QTL detection of seven spike-related traits and their genetic

利用90k芯片技术进行小麦穗部性状QTL定位武炳瑾;简俊涛;张德强;马文洁;冯洁;崔紫霞;张传量;孙道杰【摘要】小麦穗部性状与产量密切相关,挖掘穗部性状基因及其关联分子标记具有重要意义.本研究以周8425B×小偃81衍生的RIL群体(F8)为材料,利用90k芯片标记构建的高密度遗传图谱对3个环境下的穗长、小穗数、不育小穗数、穗粒数、千粒重进行QTL定位.共检测到19条染色体上的71个QTL,变异解释率(PVE)范围为2.10%~45.25%,其中37个位点为主效QTL(PVE>10%).QSl.nafu-6A.2(穗长)、QSl.nafu-7A(穗长)、QSsn.nafu-2A.1(不育小穗数)、QSsn.nafu-2D(不育小穗数)和QGns.nafu-2B(穗粒数)在多个环境中被检测到,且LOD>10,PVE>20%.位于同一个基因簇中的QSl.nafu-6A.2(穗长)、QGns.nafu-6A(穗粒数)和QTgw.nafu-6A(千粒重)在多个环境中被检测到,且与已报道的相关位点位置相同或相近,在分子标记辅助育种中具有较大参考价值.%Spike traits are important to grain yieldin wheat. Molecular markers associated with genes/QTLs controlling spike traits are highly valuable to marker-assisted breeding. A recombinant inbred line (F8) population derived from Zhou 8425B ×Xiaoyan 81 were evaluated in three environments, and QTLs for spike length, spikelet number per spike, sterile spikelet number, grain number per spike and thousand-grain weigh were mapped into a high-density genetic map built by 90k chip. A total of 71 QTLs were located on 19 chromosomes, and the phenotype variation explained (PVE) by a single locus ranged from 2.10%to 45.25%. Thirty-seven loci were considered as main-effect QTLs owing to the PVE larger than 10%. QTLs QSl.nafu-6A.2 for spike length, QSl.nafu-7A for spike length, QSsn.nafu-2A.1 for sterile spikelet number, QSsn.nafu-2Dfor sterile spikelet number and QGns.nafu-2B for grain number per spike were identified repeatedly in different environments with the LOD value higher than 10 and PVE larger than 20%. QSl.nafu-6A.2 for spike length, QGns.nafu-6A for grain number per spike and QTgw.nafu-6A for thou-sand-grain weight were mapped in a cluster on chromosome 6A and might be applicable in marker-assisted selection because they have been detected in multiple environments and close to the loci reported.【期刊名称】《作物学报》【年(卷),期】2017(043)007【总页数】9页(P1087-1095)【关键词】小麦;穗部性状;90k基因芯片;QTL定位【作者】武炳瑾;简俊涛;张德强;马文洁;冯洁;崔紫霞;张传量;孙道杰【作者单位】西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌 712100;西北农林科技大学农学院, 陕西杨凌712100;西北农林科技大学农学院, 陕西杨凌 712100【正文语种】中文武炳瑾简俊涛张德强马文洁冯洁崔紫霞张传量孙道杰*西北农林科技大学农学院, 陕西杨凌 712100小麦穗部性状是产量的重要构成要素, 对控制穗粒数、千粒重等主要穗部性状进行QTL定位, 明确其在染色体上的位置和效应, 对产量性状的遗传改良具有重要意义。

脑电双频指数（BIS）指导高龄患者七氟醚吸入麻醉的临床观察发表时间：2012-09-04T17:26:11.747Z 来源：《中外健康文摘》2012年第22期供稿作者：刘辉王胜国[导读] 高龄患者对麻醉药的敏感性增高，代谢降低，全麻中易发生麻醉药物过量，麻药残余从而导致术后苏醒延迟。

刘辉王胜国 (抚顺矿务局总医院麻醉科 113008）) 【中图分类号】R 【文献标识码】A【文章编号】1672-5085(2012）22-0445-01 【摘要】目的观察脑电双频指数（BIS）指导高龄患者七氟醚吸入麻醉的可行性。

方法 65岁以上行腹部手术病人70例，ASAⅡ－Ⅲ级，随机分为对照组和实验组，每组35例，对照组的麻醉医师根据平时的麻醉经验以及术中血压、心率的变化用七氟醚的吸入浓度调节麻醉深度；实验组根据BIS值调整术中七氟醚吸入浓度来调节麻醉深度。

术中维持BIS值在40-60,手术结束前调整BIS在60-70。

记录患者睁眼时间（从停止吸入麻醉药至病人睁眼时间），拔管时间，拔管即刻的七氟醚呼出末浓度，记录术中各种用药量；术后随访患者是否有术中知晓。

结果与对照组相比实验组睁眼时间、拔管时间明显缩短（P＜0.05），两组术后随访均无术中知晓。

结论 BIS指导高龄患者吸入七氟醚能加快其麻醉恢复时间。

【关键词】BIS 高龄七氟醚 1 资料与方法 1.1 一般资料:年龄65以上，ASAⅡ－Ⅲ级择期行腹部手术患者70例，随机分为实验组和对照组，每35例，术前均无严重的中枢系统病史心、肝、肾等器官疾患。

预计手术时间2～4小时左右。

1.2 麻醉方法：所用病人入室后常规监测心电图、无创血压、心率、脉搏血氧饱和度，连接脑电双频指数（BIS）传感器。

以芬太尼２～3ug/kg、依托米脂0.3mg/kg，罗库溴铵1mg/kg诱导气管插管后连接Drager.medical麻醉工作站进行机械通气。

麻醉维持采用七氟醚、芬太尼、维库溴铵静吸复合麻醉。

a r X i v :a s t r o -p h /9812244v 1 12 D e c 1998Submitted to ApJ,Nov 1998Preprint typeset using L A T E X style emulateapj v.04/03/99DISCOVERY OF A ∼7HZ QUASI-PERIODIC OSCILLATION IN THE LOW-LUMINOSITYLOW-MASS X-RAY BINARY 4U 1820–30Rudy Wijnands,Michiel van der Klis,&Erik-Jan RijkhorstAstronomical Institute “Anton Pannekoek”and Center for High Energy Astrophysics,University ofAmsterdam,Kruislaan 403,NL-1098SJ Amsterdam,The Netherlands;rudy@astro.uva.nl,michiel@astro.uva.nl,rijkhors@astro.uva.nlSubmitted to ApJ,Nov 1998ABSTRACTWe have discovered a 7.06±0.08Hz quasi-periodic oscillation (QPO)in the X-ray flux of the low-luminosity low-mass X-ray binary (LMXB)and atoll source 4U 1820–30.This QPO was only observable at the highest observed mass accretion rate,when the source was in the uppermost part of the banana branch,at a 2–25keV luminosity of 5.4×1037erg s −1(for a distance of 6.4kpc).The QPO had a FWHM of only 0.5±0.2Hz during small time intervals (32-s of data),and showed erratic shifts in the centroid frequency between 5.5and 8Hz.The rms amplitude over the energy range 2–60keV was 5.6%±0.2%.The amplitude increased with photon energy from 3.7%±0.5%between 2.8and 5.3keV to 7.3%±0.6%between 6.8and 9.3keV,above which it remained approximately constant at ∼7%.The time lag of the QPO between 2.8–6.8and 6.8–18.2keV was consistent with being zero (–1.2±3.4ms).The properties of the QPO (i.e.,its frequency and its presence only at the highest observed mass accretion rate)are similar to those of the 5–20Hz QPO observed in the highest luminosity LMXBs (the Z sources)when they are accreting near the Eddington mass accretion limit.If this is indeed the same phenomenon,then models explaining the 5–20Hz QPO in the Z sources,which require the near-Eddington accretion rates,will not hold.Assuming isotropic emission,the 2–25keV luminosity of 4U 1820–30at the time of the 7Hz QPOs is at maximum only 40%(for a companion star with cosmic abundances),but most likely ∼20%(for a helium companion star)of the Eddington accretion limit.Subject headings:accretion,accretion disks —stars:individual (4U 1820–30;NGC 6624)—stars:neutron —X-rays:stars1.INTRODUCTIONThe bright LMXBs can be divided on basis of their cor-related X-ray spectral and timing behavior in the Z sources and the atoll sources,named after the tracks they pro-duce in the X-ray color-color diagram (CD;Hasinger &van der Klis 1989).The globular cluster source 4U 1820–30(NGC 6624)was classified as an atoll source.Before the launch of the Rossi X-ray Timing Explorer (RXTE )two types of QPOs were observed in the Z sources,which were not observed in the atoll sources (although several in-dications for QPOs or peaked noise were found;see,e.g.,Stella,White,&Priedhorsky 1987a;Hasinger &van der Klis 1989;Yoshida et al.1993).On the top branches (the so-called horizontal branches)of the Z sources a 15–60Hz QPO was detected (the horizontal-branch oscillation or HBO)for whose explanation the magnetospheric beat-frequency model was put forward (Alpar &Shaham 1985;Lamb et al.1985).That the HBO was seen only in Z sources was thought to be related to a higher magnetic field in the Z sources compared to that in the atoll sources (Hasinger &van der Klis 1989).In such an interpretation the HBO would be much weaker in the atoll sources,but they could be observable at some level.Another type of QPO was observed on the diagonal branches (the normal branches)of the Z sources (the normal-branch oscillation or NBO),when the mass accretion rate is near the Ed-dington mass accretion rate (e.g.,Hasinger &van der Klis 1989;Penninx 1989;Smale 1998).The NBOs were there-fore thought to be due to a process which was activated by such high accretion rates (Fortner et al.1989;Alpar etal.1992),and should be observable in the atoll sources if they would reach near Eddington accretion rates.Shortly after the launch of RXTE in December 1995a third type of QPO was discovered in both the Z sources and the atoll sources with frequencies between 200and 1200Hz (the kHz QPOs;see,e.g.,van der Klis et al.1996;Strohmayer et al.1996;see Smale,Zhang,&White 1997for the discovery of kHz QPOs in 4U 1820–30).In both types of sources,the kHz QPOs were remarkably similar and were most likely caused by the same physical mecha-nism.In the atoll sources,besided the kHz QPOs,other QPOs with frequencies between 20and 70Hz were ob-served (e.g.,Strohmayer et al.1996;Ford et al.1997;Wi-jnands et al.1998).The properties of these QPOs (their frequencies and their relation to broad band noise just be-low the QPO frequency;Wijnands et al.1998)suggested a link with the HBOs of the Z sources.So far,similar QPOs as the Z source NBOs have not been reported in the atoll sources.In this Letter,we report the discovery of a QPO near 7Hz in the atoll source 4U 1820–30at its highest observed mass accretion rate.If this QPO is caused by the same physical mechanism as the NBOs in the Z sources,then the production mechanism for these QPOs can also be ac-tived when the luminosity is much less than the critical Eddington luminosity.2.OBSERVATIONS,ANALYSIS,AND RESULTSWe used archival data obtained with the RXTE satellite of 4U 1820–30on 1996May 109:00–22:51UT,and 199612Discovery of a ∼7Hz QPO in 4U 1820–30Fig.1.—Color-color diagram (left )and hardness-intensity diagram (right )of 4U 1820–30.The soft color is the 3.5–6.4/2.1–3.5keV count rate ratio,the hard color is the 9.7–16.0/6.4–9.7keV ratio,and the intensity is the count rate in the energy range 2.1–16.0keV.The colors and the intensity were calculated for the 3detectors that were always on.The count rates were background subtracted,but no dead-time correction was applied.The dead-time correction is approximately 1%.The boxes in the CD indicate the regions which were used to select the power spectra.Typical error bars on the colors and the intensity are shown.All data points are 16-s averages.May 322:15–May 418:05UT.A total of ∼40ks of data were obtained.No X-ray bursts were observed.The data were simultaneously collected with 16s time resolution in 129photon energy channels (covering 2–60keV),with 2ms in 16channels (covering 2–18.2keV),and with 16µs in 16channels (18.2–60keV).During ∼10%of the time,de-tector 4and/or 5(out of five)were off.For the color-color analysis we only used the data of the three detectors which were always on;for the power spectral analysis we used all available data.In order to create the CD and the hardness-intensity diagram (HID),we used as soft color the 3.5–6.4/2.1–3.5keV count rate ratio and as hard color the 9.7–16.0/6.4–9.7keV ratio.As intensity we used the count rate in the energy range 2.1–16.0keV.The CD and HID of all data are shown in Figure 1.In the right hand side of both di-agrams what seems to be a banana branch is observed,with an additional patch of data that might be either the lower banana branch or part of an island state.The power spectrum observed during this part (see below)indicates that the source was not in an island state but in the lower part of the banana branch,because the strong (∼20%rms amplitude)band-limited noise,characteristic of the island state,was not observed.We conclude that during these observations the source was in the banana branch contin-uously.The gap between the lower part of the banana branch with the rest is caused by the two day data gap between the 1996May 1and 1996May 3–4observations.During the May 1observation the source was in the lower part of the banana branch and during the May 3–4obser-vations the source moved up an down the banana branch.In order to study the timing behavior as a function of the position of 4U 1820–30on the banana branch,we made power spectra of 16-s data segments of the 2ms and 16µs data combined.This resulted in ∼2500power spec-tra between 1/16and 256Hz.The rms amplitude values quoted are those obtained for the energy range 2–60keV,unless otherwise stated.We selected the power spectra on basis of the position of the source in the CD by dividing the banana branch in the CD into six regions (Figure 1left ).Each region was analyzed separately.The power spectra corresponding to each region were averaged and the dead-time modified Poisson level (Zhang 1995;Zhang et al.1995)was subtracted.The average power spectra of regions 2and 3were fitted with a fit function consisting of a power law (representing the very-low frequency noise [VLFN])and an exponentially cutoffpower law (repre-senting the high-frequency noise [HFN]).For region 1a Lorentzian was included in the fit function as well,to fit a QPO near 70Hz.For the power spectra corresponding to the other three regions,we only used a power law for the VLFN and a Lorentzian for the 7Hz QPO (region 6)or the broad bump near 7Hz (regions 4and 5).The power spectra corresponding to each region are shown in Figure 2.In the lower banana branch (region 1)the atoll source VLFN and HFN components (see Hasinger &van der Klis 1989)were observed.A QPO at 71±1Hz was also observed,with an rms amplitude of 2.2%±0.2%and a FWHM of 21±4Hz.There are also indications for a broad noise components at ∼100Hz,similar to what has found in other atoll sources (Ford,van der Klis,&Kaaret 1998;Ford &van der Klis 1998;Wijnands &van der Klis 1998a),however,the limited time resolution be-low 18.2keV did not allow to investigate this in more de-tail.The VLFN was detected throughout the entire ba-nana branch except in region 6.Its rms amplitude (in-tegrated over 0.01–1Hz)varied erratically between 2.7%and 7.9%,with a 95%confidence upper limit in region 6of 3.4%.The power law index varied erratically between 1.0and 1.7.The HFN was observed in regions 1–3.Its3Region 1Region 2 (x 0.1)Region 3 (x 0.01)Region 4 (x 0.001)Region 5 (x 0.0001)Region 6 (x 0.000001)Fig. 2.—Power spectra of4U1820–30corresponding to the different regions in the CD indicated in Figure1.The power spectra appear flat at high frequencies,as for display purposes,only96%of the dead-time modified Poisson level was subtracted.rms amplitude(integrated over1–100Hz)and cutofffre-quency decreased from6.3%±0.1%and13.7±0.7Hz inregion1,to3.1%±0.1%and5.5±0.6Hz in region3.Thepower law index varied erratically between−0.9and−1.4.In regions4and5,broad peaked noise is present near7Hz.It is unclear whether the HFN evolved into this broadpeaked noise component or was replaced by it.In region6,a very significant(9σ)QPO is present near7Hz,whichmight be related to the peaked noise in region4and5.Wefitted this peaked noise as well as the QPO with aLorentzian and found frequencies of7.4±0.3Hz in region4and7.1±0.1Hz in region5,consistent with the QPOfrequency of7.06±0.08Hz in region6.While the FWHMof the Lorentzian decreased from6.4±1.8Hz in region4to1.3±0.3Hz in region6,the rms amplitude increased from3.4%±0.4%to6.2%±0.3%.We investigated the presence of the7Hz QPO in moredetail and we found that it was only present during ap-proximately160s of data during the1996May4obser-vation.The QPO could then be directly observed in the4Discovery of a∼7Hz QPO in4U1820–30light curve(Figure3bottom panel).When measured in 32-s time intervals the QPO frequency shifted erratically between5.5and8Hz and had at certain times a FWHM of only0.5±0.2Hz.The frequency drifts of the QPO caused the FWHM to be∼2Hz in all QPO data com-bined.We used these160s of data showing the QPO to study the energy dependence of its amplitude.Wefixed the frequency(7.2±0.1Hz)and FWHM(2.2±0.4Hz)to the values obtained by using the total energy range(rms amplitude of5.6%±0.2%;11.8σ).The rms amplitude in the energy bands2.8–5.3,5.3–6.8,6.8–9.3,9.3–10.8,and 10.8–18.2keV,were3.7%±0.5%,5.0%±0.8%,7.3%±0.6%, 7.1%±1.3%,and6.9%±0.9%,respectively.The95%con-fidence upper limits on the presence of the QPO outside the160s interval were between1%and1.5%(total energy range).We performed time lag measurements between the energy bands2.8–6.8and6.8–18.2keV.The time lag of–1.2±3.4ms is consistent with being zero.We determined the X-rayflux during the time of the QPO byfitting the X-ray spectrum with an absorbed black body plus a power law.We obtained a2–25keV X-ray flux of1.1×10−8erg s−1cm−2.This corresponds to a2–25keV X-ray luminosity of5.4×1037erg s−1,assuming a distance of6.4kpc(Vacca,Lewin,&van Paradijs1986). The power law index was∼2.8indicating that not much flux was present above25keV.3.DISCUSSIONWe have discovered a very significant∼7Hz QPO in the X-rayflux of the globular cluster LMXB and atoll source 4U1820–30.This QPO was only observed during a small part of the data,when the source was in the uppermost part of the banana branch in the CD.It is thought that the mass accretion rate increases monotonically along the ba-nana branch from the lower to the upper banana(Hasinger &van der Klis1989).If true,then the7Hz QPO was only detected during the highest observed mass accretion rate in this source.Note that,although the QPO was only detectable when the source was at the uppermost part of the banana branch,the count rate then was not the high-est observed(Fig.3).It seems that in this source,similar to what has been observed in the atoll sources4U1636–53 (van der Klis1990;Prins&van der Klis1997)and4U 1608–52(M´e ndez et al.1998),the count rate does not have a one-to-one relation with the mass accretion rate. Owing to the small amount of data showing the QPO it is difficult to compare this QPO with QPOs observed in other X-ray binaries.Similar frequency QPOs have been observed in a wide range of sources.For example,in black hole candidates(BHCs)QPOs with frequencies around7 Hz were observed in several systems(see van der Klis1995 for a review).However,recently it was shown(Wijnands& van der Klis1998b)that at least some of these BHC QPOs are most likely related to the QPOs seen in atoll sources between20and70Hz.When4U1820–30is on the lower part of the banana branch,thus at lower mass accretion rates,we detect a significant∼70Hz QPO(Fig.2),similar to what is observed in other atoll sources.This indicates that the7Hz QPO is most likely not related to the7Hz BHC QPOs,unless the70Hz QPO decreased in frequency from70to7Hz from the lower banana branch to the up-per part,opposite to what would be expected(e.g.,Ford &van der Klis1998).In the X-ray dipper4U1323–62a strong(∼10%rms am-plitude)QPO was recently discovered near1Hz(Jonker et al.1998).The production of this QPO is thought to be related to the high(>70◦)inclination of this system. Although the modulation of the X-rayflux at the11-min orbital period(Stella,Priedhorsky,&White1987b)sug-gested a high inclination for4U1820–30,the strong mod-ulation observed in the ultravioletflux of this source indi-cates that the inclination most likely is between35◦and 50◦(Anderson et al.1997),making a common production mechanism of the two types of QPOs unlikely.This con-clusion is further strengthened by the differences between the QPOs.The strength of the1Hz QPO in4U1323–62only marginally increased with photon energy and it is observed almost continuously(even in the dips and the X-ray bursts),both contrary to the case of our7Hz QPO. The most likely identification of the7Hz QPO in4U 1820–30is with the7Hz QPOs observed in the Z sources, when they are accreting near the Eddington mass accretion rate(see van der Klis1995).This identification cannot be tested by comparing the time lags of the different QPOs. The non-detection of time lags in4U1820–30is consis-tent with the non-detection in Scorpius X-1(Dieters et al.1999),but inconsistent with the large(∼80ms)time lags reported in Cygnus X-2(Mitsuda&Dotani1989). However,besides the similar frequencies,also the power spectral evolution with increasing mass accretion rate is very similar between the Z sources and4U1820–30.In the Z sources at low observed accretion rates,relatively strong(10–20%)band limited noise is present,which de-creases in amplitude when the accretion rate is increasing. At a certain accretion rate,this noise is hardly detectable, but a new component arises near7Hz,which evolves in a clear QPO.The power spectral evolution of4U1820–30 is remarkably similar(Fig.2).Seen in this light,it is not surprising that the7Hz QPO in4U1820–30is only ob-served in the highest observed mass accretion rate.The NBOs in the Z sources are observed when these sources accretion near the Eddington accretion rate(Hasinger& van der Klis1989;see,e.g.,Penninx1989and Smale1998 for the value of the accretion rate when the Z sources are on their normal branches).However,the X-ray luminosity in4U1820–30is,assuming isotropic emission,at max-imum∼40%of the Eddington critical luminosity if the companion star has cosmic abundance.As the compan-ion star is most likely a helium white dwarf(Stella et al. 1987a),the X-ray luminosity might be only∼20%of the (helium)Eddington critical luminosity.Thus,barring a large anisotropy in the X-ray emission,the accretion rate in4U1820–30is well below the Eddington critical accre-tion rate and below the accretion rate of the Z sources when they exhibited their7Hz QPOs.This would mean that,if the7Hz QPO in4U1820–30is caused by the same physical mechanism as similar frequency QPOs in the Z sources,then the formation mechanism behind these QPOs is already activated in4U1820–30well below the critical Eddington luminosity.Note added in manuscript:After we submitted this Let-ter,we analyzed the PCA data of4U1820–30used by Smale et al.(1997)and Zhang et al.(1998).During some of their observations the7Hz QPO was detected,again only at times when the source was in the uppermost part of the banana branch.When the source was at slightly5 Fig. 3.—The2–18.2keV light curves of4U1820–30on1996May4.In the top panel each point corresponds to1s,in the middle panelto0.25s,and in the bottom panel to1/64s.Typical errors are70counts s−1in the top panel,125counts s−1in the middle panel,and500 counts s−1in the bottom panel.The QPO is only visible between∼3150and3350s since the start of the observation.lower inferred mass accretion rate,broad peaked noise waspresent near10Hz,which might be related to the QPO.These observations will be discussed in a forthcoming pa-per.This work was supported in part by the NetherlandsFoundation for Research in Astronomy(ASTRON)grant781-76-017.This research has made use of data ob-tained through the High Energy Astrophysics ScienceArchive Research Center Online Service,provided by theNASA/Goddard Space Flight Center.We thank JeroenHoman for stimulating discussions and comments on anearlier version of this document.6Discovery of a∼7Hz QPO in4U1820–30REFERENCESAlpar,M.A.&Shaham,J.1985,Nature,316,239Alpar,M.A.,Hasinger,G.,Shaham,J.,&Yancopoulos,S.A&A, 257,627Dieters,S.,Vaughan,B.,Kuulkers,E.,&van der Klis,M.1999, A&A,submittedAnderson,S.F.,Margon,B.,Deutsch,E.W.,Downes,R.A.,& Allen,R.G.ApJ,482,L69Ford,E.,Kaaret,P.,Tavani,M.,Barret,D.,Bloser,P.,Grindlay, J.,Harmon,B.A.,Paciesas,W.S.,Zhang,S.N.1997,ApJ,475, L123Ford,E.,&van der Klis,M.1998,ApJ,506,L39Ford,E.C.,van der Klis,M.,&Kaaret,P.1998,ApJ,498,L41 Fortner,B.,Lamb,F.K.,&Miller,G.S.1989,Nature,342,775 Hasinger,G.,&van der Klis,M.1989,A&A,225,79Jonker,P.G.,van der Klis,M.,&Wijnands,R.1998,ApJLetters, submittedM´e ndez,M.,van der Klis,M.,Ford,E.C.,Wijnands,R.,&van Paradijs,J.1998,ApJLetters,in pressMitsuda,K.&Dotani,T.1989,PASJ,41,557Penninx,W.1989,In:23rd ESLAB Symposium on Two Topics in X Ray Astronomy,Bologna,Italy,13–20September,1989,p.185–196(eds.J.Hunt&B.Battrick),ESA SP–296Prins,S.&van der Klis,M.1997,A&A,319,498Smale,A.1998,ApJ,498,L141Smale,A.,Zhang,W.,&White,N.E.1997ApJ,483,L119 Stella,L.,White,N.E.,&Priedhorsky,W.1987a,ApJ,315,L49Stella,L,Priedhorsky,W.,&White,N.E.1987b,ApJ,312,L17 Strohmayer,T.E.,Zhang,W.,Swank,J.H.,Smale,A.,Titarchuk, L.,&Day,C.1996,ApJ,469,L9van der Klis,M.,Hasinger,G.,Damen, E.,Penninx,W.,van Paradijs,J.,&Lewin,W.H.G.1990,ApJ,360,L19van der Klis,M.1995,in X-ray Binaries,W.H.G.Lewin,J.van Paradijs,&E.P.J.van den Heuvel(eds.),(Cambridge University Press),252van der Klis,M.,Swank,J.H.,Zhang,W.,Jahoda,K.,Morgan,E.H.,Lewin.W.H.G.,Vaughan,B.,&van Paradijs,J.1996,ApJ,469,L1Vacca,W.D.,Lewin,W.H.G.,&van Paradijs,J.1986,MNRAS, 220,339Wijnands,R.&van der Klis,M.1998a,ApJ,507,L63 Wijnands,R.&van der Klis,M.1998b,ApJ,in press(astro-ph/9810342)Wijnands,R.,van der Klis,M.,M´e ndez,M.,van Paradijs,J.,Lewin, W.H.G.,Lamb,F.K.,Vaughan,B.,Kuulkers,E.1998,ApJ,495, L39Yoshida,K.,Mitsuda,K.,Ebisawa,K.,Ueda,Y.,Fujimoto,R., Yaqoob,T.,Done,C.1993,PASJ,45,605Zhang,W.1995,XTE/PCA Internal MemoZhang,W.,Jahoda,K.,Swank,J.H.,Morgan,E.H.,&Giles,A.B.1995,ApJ,449,930Zhang,W.,Smale,A.P.,Strohmayer,T.E.,Swank,J.H.1998,ApJ, 500,L171。

麦类作物学报　２０２３，４３（１０）：１３４４－１３５０ＪｏｕｒｎａｌｏｆＴｒｉｔｉｃｅａｅＣｒｏｐｓｄｏｉ：１０．７６０６／ｊ．ｉｓｓｎ．１００９ １０４１．２０２３．１０．１６网络出版时间：２０２３ ０７ １３网络出版地址：ｈｔｔｐｓ：／／ｋｎｓ．ｃｎｋｉ．ｎｅｔ／ｋｃｍｓ２／ｄｅｔａｉｌ／６１．１３５９．ｓ．２０２３０７１２．１９２７．０２１．ｈｔｍｌ小麦分蘖数目遗传研究进展与展望收稿日期：２０２２ ０６ １４ 修回日期：２０２２ ０７ ３１基金项目：镇江市农业科学院青年基金项目（ＱＮＪＪ２０２１００２）；江苏省作物基因组学和分子育种重点实验室开放课题项目（ＰＬ２０２００８）；江苏省农业自主创新资金项目（ＣＸ（２１）３０６５）第一作者Ｅ ｍａｉｌ：ｘｕｅｙｉ＿ｓｈｅｎ＠１６３．ｃｏｍ通讯作者：温明星（Ｅ ｍａｉｌ：ｗｍｘｃｅｌｌ２００７＠１６３．ｃｏｍ）申雪懿，李东升，陈琛，曲朝喜，郭瑞，姚维成，刘家俊，邓篧，温明星（江苏丘陵地区镇江农业科学研究所，江苏句容２１２４００）摘　要：分蘖数目是决定小麦产量的重要性状之一。

在小麦生长发育过程中，分蘖是一个复杂的生理过程。

了解小麦分蘖数目的分子遗传机制有利于对小麦株型进行精准改良。

本文从分蘖生长发育过程、分蘖数目遗传位点的挖掘以及相关基因的克隆三方面进行综述，并对小麦分蘖数目性状的研究进行展望，以期为小麦分蘖遗传研究和品种改良提供参考。

关键词：小麦；分蘖数目；遗传位点；育种改良中图分类号：Ｓ５１２．１；Ｓ３３０ 文献标识码：Ａ 文章编号：１００９ １０４１（２０２３）１０ １３４４ ０７犘狉狅犵狉犲狊狊犪狀犱犘狉狅狊狆犲犮狋狅犳犌犲狀犲狋犻犮犚犲狊犲犪狉犮犺狅狀犜犻犾犾犲狉犖狌犿犫犲狉犻狀犠犺犲犪狋犛犎犈犖犡狌犲狔犻，犔犐犇狅狀犵狊犺犲狀犵，犆犎犈犖犆犺犲狀，犙犝犆犺犪狅狓犻，犌犝犗犚狌犻，犢犃犗犠犲犻犮犺犲狀犵，犔犐犝犑犻犪犼狌狀，犇犈犖犌犢犪狅，犠犈犖犕犻狀犵狓犻狀犵（ＺｈｅｎｊｉａｎｇＩｎｓｔｉｔｕｔｅｏｆＡｇｒｉｃｕｌｔｕｒａｌＳｃｉｅｎｃｅｓｉｎｔｈｅＨｉｌｌｙＡｒｅａｏｆＪｉａｎｇｓｕＰｒｏｖｉｎｃｅ，Ｊｕｒｏｎｇ，Ｊｉａｎｇｓｕ２１２４００，Ｃｈｉｎａ）犃犫狊狋狉犪犮狋：Ｔｉｌｌｅｒｎｕｍｂｅｒｉｓｏｎｅｏｆｔｈｅｍｏｓｔｉｍｐｏｒｔａｎｔｔｒａｉｔｓｗｈｉｃｈｄｅｔｅｒｍｉｎｅｓｗｈｅａｔｙｉｅｌｄ．Ｄｕｒｉｎｇｔｈｅｇｒｏｗｔｈａｎｄｄｅｖｅｌｏｐｍｅｎｔｏｆｗｈｅａｔ，ｔｈｅｒｅｇｕｌａｔｉｏｎｏｆｔｉｌｌｅｒｉｎｇｉｓａｃｏｍｐｌｅｘｐｈｙｓｉｏｌｏｇｉｃａｌｐｒｏｃｅｓｓ．Ｕｎ ｄｅｒｓｔａｎｄｉｎｇｔｈｅｇｅｎｅｔｉｃａｎｄｍｏｌｅｃｕｌａｒｂａｓｉｓｏｆｔｉｌｌｅｒｎｕｍｂｅｒｉｎｗｈｅａｔｉｓｂｅｎｅｆｉｃｉａｌｆｏｒｐｒｅｃｉｓｅｉｍｐｒｏｖｅ ｍｅｎｔｏｆｐｌａｎｔａｒｃｈｉｔｅｃｔｕｒｅ．Ｉｎｔｈｉｓｐａｐｅｒ，ｗｅｓｕｍｍａｒｉｚｅｄｔｈｒｅｅａｓｐｅｃｔｓｍａｄｅｉｎｔｈｅｇｒｏｗｔｈａｎｄｄｅｖｅｌ ｏｐｍｅｎｔｏｆｔｉｌｌｅｒｉｎｇ，ｔｈｅｄｉｓｃｏｖｅｒｙｏｆｇｅｎｅｔｉｃｌｏｃｉｃｏｎｔｒｏｌｌｉｎｇｔｉｌｌｅｒｎｕｍｂｅｒ，ａｎｄｔｈｅｃｌｏｎｉｎｇｏｆｔｉｌｌｅｒｎｕｍｂｅｒｒｅｌａｔｅｄｇｅｎｅｓ，ａｎｄｇａｖｅａｎｏｕｔｌｏｏｋｆｏｒｆｕｔｕｒｅｒｅｓｅａｒｃｈｏｎｔｉｌｌｅｒｎｕｍｂｅｒｉｎｗｈｅａｔ．Ｔｈｉｓｒｅｖｉｅｗｍａｙｐｒｏｖｉｄｅｒｅｆｅｒｅｎｃｅｆｏｒｔｈｅｇｅｎｅｔｉｃｒｅｓｅａｒｃｈｏｆｔｉｌｌｅｒｉｎｇａｎｄｉｍｐｒｏｖｅｍｅｎｔｉｎｗｈｅａｔｂｒｅｅｄｉｎｇ．犓犲狔狑狅狉犱狊：Ｗｈｅａｔ；Ｔｉｌｌｅｒｎｕｍｂｅｒ；Ｇｅｎｅｔｉｃｌｏｃｕｓ；Ｂｒｅｅｄｉｎｇａｎｄｉｍｐｒｏｖｅｍｅｎｔ 小麦是中国三大粮食作物之一。

引文格式：蒲芝雨, 杨玉菊, 张安勉, 等. 7个候选内参基因在樟叶越橘不同组织中的表达及稳定性分析[J]. 云南农业大学学报(自然科学), 2023, 38(5): 868−877. DOI: 10.12101/j.issn.1004-390X(n).2022080367个候选内参基因在樟叶越橘不同组织中的表达及稳定性分析*蒲芝雨1， 杨玉菊1， 张安勉1， 李国泽2， 余进德1， 赵　平3， 丁　勇1 **(1. 西南林业大学，云南省高校林木生物技术重点实验室，云南 昆明 650224；2. 保山中医药高等专科学校基础医学院，云南 保山 678000；3. 西南林业大学，西南地区林业生物质资源高效利用国家林业与草原局重点实验室，云南 昆明 650224)摘要: 【目的】筛选樟叶越橘不同组织部位基因表达分析的最适内参基因。

【方法】基于樟叶越橘三代转录组测序数据，筛选出PP2A -1、PP2A -2、EIF -4A -1、EIF -4A -2、60S -1、60S -2和ARP -1共7个候选内参基因；利用qRT-PCR 技术对目标基因在樟叶越橘不同组织(嫩叶、成熟叶、花芽、花、绿色果实、红色果实、绿果果梗和红果果梗)的表达水平进行检测，应用geNorm 、NormFinder 和BestKeeper 3种方法分析评估基因表达的稳定性，通过RefFinder 方法综合评价以筛选出樟叶越橘不同组织的最适内参基因；以樟叶越橘绿原酸合成途径中苯丙氨酸解氨酶基因(PAL )的组织表达情况验证内参基因稳定性评价结果的可靠性。

【结果】樟叶越橘的不同组织中，60S-2基因表达的稳定性居于首位，其次是PP2A-2基因，ARP -1、60S -1和EIF -4A -2基因表达的稳定性居中，EIF-4A-1基因表达的稳定性最差。

应用60S -2内参基因分析获得的樟叶越橘不同组织中PAL 基因表达量与绿原酸含量的变化趋势一致，表明PAL 基因参与了樟叶越橘体内绿原酸的合成。

能谱（Revolution ）CT 胸腹联合胸痛三联CTA 扫描对急性胸痛患者疾病的差异分析左明飞左明飞，，温丽娟温丽娟，，焦宇齐齐哈尔医学院附属第三医院放射影像科，黑龙江齐齐哈尔 161000摘要 目的 分析能谱CT 胸腹联合胸痛三联CT 血管造影术（computed tomography angiography, CTA ）扫描对急性胸痛患者疾病的差异。

方法 选取2022年9月—2023年2月齐齐哈尔医学院附属第三医院急诊收治的50例胸痛患者为研究对象，按照扫描时监测的心率分为低心率组（≤75次/min ）和高心率组（>75次/min ），各25例，所有患者均行能谱CT 胸腹联合胸痛三联CTA 扫描，对比两组不同血管节段管腔平均CT 值、SNR 、CNR 。

结果 低心率组和高心率组患者肺动脉干的CT 值分别为（383.20±67.34）、（371.76±59.35）HU ，信噪比（signal noise ratio, SNR ）分别为（10.35±2.65）、（10.65±2.99），噪声比（contrast noise ratio, CNR ）分别为（19.75±3.16）、（20.18±4.65），两组比较，差异无统计学意义（t =0.637、0.375、0.388，P >0.05）。

两组患者主动脉、肺动脉、冠状动脉各个血管节段平均CT 值、SNR 、CNR 比较，差异无统计学意义（P >0.05）。

结论 能谱（Revolution ）CT 胸腹联合胸痛三联CTA 诊断在不同心率的急性胸痛患者中应用无差异，可以满足临床应用的需求。

关键词 胸腹能谱CT ；胸痛三联CT 血管造影术；急性胸痛中图分类号 R 445 文献标志码 Adoi10.11966/j.issn.2095-994X.2023.09.08.01Differential Analysis of Disease in Patients with Acute Chest Pain by Revolution CT Chest and Abdomen Combined with Triple CTA Scanning for Chest PainZUO Mingfei, WEN Lijuan, JIAO YuDepartment of Radiologic Imaging, the Third Affiliated Hospital of Qiqihar Medical College, Qiqihar, Heilongjiang Province, 161000 China Abstract Objective To analysis differential of disease in patients with acute chest pain by revolution CT chest and abdomen combined with triple computed tomography angiograph (CTA) scanning for chest pain. Methods Fifty patients with chest pain admitted to the emergency de⁃partment of the Third Affiliated Hospital of Qiqihar Medical College from September 2022 to February 2023 were selected as study objects. According to the heart rate monitored at the time of scanning, they were divided into low heart rate group (≤75 beats/min) and high heart rate group (>75 beats/min), with 25 cases in each group. All patients underwent revolution CT chest and abdomen combined with chest pain triple CTA scanning, and the mean CT, SNR, CNR values of the lumen of different vascular segments were compared between the two groups. Re⁃sults The CT values of pulmonary arteries in low heart rate group and high heart rate group were (383.20±67.34) HU and (371.76±59.35) HU, signal noise ratio (SNR) were (10.35±2.65) and (10.65±2.99), and contrast noise ratio (CNR) were (19.75±3.16) and (20.18±4.65), respec⁃tively, and the differences were not statistically significant (t =0.637, 0.375, 0.388, P >0.05). There was no statistically significant difference in the mean CT value, SNR and CNR of each vascular segment of the aorta, pulmonary artery and coronary artery between the patients of two groups(P >0.05). Conclusion There is no difference in the application of revolution CT chest and abdomen combined with triple CTA diagnosis of chest pain in patients with acute chest pain with different heart rates, which can meet the needs of clinical application.Key words Revolution CT chest and abdomen; Chest pain triple CTA; Acute chest pain* 论著 *收稿日期：2023-06-01；修回日期：2023-06-21基金项目：齐齐哈尔市科技计划联合引导项目（LSFGG-2022027）。

Detection of Escherichia coli O157:H7virulence genes in isolates from beef,pork,water,human and animal species in the northwest province,South Africa:public health implicationsCollins Njie Ateba *,Moses Mbewe 1Dale Beighle Centre for Animal Health Studies,School of Agricultural Sciences,North-West University e Mafikeng Campus,P .Bag X2046,Mmabatho 2735,South AfricaReceived 6October 2010;accepted 8November 2010Available online 25January 2011AbstractThe aim of theandidentify Escherichia coliO157:H7from pigs,cattle,andwatersamplestheir by A total of 220samples coli O157:H7were for the by PCR and 130isolates was pigs and pork 88(67.7%)than in cattle water 3(2.3%)or was more frequently isolated from faecal (16.9%e 43.1%)than from meat samples (10.8%e 24.6%).A large proportion d 73isolates possessed the hlyA gene,while 48(36.9%)harboured the eaeA gene.Although there were no major differences in the number of isolates harbouring the stx 1and stx 2genes,respectively,only a small proportion 13(10%)harboured both shiga toxin genes.Despite this,the proportion of isolates that possessed the stx 129(22.3%)was higher the stx 2gene.None of the E.coli O157:H7isolates harboured all four shiga-toxin producing E.coli (STEC)virulence genes When comparing the proportion of isolates obtained from the different sample sources and/or stations,significant positive between isolates from Mafikeng and Lichtenburg (r ¼0.981,p <0.05)and those from Mafikeng and Rustenburg (r ¼0.991,p <0.05).These results therefore indicate that meat and faeces samples obtained from major cities in the northwest province were contaminated with E.coli O157:H7.We suggest that there is a need for improving the sanitary conditions of farms,abattoirs and butcher shops.This could reduce transmission of E.coli O157:H7to humans.Ó2011Institut Pasteur.Published by Elsevier Masson SAS.All rights reserved.Keywords:Escherichia coli O157:H7;rfb O157;fliC H7;Cattle;Pigs;Humans1.IntroductionShiga-toxin-producing Escherichia coli are food-borne pathogens that cause diseases in humans (Bell,2000;Leelaporn et al.,2003;Nunes et al.,2003;Maruzumi et al.,2005;Sugiyama et al.,2005).Serotype O157:H7,in particular,has attracted significant attention due to its ability to cause disease even when only a few bacterial cells are present in food and/or water(Armstrong et al.,1996;Buchanan and Doyle,1997).Diseases caused by E.coli O157:H7in humans include watery and/or bloody diarrhoea,haemorrhagic colitis (HC),haemolytic urae-mic syndrome (HUS)and thrombotic thrombocytopenic purpura (TTP)(Griffin and Tauxe,1991;Armstrong et al.,1996;Weir,2000;Sugiyama et al.,2005).These infections are usually severe in young children,elderly subjects and immunocom-promised individuals (Riley et al.,1983;Duffy et al.,2006;Razzaq,2006;Walch et al.,2006).The ability of E.coli O157:H7to cause disease is associated with production of potent toxins.Shiga toxin genes designatedstx 1and stx 2are the major virulence factors (Pie´rard et al.,1997;Law,2000).Alongside shiga toxins,other variants of stx 2,eaeA ,*Corresponding author.Tel.:þ27183892247;fax:þ27183892134.E-mail addresses:atebacollins1@ (C.N.Ateba),moses.mbewe@nwu.ac.za (M.Mbewe).1Tel.:þ27183892702,þ27728657464(mobile);fax:þ27183892748.Research in Microbiology 162(2011)240e 248/locate/resmic0923-2508/$-see front matter Ó2011Institut Pasteur.Published by Elsevier Masson SAS.All rights reserved.doi:10.1016/j.resmic.2010.11.008本页已使用福昕阅读器进行编辑。