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At Last, Routine Particle Size DistributionMeasurement Enters the realm of the NanometerHoriba has refined its expertise in developing state-of-the-art particle size distribution measuring equipment for more than 20 years. Building on this wealth of experience and technology, we have developed the LB-500 Dynamic Light Scattering Particle Size Distribution Analyzer. Advanced application of dynamic light scattering theory has enabled HORIBA to reach a wide measurement range, spanning from the infinitesimal 3 nm, up to 6 micro meter. The handy cell-type system and user-friendly software com-bine to bring you remarkable ease of operation. In addition, the unit provides excellent capabilities for monitoring effects due to temperature and concentration of the sample,making the LB-500 ideally suited for both quality control and research applications.Point 1:High accuracy measurement of microscopic particlesPoint 2:Measurement of a wide range of sample concentrations and at concentrationsnear or equal to that of the original dispersion Point 3:Outstanding ease of operationEfficient, easy to use cell-type system. Optimal performance in measuring valuable or extremely small samples.Point 4:Feature-Loaded SoftwareMany new features have been included in the software, such as 3D display, learning, on-line help, print layout, and a cell check, among others.Applications:Advanced Materials Science, R&D, Quality Control•Abrasive slurries such as CMP and diamond •Carbon black•High resolution ink•UV blocking cosmetics (foundation, emul-sions, etc.)•Inks etc.•Paints, dyes and pigments •LatexesRecommended for Customers:•Already using dynamic light scattering particle size equipment who need to measure high concentration samples.•Already using laser diffraction or dynamic light scat-tering particle diameter distribution measuringequipment who need to measure smaller size particles than possible on the equipment currently being used.•Working in fields for which a micron sized particle is already considered to be a "large" particle.•Who want to know the variation in cohesion of dis-tributed particle diameter vis-a-vis concentration strength.•Who want to know the change in sample properties vis-a-vis temperature.The cell-type system is optimal for measuring precious experi-mental materials or extremely small samplesAn easy to use cell-type system has been adapted for use as the sample-holding vessel (a rectangular glass container). Simply pour the sample solution into the cell and it is readyto be measured with full accuracy. A 2 cc quantity of sample dispersion is sufficient.What's more, the dispersion can bereclaimed after measurement, preserving valuable samples. Optional unit providesgreater accuracy through precise temperature control. In order to allow measurement of samples whose size distributions are sensitive to temperature changes, the temperature of a sample can be adjusted via a heater or an electronic cooler (temperature adjustable model). Compared to the temperature bath controlled type, the data sampling function is much smoother. The temperature can be effectively controlled in the 20-70o C range.Supporting Simplicity, Accuracy,and Unmatched ease of operationApplied Dynamic Light Scattering Theory allows measurement fApplying “dynamic light scattering”theory, we bring you measurement capability over a wide range, from 3nm to 6 µm. Moreover, the time required from the start of the mea-surement to the displaying of the results is a speedy 2 minutes.Mirror with holeMirror surfaceLaser collimator lensLaser diodeLensPinhole filterLensSample particles contained in cellScattered laser light collecting lens Light collecting detection lensDetectorSignal converterLB-500 Optics SystemLight irradiated from a laser is passed through a lens and focused onto particles contained in the cell. The focal point of the lens is positioned on the inner wall of the cell, concentrating maximum light in order to suppress multiple-dispersions' that occurs when high concentration dispersion are measured.In addition, a pinhole filter removes errant beams,Find refractive index data for 1500 sampletypes and 800 types of dispersion media, inaddition to operation procedures, quickly andeasily using the on-line help function.Parameter settings necessary for measurementand operation procedures can be registered inadvance, enabling one-click automated opera-tions. The learning wizard provides conveniententry for data and operation procedures.Comparative measurement results as well asvariations in agglomeration due to changes intemperature ,can be viewed via the 3D display.The Real Time display makes changes in posi-tion readily detectable at a glance.Graphs, measurement results, etc. can bearranged as you like on the display screen.There is also a function enabling the insertionof a company name and logo. Measurementdata reports can be presented clearly andprofessionally to meet your every need. lity at Your Fingertipsfrom Nanometer-to-Micron RangeAble to measure red, blue, and 3 types of yellowinks without dilution.0.05 µm and 0.2 µm polystyrene latex compoundsample. Sample mixture was analyzed precisely andseparated into 2 peaks.Measurement Range for the LB-500Measurement Results ScreenCalculation resultsMemory graphData tableMeasurement results dataParticle diameter dispersion graphMeasurement ScreenReal time sample concentration displaySimple particle diameter distribution graphAutomatic check for cell contamination●The contents of this catalog are subject to change without prior notice, and without any subsequent liability to this company.●The color of the actual products may differ from the color pictured in this catalog due to printing limitations.●It is strictly forbidden to copy the content of this catalog in part or in full.Horiba continues contributing to the preservation of the global environment through analysis and measuring technology.●HORIBA, Ltd.Head OfficeMiyanohigashi, Kisshoin Minami-ku, Kyoto, Japan Phone: 81 (75) 313-8123Fax: 81 (75) 321-5725Tokyo Sales Office 1-7-8 Higashi-KandaChiyoda-ku, Tokyo, Japan Phone: 81 (3) 3861-8231Fax: 81 (3) 3861-8259Beijing Representative Office Room No. 410,No. 33 Cheng Fang Street, Xicheng District, Beijing P .R.O.C. 100032T.O.D. Beijing-9503-316Phone: 86 10-66077630/5Fax: 86 10-66077554Taiwan Representative Office No.15 Alley6, Lane 485, Sec. 1, Kuang Fu Rd.,Hsin-Chu, Taiwan, R.O.C.Phone: (886) 3-5799143Fax: (886) 3-5799164●HORIBA KOREA L t d .112-6 Sogong-DongChoong-ku, Seoul, Korea Phone: 82 (2) 753-7911Fax: 82 (2) 756-4972●HORIBA INSTRUMENTS INCORPORATEDIrvine Facility17671 Armstrong AvenueIrvine, CA 92614, U.S.A.Phone: 1 (949) 250-4811Fax: 1 (949) 250-0924Ann Arbor Facility 5900 Hines Drive Ann Arbor, MI 48108U.S.A.Phone: 1 (734) 213-6555Fax: 1 (734) 213-6525Leichlingen FacilityJulius-kronenberg Strasse D-42799 Leichlingen GermanyPhone: 49 (2175) 8978-0Fax: 49 (2175) 8978-50●HORIBA / STEC INCORPORATED 1080 E. Duane, Suite. A Sunnyvale, CA 94086U.S.A.Phone: 1 (408) 730-4772Fax: 1 (408) 730-8975●HORIBA INSTRUMENTS LIMITED Kyoto CloseSummerhouse RoadMoulton Park, Northampton NN3 6FL, U.K.Phone: 44 (1604) 542500Fax: 44 (1604) 542699●HORIBA INSTRUMENTS Pte. L TD.31 Kaki Bukit Road 3,#06-12 Techlink Singapore 417818Phone: 65 745-8300Fax: 65 745-8155●HORIBA EUROPE GmbH Head OfficeHauptstrasse 108D-65843 Sulzbach GermanyPhone: 49 (6196) 6718-0 Fax: 49 (6196) 641198HORIBA FRANCE Rue L. et A. Lumie `re TechnoparcF-01630 St-Genis-Pouilly FrancePhone: 33 (4) 50-42-27-63Fax: 33 (4) 50-42-07-74●HORIBA GmbH Kaplanstrasse 5A-3430 Tulln, AustriaPhone: 43 (2272) 65225Fax: 43 (2272) 65230HORIBA CZECHIAOrganizachi slozka Praha Petrohradska 13CZ-101 00 Praha 10, Czech Republic Phone: 420 (2) 717-464-80Fax: 420 (2) 717-470-64HORIBA SWEDEN Hertig Carlsv ¨ag 55-57S-15138 So ¨derta ¨lje SwedenPhone: 46 (8) 550-80701Fax: 46 (8) 550-80567HORIBA ITALY EuropalaceCorso Torino 43/4510043 Orbassano,Torino,Italy Phone: 39 (11) 9040601Fax: 39 (11) 9000448Bulletin:HRE-3649BPrinted in Japan ZH-R(SK)14•Data from a particle size distribution graph can be copied to the clipboard.•Supports importing and displaying of measurement data files created by LA-920/300 softwareThe LB-500 employs with a Class 1 Laser。
Atomic Absorption AAnalyst 400 AASpectrometerControl and Data SystemUser Interface Complete PC control of all functions of the AAnalyst™ 400 using WinLab32™ for AA software. WinLab32 for AA includes an innovative user interface that makes the software easy to learn and use, including a clear graphical design, task-oriented organization of the windows, an understandablevocabulary, extensive tool tips in multiple languages, simple data displays and Wizards for the simplification of many tasks.WinLab32 is fully multitasking, allowing the analyst to report analytical results, view data or add priority samples without interrupting the analysis in progress.Using WinLab32 software, setup is flexible and easy. Standard operating conditions for flame, graphite furnace and FIAS techniques are included.Auto Analysis Control links methods for each technique with a sample-information file. The sample list can be created by third-party software orLIMS and downloaded to the system.WinLab32 software provides many tools to increase lab productivity. With WinLab32 Offline, method and sample-information files can be createdand data reviewed or reprocessed without interrupting the current analysis.WinLab32 software provides extensive QC protocols to meet internal and regulatory requirements. Data Reprocessing allows changes to manymethod and sample-information parameters after data collection and the recalculation of the results using the new parameters. With DataReprocessing, the raw data are never altered, thereby ensuring data integrity is maintained.WinLab32 Reporter provides the ability to generate post-run reports in a variety of formats. The Export feature of Data Manager can be used toexport results as comma-delimited ASCII files for compatibility with commercial third-party programs such as Microsoft® Excel®, Access® and Word.21 CFR Part 11 An optional WinLab32 Enhanced Security™ package is available for labs needing to be compliant with 21 CFR Part 11 regulations.HardwareSystem True double-beam echelle optical system. Front surfaced, reflecting optics with protective coating. Deuterium background corrector and two built-in EDL power supplies.Optical System Echelle monochromator. Focal length: 300 mm. Grating: 36 x 185 mm area, 79 lines/mm, blaze angle 76˚. Fused-quartz prism: 95 x 40 mm, 60°.Wavelength: 189-900 nm. Spectral bandpass: 0.15 nm at 200 nm. Reciprocal linear dispersion: 2.4 nm/mm. The photometer optics are covered toprotect against dust and corrosive vapors. For maximum protection, the optical system can be purged with an inert gas.Detector High-efficiency, segmented solid-state detector.Light Sources Hollow cathode or electrodeless discharge lamps (EDLs). EDLs provide much higher light output and longer lifetime when compared to conventional hollow cathode lamps. Lamp elements, recommended operating currents and slit selection are automatically recognized and set when usingPerkinElmer® Lumina™ series AA lamps. Lamp alignment is completely automatic with the four-lamp turret.E-box All electronics are located in a single user-replaceable module that the operator can easily replace without requiring a service visit.For a complete listing of our global offices, visit /ContactUsCopyright ©2004-2010, PerkinElmer, Inc. All rights reserved. PerkinElmer ® is a registered trademark of PerkinElmer, Inc. All other trademarks are the property of their respective owners. PerkinElmer reserves the right to change this document at any time without notice and disclaims liability for editorial, pictorial or typographical errors. 006675E_01PerkinElmer, Inc. 940 Winter Street Waltham, MA 02451 USA P: (800) 762-4000 or (+1) Gas Controls and Burner SystemFlame GasFully automated gas box with computer-controlled oxidant selection, automatic gas sequencing, oxidant and fuel monitoring and control.ControlSoftware-actuated ignition with air/acetylene. Acetylene flow is automatically adjusted when switching to or from nitrous-oxide/acetylene operation.Flame SafetyFully interlocked operation prevents ignition if the proper burner head, the nebulizer, end cap or burner drain system are not correctly Featuresinstalled, the level of the liquid in the drain vessel is incorrect, or gas pressures are too low. Interlocks will automatically shut d own thegases if a flame is not detected. The flame is automatically and safely extinguished in the event of a power failure or when theemergency flame-off button is used.Burner SystemAn inert-polymer mixing chamber provides superior analysis of corrosive and high-solid matrices. The spray chamber is manufactured froma high-strength composite, eliminating the need for pressure-relief devices. The high-precision inert nebulizer maximizes stability andsensitivity. A 10-cm single-slot solid titanium burner head for air/acetylene operation is included. Optional burner heads include: 5-cmnitrous-oxide/acetylene, 10-cm three-slot air/acetylene and 5-cm single-slot air/acetylene.Sample Area 25 cm wide x 25 cm deep sample compartment for easy access to burner components.Accessories for the AAnalyst 400AutosamplersFlame autosamplers automate standard and sample introductions for instrument calibration and sample analysis, extending thespectrometer’s capabilities to those of a fully automated analytical workstation. Sample Dilution The AutoPrep 50 sample-dilution system provides an optimized tool for truly automated flame AA. With automatic, intelligent on-line dilution capabilities, the AutoPrep 50 eliminates the time-consuming, manual, error-prone portion of your flame AA analyses.Mercury/Hydride For the analysis of mercury or hydride-forming elements, an optional automated flow injection system or a manual mercury/hydride System system can be added. Flow Injection Atomic Spectroscopy (FIAS) combines the advantages of mercury/hydride AA with those of the flow injection, enabling mercury/hydride AA procedures to be truly automated.System SpecificationsDimensions70 x 65 (0.46 m 2) x 65 cm (W x D x H)Weight49 kg Power100-230 V (±10%), 50/60 Hz (±1%), 300 VA (maximum)TechnicalClassified as a laboratory instrument. Complies with the applicable European Union directives and standards for safety and electro-magnetic compatibility for CE Marking, the safety requirements for Canada and the United States for CSA/NRTL certification and the FCC requirements for radio-frequency emissions. The instrument was developed and produced in compliance with ISO 9001.Environmental Dust-free, free of vibrations, ambient temperatures: +15 ˚C to +35 ˚C with a change rate of a maximum 3 ˚C per hour. Relative humidity: 20% to 80% non-condensing.。
红外光谱特征峰对照表英文Infrared Spectroscopy Characteristic Peak Reference Table.Infrared spectroscopy is a valuable tool for the identification and characterization of compounds, as it provides information about the vibrations of the chemical bonds within a molecule. The infrared spectrum is typically divided into several regions based on the frequency of the vibrations, and each region corresponds to different typesof chemical bonds and vibrations. In this article, we will discuss the characteristic peaks commonly observed in infrared spectroscopy and provide an infrared spectroscopy characteristic peak reference table.1. Aromatic C-H Stretching Vibrations: 3100-3020 cm^-1。
This region corresponds to the stretching vibrations of aromatic C-H bonds. The presence of peaks in this region indicates the presence of aromatic rings in the molecule.2. Alkyl C-C Stretching Vibrations: 1450-1375 cm^-1。
污水湿地处理工程水力停留时间的测定①α卢学强 唐运平 李万庆 赵井林 隋 峰(天津市环境保护科学研究院, 天津 300191)摘 要 利用UA P 对一个湿地处理工程的实际水力停留时间进行了测定,进而对相关问题进行了探讨。
关键词 湿地处理 水力停留时间 UA P1 引言污水湿地处理系统,是一种利用生态工程原理构筑的自然净化工艺。
常见工艺类型有3种,即天然湿地(NW S )、自由水面型人工湿地(FW S )和地下水流人工湿地(SFS ),其中应用最广的是人工湿地,尤其是FW S 。
而人工污水湿地处理工艺的2个重要的工程参数为水力负荷和污染负荷,水力停留时间(HR T )则是决定这2个参数的基本条件。
湿地处理工程设计中常用的Eckenfelder 公式、Donan 公式、Hooghoudt 公式等都从不同角度反映了HR T 与水力负荷及污染负荷间的关系。
本文工程实例取自“八五”国家优秀示范工程,天津大港石油管理局城区污水湿地处理工程(10000t d ),工程占地313525hm 2,水力负荷4187c m d ,进水水质BOD 5<180m g L 、SS <150m g L ,出水水质BOD 5≤20m g L 、SS ≤20m g L ,工程共有处理单元28个(40m ×120～210m ),单元两侧设侧渗沟与单元中部设渗滤暗管集水,出水经泵站至鱼塘进行回用。
2 水力停留时间测定实验水力停留时间的测定主要依靠示踪技术,而常用的示踪计主要有3类,即无机盐类(以N aC l 为主)、放射性同位素和染料类。
由于大港地区具较高的盐碱本底,不宜用N aC l 作示踪剂,放射性同位素因其容易造成放射性污染且需要一定的防护措施,亦非首选方法,故而本文利用了一种特殊染料进行了HR T 实测尝试。
211 测定方法示踪剂:瑞士M erck 公司UA P 绿色荧光染料。
测试仪器:日本岛津R F -540荧光光度计。
收稿日期:2008209202 修回日期:20082102283通讯联系人:来国桥,男,教授,从事有机硅化学研究.第25卷第5期Vol.25 No.5分析科学学报J OU RNAL OF ANAL YTICAL SCIENCE 2009年10月Oct.2009文章编号:100626144(2009)0520615203含氢聚硅氧烷含氢量的红外光谱测定研究盛春荠,蒋可志,倪 勇,邱化玉,来国桥3(杭州师范大学有机硅化学及材料技术教育部重点实验室,浙江杭州310012)摘 要:本文利用含氢聚硅氧烷中的Si —H 键在2172cm -1处的吸收峰,选择四甲基四氢环四硅氧烷作为模型化合物,用偏最小二乘法建立了红外光谱法测定含氢聚硅氧烷中含氢量的方法,其有效测量范围为0.0043～0.5365mg/mL ,回收率在91%～106%之间。
关键词:红外光谱法;定量分析;含氢聚硅氧烷;偏最小二乘法中图分类号:O657.33 文献标识码:A含氢聚硅氧烷是一种重要的有机聚合物,可用作天然及合成纤维织物、丝绸、皮革的防水剂和柔软剂,纸张的防粘、防水剂等。
其分子中活泼的Si —H 键易于发生交联反应,可用于制备多种有机硅衍生物,用途非常广泛。
含氢聚硅氧烷含氢量的大小是其一个重要的指标,对产品的性能有较大的影响,因此测定含氢量就成为控制含氢聚硅氧烷质量的一种必要的手段。
目前含氢量的测定主要采用化学法[1],也可采用分光光度法[2]、质谱法[3]和核磁共振法[4],但在工业生产中的应用有一定的局限性。
由于Si —H 键在2173cm -1左右的特征吸收峰基本没有其他基团吸收的干扰,适合作为定量分析的特征峰,而且红外光谱仪价格较为低廉,测试成本较低,所以有人用红外光谱法进行简单线性回归建立定量分析法[5]。
本文用比耳定律法确定了Si —H 含量检测的有效范围在0.0043～0.5365mg/mL 。
由于偏最小二乘法将因子分析和回归分析相结合,可以消除由于样品本身和人为因素产生的偏差[6,7],所以利用偏最小二乘法和红外光谱法建立了含氢硅油含氢量检测的工作曲线,并且通过回收率的验证,结果令人满意。
第21卷第4期高分子材料科学与工程Vo l.21,N o.4 2005年7月POLYM ER M ATERIALS SCIENCE AND ENGIN EERING Jul.2005聚丙烯酰胺/蒙脱土复合材料结构研究X高德玉1,RB-海曼2,B-托马斯2,李 红3,刘宇光1,侯 静1,郑 辉1,倪靖滨1(1.黑龙江省科学院技术物理研究所,黑龙江哈尔滨150086; 2.德国弗莱堡矿业大学;3.黑龙江大学,黑龙江哈尔滨150080)摘要:用红外(F T-I R),X射线衍射(X RD),核磁共振(NM R,13C,27A l,29Si)对电子束和紫外辐照制备的纳米结构聚丙烯酰胺/蒙脱土复合材料进行了表征。
结果表明,丙烯酰胺以双分子层嵌入蒙脱土层间形成复合体,使蒙脱土层距由1.25nm增大到2.09nm。
在复合材料中丙烯酰胺有三种形式:嵌入蒙脱土层间,通过氢键结合在蒙脱土表面和“自由”聚合物。
关键词:蒙脱土;聚丙烯酰胺;纳米复合材料中图分类号:T B383 文献标识码:A 文章编号:1000-7555(2005)04-0201-04 蒙脱土由于其特有的层状结构,目前被广泛用于纳米材料的制备[1～5]。
关于聚丙烯酰胺和蒙脱土复合材料的制备及应用已有很多研究[6～10]。
制备蒙脱土/聚合物插层复合材料通常有两种方法,一种是将聚合物直接嵌入蒙脱土;另一种是将单体先嵌入蒙脱土然后进行原位聚合。
本文使用仪器分析方法对第二种方法制备的聚丙烯酰胺/蒙脱土复合材料结构进行了初步研究。
1 实验部分1.1 试样制备试剂:丙烯酰胺(AM),丙烯酸钠(AANa),苯乙烯磺酸钠(SSNa),乙烯磺酸钠(VSNa),以上试剂均为分析纯,Fluka Chem ie,瑞士产品;蒙脱土:分析纯,S D-CHEMIE,德国产品。
SAP/蒙脱土复合试样(SAPC)的制备:将蒙脱土(30%质量比)悬浮在蒸馏水中,与含有丙烯酰胺及添加剂的水溶液混合(30%),然后使用电子束或紫外线照射完成聚合过程[6,7]。
论文题目（英文题目要译成中文）期刊名倾斜极化磁多层膜的铁磁共振理论Phys. Rev. B Rapid response mechanism of pi cell（Pi 盒的快速响应机制）Appl. Phys. Lett.Response times in Pi-cell liquidcrystal displaysLiq. Cryst.弱锚定垂面排列液晶显示器的响应时间液晶与显示栅状表面液晶盒的光学属性计算物理中文图形12864点阵液晶显示模块与51单片机的并行接口电路及C51程序设计现代显示Monte Carlo 模拟空间各向异性势向列相液晶微滴计算物理基于修正Gruhn-Hess 两体势模型的内禀锚定研究Physics letters. 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第29卷,第9期 光谱学与光谱分析Vol 129,No 19,pp2480-24842009年9月 Spectro sco py and Spectr al AnalysisSeptember ,2009周口店花岗闪长岩中斜长石晶体化学及谱学特征研究张永旺1,2,曾溅辉1,2,刘 琰3,郭建宇41.中国石油大学油气资源与探测国家重点实验室,北京 1022492.中国石油大学(北京)盆地与油藏研究中心,北京 1022493.中国地质大学地质过程与矿产资源国家重点实验室,北京 1000834.中国石油勘探开发研究院海外研究中心,北京 100083摘 要 前人研究多集中于碱性长石等其他长石系列,对斜长石的研究较少。
在野外地质工作的基础上,采用电子探针仪、X 光粉晶衍射仪、红外光谱仪和拉曼光谱仪对周口店花岗闪长岩中自然产出的斜长石进行了谱学特征和化学成分分析。
电子探针分析获得该地斜长石的化学成分,端元组分在Ab (85121)Or (0118)An (9111)到A b (90106)Or (3100)A n (13127)之间;斜长石的X 光粉晶衍射特征说明样品组成为较为纯净的钠长石,根据粉晶衍射峰及其衍射强度计算得出了样品晶胞参数;采用红外光谱和拉曼光谱分析了斜长石的谱学特征并对特征吸收谱带和特征峰进行了归属。
在OH -红外吸收区(3000~3800cm -1)出现了由O H 的伸缩振动导致的特征吸收谱带:3200,3310,3420和3615cm -1,表明研究区的钠长石普遍含有结构水,以O H -的形式存在。
在以上分析的基础上对此种长石的晶体化学和结构特征进行了归纳总结。
关键词 X 光粉晶衍射;红外光谱;拉曼光谱;电子探针;斜长石中图分类号:O 65713 文献标识码:A DOI :1013964/j 1issn 11000-0593(2009)09-2480-05收稿日期:2008-09-28,修订日期:2008-12-29基金项目:中国博士后科学基金项目(20070420492)和国家自然科学基金项目(40472075)资助 作者简介:张永旺,1975年生,中国石油大学(北京)油气资源与探测国家重点实验室博士后e -mail:zyw 75@1261com,z yw75@s ohu 1com引 言作为燕山运动产物的周口店岩体,产于距北京城西南约40km 的西山地区。
a r X i v :a s t r o -p h /0608014v 1 1 A u g 2006Mon.Not.R.Astron.Soc.000,1–5(2006)Printed 5February 2008(MN L A T E X style file v2.2)Spectropolarimetry of PKS 0040−005and the Orientationof Broad Absorption Line Quasars ⋆M.S.Brotherton 1†,C.De Breuck 2⋆‡,and J.J.Schaefer 3§¶1Department of Physics and Astronomy,University of Wyoming,Laramie,WY,82072,USA2EuropeanSouthern Observatory,Karl Schwarzschild Strasse 2,Garching Bei Munchen,85748,Germany3Department of Astronomy,University of Florida,211Bryant Space Science Center,Gainesville,FL 32604,USA5February 2008ABSTRACTWe have used the Very Large Telescope (VLT)to obtain spectropolarimetry of the radio-loud,double-lobed broad absorption line (BAL)quasar PKS 0040−005.We find that the optical continuum of PKS 0040−005is intrinsically polarized at 0.7%with an electric vector position angle nearly parallel to that of the large-scale radio axis.This result is naturally explained in terms of an equatorial scattering region seen at a small inclination,building a strong case that the BAL outflow is not equatorial.In conjunction with other recent results concerning radio-loud BAL quasars,the era of simply characterizing these sources as “edge-on”is over.Key words:polarization -quasars:individual (PKS 0040−005).1INTRODUCTIONDepending on the selection techniques used,some 10-30%of luminous quasars show blueshifted broad absorption lines (BALs)indicative of substantial outflows.By carrying away angular momentum,these outflows may be a fundamental part of the accretion process,and they may also be impor-tant for chemically enriching the interstellar and even in-tergalactic mediums.There is still no consensus about the nature of BAL quasars,however,although many possibilities have been discussed (e.g.Weymann et al.1991).One possibility is that quasars only possess such high-velocity outflows during a relatively short-lived evolutionary phase during which they blow material out of the nuclear region (e.g.,Voit et al.1993;Becker et al.2000;Gregg et al.2002;Gregg et al.2006).Another is that BAL quasars and normal quasars may be unified through orientation as for some other AGN classes.In this popular equatorial paradigm,BALs are seen in quasars viewed at high incli-nation angles such that the line of sight passes through an equatorial wind (e.g.,Hines &Wills 1995;Cohen et al.1995;Goodrich &Miller 1995;Murray &Chiang 1995).Polarimetry can be a useful tool for testing the latter idea,“unification by orientation,”because scattering pro-cesses leading to polarization when geometric asymmetries⋆Based on observations collected at the European Southern Ob-servatory,Paranal,project 71.B-0121(A).†E-mail:mbrother@ (MSB),ESO Visitor ‡E-mail:cdebreuc@.¶E-mail:schaefjj@ufl.eduare present.Antonucci (1983)first pointed out that Seyfert 1and Seyfert 2galaxies both display optical polarization,but in the type 1galaxies the polarization electric vector is paral-lel to the radio axis,while in type 2galaxies the two are per-pendicular,suggesting different geometries for the two types and helping to lead to the unification of Seyfert galaxies through orientation.Spectropolarimetry of NGC 1068(An-tonucci &Miller 1983)showing a type 1broad-lined spec-trum in polarized light made the case compelling.Broad-lines and continuum may be scattered by a polar scattering region along the jet axis,leading to perpendicular angles,while equatorial scattering in a Seyfert 1leads to the par-allel angles.This work has been greatly expanded in recent years (e.g.,Smith et al.2004)and also applied to radio-loud AGNs at both low and high redshift (e.g.,Cimatti et al.1993;Cohen et al.1999;Vernet et al.2001).When radio-loud BAL quasars began to be found (Becker et al.1997;Brotherton et al.1998;Becker et al.2000),Brotherton et al.(1997)proposed that the alignments of the jet axes and polarization angles should be measured to test BAL quasar geometry in the same way as in other AGNs.Despite the discovery of radio-loud BAL quasars,very few have shown extended jets permitting this test.In order to pursue questions concerning the nature of BAL quasars,we searched for BAL quasars with extended radio structures by examining Sloan Digital Sky Survey quasars (Schneider et al.2002)and their radio maps from FIRST Survey (Becker,White,&Helfand 1995).We classi-fied SDSS 004323.43−001552.43as an extended,radio-loud FR II BAL quasar.This quasar was previously detected by2M.S.Brotherton,C.De Breuck,and J.J.SchaeferFigure1.Spectropolarimetric results for PKS−005.The top panel shows the totalflux spectrum in units of ergs s−1cm−2˚A−1×1016. The middle panel shows the debiased percentage linear polarization,while the bottom panel shows the position angle.Error bars on the big bins represent1σuncertainties.The light grey bins in the bottom panels are9˚A.many radio surveys and is better known as PKS0040−005. PKS0040−005(z=2.806)has also been recently classified as a FR II BAL quasar by Gregg et al.(2006)and Zhou et al. (2006).We targeted PKS0040−005for spectropolarimetry to test the geometry of BAL quasars.2OBSER V ATIONS AND DATA2.1VLT SpectropolarimetryWe obtained spectropolarimetric observations of PKS 0040−005on UT2003September20and21using the PMOS mode of the FORS1spectrograph(Appenzeller et al.1998) on the Antu unit of the ESO Very Large Telescope(VLT). On September20,we observed the source at airmass be-tween1.83and1.62with1.0′′seeing.To obtain more sen-sitive data,we re-observed the source during the next night with airmass1.15and0.7′′seeing.Conditions were photo-metric on both nights.The observations were split into four 300s exposures,each at a different orientation of the half-wave plate(0◦22.5◦,45◦,67.5◦).We used the300V grism with a1.0′′wide slit oriented North-South,resulting in a spectral resolution of∼10˚A(FWHM).We reduced the data using standard IRAF procedures. We extracted the spectra with identical4′′wide apertures for the o and e-rays,and re-sampled all8individual spec-tra(o and e-rays for the4half-wave plate positions)to the same linear dispersion(2.6˚A/pix)in order to calculate the polarization in identical spectral bins.We used the proce-dures of Vernet(2001;see also Vernet et al.2001),which are based on the method described by Cohen et al.(1997). We checked the polarization angle offset between the half-wave plate coordinate and the sky coordinates against values obtained for the polarized standard stars BD5133and NGC2024NIR1and the unpolarized standard star GD50; our values are within<1◦from the published values,and the polarization percentage within0.1%.Figure1shows our results.2.2Supplemental Data and InformationThe1.5GHz map of PKS0040−005from FIRST(Becker et al.1995)shows a double-lobed source that has a position angle of51◦.Gregg et al.(2006)show the map,and provide additional measurements based on the radio image and the optical SDSS spectrum.They assume a cosmology of H0= 71km s−1Mpc−1and q0=0.5,and report a1.4GHz radio luminosity(ergs s−1)of log L1.4GHz=34.1,an absolute g magnitude of M g=−26.44(and−26.78after correcting for an estimate of small intrinsic reddening),and a radio loudness parameter log R*(Stocke et al.1992)of2.9(2.7 dereddened).The radio source is117kpc across for this cosmology,the smallest of their eight sources.The radio core dominance,or core-to-lobeflux at1.4GHz,they report to be0.09.The C IV BAL has a balnicity index(Weymann et al.1991)of1073km s−1.The homogenized radio data available through the NASA Extragalactic Database(NED)shows that the radio spectrum of PKS0040−005is steep,with a radio spectral indexα=−1.2(Sν∝να).3RESULTSAveraging over the central spectral region where the signal-to-noise ratio is high and the data are well behaved,PKS 0040-005shows intrinsic continuum polarization(0.72±0.08%)at a well-defined position angle(36±3◦).The polar-ization is intrinsic.The interstellar polarization(ISP)fromPKS0040−005and BAL Quasar Orientation3 aligned dust grains is expected to be very low toward thissight line,since the Schlegel et al.(1998)extinction E(B-V)is only0.017mag,and the maximum ISP polarization shouldbe less than9×E(B−V)%(Serkowski et al.1975),or0.15%.Furthermore,the polarization rises in the C IV BAL troughbottom(and perhaps Lymanα)showing that the polariza-tion must be intrinsic.Rising polarization in trough bottomsis seen in many BAL quasars and has been interpreted asthe result of the scattered line of sight being less absorbedthan the direct line of sight(e.g.,Ogle et al.1999).While we prefer an explanation of scattering as the ori-gin of the polarization,the data quality is insufficient to completely rule out synchrotron emission.The polarizedflux spectrum is noisy and not inconsistent with a power-law. PKS0040−005is a steep spectrum FR II radio source with strong lobes and a weak core,suggestive that it is not be-ing viewed directly jet on which is usually required for syn-chrotron to be important,but the polarization level here is relatively weak and it is possible and has been seen in other sources(Schmidt&Smith2000).We argue below,under the assumption that the polarization arises from scattering, that PKS0040−005and its BAL outflow is not seen at a particularly high inclination angle.The case for this is only stronger if the polarization is from beamed synchrotron.4DISCUSSIONThe position angle of the continuum polarization(36±3◦) is close to parallel to the large-scale radio axis(∼51◦),a difference of15◦,and is thefirst BAL quasar found with this property.In analogy to the Seyfert galaxies and radio galaxies/quasars,this suggests a geometry in which PKS 0040−005is not seen edge-on,but at some modest incli-nation angle(consistent with the smallish but double-lobed radio structure),and the scattering takes place in an equa-torial scattering region.Good illustrations of this geometry can be seen in Figures6and10of Smith et al.(2004).Lamy&Hutsem´e kers(2004)explored the concept of a “two component wind”for BAL quasar outflows,that in-cluded both equatorial and polar outflows,and had support from theoretical models(e.g.,Proga2000,2003;Pereyra et al.2004),which are variations of the disk wind of Murray et al.(1995).Lamy&Hutsem´e kers(2004)were trying to explain not only some correlations they found in the polari-metric properties and their relationship to BAL properties, but also the source of the polar scattering region.The fact that sometimes polarization angle rotations are seen across emission lines in BAL quasars,or with changes in wave-length,is suggestive that more than one scattering path is likely present.Our observation of PKS0040−005fits into this picture,and in fact its other properties are also con-sistent with the relationships Lamy&Hutsem´e kers(2004) report:the continuum polarization is low which corresponds to a large BAL detachment and weak absorption in the po-larizedflux spectrum.We can compare the alignment in PKS0040−005to other BAL quasars.Table1summarizes the optical polar-ization properties and radio position angles of BAL quasars for which both quantities have been reported.References provided for each are relevant to the discovery or classifi-cation,or provide details for the information given inthe Figure2.Histograms of∆θ,the difference between the radio axis position angle and the electric vector of the optical/ultraviolet continuum linear polarization.The top panel shows broad-lined type1AGNs,including Seyfert1galaxies(shaded),broad line radio galaxies,and some scattered-light quasars(see text).The bottom panel shows narrow-lined type2AGNs,including hidden-broad-line Seyfert2(shaded)and radio galaxies(see text).The middle panel shows BAL quasars from Table1.table.Some entries are averages over a wide range of wave-lengths(e.g.,broad band or white light observations),but when explicit ranges are given,it indicates that the values change as a function of wavelength.Figure2shows histograms of the difference in position angle between the electric vector of the continuum polariza-tion and the radio axis for BAL quasars from Table1,and for comparison also broad-lined type1and narrow-lined type2 AGNs.When the position angle has a range,we take the middle value to place the object in a bin.The broad-line AGNs include Seyfert1galaxies from Brindle et al.(1990), broad line radio galaxies from Cohen et al.(1999),and sev-eral higher redshift radio-loud quasars with high scatter-ing polarization(Goodrich&Miller1988;Brotherton et al. 1998;De Breuck et al.1998).Type1AGNs with scattering polarization,both radio loud and radio quiet,show both par-allel and perpendicular behavior.The type2AGNs include Seyfert2galaxies from Brindle et al.(1990),using only those with hidden broad-line regions(see Tran2003)and well-defined angles,and high-redshift radio galaxies from Vernet et al.(2001).When type2objects are restricted to those with scattering polarization,the radio and polarization axes are perpendicular.Before our observation of PKS0040−005,it would have been easy to conclude based only on the available angle dif-ferences that BAL quasars were,like type2AGNs,seen edge-on.There are some selection effects at work,however, with so few BAL quasars having this measurement available. A“jet on”quasar will be a smaller radio source than it would4M.S.Brotherton,C.De Breuck,and J.J.SchaeferTable1.Polarization-Radio Alignments of Broad Absorption Line QuasarsPKS0040−005 2.81HiBAL0.72±0.08%36±35115This PaperFIRST J1016+5209 2.46HiBAL2-375-8514671-81Gregg et al.2000UN J1053−0058 1.55LoBAL 1.9902763Brotherton et al.1998Lamy&Hutsem´e kers2000(pol) FBQS1312+2319 1.52HiBAL 1.11665983Becker et al.2000Sluse et al.2004(pol)Jiang&Wang2003(rad) LBQS1138−0126 1.27LoBAL3-4150-1805252-82Brotherton et al.2002PG1700+51530.29LoBAL0.65514588Kellerman et al.1994(rad)Schmidt&Hines1999(pol) PKS1004+1300.24HiBAL0.7-1.624-6311754-87Wills et al.1999Webb et al.1993(pol)PKS0040−005and BAL Quasar Orientation5ways clear at what wavelength the polarization position an-gle should be compared to the radio position angle.Angle rotations indicate multiple scattering axes in a number of BAL quasars,and type1Seyferts can show both polar and equatorial scattering(Smith et al.2004).Supporting a polar outflow in Mrk231,Punsly&Lipari(2005)claim there is an outflow aligned with the small-scale jet angle based on two-dimensional spectroscopy of the blue wing of Hα.5CONCLUSIONSPKS0040−005is a radio-loud BAL quasar with low but intrinsic continuum polarization.The electric vector of the continuum polarization is close to parallel to the position an-gle of the quasar’s extended radio structure.This is naturally explained as the result of scattering in an equatorial region with a face-on geometry,just as in Seyfert1and broad-line radio galaxies.Our result,taken in conjunction with other results in the literature,seems to be the end of the popu-lar but apparently too simple idea that BAL outflows are always equatorial.ACKNOWLEDGMENTSWe thank Joel Vernet for his reduction software package and discussions concerning the data.MSB thanks the ESO Scientific Visitor Programme for support and hospitality. 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