PSPC(The 1st PSPC experience, Korea)

银道扫描科学目标分析（银道扫描科学工作组）一，硬X空间观测背景介绍1，目前硬X探测器SWIFT/BAT已经完成的巡天54 months, 2004-2009, 探测到1256 sources (>4.8 sigma)15-150keV50% sky coverage|b|<10, 0.43 mcrab|b|>10, 0.4 mcrab100% sky coverage|b| <10, 0.6 mcrabTill 2014: 5 years more exposure100% sky coverage|b| <10, 0.4 mcrab50% sky coverage|b|<10, 0.3 mcrab小结：Swift/BAT目前银道扫描已经达到灵敏度为0.4mcrab，到2014年前后可达到0.3mcrab.2，目前硬X探测器INTEGRAL/ISGRI 已经完成的巡天2002-2009, 7 years survey, 17-60 keV, 521 sourcesSky coverage:90% sky at 4.32 mCrab10% sky at 0.6 mCrabThe best sensitivity is about 0.26 mCrabGalactic center:22 Ms till 2011(1 Ms ~ 11.6 days)|b|<10 skyIn units of Ms, 2002.10-2011.03 (8.5 years)ISGRI总曝光在|b| <10为~ 70 Ms (~ 830days=2.3 yrs)Assuming a power law spectrum of an index -2.14, a Galactic absorption, an exposure of the above table corresponds to source detection of the follows (4 sigma level, in units of mCrab, in 15-200 keV) （results taken by using the ‘INTEGRAL observation time estimator’）1 Crab ~2.5x 10^-8 erg/cm2/s (15-200 keV)，（0.4 ct/cm2/s）小结: 以上是INTEGRAL的总曝光量，数据分析中还需要去掉坏时间段和slew等数据，而且还和假设的谱形和谱指数有关，可看做探测源灵敏度的上限。

a rXiv:as tr o-ph/13348v121Mar21**TITLE**ASP Conference Series,Vol.**VOLUME**,**PUBLICATION YEAR****EDITORS**The BMW Deep X–ray Cluster Survey Alberto Moretti,Luigi Guzzo,Sergio Campana,Stefano Covino,Davide Lazzati,Marcella Longhetti,Emilio Molinari,Maria Rosa Panzera,Gianpiero Tagliaferri Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807Merate,Italy Ian Dell’Antonio Physics Department,Brown University,Box 1843,Providence,RI,USA Abstract.We describe the main features of the BMW survey of serendip-itous X–ray clusters,based on the still unexploited ROSAT–HRI archival observations.The sky coverage,surface density and first deep optical CCD images of the candidates indicate that this sample can represent an excellent complement to the existing PSPC deep cluster surveys and will provide us with a fully independent probe of the evolution of the cluster abundance,in addition to significantly increasing the number of clusters known at z >0.6.1.Introduction In the last few years,X–ray selected samples of clusters of galaxies have become a formidable tool for cosmology.Deep surveys using ROSAT PSPC archival data have been used to study the evolution of the cluster abundance and X–ray luminosity function (XLF)and constrain cosmological parameters (e.g.Borgani et al.1999).The lack of evolution of the XLF observed for L ∼L ∗≃4·1044h 2erg s −1out to z ∼0.8favours low values for ΩM under reasonable assumptionsabout the evolution of the L −T relation.At the same time,the original hint from the EMSS (Gioia et al 1990;Henry et al.1992)of evolution at the very bright end of the XLF seems to be confirmed (Vikhlinin et al.1998,Nichol et al.1999,Rosati et al.2000and references therein).The main statistical limitation of this conclusion rests with the small sky coverage of the ROSAT deep surveys,which clashes with the intrinsic rarity of highly luminous clusters.XMM–Newton and Chandra are already attracting justified attention as the likely source for future samples,but no significant sets of serendipitously selected clusters can be reasonably expected from these observatories for at least another 2years.This presents the window of opportunity for our survey,which uses data from the ROSAT High–Resolution Imager (HRI)archive.With respect to the PSPC,the HRI offers superior angular resolution.Our results indicate that it is actually a surprisingly good source of samples of high-redshift clusters.Our new X–ray selected sample of candidate clusters of galaxies is based on the recently completed BMW survey of serendipitous X–ray sources over 300012Alberto Moretti et al.Figure1.Left:Sky coverage of the BMW survey,as a function ofX–rayflux and extension of the sources.Right:Same,but for a typicalfaint–source core radius∼10arcsec,compared to some previous X–raycluster surveys(see Rosati et al.2000for relevant references).Note thegood compromise between the fairly large area at intermediatefluxes(∼100sq.deg.around∼10−13erg cm−2s−1),and the depth of theBMW sample(1sq.deg.at2.5×10−14erg cm−2s−1).ROSAT HRIfields.The sample includes287candidates,with a significantly large sky coverage in comparison with other recent deep surveys.We are con-ducting a multi-site imaging campaing to fully identify the cluster sample.First results at ESO and TNG are extremely encouraging:with approximately an 80%rate of photometric confirmation in thefirst subsample of35candidates.2.The BMW ProjectThe Brera Multi-scale Wavelet(BMW)project has currently completed the systematic analysis of about3100HRI pointings using a wavelet detection algo-rithm(Lazzati et al.1999).This resulted in a catalog of∼19000serendipitous sources with measuredfluxes and extensions(Campana et al.1999,Panzera et al.2001).A clever selection of the HRI energy channels produced a reduction of the background noise by a factor of∼3,thus greatly improving the ability to detect low–surface–brightness sources as clusters.The BMW general cata-logue is built excludingfields with|b II|≤20◦or pointed on the LMC and SMC. Furthermore to build BMW cluster catalogue we have excluded cluster–targeted HRIfields to avoid the bias produced by the cluster–cluster angular correlation function,for which we have a clear positive detection in thesefields.Cluster candidates were isolated on the basis of their extension,selecting at a high sig-nificance level(corresponding to>5σ)and using only the well–sampled HRI area between3and15armin off-axis.We ended up with a list of287cluster candidates which were visually classified on the DSS2to reject obvious contam-inants(30rejections,mostly nearby galaxies).The BMW project is still under development such that a small assessment in the absolute number is expected.APS Conf.Ser.Style3 3.Survey Sky CoverageAn important parameter characterising a survey of serendipitous sources as the BMW is its sky coverage,i.e.the effective solid angle covered as a function of the limitingflux.Being based on archival pointings,different parts of the sky are observed with different exposure times.Thus,for each value of the X–ray flux f x the sky coverage is given by the total area of all observedfields with limitingflux f lim≤f x.In addition,due to the radial dependence of the point–spread function(PSF)of the ROSAT X–ray telescope,within a singlefield the effectiveflux limit is different for different off–axis angles and extensions of the sources.For this reason,the effective solid angle covered at different flux limits must be carefully estimated considering the instrumental set–up and the detection and characterisation methods adopted(e.g.Rosati1995).We have thereforefirst estimated the sky coverage of the BMW survey for extended objects by assuming aβmodel withβ=2/3,with a set of different core radii. For each core radius we have convolved the analytic profile with the PSF of the instrument at different off-axis angles and we have calculated the corresponding maximum in the wavelet space.Each HRI image has a detection threshold which is calculated in the wavelet space(Lazzati et al.1999)and is only function of the background.Thus for each image we could estimate directly the limiting detectionflux as a function of both the off-axis angle and source extension.In Figure1we compare the BMW cluster sky coverage to some previous X–ray cluster surveys.This relatively quick and straightforward method has some limitations(e.g.it does not tell us how well the wavelet extension is measured), that need to be explored through simulations.To this end,we are currently running an extensive set of simulations following the approach of Vikhlinin et al.(1998),and thefirst outputs for a small sample offields give results which are very close to the semi–analytic calculation,confirming that the sky coverage of Figure1should be a fair representation of our data.4.First Results from Optical Follow–up¿From the287candidates we have further selected a high priority sample of165 objects by excluding the HRIfields with exposure time smaller then10ksec. In spring2000,we started a long–term program of multi–band photometry and spectroscopy of thesefields,which is currently underway using telescopes in both emispheres(mostly the TNG in La Palma and the ESO3.6m telescopes).We have recently(September2000)reached a total of35candidates for which deep optical imaging has been secured in at least two bands.Preliminary analysis of these observations suggests a success rate(i.e.evidence for a galaxy overdensity correlated with the X–ray source)of about80%.The still unidentified20% fraction does not show any obvious pathology and we plan to add deep imaging in K′band,where the contrast of early–type galaxies is maximised,to definitely ascertain their nature.4Alberto Moretti et al.Figure2.Deep g+r+i images(typical exposure times∼5000 sec)with overlaid ROSAT–HRI X–ray contours,for a few examples of identified groups/clusters in the BMW survey.Indicative redshifts for these clusters range from z∼0.2(top left)to∼0.8(bottom right).In each image thefield of view is3x3arcmin.APS Conf.Ser.Style5D image of BMW080459+241(left,6000sec exposurein r+i Gunn bands)with X–ray contours superimposed,and its colour–magnitude diagram(right).A number of galaxies display a similarcolour along an apparent red sequence(filled dots)and their position onthe sky correlates significantly with the X–ray emission(diamonds overleft image).The colour is that expected for an early–type populationat z=0.6.5.DiscussionA hint of the scientific potential of the BMW catalogue can be obtained from the left panel of Figure4where the expected number of clusters as a function of redshift is plotted.These predictions use the computed BMW sky coverage of the high priority sample(165objects)and integrate the local X–ray luminosity function(De Grandi et al.1999)considering or not the evolution suggested by the RDCS,as reported in Rosati(1999).Simple comparison to the total expected numbers from Figure4would seem to imply that the BMW survey sees evolution in the XLF similar to the RDCS results.However,one has to await for the completion of the identification campaign to be able to place serious constraints on evolution.We should remark here the potential advantage of working with HRI data.In the right panel of Figure4we have plotted the apparent diameters of a rich cluster(r c=250kpc)and of a group of galaxies(r c=100kpc)as a function of redshift,together with a measure of the resolution of the ROSAT HRI compared to the PSPC.As one can see,the PSPC is not as suitable as the HRI for distinguishing groups of galaxies from point-like sources beyond redshift0.4. Of course,this simplistic plot depends on several variables,as the underlying cosmology,the source profile and in particular does not take into account the different noise level of the2instruments.Nevertheless,it shows that we should be able to explore the faint end of the XLF,the realm of groups,which could not be studied from PSPC data.In fact,the potentially large number of clusters in the BMW sample,when compared to prediction of evolution or no–evolution models,could also be produced by a steeper local XLF.References6Alberto Moretti et al.Figure4.Left:Expected integral distribution of BMW clusters asa function of redshift,with or without the evolution of the X–ray lumi-nosity function suggested by the RDCS(Rosati et al.1999).Right:Apparent angular diameter of a rich cluster(core radius250kpc)anda group of galaxies(core radius100kpc)as function of redshift,com-pared to the PSF of the two ROSAT instruments at the same off–axisangle(5armin).Borgani,S.,et al.1999,ApJ,517,40.Campana,S.,et al.1999,ApJ,524,423.De Grandi,S.,et al.1999,ApJ,513,L17.Henry,P.et al.1992,ApJ,386,408.Gioia,I.M.,et al.1990,ApJS,72,567.Lazzati,D.,et al.1999,ApJ,524,414.Nichol,R.C.,et al.1999,ApJ,521,L21Panzera,M.R.,et al.2001,in preparation.Rosati,P.1995,PhD thesis(University of Rome).Rosati,P.,et al.1998,ApJ,492,L21.Rosati,P.,et al.2000,in“Large-scale structure in the X–ray Universe”,in press (astro-ph/0001119).Vikhlinin,A.,et al.1998a,ApJ,498,L21.Vikhlinin,A.,et al.1998b,ApJ,502,558.。

关于PCC地理位置上，PCC是LA地区的一所community college，位于Pasadena，处在几个华人区之中，如Alhambra, Arcadia, Rosemead, San Gabriel。

因此PCC里面讲中文的人数是非常庞大的，不仅有国内来的留学生，也有不少当地High School升上来的华人学生。

所以其实在校园里看到中文其实是很平常的事情。

从地图上看，PCC也只不过是几个block的大小，但实际上这所学校的人数却能比得上很多University。

（具体数据可参照）之所以能够吸引附近几个城市的学生过来读书，很重要的原因是因为PCC的环境在LA，乃至整个南加州算是比较优秀的。

一者，Pasadena是一个富人区，高水平的物质生活带动起了整个城市其他方面的发展。

二者，世界闻名的加州理工就在PCC旁边，（过一条马路就到了）有不少教授都会以part-time的身份来到PCC教书，因此PCC的师资是不容小觑的。

小插曲一下，据说当年爱因斯坦来到美国之后，曾经在PCC学了一段时间的英语，然后才去Cal Tech深造的。

相信很多人来读PCC，很重要的一个原因是为了UC。

从转学率来看，PCC在整个加州还是很有竞争力的，尤其在南加州。

以UCLA 为例，以下网址为2010年的统计（2011的还没更新）/prospect/Adm_tr/Tr_Prof10_CAcc.htm。

2010年从PCC申请UCLA的有839人，其中录取的就有260人。

此数字虽为近几年最低，但也约为每三个申请UCLA的人就有一人成功。

而UCLA在2010年，从整个加州的超过100所community college中admit了4900+的学生，当中PCC占了5.30%，仅在Santa Monica College之后，排名第二（因为SMC与UCLA有commitment，而PCC目前还没有，所以难以比较）。

鉴于UCLA在整个美国的USNews大学排名中一直稳定在前30，公立学校甚至为前三，此录取率已是相当可观。

圣诞白金大作PSP《啪嗒砰》完美攻略第一章 MISSION 1 序欢迎来到Patapon的世界,在这里有一群快乐的"烧饼",我们只要按照背景音乐的节奏就可以指挥它们"前进,进攻"来打败敌人,重建家园。

首先我们先要熟悉Patapon们的音乐节奏,我们只要随着背景音乐的节奏按下"O"键就可以让幸存的烧饼旗手站了起来。

如果实在找不到感觉的话，那你就盯着游戏画面的边框，因为每次打节拍边框都会闪一下，尝试着随着音乐点点头或者跺跺脚就可以迅速适应。

接着我们获得了节拍PATA。

（按“□”键）并学会了我们的第一个命令：前进！PATA PATA PATA PON（□/□/□/O）。

和着背景音乐的拍子每次按下一个相应的按键就可以让可爱的烧饼们前进啦！当然，每按一次□/□/□/O只能让烧饼们前进一小截，如果你按下□/□/□/O/，然后听烧饼们喊：啪嗒啪嗒啪嗒砰，然后在按□/□/□/O，反复如此，就可以让烧饼们一直前进了。

突然画面左边冲出来一只大鸟龙，准确的按下□/□/□/O让烧饼们逃命吧。

通关后就来到村子里，村子还不够大，但以后会逐渐扩大。

在这里按L/R可以切换到其他场景，不过暂时现在还没有啥有用的。

按SELECT可以存盘，一定不要忘了。

按START可以退回主菜单。

第一章 MISSION 2 啪踏踏平原狩猎在纪念碑区按O就可以到Patapon的世界去冒险了。

选中关卡后会进入整备界面。

但是同志们呀，咱们还处于社会主义初级阶段，一没人二没房三没兵器四没粮，也没啥好整备的，直接按START进入吧。

一路上，我们学到了第二个命令：进攻！PON PON PATA PON O/O/□/O。

灵活的利用进攻和前进这两个命令一边前进一边狩猎，就可以轻松过关啦，过关后会根据你狩猎的成果得到一定量的肉LV1。

这可是生产新烧饼的必要材料哦。

第一章 MISSION 3 边境突出这个关隘是由英勇的士兵支撑的。

Appendix 3:Procedures for coating inspection and coating system repairduring ship constructionfor Dedicated Seawater Ballast Tanks in alI type of ships and Double-side Skin Spaces of Bulk Carriers(based on Resolution MSC. 215(82))2008在建船舶涂层检验与涂层系统修补程序针对所有船型专用压载水舱和散货船双舷侧处所（基于MSC. 215(82)决议）1Preface前言The Painting & Inspection Practice is prepared on the basis of the following:涂装及检验基于下述内容：1) Performance Standard for Protective Coatings(PSPC) for dedicated seawater ballast tanks in alltype of ships and double-side skin spaces of bulk carriers (IMO PSPC，Resolution MSC.215(82))保护涂层性能标准（PSPC）针对于所有船型专用压载水舱和散货船双舷侧处所（IMO PSPC，MSC. 215(82)决议）2) IACS Procedural Requirements No.34 on application of PSPCIACS No.34 程序需求应用于PSPC3) IMO PSPC—Q&As and Common Interpretations by IACSIMO PSPC—IACS Q&As 及通用解释4)Industry Guideline for Implementation of MSC. 215(82)MSC. 215(82)执行的工业指南The procedures are a guideline on how a successful new building project is to be executed, following the guidelines as indicated above.根据上述指南，此程序作为如何成功在新造船上实行的指南。

K K o o r r e e p p o o x x E E H H22335500双组份Two-ComponentK K o o r r e e p p o o x x E E H H22335500双组份Two-ComponentFlash Point 闪点Base [ EH2350 PTA ] : 26℃/79℉ (Closed cup) Curing Agent [ EH2350 PTB ] : 26℃/79℉ (Closed cup) 主剂[ EH2350 PTA ] : 26℃/79℉ (密闭杯)固化剂[ EH2350 PTB ] : 26℃/79℉ (密闭杯)Application Details 涂装指南Surface Preparation 表面处理Remove any oil, grease, dirt and any other contaminants from the surface before painting by proper method such as solvent cleaning and fresh water washing, etc.* Steel : Blast cleaning to Sa2.5 or power tool cleaning to St3, etc.涂装前使用适当方法例如溶剂清洁和淡水冲洗等清除待涂装表面所有油,脂,灰尘和其它污染物.* 钢材: 喷砂清洁至Sa2.5或动力工具清洁至St3.Application Conditions 施工条件The surface should be completely cleaned and dried. Do not apply when relative humidity is above 85%. The surface temperature should be at least 2.7℃(5℉) above dew point to prevent condensation. In confined areas, ventilate with clean air during application to assist solvent evaporation.涂装表面应完全清洁和干燥. 相对湿度不能超过85%, 表面温度至少高于露点2.7℃(5℉)避免结露. 封闭空间作业时提供清洁流通空气以助于溶剂挥发.Mixing 混合Base (Part A) : Curing Agent (Part B) = 4 : 1 (by volume)Mix thoroughly together prior to application in the proportions with power agitator as delivered. 主剂：固化剂= 4 ：1 (体积比)施工前按比例混合使用动力搅拌器充分搅拌.Pot Life 适用期3 Hours at 20℃/68℉3小时于20℃/68℉Preceding Coat 前道涂层Galvany Shopprimer IZ182 or according to specification. Galvany Shopprimer IZ182 或根据规范.Thinning 稀释Thinner No. 024.Do not dilute each components separately, only the mixture. 稀释剂No. 024, 不要单独稀释各组份, 应稀释混合物.Application Method施工方法Spray (Airless or Air), Roller or Brush application.For airless spray application ;Nozzle orifice : 483㎛~ 787㎛(0.019″~ 0.031″) Output pressure : 11.7 MPa ~ 15.2 MPaFan : 60˚(Airless spray data are indicative and subject to adjustment.) 辊涂, 刷涂, 喷涂(有气或无气) 施工.无气式喷涂;喷嘴口径: 483 ㎛~ 787 ㎛(0.019″~ 0.031″)喷嘴压力: 11.7 MPa ~ 15.2 MPa扇面: 60˚(无气式喷涂的有关数据可根据指导进行调整.)TypicalFilm Thickness 典型漆膜厚度100~200㎛dry.May be specified in another film thickness than indicated depending on purpose and area of use. 干膜厚度100~200㎛.干膜厚度根据使用用途及部位而异.Disclaimer : The information in this data sheet is believed to the best of our knowledge based on laboratory test and practical experience. However, there are many factors双组份Two-Componentaffecting the performance of product and the product quality itself, so we are not able to guarantee without the confirmation of the purpose of using the product from us in。