines of SiII1260λ,OI and SiII atλ1302andλ1304respectively,and CIIλ1336.Also SiIVλ1398 andλ1402are detected and shown in Fig.2of Frye&Broadhurst(1998).

The righthand panel shows the HST WFPC2color image constructed in the F606W and F814W passbands,from which we clearly distinguish four spatially stretched image com-ponents and individual HII regions along the5′′and3′′long N and S components respectively (see Fig.7).In addition,there is cluster elliptical in the center of the inset image which has been removed with a deVaucouleur’s pro?le to reveal the four image components of this ‘extended’Einstein cross.

We have constructed a simple isothermal lens model which provides an adequate?t to the data.It consists of a dominant central cluster potential modi?ed by the cluster member galaxy that splits the images(Frye&Broadhurst1998).The magni?cation is hard to constrain well since the images lie so close to the critical curve where the magni?cation diverges.The HST images allow a reasonable estimate of the size of this object given by the width of the lensed images in the radial direction which is little a?ected by lensing if the slope is close to isothermal.The measured width is0.2′′(Frye&Broadhurst1998),corresponding to an intrinsic size of～1kpc h?1for the?at case.

4.6.A2219

z=4.068

This object is labelled in Fig.8and its?uxed spectrum shown in Fig.9.The spectrum has several strong and nearly saturated metal lines which are identi?ed as SiIIλ1260,OIλ1302 SiIIλ1304,CIIλ1336,and SiIVλ1398andλ1402,from which we determined the redshift. There is a broad absorption which we take to be absorption by the A-band atλ7600?A.Ly-αis seen in emission and is redshifted by830km s?1with respect to the metal absorption lines,indicating a substantial amount of gas out?ow.The best?tted model is for a B5stellar population(solid line)with Lyman-series forest attenuation along the line of sight and an HI column at the source of logN=21.1.The Lyman-series break appears shortward of Ly-α

and no?ux is detected below the Lyman limit in the spectrum.The V and I band images in the righthand panels show the object to be faint,I AB=24.1,and a V-band dropout.The magni?cation is likely to be small since the object is at～15critical radii,resulting in only a～10%correction to the observed magnitude and size.

z=4.445

The object at z=4.068is labelled in Fig.8and its?uxed spectrum is shown in Fig.10.It is a high quality spectrum with a signal-to-noise of～7per pixel in the continuum.The most prominent features are the strong interstellar metal lines and the sharp Ly-αbreak.Ly-αis seen in emission and has a characteristically asymmetric shape extending to the red.This is likely to be a dynamical e?ect as we discuss in§6.1.The centroid of Ly-αis shifted redward by～700km s?1with respect to the clearly identi?ed lines of SiIIλ1260,OIλ1302,SiIIλ1304, CIIλ1336,and SiIVλ1398andλ1402,from which we determined the redshift.The best?tted model is for a B3stellar population(solid line)with Lyman-series forest attenuation along the line of sight and an HI column at the source of logN=21.1.The object is detected in both the V and I images shown to the right of the spectrum.

The magni?cation of the image is modest,as it lies about3critical radii from the center, resulting in a tangential stretch factor of<3and a?ux magni?cation of<6for the uncertain slope in the range0.5

z=4.654

The object at z=4.654is labelled in Fig.8and its?uxed spectrum is shown in Fig.11.The signal to noise is good,reaching≈4in the continuum at relatively high spectral dispersion of1.8?A/pixel.Ly-αis in emission and has a clearly asymmetric shape.Shortward of this,a sharp break is seen taken to be the Lyman-series break.The interstellar metal line SiIIλ1260 is clearly detected in this spectrum,and other lines commonly found in high-z galaxies are marked.From the emission line,continuum break,and absorption line we determined the redshift.Note that the broad absorption line atλ7600?A we take to be absorption by the A-band.

Somewhat surprisingly,the stellar continuum rises redward of the Ly-αemission line instead of declining as would be expected from a hot stellar population with no absorption at the source.This feature is also seen in the slightly higher signal-to-noise spectrum at z=4.445in Fig.10,and may be caused entirely by HI absorption at the emission redshift or by the combined e?ect of HI opacity and the stellar population.

The best?tted model is a B3stellar population(solid line)which has been attenuated by the Lyman-series forest and damped HI absorption with column density logN=21.5 placed at the emission redshift.There is a broad absorption which we take to be absorption by the A-band atλ7600?A.The centroid of the Ly-αemission line is shifted towards the red by425km s?1with respect to this line,and has a total rest equivalent-width of W Lyα～16?A. The V and I band images at the position of this arc are shown on the righthand side of the spectrum with a?ux of I AB=24.9and a color of(V?I)AB>2.1.The angular size in I is small and unresolved.

The magni?cation is not large as this object lies at about4critical radii,resulting in a tangential stretch factor of1.5-3and a?ux magni?cation of1.5-5for the uncertain slope in the range0.525.2.

4.7.AC114

4.248

The image and spectrum of the object at z=4.248is shown in Fig.12.The spectrum shows a strong Lyman-series absorption shortward of the position of Ly-α,weak Ly-αemission,and a marginal detection of the interstellar line SiIIλ1260(2σlevel),from which we determined the redshift.The Ly-αemission line is redshifted by460km s?1with respect to the metal line.The restframe equivalent width for Ly-αhas an upper limit of Wα=3?A.The B and I band images in the righthand panels show that the object centered in the circles is faint, I AB=23.9,and a B-band dropout.Note that the bluer band for this object is B AB and not the usual V AB,as we did not obtain V-band data for this cluster.

This image lies about20′′outside of the Einstein radius,resulting in a tangential stretch factor of2.5?5and a?ux magni?cation of2.5?10for the uncertain slope in the range 0.5

5.Consistency with Photometric Redshifts

As described in§3,we have obtained optical imaging in the UBV RIZJH and K bands for A1689,and very high quality photometric redshifts have been determined for this?eld using the Bayesian method of Ben′?tez(2000).We compare the galaxy colors with those

of a forest opacity corrected redshifted template set,formed by the main spectral types of Coleman et al.(1980),plus two starbursts from Kinney et al.(1996).We take into account the intrinsic color variation or‘cosmic variance’in the galaxy colors by convolving the resulting color likelihoods with a gaussian of width0.06(1+z),empirically measured from the Hubble Deep Field(HDF)(Ben′?tez2000).This makes the range of?nal redshift probabilities considerably wider than they would be if we included only the photometric error,but it yields a more accurate representation of the true uncertainties involved in the estimation.Since we are working on a cluster?eld which strongly magni?es the observed ?ux from background objects,we use the redshift magnitude prior p(z|T,m)introduced in Ben′?tez(2000)for?eld galaxy distributions,but with the corresponding unlensed magnitude, as calculated in§4.

The photometric redshifts estimated for the high-z objects in the A1689?eld are shown in Fig2and give excellent agreement with the spectroscopic ones.This is also true for the full spectroscopic survey sample,and with this new photometry we have identi?ed even higher redshift targets out to z～6.5,for which spectroscopic follow-up is being carried out with the Very Large Telescope(VLT).

6.Analysis

6.1.Gas Motion

6.1.1.Velocity Dispersion

In the spectrum of each object the metal line equivalent widths and the velocity shift of the Ly-αcentroid with respect to these metal lines is measured(Table2,Fig.13).There is an additional observation made for our object at z=4.04(Bunker et al.2000).The analysis yielded an independent velocity shift measurement which con?rmed our original measure-ment of420km s?1(Frye&Broadhurst1998),and so is not included separately here.

Similar measurements from other high quality spectra are compiled from the literature for comparison(Leitherer et al.1996;Franx et al.1997;Lowenthal et al.1997;Kunth et al. 1998).The results are shown graphically for a local plus high-z sample(Fig.14),and high-z sample only(Fig.15).The former includes only the two metal lines in common to all the samples,OI1302λand SiII1304λ.A fairly clear trend emerges in that the blueshift of the metal lines relative to the centroid of the Lyman-αemission correlates with the equivalent width of metal line absorption.Doppler broadening by the gas motion would leave the equivalent width unaltered for the optically thin case.However,if the lines are optically

thick,as we may expect for interstellar gas,then the width will be proportional to the velocity dispersion.The appearance of saturation is obvious in the spectra for the two objects in our survey at z=4.068and z=4.445in A2219(Fig.9and10).In other cases it is not directly clear although our limited spectral resolution is responsible for smoothing away the core of lines of equivalent width less than the resolution of～12?A.Also we may expect that the spatial coverage of dense gas does not fully cover the starlight continuum,so that the light which is not absorbed partially?lls the line.

Hence,for saturated absorption lines,a spread in gas velocity broadens the line and we propose that the trend we?nd in Figs.14and15is just a consequence of an intrinsic spread in the dispersion in the gas out?ow velocity.This in turn increases the equivalent width of the absorption lines and the mean out?ow velocity,thereby generating a larger blueshift of the metal lines with respect to the systemic velocity.Note that the velocity width of the absorption lines is only marginally resolved in the best cases with our limited spectral resolution.

In addition to our data,blueshifts of the metal lines have also been measured for the gravitational ring discovered by Warren et al.(1996),in which the wavelengths of the IR emission lines have been compared with Ly-α.The same use of IR lines has been achieved for15relatively bright z～3U-dropout galaxies by Pettini&et al(2001).They argue that restframe optical lines may better represent the systemic velocity of the galaxy,rather than the resonantly scattered Ly-αline.Perhaps the cleanest measure of the mean expansion rate is a comparison of IR lines with metal absorption lines,for which most of their objects in that paper have measurements(their Fig.13).The velocities lie in the range+200to?500 km s?1,and are in fact very similar in magnitude to the velocity o?set between Ly-αand the metal lines.

6.1.2.Models

Legrand et al.(1997)convincingly explain the discrepancy in velocity of the metal lines relative to Ly-αas arising from back scattered Ly-αphotons either emitted from the expanding HII region or scattered from the inner‘wall’of the surrounding HI,so that the Doppler redshift of far side emission is su?ciently large to clear it in wavelength of foreground absorption within the galaxy along the line of sight.For the galaxies in which Ly-αemission is absent,comprising about half the local starburst galaxies and distant z>2.5galaxies (Steidel et al.1996a,b;Steidel et al.1999),correspondingly strong Ly-αabsorption is seen. From this we deduce that the most likely cause is a combination of a lower rate of internal expansion and/or a higher HI column for absorption,rather than simply absorption by dust.

四种翻译方法,十种翻译技巧

四种翻译方法 1.直译和意译 所谓直译，就是在译文语言条件许可时，在译文中既保持原文的内容，又保持原文的形式——特别指保持原文的比喻、形象和民族、地方色彩等。 每一个民族语言都有它自己的词汇、句法结构和表达方法。当原文的思想内容与译文的表达形式有矛盾不宜采用直译法处理时，就应采用意译法。意译要求译文能正确表达原文的内容，但可以不拘泥与原文的形式。（张培基） 应当指出，在再能确切的表达原作思想内容和不违背译文语言规范的条件下，直译有其可取之处，一方面有助于保存原著的格调，另一方面可以进新鲜的表达方法。 Literal translation refers to an adequate representation of the original. When the original coincides or almost tallies with the Chinese language in the sequence of vocabulary, in grammatical structure and rhetorical device, literal translation must be used. Free translation is also called liberal translation, which does not adhere strictly to the form or word order of the original.（郭著章） 直译法是指在不违背英语文化的前提下，在英译文中完全保留汉语词语的指称意义，求得内容和形式相符的方法。

电线电缆国家标准

电线电缆国家标准 一、辐照交联电力电缆（电压等级：0.6/1KV；执行标准：GB/T12706.1-2002） 辐照交联电缆是利用高能射线轰击聚其分子链中的氢原子排出，于是分子链上产生空隙，相邻的分子链结合在一起形成－C－C－交联键，形成了网状的大分子立体结构而构成交联聚乙烯。 通过辐照后的交联聚乙烯热性能可达到105度，辐照交联为物理交联方式，整个交联没有水的介入，其绝缘中的水分子含量不大于100PPM，绝缘纯度高，从而辐照交联的电缆在电性能、机械性能方面有独特的优良特性，电缆寿命可达60年，同时电缆具有重量轻、结构简单、敷设不受落差限制等特点。 YJV、YJLV 辐照交联聚乙烯绝缘聚氯乙烯护套电力电缆 YJY、YJLY 辐照交联聚乙烯绝缘聚乙烯护套电力电缆 YJV22、YJLV22辐照交联聚乙烯绝缘钢带铠装聚氯乙烯护套电力电缆 YJV23、YJLV23辐照交联聚乙烯绝缘钢带铠装聚乙烯护套电力电缆 YJV32、YJLV32辐照交联聚乙烯绝缘细钢丝铠装聚氯乙烯护套电力电缆 YJV33、YJLV33辐照交联聚乙烯绝缘细钢丝铠装聚乙烯护套电力电缆 VV、VLV、VY、VLY、YJV、YJLV、YJY、YJLY适用于室内外敷设。可经受一定的敷设牵引，但不能承受机械外力作用的场合。单芯电缆不允许敷设在磁性管道中。 VV22、VLV22、VV23、VLV23、YJV22、YJLV22、YJV23、YJLV23敷设在室内、隧道、电缆沟，能够承受一定的机械外力，不能承受过大的拉力。 VV32、、VLV32、VV33、、VLV33、YJV32、YJLV32、YJV33、YJLV33敷设在室内、隧道、电缆沟，能够承受一定的机械外力。 VV32、、VLV32、VV33、、VLV33、YJV32、YJLV32、YJV33、YJLV33敷设在室内、隧道、电缆沟，能够承受一定的机械外力。 基本结构：导体－交联聚乙烯绝缘－内护套－钢带铠装－聚氯乙烯护套 辐照交联聚烯烃（主要材料是聚乙烯）电线电缆主要用于耐热建筑线、汽车线、航空导线、机车线电线和电机电器引接线等。 二、中压交联聚乙烯绝缘电力电缆（电压等级：6/6KV-26/35KV；执行标准： GB/T12706.2-2002） 中压交联聚乙电缆采用了全干式化学交联方法使用聚乙烯分子由线型分子结构变为空 间网状结构，使热塑性的聚乙烯转变为热固性的交联聚乙烯，使其机械性能、热老化性能及环境应力能力在很大的程度上得到提高，并具有优良的电气性能。具有异体正常运行温度高、结构简单、外径小、重量轻、使用方便、不受敷设落差限制等特性。适用于工频额定电压 1-35KV配电系统。 YJV62、YJLV62交联聚乙烯绝缘双非磁性金属带铠装聚氯乙烯护套电力电缆。 YJV63、YJLV63交联聚乙烯绝缘双非磁性金属带铠装聚乙烯护套电力电缆。 YJV63、YJLV63交联聚乙烯绝缘双非磁性金属带铠装聚乙烯护套电力电缆。 其它型号与辐照交联类似（只是电压不同） YJV、YJLV、YJY、YJLY适用于室内敷设。可经受一定的敷设牵引，但不能承受机械外力作用的场合。单芯电缆不允许敷设在磁性管道中。

证据法简答题(很全面的)

证据制度与诉讼制度的关系。 答：(1)控诉式诉讼制度与神示证据制度的关系；（2）纠问式诉讼与法定证据制度关系；（3）混合式诉讼与自由心证的关系。 2．简述我国证据制度的基本原则及其要求。 答：我国证据制度所坚持的客观真实的原则，是证据制度的基本原则。这种客观真实的证据制度，要求重证据、重调查研究、不轻信口供，要求查明案件事实真相，以便正确地据实处理。我国的证据制度为充分确实的证据制度，案件对证据的具体要求，在质上就是要求确实可靠，在量上就是要求全面细致、充分，达到了两个方面的统一，案件的真实性就可以保证。 3．简述证据学的具体研究方法。 答：1）借鉴和创新的研究方法；2）定性和定量的分析研究方法；3）系统、全面研究的方法；4）比较研究方法；5）实证研究的方法。 4．简述证据内容与证据形式的关系。 答：司法公正是核心，证据的内容和形式应为之服务。因此，在证据的内容与关系上应有的观点是：（1）坚持有真实内容的证据，原则上应使其有合法的证据形式，这有利于查明案件事实直相，从而保证案件正确处理。（2）重视对人权的保护，对于证据收集采用过程中的违法行为，一律依法严处；坚持按程序办案，坚持惩治违法行为，以实现诉讼程序公正。（3）对严重违法收集的证据，基于可靠性程序差，必须限制采用。 5．简述法定证据制度产生的历史条件。 答：法定证据制度是对神示证据制度的否定，是历史上一大进步。它的出现是人类文化科学的发展对司法经验总结的结果；同时又是和当时的政治斗争形势联系在一起的，是中央集权君主制的产物。为了结束地方封建割据的分裂状态，加强中央集权的统治，封建君主实行这项法律制度，有利于把司法权掌握在自己手中，从而打击封建割据势力。 6．简述自由心证证据制度产生的历史条件。 答：自由心证制度的形成有其特定的历史过程。为了与诉讼制度的变革相适应，1791年法国宪法会议正式废除法定证据制度，建立了自由心证制度。首先，资产阶级思想家崇尚人的理性的良心，指出“人生而自由”的观点。 7．简述自由心证理论的主要内容。 答：自由心证理论的主要内容有两点：一是法官的理论性和良心；二是心证达到确信的程度。两根支柱，一是抽象的理性；一是抽象的良心。其中心则是“自由”，即法官根据理性和良心自由地判断，在内心达到真诚确信的程度。自由心证制度的核心内容，就是对于各种证据的真伪、证明力的大小以及案件事实如何认定，法律并不作具体规定，完全听凭法官根据理性和良心的指示，自由地判断。 8．我国奴隶制度时期证据制度的特点。 答：奴隶制度的证据制度特点是：1）法官认定案件主要依据审判时间经验的总结；2）神示证据制度消失的较早。我国古代奴隶制各个王朝的证据制度，主要是根据审判实践经验形成的，比较重视与案情有拳客观材料，要求法官据证推断；3）除重视采用当事人的证词外，还重视其他证据的作用。 9．我国封建制度时期证据制度的特点。 答：封建制度时期证据特点是：1）坚持口供至上的原则，定罪必须取得被告人认罪的供词。2）审讯是可以依法刑讯。刑讯的程度，违法刑讯应否负刑事责任和负什么刑事责任，历代封建王朝的法律则有不同的规定。3）诬告者反坐，伪证者罚。4）疑罪惟轻兼从赎，实行有罪推定。5）重视勘验检查。6）据众证定罪的制度。7）集成和发展了“以五声听狱讼，求民情”的主观臆断的审判方法。 10．简述新中国证据制度发展的四个阶段。 答：第一阶段是从1931年至1949年的创建期，属于新民主主义时期，属于新民主主义时期。在革命根据地的法律中，已经建立起了先进的证据原则和制度。第二阶段是从1949年至1966年的发展期。中华人民共和国成立之后，人民政府在废除国民党伪法统和总结革命根据地司法工作经验的基础上建立了新

电线电缆最新国家标准(新修订)

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英语翻译技巧实例

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进行全部倒置，原则是使汉语译句安排符合现代汉语论理叙事的一般逻辑顺序。有时倒置法也用于汉译英。如： （1）At this moment, through the wonder of telecommunications, more people are seeing and hearing what we say than on any other occasions in the whole history of the world. 此时此刻，通过现代通信手段的奇迹，看到和听到我们讲话的人比整个世界历史上任何其他这样的场合都要多。（部分倒置） （2）I believe strongly that it is in the interest of my countrymen that Britain should remain an active and energetic member of the European Community. 我坚信，英国依然应该是欧共体中的一个积极的和充满活力的成员，这是符合我国人民利益的。（部分倒置） （3）改革开放以来，中国发生了巨大的变化。 Great changes have taken place in China since the introduction of the reform and opening policy.(全部倒置) 7.倒置法： 在汉语中，定语修饰语和状语修饰语往往位于被修饰语之前；在英语中，许多修饰语常常位于被修饰语之后，因此翻译时往往要把原文的语序颠倒过来。倒置法通常用于英译汉, 即对英语长句按照汉语的习惯表达法进行前后调换，按意群或进行全部倒置，原则是使汉语译句安排符合现代汉语论理叙事的一般逻辑顺序。有时倒置法也用于汉译英。如： （1）At this moment, through the wonder of telecommunications, more people are seeing and hearing what we say than on any other occasions in the whole history of the world.

电线.电线执行标准.常用电缆

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BVV-ZR-105 铜芯耐热105℃阻燃型聚氯乙烯护套圆型电缆 AV-ZR-105 铜芯耐热105℃阻燃型聚氯乙烯绝缘安装电线 AVR-ZR-105 铜芯耐热105℃阻燃型聚氯乙烯绝缘安装软电线 AV-ZR 铜芯阻燃型聚氯乙烯绝缘安装电线 AV-ZR 铜芯阻燃型聚氯乙烯绝缘安装软电线 RVB--铜芯聚氯乙烯绝缘平型连接软电线 RVS--铜芯聚氯乙烯绝缘绞型连接软电线 RVV--铜芯聚氯乙烯绝缘聚氯乙烯护套平型连接软电缆（电线） RV-105--铜芯耐热105度聚氯乙烯绝缘连接软电线 SYV：实心聚乙烯绝缘射频同轴电缆 SYWV(Y)：物理发泡聚乙绝缘有线电视系统电缆，视频（射频）同轴电缆 （SYV、SYWV、SYFV）适用于闭路监控及有线电视工程 SYWV（Y）、SYKV 有线电视、宽带网专用电缆结构：（同轴电缆）单根无氧圆铜线+物理发泡聚乙烯（绝缘）+（锡丝+铝）+聚氯乙烯（聚乙烯）RVVP屏蔽线：铜芯聚氯乙烯绝缘屏蔽聚氯乙烯护套软电缆电压300V/300V 2-24芯用途：仪器、仪表、对讲、监控、控制安装

常用翻译技巧和方法

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