Testing intermediate-age stellar evolution models with VLT photometry of LMC clusters. I. T

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a r X iv:as tr o -p h /0307556v 1 31 J u l 2003Astronomy &Astrophysics manuscript no.LSB˙accept February 2,2008(DOI:will be inserted by hand later)Starburst in HS 0822+3542induced by the very blue LSB dwarfSAO 0822+3545S.A.Pustilnik 1,4,A.Y.Kniazev 1,2,4,A.G.Pramskij 1,4,A.V.Ugryumov 1,4,and J.Masegosa 31Special Astrophysical Observatory RAS,Nizhnij Arkhyz,Karachai-Circassia,369167Russia 2Max Planck Institut f¨u r Astronomie,K¨o nigstuhl 17,D-69117,Heidelberg,Germany3Instituto de Astrofisica de Andaluc ´ia,Granada,Spain4Isaac Newton Institute of Chile,SAO BranchReceivedFebruary 26,2002;acceptedJuly 30,2003Abstract.One of the most metal-deficient blue compact galaxies (BCGs)HS 0822+3542(Z =1/34Z ⊙),is also one of the nearest such objects (D ∼11Mpc).It is in addition well isolated from known bright galaxies.A trigger mechanism for its current star-formation (SF)burst has thus remained unclear.We report the discovery of a veryblue ((B −V )0tot =0.08and (V −R )0tot =0.14)low surface brightness (LSB)(µ0B 23.m 4arcsec−2)dwarf irregular (dIrr)galaxy,which we have named SAO 0822+3545.Its small relative velocity and projected distance of only ∼11kpc from the BCG imply their physical association.For this LSB dIrr galaxy,we present spectroscopic results,total B,V,R magnitudes,and the effective radii and surface brightness (SB),and we describe its morphological properties.We compare the very blue colours of this dwarf with PEGASE.2models of the colour evolution of a Z =1/20Z ⊙stellar population,and combine this analysis with the data on the LSBD EW (H α)values.The models best describing all available observational data depend on the relative fraction of massive stars in the IMF used.For a Salpeter IMF with M up =120M ⊙,the best model includes a “young”single stellar population (SSP)with an age of ∼10Myr and an “old”SSP with the age of ∼0.2–10Gyr.The mass ratio of the old to young components should be in the range of 10to 30.If the age of the old component is more than ∼1Gyr,an additional coeval component of “intermediate”age (∼100Myr)with a mass comparable to that of the “young”population,although not required,provided a good fit to the current data.For the two options of a model IMF biased toward the low-mass end,the best match of the observed BV R and EW(H α)is for continuous star-formation rate (SFR)single-component models,with SF durations in the range of ∼0.1to ∼1Gyr.However,only a longer time-scale SF gives the stellar mass,compatible with the LSB galaxy mass estimates.Nevertheless,such a scenario would be inconsistent with the recent encounter of these two dwarfs.The role of interaction between the LSBD and BCG HS 0822+3542in triggering their major SF episodes during the last ∼100–200Myr is emphasized and discussed.For the BCG,based on the results of new spectroscopy with the Russian 6m telescope,we estimate the physical parameters of its SF region and present the first evidence of an ionized gas supershell.This pair of dwarfs lies deep within the nearby Lynx-Cancer void,with the nearest bright (L >L ∗)galaxies at distances >3Mpc.This is probably one of the main factors responsible for the unevolved state of HS 0822+3542.Key words.galaxies:star formation –galaxies:low surface brightness –galaxies:interaction –galaxies:photometry –galaxies:abundances –galaxies:individual (HS 0822+3542,SAO 0822+3545)–large-scale structure1.IntroductionA few known blue compact galaxies (BCGs)with ex-tremely low metallicities (1/50to 1/20Z ⊙)are considered to be the best candidates for truly young local low-mass galaxies,in which we are witnessing the first star forma-tion episode,with the oldest stars formed less than ∼100–200Myr ago.The best known examples are SBS 0335−052(Izotov et al.1997;Papaderos et al.1998;Pustilnik et al.2001a),and I Zw 18(Searle &Sargent 1972;Izotov1Note that debates on the possible youth of these BCGsstill continue in the literature (see,e.g.,the most recent ¨Ostlin2000;¨Ostlin &Kunth 2001;Kunth &¨Ostlin 2001).2S.A.Pustilnik et al.:Starburst in HS0822+3542induced by SAO0822+3545van Zee et al.1998,Izotov et al.2001).This,presumably, is a key moment of their history.Moreover,it is probably not by chance that in both the cases of Dw1225+0152 and SBS0335−052E the nearest neighbour is very gas-rich,and either is an H i cloud without any hint of past star formation(as in the case of Dw1225+0152,Salzer et al.1991),or is also an extremely metal-deficient,proba-bly truly young,blue compact galaxy(SBS0335−052W, Pustilnik et al.1997;Lipovetsky et al.1999).Low surface brightness galaxies(LSBGs)comprise a large fraction of the generalfield galaxy population and outnumber by a factor of several times the high sur-face brightness(HSB)population(e.g.,McGaugh1996, Dalcanton et al.1997,O’Neil&Bothun2000).Therefore, these LSBGs can be an important factor for interaction-induced star-formation activity in gas-rich galaxies in gen-eral,mostly through distant/weak tidal encounters(see, e.g.,Taylor et al.1995;O’Neil et al.1998;Pustilnik et al. 2001b).In particular,through interaction they can trig-ger thefirst starbursts in the hypothetical population of local protogalactic H i clouds.To check this hypothesis the authors are conducting a systematic study of the lo-cal environment of the most metal-deficient BCGs.We present here new evidence in support of this idea.We re-port the discovery of a LSB dwarf irregular galaxy(named SAO0822+3545)at a projected distance of∼11.4kpc from one of the most metal-deficient BCGs,HS0822+3542 (Kniazev et al.2000).We have used the SAO RAS6m telescope spectrum in the Hαregion,as well as BV R photometry from the Nordic Optical Telescope(NOT)to study its properties and estimate its tidal effect on the BCG HS0822+3542.We also present new high signal-to-noise(S/N)6m telescope spectra for HS0822+3542which allow us to make more accurate measurements of some of the physical parameters of its star-forming(SF)region and discover thefirst kinematic evidence of an ionized gas supershell.In Section2we describe the observations and their reduction.Results of the data analysis are presented in Section3.We discuss these results in Section4,and summarize ourfindings and draw conclusions in Section5.2.Observations and reduction2.1.Nordic Optical Telescope photometryThere are no cataloged galaxies around HS0822+3542in either NED or LEDA databases with V hel<1200km s−1 and projected distances less than 5.8◦.To search for fainter/non-cataloged galaxies in the close vicinity of this BCG we used B,V,R CCD images obtained with the2.5m NOT on May28,1998.These are the same frames which were used to derive B,V,R magnitudes for HS0822+3542. They were acquired with the ALFOSC spectrograph equipped with the LORAL(W11-3AC)CCD,which has a direct imaging mode.Exposure times were900s for the B-band image,and600s for both V and R images.For further details of these observations and data reduction we refer to the paper by Kniazev et al.(2000).2.2.Looking for possible companionsThe photometric data were reduced with MIDAS2 Command Language programs according to the method described in Kniazev(1997).The MIDAS INVENTORY package was used to classify all objects.Isophotal and total BV R magnitudes were computed using the trans-formation coefficients of Kniazev et al.(2000).Since the interaction between HS0822+3542and a possible neighbouring galaxy would probably result in some enhanced star formation in the latter,wefirst of all searched for candidate blue galaxies.The second criterion applied was that the brightness of any candidates should be comparable to that of HS0822+3542,since signifi-cantly fainter neighbours could tidally affect the BCG only from very small distances(see,e.g.,estimates in Pustilnik et al.2001b).Only two blue galaxies were found in the examined field.Thefirst one is HS0822+3542itself.The second is a LSB irregular galaxy(SAO0822+3545)at3.5′to the north-east from HS0822+3542(its coordinates are given in Table5).The Digitized Sky Survey(DSS-II)blue image of thisfield with the2objects of interest and Anon J0825+3534is presented in Fig.1.All other galaxies in the NOTfield were either significantly fainter or redder.2.3.Analysis of photometric dataWe performed the reduction of photometric data for SAO0822+3545using the IRAF3package ELLIPSE.The growth curve(GC)of the galaxy was constructed by sum-ming up the pixel values from the center outwards in the circles of successive radius.The total magnitudes(B tot,V tot,R tot)were estimated by asymptotic extrapolation of the respective radial GCs. Model-independent parameters were derived from each growth curve.The effective radii(r eff)were read on each GC at one half the asymptotic intensity,and effective SBs (SB eff)were determined as the mean brightness within a circle with the effective radius.These values are summa-rized in Table2.2.4.Long-slit spectroscopySpectroscopic data were obtained with the6m tele-scope of the Special Astrophysical Observatory of Russian Academy of Sciences(SAO RAS).The long-slit spec-trograph(LSS)(Afanasiev et al.1995)was used with a Photometrics1024×1024pixel CCD detector with a 24µm pixel size.The wavelength ranges of the spec-tra obtained for different hardware configurations areS.A.Pustilnik et al.:Starburst in HS0822+3542induced by SAO0822+35453Fig.1.The Digitized Sky Survey(DSS-II)blue image of thefield in the vicinity of BCG HS0822+3542.North is up, East is to the left.At the adopted distance of HS0822+3542(11Mpc)the scale is∼54pc=1′′.The two marked galaxies–LSBD SAO0822+3545and Anon J0825+3534have been checked as possible companions of the BCG.On our data the LSBD has V hel∼700km s−1,close to that of HS0822+3542.Its projected distance to the BCG is213′′or 11.4kpc.The galaxy Anon J0825+3534,very close to the position of2MASXi J0825440+353459(NED),is a distant background object with V hel=15590km s−1.Table1.Journal of the6m telescope spectroscopic observationsObject Date Exposure Wavelength Dispersion Seeing Airmass PAtime[s]Range[˚A][˚A/pixel][arcsec][degree](1)(2)(3)(4)(5)(6)(7)(8)4S.A.Pustilnik et al.:Starburst in HS 0822+3542induced by SAO0822+3545Fig.2.Top panel:2D spectrum of SAO 0822+3545with the H αline at λ6579˚A .Positive Y corresponds to the NW direction for the slit position shown in Fig.3.H α-emission is clearly seen on top of the continuum in the region of ±∼5′′from the central position.Furthermore,some very faint H α-emission (with S/N ratio of ∼1)can be traced out to ±∼10′′,in the regions without detectable continuum.Bottom panel:1D spectrum of the central region (±3′′),summed along the slit,EW (H α)=17˚A .grating,giving a sampling of 1.2˚A pixel −1and an effec-tive resolution (with the 2′′slit width)of 3.5˚A .Seeingduring these observations was 1.7′′.For the reduction of 2D spectra we obtained biases,flat fields and illumination correction images.The primary re-duction consisted of standard steps and was done using the IRAF package CCDRED .The IRAF package LONGSLIT was used to perform wavelength calibration,background subtraction,extinction correction and flux calibration.Straightening of the 2D spectra was performed using APALL ,another IRAF package.After that,aperture ex-tractions,continuum determination,flux and equivalent width measurements of spectral lines were performed in MIDAS (for details,see Kniazev et al.2000).The reduced 2D spectrum and extracted averaged 1D spectrum of SAO 0822+3545are shown in Fig.2.Fluxes and equivalent widths of blended lines were measured using Gaussian decomposition fitting.An av-erage sensitivity curve was produced for each night with r.m.s.deviations of 5%in the whole spectral range.The sensitivity curve and line intensity errors have been prop-agated in calculating elemental abundances.To construct the P–V diagram,the methodology described in Zasov et al.(2000)was used,which allowed us to measure points with sufficiently bright H αemission with r.m.s.errors on the level of 2–4km s −1.3.Results3.1.Spectrum of SAO 0822+3545The 2D spectrum of SAO 0822+3545in Fig.2shows H αemission spanning ∼10′′,comparable to the appar-ent extent of the galaxy continuum.Some fainter H αfea-tures can be detected in the peripheral regions,where no continuum is seen in our spectrum.The equivalent width of the H αline,measured on the 1D spectrum av-eraged over the central region with the a spatial extent of 6′′,is EW (H α)=17±2˚A .The integrated flux in thisline is 4.65(±0.55)×10−16erg s −1cm −2.Small variations of EW (H α)along the slit near the center of the galaxy on the level of ∼15−20˚A are within the observa-tional uncertainties.Closer to the edges the EW (H α)can be larger,but there the uncertainty reaches 70–100%,so we do not discuss these regions further.The measured velocity V hel =700±50km s −1is very close to that of HS 0822+3542.3.2.Photometry and morphology of SAO 0822+3545We calculated total magnitudes B tot =17.56±0.05,V tot =17.43±0.03and R tot =17.26±0.05for SAO 0822+3545us-ing the growth curve method as described in Sec.2.3.The respective integrated colours are (B −V )tot =0.13and (V −R )tot =0.17.Relatively large errors originate from the zero-point uncertainties of the transformation equa-tions (Kniazev et al.2000).Accounting for a foreground extinction of E (B −V )=0.047in our Galaxy (Schlegel et al.1998),and applying the extinction curve from Whitford (1958),these colours become somewhat bluer:(B −V )0tot=0.08±0.06,(V −R )0tot =0.14±0.06.The 2D spectrum in Fig.2and the irregular structure of the central part of SAO 0822+3545(see Fig.3)indicate that enhanced star formation took place at least in the inner part of that galaxy.The possibility of better distin-guishing individual regions of higher brightness (possible young superclusters and aged H ii regions)in the central part of the LSBD was the motivation for using the MIDAS package IMRES for deconvolution of the NOT images.This package employs an image restoration scheme devised by Richardson and Lucy and described in Adorf et al.(1992),Hook &Lucy (1992;and references therein).The num-ber of iterations was determined by comparisons between the input image and the output deconvolved images,after convolution with the point-spread function (PSF).The results of deconvolving the B -band image after 15iterations are plotted in the right panel of Fig.3.A number of filaments and relatively bright knots in the inner part of this LSB/dIrr galaxy are well resolved.Practically all of them are seen on the original image (left panel of Fig.3),although deconvolution makes the structure more visible.All these structures are easily visible in a deconvolved V -band image,but are less distinct in R -band.There is a faint tail in the SE direction in the outer part of the LSBD.This tail is visible on both blue DSS-S.A.Pustilnik et al.:Starburst in HS 0822+3542induced by SAO 0822+35455Fig.3.Left panel:Thesame B -band image of SAO 0822+3545,deconvolved after 15iterations using the FFT based Lucy algorithm (Adorf et al.1992).The angular resolution has improved from 1.′′25to ∼0.′′85(FWHM).Several filaments and many knots are easily visible within the brighter part of the galaxy.Knots are marked by letters from “a”to “i”,respectively.II and B -band NOT images.The surface brightness of this tail corresponds to µB =25.m 7arcsec −2,or 2σof the noise level for the B -band image.The tail direction coincides with that of the LSBD major axis.The major axis P A varies from –75◦for the inner part of the galaxy up to –60◦for the outer part.The axial ratio is essentially constant over the body:b/a ∼0.55.Evidence for recent star-formation activity over the in-ternal part of this dIrr galaxy is also seen,e.g.,in the (B −V )0colour map (Fig.4).This map shows a rather uniform distribution (mainly in the range from –0.05to +0.10)over a large part of the main body.Its maximum (+0.2to +0.25)and minimum (–0.15to –0.10)values are measured in the positions close to the edges,where the S/N is small,and these large colour variations are appar-ently spurious.SAO 0822+3545is a genuine LSB galaxy with traces of recent SF near its center.Since the central bright knots are seen with the lowest contrast in R -band,we made a rough estimate of the central SB of an underly-ing “disk”in R .From the data in Table 2,its effective surface brightness corrected for extinction (A R =0.12)isµR eff,0=23.m 63arcsec−2.For a purely exponential disk this corresponds to a central brightness of µR 0=22.m 50arcsec −2.Since the galaxy is significantly inclined to the line-of-sight,we need to make a corresponding correction to µR 0.For an observed axial ratio p =b/a =0.55,assuming anintrinsic axial ratio of q =0.2,and using the well-known formula cos 2(i )=(p 2−q 2)/(1−q 2),we calculate that i =58.5◦.The inclination correction for surface brightness is then −2.5·log(cos i )=0.m 7,giving a corrected centralbrightness of µR0,c =23.m 20arcsec −2.Even if the underly-ing “disk”is as blue,as the integrated light of this galaxy (that is,(B −R )0∼0.2),its central brightness in B -bandµB 0,c =23.m 40arcsec−2is well within the LSB galaxy regime.For an exponential law,r eff=7.94′′in R corresponds to the scalelength αR =4.73′′.Table 2.Photometric parameters of SAO 0822+3545BandTotal r effSB effmag arcsec mag arcsec −2(1)(2)(3)6S.A.Pustilnik et al.:Starburst in HS 0822+3542induced by SAO0822+3545Fig.4.Grey-scale map of (B −V )-colour for SAO 0822+3545smoothed with 2D median with the win-dow size of 1.′′6×1.′′6.The extinction corrected (E (B −V )=0.047)colour distribution is shown only for regions with S/N ratio larger than 4.The colour scale is shown in the right side column.B -band surface brightness (SB)isolines are superimposed,with the lowest SB level of 25.m 7arcsec −2.The other levels are:24.5,24.0,23.6,23.3,23.1,22.9,22.8and 22.6mag arcsec −2.tor of two (FWHM=0.′′6),and the restored BCG complex morphology is shown in Fig.5in grey scale,with a contour indicating the outer isophote µB =25.m 0arcsec −2super-imposed.With the letters “a”to “f”we have marked all bright features well resolved after deconvolution in each of B,V ,and R bands.The brightest region consists of two components,“a”and “b”,separated by ∼1.3′′(∼70pc),roughly in the N–S direction.The contrast in Fig.5is adjusted to show faint features.The real ratio of the intensities of knots “a”and “b”,derived from this image,is ∼8.While deconvolution does not preserve brightness proportions between individual features,we consider this ratio to be indicative of the real value.In addition to several bright knots,some filamen-tary structures are also visible.Some traces of them are also seen in other filters,but due to their lower surface brightness they are not as easily visible as the knots.Nevertheless,the prominent arc-like structure at the NW edge of the main body (stretching from X =+2,Y =+4to X =+6,Y =+4in Fig.5),is clearly visible on both B and V images,but is more noisy in R -band,presumably due to the lower S/N ratio.This feature probably repre-sents an ionized gas shell with a diameter of ∼4′′(∼200pc),caused by recent active SF in this region,Four more knots are seen in the restored image.One (“d”)is near the geometrical center of the main body.This,perhaps,might naturally be expected because of the gravitational well in the center of the galaxy.The others knots provide further evidence that the current SF episode in the BCG is spread across the galaxy.The P–V diagram in Fig.6indicates a supershell with a size of ∼480pc,comparable to the extent of H α-emission in the long-slit direction.The supershell velocity ampli-tude,as seen from our data,is about 30km s −1.Such supershells are well-resolved on high-resolution H αlong-slit spectra for many nearby starbursting galaxies (e.g.,Marlowe et al.1995;Martin 1996,1997,1998).The re-lated supershells of neutral gas are also seen in H i maps of such galaxies (e.g.,Walter &Brinks 1999).For the typ-ical case of a starburst off-set in position relative to the midplane of the gas disk,the asymmetry of the gas den-sity distribution in the z -direction results in the shell’s asymmetric appearance.This was shown,e.g.,in numer-ical simulations by Silich et al.(1996),and by Walter &Brinks (1999)for the observed types of P–V diagrams.That part of the shell propagating out of the plane should have a significantly lower Emission Measure due to de-creasing gas density,and usually appears much fainter in comparison to the part of the shell moving towards the midplane (e.g.,Martin 1996).Shells (or supershells)are produced by hot bubbles,caused by the injection of the energy from numerous massive star winds and supernova (SN)explosions into the interstellar medium (ISM)(e.g.,Tenorio-Tagle &Bodenheimer 1988).The asymmetric appearance of super-shells in H αemission is easily seen with the high-resolution data mentioned above.When the velocity resolution is not sufficient to distinguish motions on both sides of the shell,we measure the intensity-weighted velocity in the H α-line at each slit position.If the H αintensities in the segments on opposite sides of the shell differ significantly,we will see mainly the side approaching the midplane of the gas disk.However,since the observed velocity at each slit position is the weighted mean of the emission from the opposite sides of the shell,a shell velocity derived in this way rep-resents a lower limit of the real value.Depending on the relative strengths of H αemission on the shell sides the expected correction could reach tens of percent.If we accept the full amplitude of the radial veloc-ity difference between the two edges on the P–V di-agram (∼35km s −1)as the result of rotation in the BCG,then the apparent V rot is 17.5km s −1.With an apparent axial ratio p =b/a =0.5,and an assumed in-trinsic ratio q =0.2,using the same relation as for SAO 0822+3545in section 3.2we get an inclination an-gle i =63.6◦,and thus an inclination-corrected value of V rot =19.5km s −1.The latter value is quite consistent with that expected from the Tully-Fisher relation be-tween galaxy V rot and its blue luminosity,namely,using the relations derived by Karachentsev et al.(1999)for dwarf galaxies in the Local Volume.For HS 0822+3542,M B =–12.5(or L B =1.56×107L ⊙)and so the expected V rot =17km s −1,with a ±1σconfidence range of 12to 24km s −1.S.A.Pustilnik et al.:Starburst in HS 0822+3542induced by SAO 0822+35457Fig.6.Upper panel:P–V dia-gram of ionized gas in HS 0822+3542based on the H αline from the same spectrum.Its form within a radius of ±4′′,and the characteristic diameter and velocity ampli-tude (∼480pc and ∼30km s −1),are consistent with the appearance of supershells observed in many star-bursting galaxies.Filled boxes show the velocities on both sides of the shell as derived from the Gaussian decomposition of the H αline at several positions along the slit.For details see section 3.3.In Fig.6we use filled squares to show the velocities on both sides of the shell,obtained by Gaussian decom-position of the H αprofiles.The two-component struc-ture is detectable only for sufficiently large S/N ratios and maximal velocity separation.The flux from the re-ceding components is several times lower than that from the approaching ones.These data confirm the existence of a large shell with a characteristic velocity amplitude of ∼30km s −1and exclude the interpretation of this feature in the P–V diagram as part of a rotation curve.Indeed,the rotation velocity should monotonously increase from one edge to another.The real P–V diagram certainly does not look like this.Thus,if the ionized gas in the BCG is rotating,its rotation velocity is sufficiently small to be practically hidden by the visible large shell.3.4.Chemical abundances in HS 0822+3542The spectrum of the brightest knot of HS 0822+3542,ex-tracted with an aperture of 3.′′6×1.′′2,is shown in Fig.7.It is dominated by very strong emission lines.The rel-ative intensities of all emission lines,together with the equivalent width EW (H β),extinction coefficient C (H β)and the EW of Balmer absorption lines are given in Table 3.C (H β)was derived from the Balmer decrementusing the self-consistent method of Izotov et al.(1994).The derived value of C (H β)=0.0±0.09is consistent,to within the uncertainties,with a reddening of E (B −V )=0.047±0.007,expected from foreground extinction in the Galaxy (Schlegel et al.1998).We analyzed chemical abundances and physical pa-rameters with the method described by Kniazev et al.(2000).The measured electron temperatures and den-sity,and derived chemical abundances are presented in Table 4.Our new data give a slightly higher value of 12+log(O/H)(7.44±0.06versus 7.35±0.04from the NOT spectrum),but the difference is not significant.The main source of this difference is the intensity of the [O iii ]λ4363line,relative to H β.Its measured value is 0.104on the 6m telescope spectrum,in comparison to 0.123on the NOT spectrum.Part of the derived differences in O/H could be due to the differences in observational conditions,resulting in the sampling of slightly different regions.However,both results are in fact consistent to within their uncertainties.The ratios of other heavy element abundances (Ne ,S ,N )to that of oxygen,derived from the NOT and the 6m tele-scope data,are also similarly consistent.With the higher resolution (1.2˚A pixel −1)spectrum near H αwe improved the precision of the N abundance,since the [N ii ]λ6584emission line was detected with a higher S/N ratio than in the NOT spectrum.The intensities of Ar lines are mea-sured for the first time in this BCG,and we present here its abundance.At the position of the [Fe iii ]line λ4658˚A we detected a signal at a level of 4σ.However,if log(Fe/O)is typical of other very metal-poor BCGs (∼−1.65),the signal in this line should be only ∼1.3σ.One possible ex-planation of the strength of this line is the contribution of the WR spectral feature C iv λ4658.In many BCGs with detected WR features the intensity of the C iv λ4658line is comparable to that of He ii λ4686(e.g.,Guseva et al.2000).Thus,a likely interpretation of the observed fea-ture is that it is the sum of the lines of [Fe iii ]and C iv .This suggests that higher S/N spectroscopy could detect the other WR features in this young starburst region.The He ii λ4686line in our spectrum is broadened to ∼15˚A ,but the S/N ratio is too low to accept this as direct evi-dence of a WR population.4.Discussion4.1.General parameters of the systemIn Table 5we present the main parameters relevant for further discussion of the properties and status of these dwarf galaxies.Their small mutual projected dis-tance (3.′5,or ∼11kpc)and relative velocity (∆V <25km s −1,Chengalur et al.2003)imply that both galaxies are physically associated.Some of the param-eters for HS 0822+3542in Table 5have been revised from those in Kniazev et al.(2000).In particular,the distance-dependent parameters have changed due to an improved distance estimate.H i related parameters have also changed due to correction of the 21-cm line flux8S.A.Pustilnik et al.:Starburst in HS 0822+3542induced by SAO0822+3545Fig.5.Left panel:Same as before,but for NOT V -band image.The filamentary structure on NW edge iswell seen on both images.(GMRT,Chengalur et al.2003).The integrated H i flux presented by Kniazev et al.(2000),based on observations with the NRT,appeared to be offby a factor of two due to the effects of confusion with the galaxy SAO 0822+3545.The adopted oxygen abundance is the weighted mean of current and previous (Kniazev et al.2000)values.4.2.On the evolutionary status of SAO 0822+35454.2.1.The very blue colours of SAO 0822+3545The integrated colours of SAO 0822+3545are unusually blue.Only two out of about 250LSB/dIrr galaxies with known integrated colours (B −V ),(V −R ),or (B −R )(from papers by Ronnback &Bergvall 1994,McGaugh &Bothun 1994,de Blok et al.1995,van Zee et al.1997,O’Neil et al.1997,van Zee et al.2001,and Burkholder et al.2001)have such blue colours.Only one of the 65dIrr galaxies studied by Makarova et al.(1998),Makarova &Karachentsev (1998),and Makarova (1999)appeared that blue;Makarova et al.(1998)noted that this particular LSBG (UGCA 292)has several blue stellar complexes,in which van Zee (2000)detected strong line emission,indicating young starbursts.Thus,the unusual colours of SAO 0822+3545could be due to its recent enhanced SF.To estimate the age of its stellar population,we can compare its (B −V )0totand (V −R )0tot colours with model values.Unfortunately,due to the age-metallicity degeneracy,similar colours cancorrespond to very different ages.Therefore some a priori information on galaxy metallicity is necessary to disen-tangle the degeneracy.This can be obtained from the dIrr galaxy metallicity–luminosity relation (Skillman et al.1989;Pilyugin 2001).For SAO 0822+3545it predicts Z ∼1/20Z ⊙.In fact,for LSB galaxies this relation likelygoes significantly below (e.g.,Kunth &¨Ostlin 2000)thatfrom Skillman et al.,so 1/20Z ⊙is probably the upper limit for the metallicity of SAO 0822+3545.parison of observed and model parametersTo get some insight on the evolution status of SAO 0822+3545,we compared its observed colours and EW (H α)with model predictions.For colours we used results derived from PEGASE.2models (Fioc &Rocca-Volmerange 1997,2000).We also used these models to estimate the mass of the stellar population.We calculated spectral energy distributions (SEDs)for instantaneous SF bursts with Z =1/20and 1/50Z ⊙,as well as the time be-havior of B ,V ,R luminosities and the respective colour tracks.In Fig.8,we show BV R colour tracks for instan-taneous SF bursts with Z =1/20and 1/50Z ⊙,using solid and dotted lines,respectively,assuming a Salpeter IMF with M low =0.1M ⊙,M up =120M ⊙.The track for con-tinuous SF with constant SFR (Z =1/20Z ⊙)and the same IMF is shown by dashed line.SAO 0822+3545ex-。

高三英语职业单选题50题1. A doctor needs to have excellent ____ skills to diagnose diseases accurately.A. communicationB. observationC. calculationD. writing答案：B。

解析：本题考查医生职业所需技能相关词汇。

医生需要有出色的观察（observation）技能来准确诊断疾病。

communication 沟通）技能对医生也重要，但相比之下，观察技能更直接与准确诊断疾病相关；calculation（ 计算）更多与工程师等职业相关；writing（ 写作）不是诊断疾病最关键的技能。

2. In a school, a teacher is often required to ____ different teaching methods to meet students' needs.A. adaptB. adjustC. adoptD. adept答案：C。

解析：本题考查与教师职业相关的词汇。

adopt有采用、采纳的意思，教师需要采用不同的教学方法来满足学生需求。

adapt是适应、改编；adjust是调整；adept是熟练的，是形容词，不符合此处语法要求。

3. An engineer must be good at ____ blueprints accurately.A. drawingB. paintingC. writingD. typing答案：A。

解析：本题考查工程师职业相关技能。

工程师必须擅长准确地绘制（drawing）蓝图。

painting更多指绘画艺术方面；writing 是书写文字；typing是打字，都不符合工程师绘制蓝图这一工作内容。

4. A nurse should have strong ____ skills to take good care of patients.A. care - takingB. patient - handlingC. emotional - intelligenceD. physical - strength答案：C。

Certificate of Analysis Takara Bio USA, Inc.1290 Terra Bella Avenue, Mountain View, CA 94043, USA U.S. Technical Support: ********************United States/Canada 800.662.2566 Asia Pacific+1.650.919.7300Europe+33.(0)1.3904.6880Japan+81.(0)77.565.6999Page 1 of 6Tet-On® 3G Vector Set (with ZsGreen1)Table of ContentsDescription (1)pCMV-Tet3G Vector Information (2)pTRE3G-ZsGreen1 Vector and pTRE3G-Luc Control Vector Information (4)Quality Control Data (6)Catalog No. Lot Number631159 (Not sold separately) Specified on product label.DescriptionThe Tet-On 3G Vector Set (with ZsGreen1) is used to create tightly regulated and highly responsive tetracycline (Tet)-inducible mammalian expression systems that are turned on by the addition of doxycycline to the culture medium. The Tet-On 3G Vector Set (with ZsGreen1) allows the simultaneous expression of a gene of interest and a green fluorescent protein marker.Package Contents•20 μl pCMV-Tet3G Vector (500 ng/μl)•20 μl pTRE3G-ZsGreen1 Vector(500 ng/μl)•20 μl pTRE3G-Luc Control Vector(500 ng/μl)•40 μl Linear Hygromycin Marker (50 ng/μl)•40 μl Linear Puromycin Marker (50 ng/μl)Storage Conditions•Store plasmids at –20°C.•Spin briefly to recover contents.•Avoid repeated freeze/thaw cycles.Shelf Life• 1 year from date of receipt under proper storage conditions.Storage Buffer•10 mM Tris-HCl (pH 8.0), 1 mM EDTA (pH 8.0)Shipping Conditions• Dry ice (–70°C)Product DocumentsDocuments for our products are available for download at /manualsThe following documents apply to this product:•Tet-On 3G Expression Systems User Manual (PT5148-1)pCMV-Tet3G Vector InformationFigure 1. pCMV-Tet3G Vector Map.DescriptionThe pCMV-Tet3G Vector expresses Tet-On 3G, a tetracycline-controlled transactivator that exhibits high activity in the presence of the inducer doxycycline (Dox), and exceptionally low activity in its absence. Tet-On 3G results from the fusion of amino acids 1–207 of a mutant Tet repressor (TetR) to 39 amino acids that form three minimal "F"-type transcriptional activation domains from the herpes simplex virus VP16 protein. Tet-On 3G was derived from Tet-On Advanced (Zhou et al. 2006; Urlinger et al. 2000; Gossen and Bujard 1992; Gossen et al. 1995); as a result, it’s fully synthetic, lacks cryptic splice sites, and is codon-optimized for stable expression in mammalian cells. Compared to both of its predecessors, however, this 3rd generation Tet-On transactivator demonstrates increased sensitivity to Dox (Zhou et al. 2006). Constitutive expression of Tet-On 3G is driven by the human cytomegalovirus immediately early promoter (P CMV IE).Location of Features in pCMV-Tet3G•P CMV IE(human cytomegalovirus immediate early promoter): 2–688•Tet-On 3G (transactivator gene): 775–1521•SV40 polyA signal: 1536–1991•pUC origin of replication: 2342–2996•Amp r (ampicillin resistance gene; β-lactamase): 3144–4004 (complementary)•SV40 polyA signal: 4275–4809 (complementary)•Kan r/Neo r (kanamycin/neomycin resistance gene): 5417–6211 (complementary)•P SV40 e (SV40 early promoter): 6532–6891 (complementary)Additional InformationpCMV-Tet3G is used to develop stable Tet-On 3G cell lines, which are hosts for Tet-inducible gene expression systems. To create a Tet-inducible expression system, a vector containing a gene of interest under the control of the Tet-inducible TRE3G promoter(P TRE3G) is transfected into a Tet-On 3G cell line. The addition of Dox to the system causes Tet-On 3G to undergo a conformational change that allows it to bind to P TRE3G, activating transcription of the gene of interest in a highly dose-dependent manner. Additional information on TRE-containing vectors, and protocols describing the construction of Tet-On 3G cell lines can be found in the Tet-On 3G Expression Systems User Manual (PT5148-1).Propagation in E. coli•Suitable host strain: Stellar™ Competent Cells•Selectable marker: plasmid confers resistance to ampicillin (100 μg/ml) in E. coli hosts.• E. coli replication origin: pUCpTRE3G-ZsGreen1 Vector and pTRE3G-Luc Control Vector InformationFigure 2. pTRE3G-ZsGreen1 Vector and pTRE3G-Luc Control Vector Maps.Figure 3. pTRE3G-ZsGreen Vector Multiple Cloning Site. The internal start site (ATG) at the IRES2/MCS junction is indicated in bold.DescriptionpTRE3G-ZsGreen1is a Tet-inducible, mammalian expression vector designed to coexpress a gene of interest and the green fluorescent protein ZsGreen1 under the control of the Tet-responsive promoter P TRE3G. This promoter consists of a highly optimized Tet-responsive element (TRE) just upstream of a minimal CMV promoter. P TRE3G exhibits exceptionally low basal activity; it’s induced by the binding of Tet-On 3G but is virtually silent in its absence. The vector is designed to be used as part of our Tet-On 3G Inducible Expression System (Cat. No. 631164).ZsGreen1 is a human codon-optimized variant of the reef coral Zoanthus sp. green fluorescent protein (ZsGreen) that has been engineered for brighter fluorescence (excitation and emission maxima: 493 and 505 nm, respectively; Matz et al. 1999; Haas, Park, and Seed 1996). p TRE3G-ZsGreen allows Dox-inducible coexpression of ZsGreen1 and a gene of interest from a bicistronic mRNA transcript. An encephalomyocarditis virus (EMCV) internal ribosome entry site (IRES2), positioned between ZsGreen1 and the gene of interest, facilitates cap-independent translation of the gene of interest from an internal start site at the IRES2/MCS junction (Jang et al. 1988). This ensures that a high percentage of ZsGreen1-expressing clones also express the gene of interest, allowing ZsGreen1 to be used as an indicator of inducibility and transfection efficiency, as well as a marker for selection by flow cytometry. The vector also contains a pUC origin of replication and an ampicillin resistance gene (Amp r) to allow for propagation and selection in E. coli.The pTRE3G-Luc is a Tet-inducible control vector that expresses firefly luciferase under the control of P TRE3G. When used with standard luciferase detection reagents, this vector can be used as a reporter of induction efficiency (see User Manual for protocol). pTRE3G-Luc is not intended to be used as a cloning vector.Location of Features in pTRE3G-ZsGreen1•P TRE3G (3rd generation Tet-responsive promoter): 7–382•ZsGreen1: 389–1084•IRES2 (encephalomyocarditis virus internal ribosome entry site): 1091–1673•MCS (multiple cloning site): 1686–1721•SV40 polyA signal: 1776–2573•pUC origin of replication: 2838–3481•Amp r (ampicillin resistance gene; β-lactamase): 3629–4489 (complementary)Location of Features in pTRE3G-Luc•P TRE3G (3rd generation Tet-responsive promoter): 7–382•Luciferase: 432–2084•SV40 polyA signal: 2151–2948•pUC origin of replication: 3213–3856•Amp r (ampicillin resistance gene; β-lactamase): 4004–4864 (complementary)Additional InformationpTRE3G-ZsGreen1 is a mammalian expression vector that allows tightly regulated, doxycycline-controlled coexpression of a gene of interest and ZsGreen1. The gene of interest must have both a start and a stop codon. The gene of interest should be cloned in-frame with the start codon at the IRES2/MCS junction (this codon is shown in bold in the MCS sequence in Figure 3, page 3; see the User Manual for details on how to use In-Fusion® to simplify your cloning). Cotransfection of pTRE3G-ZsGreen1 constructs with Linear Hygromycin or Puromycin Markers allows antibiotic selection of stable transfectants. In order to function, the system requires the presence of the Tet-On 3G transactivator protein, supplied by a stable Tet-On 3G cell line created with our Tet-On 3G Inducible Expression System (Cat. No. 631164).Propagation in E. coli•Suitable host strain: Stellar™ Competent Cells•Selectable marker: plasmid confers resistance to ampicillin (100 μg/ml) in E. coli hosts.• E. coli replication origin: pUCExcitation and Emission of pTRE3G-ZsGreen1•Excitation: 493 nm•Emission: 505 nmReferences•Gossen, M. et al. Transcriptional activation by tetracyclines in mammalian cells. Science268, 1766–9 (1995).•Gossen, M. & Bujard, H. Tight control of gene expression in mammalian cells by tetracycline-responsive promoters. Proc. Natl. Acad. Sci. U. S. A.89, 5547–51 (1992).•Haas, J., Park, E. C. & Seed, B. Codon usage limitation in the expression of HIV-1 envelope glycoprotein. Curr.Biol.6, 315–24 (1996).•Jang, S. K. et al. A segment of the 5’ nontranslated region of encephalomyocarditis virus RNA directs internal entry of ribosomes during in vitro translation. J. Virol.62, 2636–43 (1988).•Matz, M. V et al. Fluorescent proteins from nonbioluminescent Anthozoa species. Nat. Biotechnol.17, 969–73 (1999).•Urlinger, S. et al. Exploring the sequence space for tetracycline-dependent transcriptional activators: novel mutations yield expanded range and sensitivity. Proc. Natl. Acad. Sci. U. S. A.97, 7963–8 (2000).•Zhou, X., Vink, M., Klaver, B., Berkhout, B. & Das, A. T. Optimization of the Tet-On system for regulated gene expression through viral evolution. Gene Ther.13, 1382–90 (2006).Quality Control DataPlasmid Identity & Purity•Digestion with the indicated restriction enzymes produced fragments of the indicated sizes on a 0.8% agarose/EtBr gel:Vector Enzyme(s) Fragment(s)pCMV-Tet3G EcoRI 7.1 kbEcoRI & HindIII 1.2 & 5.9 kbpTRE3G-ZsGreen1 XhoI 4.7 kbEcoRV 1.2 & 3.5 kbpTRE3G-Luc XhoI 5.1 kbEcoRI & BamHI 2.1 & 3.0 kbLinear Hygromycin Marker HindIII & XbaI0.5, 0.6 & 1.1 kbLinear Puromycin Marker HindIII & XbaI0.45, 0.6, & 0.75 kb•Vector identity was confirmed by sequencing.•A260/A280: 1.8–2.0Functional Testing of Linear Markers•HEK 293 cells were transfected with 200 ng of either the Linear Hygromycin Marker or the Linear Puromycin Marker. After 5 hr at 37°C, the transfection solution was removed, and the cells were given fresh medium. 48 hr later, the cells were plated in two 10 cm plates. 48 hr after plating, medium containing either hygromycin orpuromycin (depending on the linear marker used to transfect the cells) was added to the plates. After 2–3 weeks, >20 clones were identified.It is certified that this product meets the above specifications, as reviewed and approved by the Quality Department.CATALOG NO.631159NOTICE TO PURCHASER:Our products are to be used for research purposes only. They may not be used for any other purpose, including, but not limited to, use in drugs, in vitro diagnostic purposes, therapeutics, or in humans. Our products may not betransferred to third parties, resold, modified for resale, or used to manufacture commercial products or to provide a service to third parties without prior written approval of Takara Bio USA, Inc.Your use of this product is also subject to compliance with the licensing requirements listed below and described on the product´s web page at . It is your responsibility to review, understand and adhere to any restrictions imposed by these statements.STATEMENT 24The RCFPs (including DsRedExpress, DsRedExpress2, and E2-Crimson) are covered by one or more of thefollowing U.S. Patent Nos. 7,166,444; 7,157,565; 7,217,789; 7,338,784; 7,338,783; 7,537,915; 6,969,597; 7,150,979;7,442,522 and 8,012,682.STATEMENT 72Living Colors Fluorescent Protein Products: Not-For-Profit Entities: Orders may be placed in the normal manner by contacting your local representative or Takara Bio USA, Inc. Customer Service. Any and all uses of this product will be subject to the terms and conditions of the Non-Commercial Use License Agreement (the “Non-Commercial License”), a copy of which can be found below. As a condition of sale of this product to you, and prior to using this product, you must agree to the terms and conditions of the Non-Commercial License. Under the Non-Commercial License, Takara Bio USA, Inc. grants Not-For-Profit Entities a non-exclusive, non-transferable, non-sublicensable and limited license to use this product for internal, non-commercial scientific research use only. Such licensespecifically excludes the right to sell or otherwise transfer this product, its components or derivatives thereof to third parties. No modifications to the product may be made without express written permission from Takara Bio USA, Inc.Any other use of this product requires a different license from Takara Bio USA, Inc. For license information, please ***************************************************************************************.For-Profit Entities wishing to use this product are required to obtain a license from Takara Bio USA, Inc. For license information, please contact a licensing representative by phone at 650.919.7320 or by e-mail at ***********************.STATEMENT 42Use of the Tetracycline controllable expression systems (the "Tet Technology") is covered by a series of patents including U.S. Patent # 7541446, # 8383364, # 9181556 , European patents EP # 1200607, # 1954811, #2352833Academic research institutions are granted an automatic license with the purchase of this product to use the Tet Technology only for internal, academic research purposes, which license specifically excludes the right to sell, or otherwise transfer, the Tet Technology or its component parts to third parties. Notwithstanding the above, academicand not-for profit research institutions whose research using the Tet Technology is sponsored by for profitorganizations, which shall receive ownership to any data and results stemming from the sponsored research, shall need a commercial license agreement from TET Systems in order to use the Tet Technology. In accepting this license, all users acknowledge that the Tet Technology is experimental in nature. TET Systems GmbH & Co. KG makes no warranties, express or implied or of any kind, and hereby disclaims any warranties, representations, or guarantees of any kind as to the Tet Technology, patents, or products. All others are invited to request a license from TET Systems GmbH & Co. KG prior to purchasing these reagents or using them for any purpose. Takara Bio USA, Inc. is required by its licensing agreement to submit a report of all purchasers of the Tet-controllable expression system to TET Systems.For license information, please contact:GSF/CEOTET Systems GmbH & Co. KG,Im Neuenheimer Feld 58269120 Heidelberg GermanyTel: +49 6221 5880400Fax: +49 6221 5880404email:*******************or use the electronic licensing request form via /ip-licensing/licensing/for-profit-research TRADEMARKS:© 2015 Takara Bio Inc. All Rights Reserved.All trademarks are the property of Takara Bio Inc. or its affiliate(s) in the U.S. and/or other countries or their respective owners. Certain trademarks may not be registered in all jurisdictions.。

Specimen Collection Tube Guidefor specimens submitted to UCHealth South Region LaboratoriesAlt. Tube Alt. Tube Alt. TubeGold Red/Gold None None Red/Gold Pink None Red/Gold None Green Red/Gold None Gold Red/Gold None Red No GelRed/Gold None Red No Gel Red/Gold None Red No GelAcetaminophen Red/Gold None Hep B Core IgM AbRed No Gel Ammonia **None None None AmylaseRed/Gold None Gold Anti-Streptolysin O Red/Gold Cord Blood None Red No GelBeta-HCG Tumor MarkerRed/Gold Homocysteine **NoneGreen None GoldC-Peptide Gold Red No Gel Red/Gold None CA19-9Red/Gold Gold CA 125Red/Gold Alt. TubeRed No Gel CA 15-3Red/Gold None Green/Lav Red/Gold None Red No Gel Carbamazapine Red/Gold None Red No Gel Carboxyhemoglobin None None Green CRP/hsCRP Red/Gold None Green/Lav CK Total Red/Gold None Red No GelCK MB Red/Gold None InsulinRed No Gel Cortisol Red/Gold None Red No Gel Estradiol Red/Gold None Red No Gel Ethanol Red/Gold None EDTAFolate ##Red W Gel None OsmolalityGold FSH Red/Gold None Gold GGTRed/Gold None Gold Gentamicin Red/Gold None Gold IgA/IgG/IgMRed/Gold None Gold Ionized Calcium **Na Hep None Gold Lactic Acid **Red/Gold NoneRed No Gel LDH Red/Gold Red No Gel LH Red/Gold Red No Gel LipaseRed/Gold GoldMagnesium Red W Gel MyoglobinPeds Red Alt. TubeNeonatal Bili ##Red/Gold None Phenytoin Red/Gold Alt. Tube Phosphorus Red/Gold Prealbumin None None Procalcitonin Red/Gold NoneNone Prolactin Red/Gold None Progesterone Red/Gold None ProNT-BNPRed/Gold PSANone PTHRed/Gold Alt. Tube Red/Gold Red/Gold Red/Gold Red/Gold Red/Gold Red/Gold Red/Gold Alt. TubeRed/Gold Red W/ Gel Na Hep None NoneOrder of DrawAlt. TubeNone None NoneArylsulfatase Vitamin B6 ##Vitamin C **##TestosteroneTheophyllineTobramycin Troponin I Be sure to fill tubes to line!Fetal Screen, KB, DAT, Type and Screen, retypeEDTA ROYAL BLUE 10.8 mg K2 EDTA YELLOW ACID-CITRATE-DEXTROSELead and Heavy Metal Testing Blood Culture > Blue > Red /SST > Green > Purple > Gray > Royal Blue > Yellow ACDSalicylate Rheumatoid FactorMethotrexate ##Gold/GreenEDTA Glucose Tolerance testing## = Protect specimens from light** = Specimen sent on Ice, time sensitive!Test NamePartial thromboplastin time (PTT)Test NameGold/GreenThis document serves as a guide only. Please visit our lab test catalogon the Source for more detailed collection requirements.https:///MemorialHospitalMemorial Hospital Laboratory ServicesUniversity of Colorado(719)365-5260Rubella IgGThrombin TimePlatelet Function assay Protein C & SProthrombin time (PT)West Nile Testosterone Free and Total Amikacin, Glycols, Isopropanol, Keppra, Lamotrigine, Lidocaine, Mixed Alcohols, Pentobarbital, Phenytoin Free, Thiocyanate Thyroglobulin Thyroid antibodies Vancomycin Vitamin D, 25-hydroxy Lithium RED NO GEL Valproic acid Vitamin B12NoneLAVENDER – EDTA (Lav EDTA)GOLD OR RED W/ GEL – SERUM SEPARATOR (SST)GREEN WITH GEL – LITHIUM HEPARIN (LiHep)LIGHT BLUE – SODIUM CITRATE (2.7ml or 1.8ml)PINK - EDTA GRAY 10mg/8mg OXALATE WITH FLUORIDE RBC Folate ##Autoimmune Serology Ana, Anti-Cardiolipin, Anti-CCP ANCA (MPO/PR3)Anti-DNA, Anti-Mitochondrial, Anti-Smooth Muscle Test NameAntithrombin III activity APC resistance D-dimerFDP (special blue top tube)FibrinogenHeparin level (LMWH & Unfractionated)Lupus anticoagulant testingSpecific factor activity Specific factor inhibitor DHEAS Digoxin Test NameTest NameComplete Metabolic Panel (CMP)Basic Metabolic Panel (BMP)Alpha-galactosidase HIV by PCR (quantitative, genotype, phenotype)Test Name HLA testingACTH (Pre-chilled tube) ** CMV and HCV by PCRReticulocyte countFlow cytometry Hemoglobin A1cHemoglobin Electrophoresis Sickle Screen Von Willebrand factorPF4 HIT Screen and ConfirmatoryCoagulation Testing:ESRUric acidTest NameC3 & C4Complete Blood Count (CBC)Beta-Hydroxybutyrate (BHOB)Electrolyte Panel (Lytes)Hepatic Function PanelIron Studies (Iron/Transferrin/%Sat)Cyclosporin, Sirolimus, Tacrolimus Mono screen PSA free Quad Screen Serum Protein Electrophoresis Lipid Panel (Chol, Trig, HDL, LDL)Renal Function Panel Pregnancy Qualitative Serum Apolipoprotein Phenobarbital Infectious Serology CMV, EBV, H. Pylori, HSV, Mumps, HIV 1+2, RPR, Rubeola, Varicela, WestNile, HCV, HBV F-Actin (Smooth Muscle) IgG Ferritin CEAGrowth Hormone Test NameAFP Tumor Alpha-1-antitrypsin Haptoglobin Kappa:Lambda Free Light Chains Ceruloplasmin Acute Hepatitis Panel (HepA, HepBc, HepBs Ab/Ag, Hep C)Thyroid Function Tests {TSH, Free T4, Free T3, Totat T3, Total T4}Toxicology & Drug Levels:Test Name Effective Date 3/23/2022。

PACER TESTGeneral Information:Stands for: Progressive Aerobic Cardiovascular Endurance RunMulti stage fitness testAdapted from 20m Shuttle Run TestProgressive – Easy to HardRecommended for all AgesObjective:Run as long as possible back and forth20mSpecified Pace – Gets Faster each MinuteK-3 Should learn How to take Test – for fun4th-12th Score all StudentsEquipment and Set up:Flat Non-Slippery Surface20mCD/Cassette PlayerMeasuring TapeMarkerConesPencils & Score SheetDivide lanes –60” widthChalk or Tape Line – Each EndLet Students Listen to CadenceAllow Two Practice SessionsScorers Sit behind Starting LineTesting:Students Start Behind Line5 Second Countdown to StartBeep – Jog to Opposite EndTurn Around, Wait for Beep – RepeatTriple Beep – Same as Single, Alerts Runners Increase Speed – Every MinuteWalking PermittedNote: A student that does not completely get to opposite side prior to the beep, stops, turns, waits for beep (count the lap) and continues. The second time student does not get to line they are finished testing (do not count this lap).PUSH-UPSGeneral Information:Measures Upper Body Strength & EnduranceRecommended TestObjective:Complete as man Push-ups at Rhythmic PaceCadence = 1/3 SecondsReady PositionProne Position on MatHands Under ShouldersFingers Stretched OutLegs Stretched Out & Slightly ApartToes Tucked UnderTestingPush Off Mat Until Legs, Back, Arms are Straight Back Straight from Head to Toes Throughout Test Lower Until Elbow 90 DegreeUpper Arms Parallel20 Push-Ups/MinuteForm CorrectionsStoppingFailure To Maintain Pace90 Degree AngleBody PositionNot Fully Extending ArmsFirst Correction = 1 Push UpTRUNK LIFTGeneral InformationTests Trunk Extensor Strength & FlexibilityEquipment & Set UpGym MatYard Stick Marked W/Tape @ 6”,9”,12”Ready PositionProne PositionToes PointedHands Under ThighsPlace Tape on Floor for Focus Point of EyesTestingStudent Maintain Focus on TapeHead Stay in Neutral PositionStudent Moves Upper Body in Slow Controlled Manner Up Hold Long Enough to MeasureYard Stick –1” in Front of Testers ChinStudent Slowly Returns to Start Position2 Trials – Record BestCorrectionsBouncingEyesChinFeet Stay on GroundCURL-UPSGeneral InformationTests Abdominal StrengthEquipment & Set UpMat3” Wide Strip for Ages 5-94 ½” Wide Strip for 9-UpPaperReady PositionSupine Position on MatKnee Bend 140 DegreeFeet Flat on MatLegs Slightly ApartArms Straight & Parallel to TrunkPalms of Hands – Resting on MatFingers Stretched OutStudent on Mat Where Strip is Under LegsFingers Resting on Nearest Edge of StripPaper Under HeadTestingStart Movement with Flattening of BackSlow Curling of Upper SpineHands Slide until Fingertip Reaches Opposite Side of Strip(Fingertip Passes Edge)Return to Supine PositionHead Touches PaperCadence – 1/3 SecondsEncourage Steady MovementForm CorrectionsReach with Hands & ArmsMove in Reaction of Trunk & ShouldersNo Jerking MovementsSIT & REACHGeneral InformationTests Flexibility of Hamstring MusclesEquipment & Set Up12” BoxYard StickTape Yard Stick on Box @ 9” at Front Edge of Box with 0” Nearest to StudentReady PositionRemove ShoesStudent Places Both Feet Front Edge of BoxBoth Heals Flat Against BoxFully Extend Left LegRight Foot Flat on Floor 2-3” to Side of Straight KneeArms Extended Forward Over Yard StickHands Together with Fingers ExtendedTestingMove Hands Along Yard Stick 4 TimesPartner May Hold Knee Down4th Time Hold for 1 Second to MeasureMaximum = 12”Record to Nearest ½”Do Left Leg 1stRepeat with Right Leg。

IMMULITE化学发光TSI检测分析性能验证及临床性能评估钟丽，张静，张双婕，王志国(南京中医药大学附属中西医结合医院江苏省中医药研究院检验科，南京210028)摘要：目的探讨IMMULITE2000XPi全自动化学发光免疫分析TSI检测方法的精密度、正确度、线性范围等分析性能,及与Rochc Colas c602电化学发光A nti-TSHR检测方法间的临床性能差异.方法参考美国临床与实验室标准化协会(CLSI)有关文件，分别采用EP-15A3方案验证TSI精密度与正确度，采用EP6-A2方案验证TSI线性区间，并利用EP-17A2方案对TSI和A nti-TSHR进行方法学评估，比较二者临床性能在Graves病中诊断价值的差异.结果IMMULITE2000XPi TSI正常及异常2个水平的重复性精密度分别为：3.38%、3.14%；中间精密度分别为：3.70%、622%；正确度验证区间涵盖验证物质的靶值；线性区间数据分析，二次及三次曲线非线性系数b和b均无显著性，数据呈线性.358例临床样本TSI与A nti-TSHR结果比较，灵敏度：89.0%vs49.0%,配对灵敏度差异：40%(CI：31.9%〜47.2%)；特异性942%vs542%,配对特异性差异：40%(CI：282%〜50.5%).结论IMMULITE：2000XPi全自动发光TSI检测本实验室分析性能均能符合厂家声明，与Rochc Colas c602Anti-TSHR比较,TSI检测方法在Graves病的辅助诊断中显示出更优的临床性能.关键词：促甲状腺激素刺激性抗体；促甲状腺激素受体抗体；格雷夫斯病；分析性能；临床性能中图分类号：R3732文献标识码：AAnAnalyticalVerificationandClinicalPerformanceEvaluationfor IMMULITE Chemiluminescence TSI DetectionZHONG Li,ZHANG Jing,ZHANG Shuangjie,WANG Zhiguo(Clinical Laboratory,Affiliated Hospital of Integrated Traditional Chinese and Western Medicine,Nanjing University of Chinese Medicine,Nanjing210028,China)Abstract：Objective To verifythe analytical results of performance with precision,accuracy,and linear range of IMMULITE2000XPi automatic chemiluminescence immunoassay(CLIA)for TSI detection,so to further evaluate the clinical performance difference between the Roche Cobas e602 electrochemiluminescence immunoassay for Anti-TSHR detection.Methods According to the relevant documents of the American Society for Clinical and Laboratory Standardization(CLSI),the precision,accuracyandlinearintervalofimmuliteTSIdetectionwereverifiedbyusingtheEP-15A3 or EP6-A2scheme,respectively.Furthermore,the difference of clinical performance for TSI detection in the Graves'disease diagnosis between Immulite TSI and Roche Anti-TSHR was accessed according to the EP-17A2.Results The repeatability precision of Immulite TSI at normal and abnormal concentration levels were3.38%and3.14%,respectively,while the intermediate precisions were3.70%and6.62%,respectively.The accuracy verification interval covered the target value of the verification substance.Linear interval data analysis indicated that the nonlinear coefficientsb2andb3ofthequadraticandcubiccurveswerenotsignificant,hencethedatapa t erns paring with Anti-TSHR,TSIshowedresultsasfo l owing：sensitivity：89.0%vs 49.0%,paired sensitivity difference:40%(CI:31.9%,47.2%)；TSI specificity：94.7%vs54.7%,DOI：10.11748/bjmy.issn.l006-1703.2021.02.036收稿日期：2020-11-09；修回日期：2020-01-23通讯作者：王志国.E-mail：wzgayu@paired specificity difference:40%(CI:28.2%,50.5%).Conclusion The analytical performance of immulite2000XPi TSI detection can meet the manufacturers pared with Roche Cobas e602Anti-TSHR,the T SI detection assay shows a better clinical performance in the auxiliary diagnosis of Graves'disease.Key words：Thyroid-stimulating immunoglobulin,TSI；Anti-thyroid stimulating hormone receptorantibody,Anti-TSHR；Graves'disease；格雷夫斯病（Graves'1disease,GD）是一种常见的自身免疫性甲状腺疾病，也是原发性甲亢的主要类型（约占全部甲亢病人的90%）,通常导致眼睛（Graves眼病）、皮肤（Graves皮肤病）、骨骼和心脏等多器官受累［］。