喹烯酮对刺参幼参生长、非特异性免疫及抗应激能力的影响

为探讨使用喹烯酮对刺参幼参的安全性,研究了喹烯酮对幼参生长、非特异性免疫及抗应激能力的影响。实验选用初始体重0.6g左右的幼参,采用单因素梯度设计,以不添加任何促生长剂的饲料作对照,在饲料中分别添加10、20、50、80和100mg/kg的喹烯酮,连续投喂69d,停药2周后经长途运输考察抗应激能力的变化。结果表明,添加喹烯酮的实验组的增重率、特定生长率和成活率都高于对照组,20mg/kg组最高,且显著高于其他组。适量的喹烯酮能提高刺参幼参体壁中SOD、AKP和ACP酶的活性,20mg/kg组最高;随着时间的延长,实验组与对照组的差异减小,50d后SOD、ACP活性接近对照组水平。高浓度喹烯酮(80~100mg/kg)使幼参的抗应激能力变差。研究表明,刺参苗种中间培育期间喹烯酮的最适用量为20mg/kg。     

Galactic halo age estimated from LAMOST DR4 and Gaia DR1

The stellar halo is one of the major components in the Milky Way. Research on its age can provide critical constraints on the origin of the stellar halo and further on the formation of our Galaxy.So far, different approaches and samples have been used to estimate the age of the Galactic halo. In our previous paper, we carefully selected 63 field halo turn-off stars within 1 kpc from the literature using a kinematic approach, then estimated the age of the halo. In this following work, we not only update the data from LAMOST DR4 and Gaia DR1, but also try a different method to select a clean halo sample by combining the metallicity and orbital parameters. Then we compare this halo turn-off sample with the GARSTEC model in the B-V vs. metallicity plane. After Monte Carlo simulations are performed, the age is estimated to be 10.5±1.4 Gyr, highly consistent with our previous result and other studies. However,due to the limited common sources between LAMOST DR4 and Gaia DR1, the final sample in this paper is still quite small. The estimated age will be more robust with the much larger Gaia DR2.     

硒(Ⅳ)对微藻生长的影响及NO对硒胁迫调控作用的初步研究

以小新月菱形藻和赤潮异弯藻为培养对象,研究不同浓度外源硒(Ⅳ)对微藻生长的影响,并初步研究了一氧化氮(NO)和高浓度硒对微藻生长的联合影响.结果表明:硒(Ⅳ)高浓度(10-4～10-5)时起抑制作用;低浓度时(10-7～10-9 mol/L)起促进作用,这与一般的微量元素的作用规律相似.每天2次加入1.4×10-9 mol/L NO能缓解一次性加入高浓度(10-5 mol/L)硒对微藻的毒性作用,这可能与NO能调控细胞内抗氧化系统有关.     

New background quasars in the vicinity of the Andromeda Galaxy discovered with the Guoshoujing Telescope (LAMOST)

Planetary nebulae (PNe) are good tracers of the stellar populations, chem-ical composition and dynamics of their host galaxies. This paper reports the dis-covery of new PNe in the outskirts of the Andromeda Galaxy (M 31) with the Guoshoujing Telescope (GSJT, formerly named the Large Sky Area Multi-Object Fiber Spectroscopic Telescope-LAMOST) during its early commissioning phase. In total, 36 candidates selected from SDSS photometry are confirmed in terms of their PN nature, including 17 new discoveries and another 19 previously known emission line objects. Their positions, spectra, radial velocities and m5007 magnitudes are presented.We discuss the potential for detecting more PNe in M 31 with GSJT's multi-object spectroscopy and the related applications in studies of the dynamics and chemistry of M31 and its assemblage history.     

Non－LTE Analysis of the Sodium Abundance of Metal－Poor Stars in the Galactic Disk and Halo

We performed an extensive non-LTE analysis of the neutral sodiumlines of Na I 5683/5688, 5890/5896, 6154/6161, and 8183/8195 in disk/halo starsof types F-K covering a wide metallicity range (-4 [Fe/H] +0.4), using ourown data as well as data collected from the literature. For comparatively metal-rich disk stars (-1 [Fe/H] +0.4) where the weaker 6154/6161 lines are thebest abundance indicators, we confirmed [Na/Fe] ～ 0 with an "upturn" (i.e., ashallow/broad dip around -0.5 [Fe/H] 0) as already reported in previousstudies. For the metal-deficient halo stars, where the much stronger 5890/5896 or8183/8195 lines subject to considerable (negative) non-LTE corrections amountingto 0.5 dex have to be used, our analysis suggests mildly "subsolar" [Na/Fe] valuesdown to ～ -0.4 (with a somewhat large scatter of ～±0.2 dex) on the average at thetypical halo metallicity of [Fe/H] ～ -2, followed by a rise again to a near-solar ratioof [Na/Fe] ～ 0 at the very metal-poor regime [Fe/H] ～ -3 to -4. These resultsare discussed in comparison with the previous observational studies along with thetheoretical predictions from the available chemical evolution models.     

Astrometric calibration of the Xuyi Schmidt Telescope Photometric Survey of the Galactic Anti-center （XSTPS-GAC）

We present astrometric calibration of the Xuyi Schmidt Telescope Photometric Survey of the Galactic Anti-center(XSTPS-GAC). XSTPS-GAC is the photometric part of the Digital Sky Survey of the Galactic Anti-center(DSS-GAC),which is a photometric and spectroscopic sky survey, in combination with LAMOST.In order to select an astrometric reference catalog, we made comparisons between the four widely used astrometric catalogs, GSC2.3, USNO-B1.0, UCAC3 and PPMXL.PPMXL shows relatively small systematic errors in positions and more homogeneous proper motion distributions toward the Galactic Anti-center(GAC), and was selected as the reference catalog. Based on the high quality and bright reference stars that were picked out from PPMXL, we performed a 4th-order polynomial fitting in image units,to construct the transformation relation between coordinates used by XSTPS-GAC and standard coordinates, and to simultaneously correct the image distortions in the CCD. Then we applied the derived relation to all sources to obtain their mean celestial coordinates based on the International Celestial Reference System. For bright point sources with r 17.0 mag, the accuracy of astrometric calibration could reach about80 mas for each of the g, r, i bands, with systematic errors being less than 10 mas. But for the faint sources at the brightness limit of the survey, which was r ～ 19.0 mag, the accuracy can still reach 200 mas. After combining all observations, the final weighted average coordinates could reach an accuracy of less than 70 mas for bright stars. For faint stars, the rms residuals of weighted coordinates decrease to ～ 110 mas. The final combined XSTPS-GAC coordinates show a good consistency with the Sloan Digital Sky Survey.     

New open cluster candidates discovered in the XSTPS-GAC survey

The Xuyi Schmidt Telescope Photometric Survey of the Galactic Anti-center(XSTPS-GAC)is a photometric sky survey that covers nearly 6000 deg~2 towards the Galactic Anti-center(GAC) in the g,r,i bands. Half of its survey field is located on the Galactic Anti-center disk,which makes XSTPSGAC highly suitable to search for new open clusters in the GAC region. In this paper,we report new open cluster candidates discovered in this survey,as well as properties of these open cluster candidates,such as age,distance and reddening,derived by isochrone fitting in the color-magnitude diagram(CMD).These open cluster candidates are stellar density peaks detected in the star density maps by applying the method from Koposov et al. Each candidate is inspected in terms of its true color image composed from three XSTPS-GAC band images. Then its CMD is checked,in order to identify whether the central region stars have a clear isochrone-like trend differing from background stars. The parameters derived from isochrone fitting for these candidates are mainly based on three band photometry of XSTPS-GAC.Moreover,when these new candidates are able to be seen clearly in 2 MASS data,their parameters are also derived based on the 2 MASS(J-H,J) CMD. There are a total of 320 known open clusters rediscovered and 24 new open cluster candidates discovered in this work. Furthermore,the parameters of these new candidates,as well as another 11 previously known open clusters,are properly determined for the first time.     

Mapping the emission line strengths and kinematics of supernova remnant S147 with extensive LAMOST spectroscopic observations

We present extensive spectroscopic observations of supernova remnant(SNR) S147 collected with the Large sky Area Multi-Object fiber Spectroscopic Telescope(LAMOST). The spectra were carefully sky-subtracted taking into account the complex filamentary structure of S147. We have utilized all available LAMOST spectra toward S147, including sky and stellar spectra. By measuring the prominent optical emission lines including Hα, [NⅡ]λ 6584 and [SⅡ]λλ 6717, 6731, we present maps of radial velocity and line intensity ratio covering the whole nebula of S147 with unprecedented detail. The maps spatially correlate well with the complex filamentary structure of S147. For the central 2?of S147, the radial velocity varies from-100 to 100 km s~(-1) and has peaks between～0 and 10 km s~(-1). The intensity ratios of Hα/[S Ⅱ]λλ 6717, 6731, [SⅡ]λ 6717/λ 6731 and Hα/[NⅡ]λ 6584 peak at about 0.77, 1.35 and 1.48, respectively, with a scatter of 0.17, 0.19 and 0.37, respectively. The intensity ratios are consistent with the literature values. However, the range of variations of line intensity ratios estimated here,which are representative of the whole nebula, is larger than previously estimated.     

文蛤(Meretrix meretrix)体内氨基脲含量与环境相关性研究

采用超高效液相色谱-串联质谱法进行了文蛤体内氨基脲含量与环境相关性研究。在(13±1)℃的水温条件下,将文蛤分别浸浴于氨基脲浓度1.0μg/L、5.0μg/L的海水中6天进行吸收试验,第7天起隔天换水进行消除试验,结果表明:文蛤对水体中氨基脲的富集能力较低,蓄积量随时间的延长和给药浓度的增加而增加。氨基脲在不同浓度中具有相似的消除规律:初始阶段均具有较高的消除速率,随后消除趋势趋于平缓,并在一段时间内维持一定质量分数;至试验结束时,低浓度组和高浓度组文蛤体内氨基脲最终降低至低于检出限(0.5μg/kg);本研究所得的药时曲线对贝类氨基脲污染的净化提供了数据支持。