Spectroscopy of High-Redshift Supernovae from the ESSENCE Project The First Two Years

a r X i v :a s t r o -p h /0411357v 1 12 N o v 2004

Spectroscopy of High-Redshift Supernovae from the ESSENCE Project:The

First Two Years 1

Thomas Matheson,2St′e phane Blondin,3Ryan J.Foley,4Ryan Chornock,4Alexei V.Filippenko,4

Bruno Leibundgut,3R.Chris Smith,5Jesper Sollerman,6Jason Spyromilio,3Robert P.Kirshner,7Alejandro Clocchiatti,8Claudio Aguilera,5Brian Barris,9Andrew C.Becker,10Peter Challis,7Ricardo Covarrubias,10Peter Garnavich,11Malcolm Hicken,7,12Saurabh Jha,4Kevin Krisciunas,11Weidong Li,4Anthony Miceli,10Gajus Miknaitis,13Jose Luis Prieto,14Armin Rest,5Adam G.Riess,15Maria Elena Salvo,16Brian P.Schmidt,16Christopher W.Stubbs,7,12Nicholas

B.Suntze?,5and John L.Tonry 9

ABSTRACT

We present the results of spectroscopic observations of targets discovered during the ?rst two years of the ESSENCE project.The goal of ESSENCE is to use a sample

of～200Type Ia supernovae(SNe Ia)at moderate redshifts(0.2 z 0.8)to place

constraints on the equation of state of the Universe.Spectroscopy not only provides

the redshifts of the objects,but also con?rms that some of the discoveries are indeed

SNe Ia.This con?rmation is critical to the project,as techniques developed to determine

luminosity distances to SNe Ia depend upon the knowledge that the objects at high

redshift are the same as the ones at low redshift.We describe the methods of target

selection and prioritization,the telescopes and detectors,and the software used to

identify objects.The redshifts deduced from spectral matching of high-redshift SNe Ia

with low-redshift SNe Ia are consistent with those determined from host-galaxy spectra.

We show that the high-redshift SNe Ia match well with low-redshift templates.We

include all spectra obtained by the ESSENCE project,including52SNe Ia,5core-

collapse SNe,12active galactic nuclei,19galaxies,4possibly variable stars,and16

objects with uncertain identi?cations.

Subject headings:galaxies:distances and redshifts—cosmology:distance scale—

supernovae:general

1.Introduction

The revolution wrought in modern cosmology using luminosity distances of Type Ia supernovae (SNe Ia)(Schmidt et al.1998;Riess et al.1998;Perlmutter et al.1999;Riess et al.2001;Knop et al. 2003;Tonry et al.2003;Barris et al.2004;Riess et al.2004b)relies upon the fact that the objects so employed are,in fact,SNe of Type Ia.Although the light-curve shape alone is useful(e.g., Barris&Tonry2004),the only way to be sure of the true nature of an object as a SN Ia is through spectroscopy.The calculation of luminosity distances depends upon the high-redshift objects being SNe Ia so that low-redshift calibration methods can be employed.The classi?cation scheme for SNe is based upon the optical spectrum near maximum(see Filippenko1997,for a review of SN types),so rest-wavelength optical spectroscopy is necessary to properly identify SNe Ia at high redshifts.Despite this signi?cance,relatively little attention has been paid to the spectroscopy of the high-redshift SNe Ia,with some notable exceptions(Coil et al.2000).Other publications that include high-redshift SN Ia spectra include Schmidt et al.(1998),Riess et al.(1998),Perlmutter et al.(1998),Leibundgut&Sollerman(2001),Tonry et al.(2003),Barris et al.(2004),Blondin et al. (2004),Riess et al.(2004b),and Lidman et al.(2004).

In addition to providing evidence for the acceleration of the expansion of the Universe,it was recognized at an early stage that high-redshift SNe Ia could put constraints on the equation of state for the Universe(Garnavich et al.1998),parameterized as w=P/(ρc2),the ratio of the dark energy’s pressure to its density.To further explore this,the ESSENCE project was begun.The

ESSENCE(Equation of State:SupErNovae trace Cosmic Expansion)project is a?ve-year ground-based SN survey designed to place constraints on the equation-of-state parameter for the Universe using～200SNe Ia over a redshift range of0.2 z 0.8(see Miknaitis et al.2005;Smith et al. 2005,for a more extensive discussion of the goals and implementation of the ESSENCE project).

Spectroscopic identi?cation of optical transients is a major component of the ESSENCE project.In addition to con?rming some targets as SNe Ia,the spectroscopy provides redshifts, allowing the derived luminosity distances to be compared with a given cosmological model.So many targets are discovered during the ESSENCE survey that a large amount of telescope time on6.5m to10m telescopes is required.In the?rst two years of the program,we were fortunate enough to have been awarded over60nights at large-aperture telescopes.Even with this much time,though,our resources were insu?cient to spectroscopically identify all of the potentially use-ful candidates.This remains the most signi?cant limiting factor in achieving the ESSENCE goal of?nding,identifying,and following the desired number of SNe Ia with the appropriate redshift distribution.

Nonetheless,spectroscopic observations of ESSENCE targets in the time available have been successful,with almost?fty SNe Ia clearly identi?ed,and several more characterized as likely SNe Ia. Other identi?cations include core-collapse SNe,active galactic nuclei(AGNs),and galaxies.The galaxy spectra may include an unidenti?ed SN component.

This paper will describe the results of the spectroscopic component of the?rst two years of the ESSENCE program.Year One refers to our2002Sep-Dec campaign;Year Two was our2003 Sep-Dec campaign.In Section2,we describe the process of target selection and prioritization. Section3describes the technical aspects of the observations.We discuss target identi?cation in Section4.The summary of results in terms of types of objects and success rates is given in Section 5.In addition,we present in Section5all of the spectra obtained,including those of the SNe Ia (with low-redshift templates),core-collapse SNe,AGNs,galaxies,stars,and objects that remain unidenti?ed.

2.Target Selection

The ESSENCE survey uses the Blanco4m telescope at CTIO with the MOSAIC wide-?eld CCD camera to detect many kinds of optical transients(Smith et al.2005).Temporal coverage helps to identify solar-system objects such as Kuiper Belt Objects(KBOs)and asteroids.Known AGNs and variable stars can also be eliminated from the possible SN Ia list.The remaining transients are all potentially SNe.They are also faint,requiring large-aperture telescopes to obtain spectra of the quality necessary to securely identify the object.Exposure times on8-10m telescopes are typically about half an hour,but can be as much as two hours.Such telescope time is di?cult to obtain in quantity,so not all of the detected transients can be examined spectroscopically.We apply several criteria to prioritize target selection for spectroscopic observation.

The?rst step in sorting targets is based upon the spectroscopic resources available.The equatorial?elds used for the ESSENCE program are accessible from most major astronomical sites,so the main concern with matching targets to spectroscopic telescopes is the aperture size of the telescope.The ESSENCE targets are generally in the range18 m R 24mag.When8-10m telescopes are unavailable,the fainter targets become lower in priority.The limit for low-dispersion spectroscopy to identify SNe with the6.5m telescopes is m R≈22?23mag,although this will vary with weather conditions and seeing.If the full range of telescopes is available,then targets are prioritized by magnitude for observation at a given telescope.The longitudinal distribution of spectroscopic resources can be important if con?rmation of a high-priority target is made during a night when multiple spectroscopic resources are available.By the time a target is con?rmed, the?elds may have set for telescopes in Chile,while they are still accessible from Hawaii.This requires active,real-time collaboration between the group?nding SN candidates and those running the spectroscopic observations.

One advantage of the ESSENCE program is that?elds are imaged in multiple?lters,allowing for discrimination of targets by color.Tonry et al.(2003)present a table of expected SN Ia peak magnitudes as a function of redshift;see also Poznanski et al.(2002),Gal-Yam et al.(2004),Riess et al.(2004a),Strolger et al.(2004),and Smith et al.(2005)for discussions of color selection for SN candidates.Given apparent R-band and I-band magnitudes,one can calculate the R?I color and compare that with an expected color for those magnitudes.The cadence of the ESSENCE program(returning to the same?eld every four days)will likely catch SNe at early phases(i.e., before maximum brightness).Early core-collapse SNe are bluer than SNe Ia,as are AGNs.For example,when selecting for higher-redshift targets,objects with R?I 0.2mag were considered unlikely to be SNe Ia,while objects with R?I 0.4mag were made high priority for spectroscopic observation.The exact values of R?I used for selection depended on the observed R-band magnitude.This method was used more consistently in the last month of Year Two,reducing the fraction of spectroscopic targets that were identi?ed as AGNs from～10%over the lifetime of the project to～5%during that month.

The cadence of the ESSENCE program is designed to catch SNe early.At the start of an observing campaign or after periods of bad weather,though,we may have missed SNe during their rise to maximum brightness and only caught them while they are declining from maximum.If a target is brightening,then it is a higher priority than one that is not.This prioritization by phase of the SN became even more important when our Hubble Space Telescope(HST)program to observe some of the ESSENCE SNe Ia was active(see Krisciunas et al.2005).The response time of HST for a new target,even if the rough position on the sky is known from our chosen search?elds,is still on the order of several days.To ensure that HST was not generally looking at SNe Ia after maximum brightness,we would emphasize targets for spectroscopic identi?cation that appeared to be at an early epoch.In addition,we chose fainter objects,as higher-redshift SNe Ia were a prime motivation for HST photometry.The HST observations,while still targets of opportunity,were scheduled for speci?c ESSENCE search?elds,so new targets in those?elds were given the highest

priority.

The position of the SN in the host galaxy also in?uences the priority for observation.An optical transient located at the core of a galaxy is often an AGN,rather than an SN.The color selection described above is a less-biased predictor.In addition,even if the object is an SN,the signal of the SN itself is diluted by the light of the galaxy,making proper identi?cation di?cult. Objects that are well-separated from the host galaxy are given a higher priority.Being too far from the galaxy can,however,present another problem—the di?culty in obtaining a spectrum of the host in addition to the SN.Without a high signal-to-noise ratio(S/N)spectrum of the host,there is no precise measure of the redshift.This is especially true if the host galaxy cannot be included in the slit with the target,either to orient the slit at the parallactic angle or as a result of other observational constraints.In addition,host galaxies can be faint,so the large luminosity contrast with the SN makes detection of the host problematic(the so-called“hostless”SNe),although we did not reject any candidates solely for this reason.The best compromise is to have an object well separated from the host,but with the host still in the spectrograph slit.Without narrow-line features from the host(either emission or absorption lines),the redshift can be di?cult to determine.This lack of a host-galaxy spectrum became less of a concern,though,as we found that the SN spectrum itself is a relatively accurate,if less precise,measure of the redshift(see discussion below).The light curve alone can be used to estimate distances in a redshift-independent way (Barris&Tonry2004),but only with a well-sampled and accurate light curve.

The target selection process is complex and dynamic.Biases are introduced by some of the steps;for example,SN candidates near the centers of galaxies are less likely to be observed.Since the goal is to optimize the spectroscopic telescope time to identify SNe Ia in a speci?c redshift range,we have chosen these selection processes as our best compromise.The biases introduced may make the sample of SNe Ia identi?ed problematic for uses in statistical studies of the nature of SNe Ia at high redshift.

3.Observations

Spectroscopic observations of ESSENCE targets were obtained at a wide variety of telescopes: the Keck I and II10m telescopes,the VLT8m telescopes,the Gemini North and South8m telescopes,the Magellan Baade and Clay6.5m telescopes,the MMT6.5m telescope,and the Tillinghast1.5m telescope at the F.L.Whipple Observatory(FLWO).The spectrographs used were LRIS(Oke et al.1995)with Keck I,ESI(Sheinis et al.2002)with Keck II,FORS1with VLT (Appenzeller et al.1998),GMOS(Hook et al.2002)at Gemini(North and South),IMACS(Dressler 2004)with Baade,LDSS2(Mulchaey2001)with Clay,the Blue Channel(Schmidt et al.1989)at MMT,and FAST(Fabricant et al.1998)at FLWO.Nod-and-shu?e techniques(Glazebrook& Bland-Hawthorn2001)were used with GMOS(North and South)and IMACS to improve sky subtraction in the red portion of the spectrum.

Standard CCD processing and spectrum extraction were accomplished with IRAF17.Most of the data were extracted using the optimal algorithm of Horne(1986);for the VLT data,an alternative extraction method based upon Richardson-Lucy restoration(Blondin et al.2004)was employed.Low-order polynomial?ts to calibration-lamp spectra were used to establish the wave-length scale.Small adjustments derived from night-sky lines in the object frames were applied.We employed IRAF and our own IDL routines to?ux calibrate the data and,in most cases,to remove telluric lines using the well-exposed continua of the spectrophotometric standards(Wade&Horne 1988;Matheson et al.2000).

4.Target Identi?cation

Once a calibrated spectrum is available,the next step is to properly classify the object.For brighter objects that yield high S/N spectra,an SN is often easy to distinguish and classify.Most of the ESSENCE targets are faint enough to be di?cult objects even for large-aperture telescopes.The resulting noisy spectra can be confusing.Even for well-exposed spectra,though,exact classi?cation can occasionally still be challenging.

For SNe,the classi?cation scheme is based upon the optical spectrum near maximum brightness (Filippenko1997).Type II SNe are distinguished by the presence of hydrogen lines.The Type I SNe lack hydrogen,and are further subdivided by the presence or absence of other features.The hallmark of SNe Ia is a strong Si IIλ6355absorption feature.Near maximum brightness,this absorption is blueshifted by～10,000km s?1and appears near6150?A.In SNe Ib,this line is not as strong,and the optical helium series dominates the spectrum.The SNe Ic lack all these identifying lines.

At high redshift,the Si IIλ6355feature is at wavelengths inaccessible to optical spectrographs, so the identi?cation relies upon the pattern of features in the rest-frame ultraviolet(UV)and blue-optical wavelengths.The Ca II H&Kλλ3934,3968doublet is a distinctive feature in SNe Ia,but it is also present in SNe Ib/c,so the overall pattern is important for a clear identi?cation as a SN Ia. Other important features to identify SNe Ia include Si IIλ4130,Mg IIλ4481,Fe IIλ4555,Si III λ4560,S IIλ4816,and Si IIλ5051(see,e.g.,Coil et al.2000;Je?ery et al.1992;Kirshner et al. 1993;Mazzali et al.1993).

The?rst stage of classi?cation is done by eye.Drawing upon the extensive experience of the spectroscopic observers associated with ESSENCE,we can provide a solid evaluation of the spectrum.Objects such as AGNs and normal galaxies are fairly easy to distinguish.The SNe Ia are also often clear,but some fraction of the data will require more extensive analysis.The?rst step is simply to make certain that the collective expertise is used,rather than just the individual

at the telescope.Spectroscopic results are widely disseminated via e-mail and through an internal web page,allowing rapid examination of any questionable spectrum by the entire collaboration. Broad discussion often leads to a consensus.

In addition to the traditional by-eye approach,we employ automated comparisons.If the object is likely to be a SN Ia,and if the S/N ratio is su?ciently high and the rest-wavelength coverage appropriate,we can use a spectral-feature aging routine(Riess et al.1997)that compares speci?c components of the SN Ia spectrum with a library of SN Ia spectra at known phases.This can pin down the epoch of a SN Ia to within a few days.This program,though,is limited to normal SNe Ia (i.e.,not spectroscopically peculiar objects,which are often overluminous or underluminous).In addition,it does not identify objects that do not match the Type Ia SN spectra in the library.

For a more general identi?cation routine,we use an algorithm called SuperNova IDenti?cation (SNID;Tonry et al.2005).This program takes the input spectrum and compares it against a library of objects of many types.The templates include SNe Ia of various luminosity classes and at a range of ages,core-collapse SNe,and galaxies.The o?set in wavelength caused by redshift is a free parameter,so the output includes an estimate of the redshift of the object.The routine compares the input with the library and returns the most likely match.The comparison is weighted by the amount of overlap between the input spectrum and the template.For a subset of the objects ( 10%),the SNID comparison is not optimal.This may be the result of contamination by galaxy light,the lack of a matching template in the SNID library,poor S/N of the spectrum in question, or a problem in the routine.All SNID comparisons are checked by eye for a qualitative judgment of the goodness of?t.

The redshift of the object can also be directly determined from the spectrum itself if narrow emission or absorption lines associated with the host galaxy are present.Occasionally,observations are set up to include the host galaxy in the spectrograph slit speci?cally for the purpose of obtaining a redshift.If there is a strong enough signal of a galaxy spectrum,but no clearly identi?able narrow emission or absorption lines,cross-correlation with an absorption template could be used.For the spectra that had narrow emission or absorption lines(or were cross-correlated with a template), we report the redshift to three signi?cant digits.If the redshift determination is based solely on a comparison of the SN spectrum to a low-redshift analog,the redshift is less certain,and we only report the value to two signi?cant digits.

For the objects with a more precise redshift derived from the host galaxy,we can compare the galactic redshift with the value of the redshift estimated by SNID.Figure1shows that the SNID redshifts agree well with the galaxy redshifts.Thus,for objects without precise redshifts from host galaxy spectra,the SNID redshifts can be used as reliable substitutes.In the cases where SNID did not agree with a galaxy redshift,we forced the redshift to match in order to?nd the best-?tting template,but all the supernova-based redshifts reported in this paper correspond to the“un-forced”SNID result.

Fig.1.—Comparison of redshifts as determined by SNID and from narrow emission or absorption lines in the host-galaxy spectrum.Qualitative grades for the?ts in SNID are assigned and the good?ts(solid circles)are shown as well as the poor?ts(open circles).The dispersion around one-to-one correspondence of the redshifts for the good data is excellent,withσ=0.009(when no errors are assumed for the SNID output).There is one outlier(b004)for which the redshift determination using SNID is highly degenerate as it is likely to be a peculiar SN Ia(see text); we do not show b004in the residual plot for the sake of clarity.The error bars in the lower plot correspond toσgood.Note that the mean residual is～10?4?σgood,which shows that there are

no systematic e?ects associated with the use of SNID in determining the SN redshift.

5.Results

The results of our spectroscopic observations during the?rst two years of the ESSENCE program are summarized in Table1.There are46SNe Ia(and5additional likely SNe Ia),along with5core-collapse SNe.Note also that there were54transients in the?rst two years that were not observed spectroscopically.Through the target selection methods described in Section2,we were able to prioritize the more likely candidates,but many of these were not observed solely because of the lack of su?cient spectroscopic resources.This became more of an issue toward the end of Year Two,when good weather and increasingly e?cient detection algorithms increased the number of transients discovered.

The goal of the ESSENCE project is to?nd～200SNe Ia over the redshift range0.2 z 0.8.In Figure2,we show the actual distribution in redshift of the SNe Ia from the ESSENCE project that are spectroscopically con?rmed.There are SNe over the entire targeted redshift range, although there are fewer at the high end(z 0.6).A signi?cant fraction of the signal of w is accessible at z≈0.5(Miknaitis et al.2005),but a goal for the last three years of the program is to ensure that the SNe Ia observed spectroscopically are distributed optimally over our targeted redshift range.This highlights the importance of the8-10m telescopes such as Gemini,the VLT, and Keck that are critical to spectroscopy of the faint objects at the high-redshift end of our range.

Both SNID and the spectral-feature aging method described in Section4give an indication of the age of the SN Ia.Light curves will provide a more precise measure of the age of the SN at the time of the spectroscopy,but an estimate of the epoch of the spectrum to within a few days is possible from the spectral features alone.Figure3shows the distribution in age(relative to maximum brightness)at the time of spectroscopy(not discovery,as spectra are often taken up to several days after discovery).In the15cases18where we have spectra of the same SN Ia at multiple epochs,the relative ages are consistent with the times of the spectroscopic exposures (also considering the e?ects of cosmological time dilation and probable errors of the?ts of～±3 days).There is one exception to this consistency(b027),but at later epochs when the spectra are changing less.

Table2is a list of all ESSENCE targets that were selected for spectroscopic identi?cation. The results for these?rst two years include52SNe Ia or likely SNe Ia(Figure4),4SNe II(Figure 5),1SN Ib/c(Figure5),12AGNs(Figure6),4possibly variable stellar objects(Figure7),19 galaxies(Figure8),and16objects of unknown classi?cation(Figure9).There were10objects for which we pointed the telescope at the target and did not get a spectrum,either because of poor sky conditions or the target was actually a solar-system object and had moved out of the?eld.

No attempt has been made to remove host-galaxy contamination for any object presented in Figures4and5.The amount of galaxy light is signi?cant for some objects(e.g.,f221on Figure4d).

Fig.2.—Redshift distribution of spectroscopically identi?ed SNe Ia from the?rst two years of the ESSENCE project.The SNe for which we judge that the SNID?t is good are indicated by the

cross-hatched area,while those that were poor?ts are indicated by the blank spaces.

Fig.3.—Age distribution(relative to maximum brightness)of spectroscopically identi?ed SNe Ia from the?rst two years of the ESSENCE project.Ages are determined from spectroscopic features alone.The SNe for which we judge that the SNID?t is good are indicated by the cross-hatched area,while those that were poor?ts are indicated by the blank spaces.For objects with multiple

epochs of spectroscopy,this?gure only re?ects the?rst spectrum.

3000

4000

500060007000

8000

Rest Wavelength (?)

2

4

68

10

S c a l e d f λ + C o n s t a n t

z = 0.11

b003z = 0.16d100z = 0.164

e0202003?10?27z = 0.20d0862003?11?27

z = 0.20d086z = 0.21d099z = 0.231b004z = 0.244

e132z = 0.25b017z = 0.296

d117Fig.4a.—Rest-wavelength spectra of SNe Ia (or likely SNe Ia)from the ?rst two years of the ESSENCE project in order of increasing redshift.Each ESSENCE SN (black line )is overplotted by a low-redshift SN Ia (blue line )for comparison.In addition,each spectrum is labeled with the ESSENCE identi?cation number and the deduced redshift.Spectra of the uncertain SNe Ia are indicated with an asterisk (*).The deredshifted regions of the spectra that are strongly a?ected by atmospheric absorption are shown in red.The ?ux scale is f λwith arbitrary additive o?sets

3000

400050006000

7000

Rest Wavelength (?)

2

4

68

S c a l e d f λ + C o n s t a n t

2002?11?11

z = 0.32b0272002?12?06z = 0.32b0272002?12?07

z = 0.32b027z = 0.33b016z = 0.33

d0832003?11?19z = 0.335e0292003?11?22

z = 0.335e029z = 0.339d149z = 0.340

d087Fig.4b.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.The 2003-01-03spectrum of c012is a weighted average of the Clay and GMOS spectra.

2000

3000

400050006000

Rest Wavelength (?)

2468

10S c a l e d f λ + C o n s t a n t

2002?12?04

z = 0.348c0122003?01?05

z = 0.348

c0122002?12?07z = 0.356c0152003?01?05

z = 0.356

c015z = 0.360

e1362003?10?30

z = 0.363d0932003?11?23

z = 0.363d093z = 0.39f308*z = 0.399

c023

Fig.4c.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.The spectrum of f076is a weighted average of the MMT and KI/LRIS spectra.

2000

3000

400050006000

Rest Wavelength (?)

2

46810

S c a l e d f λ + C o n s t a n t

z = 0.405

d085z = 0.408f096z = 0.406

f076z = 0.417f235z = 0.427

e148

2002?11?08

z = 0.427b013

2002?12?07z = 0.427b013z = 0.429

d0892002?11?09

z = 0.43

b0202002?12?09z = 0.43b020Fig.4d.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.

2000

3000

4000

5000

6000

Rest Wavelength (?)

2468

10

S c a l e d f λ + C o n s t a n t

z = 0.442

f221*z = 0.45

d097

2003?11?20

z = 0.47e1082003?11?21z = 0.47e108

2002?11?06

z = 0.49b008

2002?11?0z = 0.49

b008z = 0.51

e149*z = 0.52f301*2002?11?09

z = 0.52b0222002?12?05z = 0.52b022Fig.4e.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.

2000

30004000

5000

Rest Wavelength (?)

2

4

6

8

10

S c a l e d f λ + C o n s t a n t

z = 0.522

d084z = 0.524d033z = 0.54f0112002?11?11z = 0.54b0232002?12?03

z = 0.54b023z = 0.544f2442002?12?02

z = 0.56c0032002?12?07z = 0.56c003z = 0.56

f041z = 0.583

d058Fig.4f.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.

20003000

4000

5000

Rest Wavelength (?)

2

4

6

8

10

12

S c a l e d f λ + C o n s t a n t

2002?11?06

z = 0.587b0102002?11?11

z = 0.587b0102002?12?06z = 0.587b010z = 0.596

f216z = 0.606

e140z = 0.61e138z = 0.63

f231z = 0.64

e147z = 0.78

e531*z = 0.79

e315*Fig.4g.—Rest-wavelength spectra of ESSENCE SNe Ia as in Figure 4a.The GMOS and VLT spectra of b010have been combined.

3000

4000

500060007000

8000

Rest Wavelength (?)

2

4

S c a l e d f λ + C o n s t a n t

z = 0.074

e022z = 0.099e141z = 0.213c022*z = 0.27

b006*z = 0.08d010Fig.5.—Spectra of SNe II and one SN Ib/c from the ?rst two years of the ESSENCE project.Each spectrum is labeled with the ESSENCE identi?cation number and the deduced redshift.Spectra of uncertain SNe II are indicated with an asterisk (*).The deredshifted regions of the spectra that are strongly a?ected by atmospheric absorption are shown in red.The ?ux scale is f λwith arbitrary additive o?sets between the spectra.The SN Ib/c is d010=SN 2003jp.

认知心理学复习重点

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包装结构与包装装潢设计作业题参考答案 包装结构预包装装潢设计作业参考答案 一、单项选择 1、D 2、D 3、B 4、B 5、C 6、D 7、B 8、C 9、A 10、C 11、B 12、B 13、C 14、D 15、A 16、B 17、B 18、D 19、D 20、D 21、D 22、D 23、C 24、A 25、B 二、多项选择题 1、ABCD 2、ABC 3、ABCD 4、ABCD 5、ACD 6、ABC 7、ABC 8、ABCD 9、ABCD 10、ABC 11、ABCD 12、ABCD 13、ABCD 14、ABC 15、AD 16、BCD 17、BD 18、AC 三、填空题 1. 图形设计、文字设计 2. 包装装潢设计 3. 立体造型、包装样式 4. 商品的属性 5. 宋体字、粗黑体、绍线体 6. 具象图形、抽象图形 7. 插图、摄影技巧8. 装饰图形9. 形象代言人10. 主题明确、言简意明 11.图形、文字、空白12. 图形设计、文字设计13. 防护功能、装潢功能 14. 图案、情谊15. 品牌信息16. 人性化设计17. Photoshop 18.包装19. 包装容器造型设计20. 定位设计21.包裹 22.法国23.宝洁24.以人为本256、厚板纸盒方型、多棱型、特殊异型盒。折叠纸盒26、象图形，装饰图形。27、品牌、产品 28、促进商品销售 29、变化与统一、对比与调和、整体与局部、生动与稳定、视与错觉。30、箱、桶、罐；金属、陶瓷；食品、饮料、日用品等；充气、收缩 31、容纳、保护、便利、促销32、容器造型设计、装潢设计。 33、技术、形式、画面构成34、直观、感染力强 35、189136、可口可乐37、生产者38、品牌 39、箱体造型、内部结构、封口 四、名词解释 1. 适量包装：主要是指采用单件适量的包装，以方便各种不同的需求，也是为了控制一次性使用的数量，以避免有些产品一次消费不完而造成浪费。 2.系列化包装：是国际包装设计中较为普遍和流行的形式，它是一个企业或一个商标、牌号的不同种产品，用一种共性特征来统一的设计。 3.成套包装：是指将不同种类的商品或相似种类的商品进行成套包装的形式，它的对象可以是一起生产、一起陈列、一起销售、一起使用的。 式：就是实点广告或现场广告方式，通过纸盒结构的部分增加或延展．使纸盒结构具有保护商品的功能，又具有促销功能与展示效果。 5. 原始形态的包装：这些未做加工或仅做简单的加工就被用来盛放或贮存生活必需品的自然物，就是原始形态的包装。 6.间接表现：是比较内在的表现手法，即画面上不出现要表现的对象本身，而是借助于其他有关事物来表现该对象，这种手法具有更加宽广的表现余地，在构思上往往用于表现内容物的某种属性或牌号，意念等。

SJ-M 《表白》 歌词

表白(Off My Mind) Henry SOLO Girl 我一看到你，I go Cra Cra Crazy 我只想要你做我的Baby 我想看透你的心但是我没有办法， 我可不可以牵你的手？ 也许你也正在想著我， You got me goin crazy, crazy, crazy, yea 如果我们在一起，做什麽都愿意 Oh Baby baby baby 我的爱，全都给你 我就在这裏 我的心，不会放弃 你是我唯一 Girl 这不是意外，你是我的女孩 I can't get my mind off ya, off ya 我的爱，全都给你 我就在这裏 我的心，不会放弃 你是我唯一 Girl 这不是意外，你是我的女孩 I can't get my mind off ya, off ya (off my mind) 天塌下来无所谓，一定不后悔， 在大的事都有我背(有我Babeh）

只要说一声ok，就跟我走 So take my hand and baby don't let go 也许你也正在想著我， You got me goin crazy, crazy, crazy, yea 如果我们在一起，做什麽都愿意 Oh Baby baby baby 我的爱，全都给你 我就在这裏 我的心，不会放弃 你是我唯一 Girl 这不是意外，你是我的女孩 I can't get my mind off ya, off ya 我的爱，全都给你 我就在这裏 我的心，不会放弃 你是我唯一 Girl 这不是意外，你是我的女孩 I can't get my mind off ya, off ya (off my mind) Oh 我要怎麽对你说，(我要怎麽对你) 到底要该怎麽做？(到底要该怎麽) 付出的够不够， 对你的感情太重~ 太重~ (My Love)

Super Junior-U音译歌词

U cause I can't stop yeah with Double J here we go 始源】：闹了桥/莫给/推有搜 闹我那/级按口/肯带/苏嘎/衣丝嘎 韩庚】：课咯K/破级马 那我哎/给木~啊级/西加/够内搜 希澈】：那也改扫/他不/乔乃吧 闹呀一桑要/恰加吧/就太你 丽旭】：课那/加嘎/乃嘎duai改海/就太你 ALL】：cuz i can't stop thinking about u g irl 强仁】：no类够罗/嘛对够呀~ ALL】：no i can't stop thinking about u gi rl 李特】：内无里雅内/卡度够西剖 希澈】：播呀桃/怒有/皮比不 Kin冒里个太/那嘛一嫩酿gi瓦 圭贤】：那级码/看摸/扫里罗 (那儿)共giu卡你/那里giu苏no搜oh yeah~

艺声】：no dei给/博要窘magic 拜干将米索给/送giu动半级路求给 东海】：课组win一/你嘎dui改海/组太你 ALL】：cuz i can't stop thinking about u g irl 韩庚】：闹瓦喊给/一够西剖 ALL】：no i can't stop thinking about u gi rl 东海】：那留gi图过/卡博里级马 ALL】：cuz i can't stop thinking about u g irl 晟敏】：哦内够楼/满读够呀 no i can't stop thinking about u girl 始源】：内无里雅内/卡度够西剖 RAP】:到也那扫/想个哎扫出跑奥料 爬啦报呢/课戴/怒比西戴西咋be/唔料 起唔料/海到扫用/袄西个到袄西 闹了哈渺/她料乃嘎/课戴了卡改扫 闹里kin为海扫/冒等高她/课高 穷不一课但/那海到 一米改问下等能高/恰啊啦到

模板匹配

图像模式识别中模板匹配的基本概念以及基本算法 认知是一个把未知与已知联系起来的过程。对一个复杂的视觉系统来说，他的内部常同时存在着多种输入和其他知识共存的表达形式。感知是把视觉输入与事先已有表达结合的过程，而识别与需要建立或发现各种内部表达式之间的联系。匹配就是建立这些联系的技术和过程。建立联系的目的是为了用已知解释未知。（摘自章毓晋《图像工程》） 1、模板匹配法： 在机器识别事物的过程中，常常需要把不同传感器或同一传感器在不同时间、不同成像条件下对同一景象获取的两幅或多幅图像在空间上对准，或根据已知模式到另一幅图像中寻找相应的模式，这就叫匹配。在遥感图像处理中需要把不同波段传感器对同一景物的多光谱图像按照像点对应套准，然后根据像点的性质进行分类。如果利用在不同时间对同一地面拍摄的两幅照片，经套准后找到其中特征有了变化的像点，就可以用来分析图中那些部分发生了变化；而利用放在一定间距处的两只传感器对同一物体拍摄得到两幅图片，找出对应点后可计算出物体离开摄像机的距离，即深度信息。 一般的图像匹配技术是利用已知的模板利用某种算法对识别图像进行匹配计算获得图像中是否含有该模板的信息和坐标； 2、基本算法： 我们采用以下的算式来衡量模板T（m,n)与所覆盖的子图Sij（i,j)的关系，已知原始图像S(W,H)，如图所示： 利用以下公式衡量它们的相似性： 上述公式中第一项为子图的能量，第三项为模板的能量，都和模板匹配无关。第二项是模板和子图的互为相关，随（i,j）而改变。当模板和子图匹配时，该项由

最大值。在将其归一化后，得到模板匹配的相关系数： 当模板和子图完全一样时，相关系数R(i,j) = 1。在被搜索图S中完成全部搜索后，找出R的最大值Rmax(im,jm)，其对应的子图Simjm即位匹配目标。显然，用这种公式做图像匹配计算量大、速度慢。我们可以使用另外一种算法来衡量T和Sij的误差，其公式为： 计算两个图像的向量误差，可以增加计算速度，根据不同的匹配方向选取一个误差阀值E0，当E(i,j)>E0时就停止该点的计算，继续下一点的计算。 最终的实验证明，被搜索的图像越大，匹配的速度越慢；模板越小，匹配的速度越快；阀值的大小对匹配速度影响大； 3、改进的模板匹配算法 将一次的模板匹配过程更改为两次匹配； 第一次匹配为粗略匹配。取模板的隔行隔列数据，即1/4的模板数据，在被搜索土上进行隔行隔列匹配，即在原图的1/4范围内匹配。由于数据量大幅减少，匹配速度显著提高。同时需要设计一个合理的误差阀值E0： E0 = e0 * (m + 1) / 2 * (n + 1) / 2 式中：e0为各点平均的最大误差，一般取40~50即可； m,n为模板的长宽； 第二次匹配是精确匹配。在第一次误差最小点（imin, jmin)的邻域内，即在对角点为（imin -1, jmin -1), (Imin + 1, jmin + 1)的矩形内，进行搜索匹配，得到最后结果。

辑SuperJunior05歌词中韩音译3对照

1.Miracle Life couldn’t get better Life couldn’t get better [??希澈] ???????????????(Without you baby) [??希澈] 迄今为止没有你的生活那样黑暗(Without you baby) [??希澈] Jigumkaji no obdon shiganun odumiojyo (without you baby) [??始源] ???????????????(baby) [??始源] 见到你后我的生活仿如做梦(baby) [??始源] Norul mannan hu naui senghwarun kumman gathayo (baby) [??韩庚] ???????(?????) a Miracle (a Miracle) ???????????? [??韩庚] 第一次见到你的瞬间(见到你的瞬间)a Miracle (a Miracle) 我能感受到奇迹就是你 [??韩庚] Norul chum bon sungan (choum bon sungan)a miracle (a miracle) nannukkyojyo gijogun baro norangol [All] Life couldn't get better(hey) [All] Life couldn't get better(hey) [??晟敏] ????????????????(ho) ?????????Life couldn't get better(hey) [??晟敏] 我把你拥在怀里飞向蓝色的天空(ho) 亲吻熟睡的你Life couldn't get better(hey) [??晟敏] Nan nol pume ango nara，jamdun noui ib machul koya， Life couldn't get better [??丽旭] ?????????????????，Life couldn't get better [??丽旭] 向我敞开你的心请紧握我的手，Life couldn't get better [??丽旭] Noui mame munul yoro jwo，Life couldn't get better [??东海] ??????????????????(a holiday) [??东海] 原来很平凡的一天现在变的不同(a holiday) [??东海] Meil meil pyongbomhetton nal duri ijen dalla jyossoyo (a holiday) [??李特] ??????????????(I wanna thank you，baby) [??李特] 世上所有的人看起来都很幸福(I wanna thank you，baby) [??李特] Sesang modun saramduri hengboghe boyoyo (I wanna thank you baby) [??丽旭] ???????(???????) a miracle (a miracle)，

包装装潢设计_课程设计说明书

目录 1 绪论 2 1.1 设计思路的提出 2 1.2 设计的意义 2 2 旅游基本情况 3 2.1 旅游资源情况 3 2.2 旅游发展情况 3 3 旅游明信片的概念与发展 5 3.1 旅游明信片的概念 5 3.2 旅游明信片的发展 5 4 明信片设计方案 6 4.1 明信片设计前市场调查 6 4.1.1 市场调查6 4.1.2 调查问卷（见附件） 6 4.1.3 调查结果6 4.2 明信片设计中的定位 7 4.3 明信片设计方案的整体说明 7 4.4 明信片设计中的图片 7 4.5 明信片设计中的文字 11 4.6 明信片设计中的结构 12 4.7 图纸 14 参考文献 18 附件（调查问卷） 19

旅游明信片系列化设计 1 绪论 灵秀声名远扬，长江三峡驰名世界。道教名山武当山为道教圣地。中国南水北调中线工程水源地，亚洲最大的人工湖，被誉为“亚洲天池”的丹江口水库。避暑胜地九宫山、闯王陵。地质公园隐水洞。号称“华中屋脊”和“绿色宝库”的神农架。“鸽子花的故乡”，美丽的后河自然保护区。人文旅游景观具有时代跨度大，历史价值高的特点，那里既有古人类长阳人遗址，屈家岭文化遗址，又有众多的古三国胜迹和楚都遗址“纪南城”；既有辛亥革命遗址起义门、阅马场、又有中央农民运动讲习所旧址及八七会议会址。文物古迹与革命胜迹遍布全省。 但是由于截至目前为止我省旅游业的发展和宣传推广主要是依靠新闻媒体(电视、报纸、电台)、书籍、网络等传播形式，使得所取得的旅游业绩却并不是非常理想，旅游没有真正形成一个统一的视觉形象。影响了旅游文化形象和产品的宣传推广。 将旅游宣传与明信片结合起来，有利于宣传和推广旅游概念和景区品牌创建，有利于游客加深理解旅游特色。 1.1 设计思路的提出 由黄鹤楼游玩归来发现虽然黄鹤楼已经采用门票与明信片结合的方式，但是单一的景点不利于形成整体影响，不利于游客形成对旅游的概念理解。所以本文构思将旅游利用明信片的手段进行宣传。 1.2 设计的意义 将“灵秀”这一概念与明信片这种宣传方式有机的结合起来，将旅游以视觉形象的概念推向全国，有利于整个旅游业的发展。 截至目前为止我省旅游业的发展和宣传推广主要是依靠新闻媒体(电视、报纸、电台)、书籍、网络等传播形式，使得所取得的旅游业绩却并不是非常理想，在当今旅游业一片蓬勃的时候，不发展甚至发展速度慢就等于落后。 本文设计意欲将丰富的旅游资源以形象而富有纪念意义的明信片套装的形式宣传出去，让更多的人了解，了解旅游。

Super junior M 太完美专辑歌词

Super junior M 太完美 太完美 东海：她迷住我视线她迷住我视线 始源：在爱情里的宝藏被我发现 你就是我寻找的稀世宝贝 圭贤：你就不断地在正反我世界 连冰块遇见你都燃起火焰 Herry 银赫：太过心急不对用力爱会碎 太过缓慢不对我随你进或退 东海：oh 太完美你眼里我出现 Oh 不让谁替我在你身边woo woo wu o 周觅：你的眉眼你的侧脸你的颈间你的妩媚你的一切从头到尾我已沦陷 圭贤：我的心变成了口袋的一面

Just for you 不停地给不停地给 丽旭：这样子爱你到底是对不对 我一边疑惑一边更加迷恋 晟敏银赫：太过心急不对用力爱会碎太过缓慢不对我随你进或退圭贤：oh ~ 太完美你眼里我出现 Oh ~ 不让谁替我在你身边woo wo u o Herry 银赫：你的眉眼你的侧脸你的颈间你的妩媚 你的一切从头到尾我已沦陷 合声：Oh~ 太完美Oh~ 不让谁 周觅：每次见面时脉搏就当机了她在我全身狂跳不由己 银赫：一直跳一直跳想见你 东海：一直跳一直跳喜欢你 一直跳一直跳都是你 一直跳一直跳我爱你 一直跳一直跳一直跳一直跳 合声：太过心急不对用力爱会碎太过缓慢不对我随你进或退 始源：oh 太完美你眼里我出现 Oh 不让谁替我在你身边woo woo wu o 圭贤：你的眉眼你的侧脸你的颈间你的妩媚 你的一切从头到尾我已沦陷 银赫：Bounce to the music let your feet go round

To the floor and I’m a break it down Let me in let me show you all my bling bling And all my kicks kicks baby dance with me Herry：Boom Boom Boom Can I get another clap clap clap Let’s go shake your body move your body Pick feet now I’m moving to the groove baby （丽旭：yeah~！！） I’m going out 东海：给我说你想我给我说你爱我 给我说你想我说你想我给我说你爱我（圭贤：yeah~~！） 给我说你想我给我说你爱我 给我说你想我给我说你想我给我说你爱我 幸福微甜 圭贤：这城市夜晚闹哄哄人潮像快转的时钟 这不是我要的感动廉价的妆都太浓 这感觉我不知怎么形容 周觅：街道上闪烁的霓虹就像是短暂的笑容 能不能给我一分钟安安静静跟你沟通

图像匹配程序设计——模板匹配

摘要 模板匹配就是把不同传感器或同一传感器在不同时间、不同成像条件下对同一景物获取的两幅或多幅图像在空间上对准,或根据已知模式到另一幅图中寻找相应模式的处理方法。模板匹配是数字图像处理的重要组成部分之一。简单而言，模板就是一幅已知的小图像。模板匹配就是在一幅大图像中搜寻目标，已知该图中有要找的目标，且该目标同模板有相同的尺寸、方向和图像，通过一定的算法可以在图中找到目标，确定其坐标位置。 本文主要主要介绍了灰度相关的匹配方法，灰度相关的图像匹配算法是图像匹配算法中比较经典的一种，很多匹配技术都以它为基础进行延伸和扩展。它是从待拼接图像的灰度值出发，对待匹配图像中一块区域与参考图像中的相同尺寸的区域使用最小二乘法或者其它数学方法计算其灰度值的差异，对此差异比较后来判断待拼接图像重叠区域的相似程度，由此得到待拼接图像重叠区域的范围和位置，从而使用MATLAB软件实现图像匹配。 当以两块区域像素点灰度值的差别作为判别标准时，最简单的一种方法是直接把各点灰度的差值累计起来。另一种方法是计算两块区域的对应像素点灰度值的相关系数，相关系数越大，则两块图像的匹配程度越高。该方法的匹配效果要更好，匹配成功率有所提高。 关键词：图像匹配；MATLAB；灰度相关

目录 1 需求分析 (1) 1.1 问题描述 (1) 1.2 基本要求 (1) 2 设计方案 (2) 2.1 相关概念 (2) 2.2 算法设计 (2) 3 仿真内容 (5) 3.1 相关函数说明 (5) 3.2 模版匹配源代码 (8) 4 仿真结果及分析 (9) 结束语 (11) 参考文献 (12)

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Super Junior - Bonamana中文、韩文及罗马拼音对照歌词

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基于模板匹配算法的数字识别

中南民族大学 毕业论文(设计) 学院: 计算机科学学院 专业: 软件工程年级:2009 题目: 基于模板匹配算法的数字识别学生姓名: 李成学号:09065093指导教师姓名: 李波职称: 讲师 2013年5月

中南民族大学本科毕业论文（设计）原创性声明 本人郑重声明：所呈交的论文是本人在导师的指导下独立进行研究所取得的研究成果。除了文中特别加以标注引用的内容外，本论文不包含任何其他个人或集体已经发表或撰写的成果作品。本人完全意识到本声明的法律后果由本人承担。 作者签名：2013年月日

摘要 (1) Abstract (1) 1 绪论 (2) 1.1 研究目的和意义 (2) 1.2 国内外研究现状 (2) 2 本文基本理论介绍 (3) 2.1 位图格式介绍 (3) 2.2 二值化 (3) 2.3 去噪 (3) 2.4 细化 (4) 2.5 提取骨架 (4) 3 图像的预处理 (5) 3.1 位图读取 (5) 3.2 二值化及去噪声 (5) 3.3 提取骨架 (6) 4 基于模板匹配的字符识别 (8) 4.1 样本训练 (8) 4.2 特征提取 (8) 4.3 模板匹配 (9) 4.4 加权特征模板匹配 (10) 4.5 实验流程与结果 (10) 5 结论 (16) 5.1 小结 (16) 5.2 不足 (16) 6 参考文献 (17)

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