BVRcIc photometry of GRB970508 optical remnant May-August,
- 格式:pdf
- 大小:313.12 KB
- 文档页数:8
定制化产品手册北京大恒图像视觉有限公司Beijing Daheng Image Vision Co.,Ltd.产品介绍About UsIntroduction Cooperation 公司简介行业合作范恒久品质大家风着“伙伴”的责任,以唯有为客户创造价值才能实现自身价值的合作共赢模式,踏实前行,与客户共同成长。
我们希望能够发挥自己的力量,为中国机器视觉行业的发展带来新的探索和思路,为信任和支持我们的客户创造更高的价值,赢得经久不息的掌声。
北京大恒图像视觉有限公司AIA证书高层�%其他EMVA证书质量体系证书质量体系证书中国机器视觉产业联盟发起单位采用国际领先的软硬件设备品牌:美国Teledyne DALSA,德国Allied Vision、AT(Automation Technology)、Chromasens、MVTec、Schneider,瑞士AOS,日本BlueVision,加拿大Osela等。
视觉部件直接厂商供货,引进国际最先进的产品和技术,保护客户投资,保障售后维保。
产INTRODUCTION品介绍系统参数:02可检缺陷类型短路、断路、线宽、线细、绝缘间距不足、线缺口、线凸起、浆料上异物、多图形、少图形、异物、脏污图像采集分辨率�.�um/像素(特殊需求可定制)检测速度≤��s/片(�英寸(���*���mm)料片,含机构运行时间)缺陷检测精度��um(特殊需求可定制)适应料片尺寸≤�英寸(���*���mm)缺陷图例:断路缺口墨点缺口缺图形多图形浆料金属化绝缘间距不足脏污绝缘间距不足异物线宽不足03全自动化检测,在线离线可选,检测精度高达�um;自适应识别,自动规划路径,根据大小自主拍照检测;高效率,快速检测不停线,维护方便。
0405系统参数:设备类型芯片金线检测系统检测精度�.��mm/p检测类别检测速度离线、在线静态拍摄工作环境万级无尘车间,恒温恒湿金线断开、计数、焊点有无、焊点形状、线弧位置、宙吊变形、PIX膜破损等可根据客户的需求进行定制化的研发,软硬件皆可;全自动完成每个工件的入料、检测、踢废、出料等所有检测项目;能够将所有检测数据按照客户需求进行归类,存入数据库;能和客户的MES系统进行交互,反馈检测结果;缺陷尺寸的定量测量,结果稳定可靠。
OPERATING MANUAL • WARNING INFORMATION • PARTS LISTWARNINGFAILURE TO OBSERVE THESE WARNINGS COULD RESULT IN INJURY THIS INSTRUCTIO N MAN U A L CO N T AINSIM P O R T ANT SAFE T Y INFO RMATIO N.READ THIS IN S TRUC T IO N MANUAL CARE F UL L YAND UN D ER S TAND ALL IN F O R M A T IO N BE F O REO P E R A T I NG THIS TO O L.• It is the responsibility of the owner to make sure allpersonnel read this manual prior to using this air tool.It is also the responsibility of the air tool owner to keepthis manual intact and in a convenient location for allto see and read. If the manual or product labels arelost or not legible, contact Cornwell for replacements.If the operator is not fluent in English, the product andsafety instructions shall be read to and discussedwith the operator in the operator's native language by the purchaser/owner or his designee, making surethat the operator comprehends its contents.• Al w ays op e r a te, in s pect and main t ain this tool in ac c or d ance with Amer i c an Na t ion a l Stan d ardsIn s ti t ute Safe t y Code of Por t a b le Air Tools (ANSIB186.1) and any oth e r ap p li c a b le safe t y codesand reg u l a t ions.• For safety, top per f or m ance and max i m um du r a b il i t y of parts, op e r a te this tool at 90 psig: 6.2 bar max airpres s ure with 3/8" di a m e t er air sup p ly hose.• Always wear im p act-re s is t ant eye pro t ec t ion when op e r a t i ng or per f orm i ng main t e n ance on this tool(users and bystanders).• Al w ays wear hear i ng pro t ec t ion when us i ng this tool (users and bystanders). High sound levels can cause per m a n ent hear i ng loss. Use hear i ng pro t ec t ion asrec o m m end e d by your em p loy e r or OSHA reg u l a t ion.• Keep the tool in ef f i c ient op e r a t i ng con d i t ion.• Operators and main t e n ance per s on n el must be phys i c al l y able to han d le the bulk, weight andpow e r of this tool.• Keep tool out of reach of children.Air un d er pres s ure can cause se v ere in j u r y. Nev e rdi r ect air at your s elf or oth e rs. Al w ays turn off theair sup p ly, drain hose of air pres s ure and de t achtool from air sup p ly bef ore in s tall i ng, re m ov i ng orad j ust i ng any ac c es s o r y on this tool, or be f oreper f orm i ng any main t e n ance on this tool. Fail u reto do so could re s ult in in j u r y. Whip hos e s can causese r i o us in j u r y. Al w ays check for dam a ged, frayed orloose hos e s and fit t ings, and re p lace im m e d i a te l y.Do not use quick de t ach cou p lings at tool. Seein s truc t ions for cor r ect set-up on page 4.Air powered tools can vi b rate during use. Vi b ra t ion,re p et i t ive mo t ions or un c om f ort a ble po s i t ions overex t end e d pe r i o ds of time may be harm f ul to yourhands and arms. Dis c on t in u e use of tool if dis c om f ort,tin g ling feel i ng or pain oc c urs. Seek med i c al ad v icebe f ore re s um i ng use.Place the tool on the work before starting the tool.Do not point or indulge in any horseplay with this tool.• Slip p ing, tripping and/or falling while op e r a t i ng air toolscan be a ma j or cause of se r i o us in j u r y or death. Be awareof ex c ess hose left on the walk i ng or work sur f ace.• Keep body work i ng stance bal a nced and firm. Do notover r each when op e r a t i ng the tool.• Anticipate and be alert for sud d en chang e s in mo t iondur i ng start up and op e r a t ion of any pow e r tool.• Do not carry tool by the hose. Pro t ect the hosefrom sharp ob j ects and heat.• Tool shaft may continue to rotate briefly after throttleis released. Avoid direct contact with accessoriesduring and after use. Gloves will reduce the risk ofcuts or burns.• Keep away from rotating end of tool. Do not wearjewelry or loose clothing. Secure long hair. Scalpingcan occur if hair is not kept away from tool andaccessories. Choking can occur if neckwear is notkept away from tool and accessories.• Impact wrenches are not torque control devices.Fasteners with specific torque requirements mustbe checked with suitable torque measuringdevices after installation with an impact wrench.• Do not lu b ri c ate tools with flam m a b le or vol a t ileliq u ids such as ker o s ene, die s el or jet fuel.• This tool is not insulated against electric shock.• This tool must not be used in explosive atmospheres.• Do not force tool be y ond its rat e d capacity.•Use only impact sockets and accessories on thistool. Do not use hand sockets or accessories.• Use accessories recommended by Cornwell Tools.• Do not use (or modify) the tool for any otherpurpose than that for which it was designedwithout consulting the manufacturer's authorizedrepresentative.• Do not remove any labels. Re p lace any damaged la b els.• Failure to heed these warnings may result in serious orfatal personal injury and/or property damage.WARNING: This product can expose you tochemicals including nickel, which is known to theState of California to cause cancer and birth defectsor other reproductive harm. For more informationgo to .AIR SUPPLYTools operate on a wide range of air pressures. It is recommended that air pressure of these tools measures 90 psig at the tool with the trigger fully depressed and no load applied to the tool. Higher pressure (over 90 psig; 6.2 bar) raises performance beyond the rated capacity of the tool, which will shorten tool life and could cause injury.Always use clean, dry air. Dust, corrosive fumes and/or water in the air line will cause damage to the tool. Drain water from air lines and compressor prior to running tool. Clean the air inlet filter screen weekly. The recommended hookup procedure can be viewed in the above figure.The air inlet used for connecting air supply has standard 1/4" NPT. Line pressure should be increased to compensate for unusually long air hoses (over 25 feet). Minimum hose diameter should be 3/8" I.D. and fittings should have the same inside dimensions and be tightly secured.Ensure an accessible emergency shut off valve has been installed in the air supply line and make others aware of its location. LUBRICATIONLubricate the air motor daily with high quality air tool oil. If no air line oiler is used, run 1/2 oz. of oil through the tool. The oil can be squirted into the tool air inlet or into the hose at the nearest connection to the air supply, then run the tool. A rust inhibitive oil is acceptable for air tools.WARNING: After an air tool has been lubricated, oil will discharge through the exhaust port during the first few seconds of operation. The exhaust port must be covered with a towel before applying air pressure to prevent serious injury.OPERATIONThis tool is an impacting tool and not a torque meter. When specific torque is required, it must be checked with a torque meter after fitting the fastener with the impact. This impact wrench is rated at 1/2" SAE bolt size. Rating must be downgraded for spring U bolts, tie bolts, long cap screws, double depth nuts, badly rusted conditions and spring fastener, as they absorb much of the impact power. When possible, clamp or wedge the bolt to prevent spring back.Soak rusted nuts in penetrating oil and break rust seal before removing with impact wrench. If nut does not start to move in three to five seconds, use a larger size impact wrench. Do not use impact wrench beyond rated capacity as this will drastically reduce tool life. The reversing valve is used to change the direction of the tool. When the valve is out, the tool is in forward or right hand direction. When the valve is pushed in, the tool is in reverse or left hand direction.NOTE: Always turn off the air supply, drain hose of air pressure and detach tool from air supply before installing, removing or adjusting any accessory on this tool, or before performing any maintenance on this tool.NOTE: Actual torque on a fastener is directly related to joint hardness, tool speed, condition of socket and the time the tool is allowed to impact. Use the simplest possible tool to socket hook up. Every condition absorbs energy and reduces power.NOTE: During operation, safety goggles must always be worn to guard against flying debris (users and bystanders). TROUBLESHOOTINGOther factors outside the tool may cause loss of power or erratic action. Reduced compressor output, excessive drain on the air line, moisture or restrictions in air pipes or the use of hose connections of improper size or poor conditions may reduce air supply. Grit or gum deposits in the tool may cut power and may be corrected by cleaning the air strainer and flushing out the tool with gum solvent oil or an equal mixture of SAE #10 and kerosene. If outside conditions are in order, disconnect tool from hose andtake tool to your nearest authorized service center.WARRANTY COVERAGECornwell Quality Tools Company (“Cornwell”) warrants this product against defects in material and workmanship for a period of TWO (2) YEARS from the date of original retail purchase. Subject to the conditions and limitations set forth below, Cornwell will, at its option, either repair or replace any part of the product(s) that proves defective by reason of improper workmanship or materials.This warranty does not cover any damage to this product that results from accident, abuse, misuse, natural or personal disaster, or any unauthorized disassembly, repair, or modification. Repairs, disassembly and modification are only authorized to be made by Cornwell or a Cornwell Authorized Warranty Center.WARRANTY SERVICEIn order to have your tool repaired, return the tool to any Cornwell Au t ho r ized Warranty Center, freight pre p aid. Please include a copy of your proof of pur c hase and a briefde s crip t ion of the prob l em. The tool will be inspected and if any part or parts are found to be de f ec t ive in ma t e r i a l or work m an s hip, they will be re p aired free of charge, and the re p aired tool will be re t urned to you freight pre p aid.EXCLUSIONS AND LIMITATIONSTHIS WARRANTY AND THE REMEDIES SET FORTH ABOVE ARE EXCLUSIVE AND IN LIEU OF ALL OTHER WARRANTIES, REMEDIES AND CONDITIONS, WHETHER ORAL OR WRITTEN, EXPRESS OR IMPLIED. CORNWELL SPECIFICALLY DISCLAIMS ANY AND ALL IMPLIED WARRANTIES, INCLUDING, TO THE EXTENT PERMITTED BY APPLICABLE LAW, ANY WARRANTIES OF MERCHANTABILITY AND FITNESS FOR A PARTICULAR PURPOSE. IF CORNWELL CANNOT LAWFULLY DISCLAIM IMPLIED WARRANTIES UNDER THIS LIMITED WARRANTY, ALL SUCH IMPLIED WARRANTIES ARE LIMITED IN DURATION TO THE DURATION OF THIS WARRANTY.IN NO EVENT SHALL CORNWELL BE LIABLE TO THE PURCHASER OR TO THE USER OF A CORNWELL PRODUCT FOR ANY SPECIAL, INCIDENTAL OR CONSEQUENTIAL DAMAGES BASED UPON BREACH OF WARRANTY, BREACH OF CONTRACT, NEGLIGENCE, TORT, OR ANY OTHER LEGAL THEORY. SUCH DAMAGES INCLUDE, WITHOUT LIMITATION, EXPENSES, LOST REVENUES, LOST SAVINGS, LOST PROFITS, OR ANY OTHER INCIDENTAL OR CONSEQUENTIAL DAMAGES ARISING FROM THE PURCHASE, USE OR INABILITY TO USE THE CORNWELL PRODUCT.Some states do not allow the exclusion or limitation of incidental or consequential damages or exclusions or limitation on the duration of implied warranties or conditions, so the above limitations or exclusions may not apply to you. This warranty gives you specific legal rights, and you may also have other rights that vary by state.Repair kits and replacement parts are available for many Cornwell products, regardless of whether or not the product is still covered by a warranty plan.Cornwell Quality Tools Company667 Seville Road • Wadsworth, OH 44281-1094PARTS LISTItem Part No Parts Name Qty Item Part No Parts Name Qty。
物质安全技术说明书产品代码:7900005 / 9528-20填表时间:31-三月-20141.产品/制剂和公司/企业的认定企业名称:Janssen Diagnostics, LLC700 US Highway Route 202 SouthRaritan, NJ 08869电子邮件地址客户服务电话:(800) 421-3311(800) 424-9300 ChemTrec (24小时服务(800) 424-9300 ChemTrec (24小时服务电话)电话)化学品俗名或商品名:CellSave Tube产品代码:7900005 / 9528-20别名:无。
鉴定了的用途:CellSave Preservative Tube是专门用于以全血形式收集和保存循环上皮细胞(肿瘤细胞),以用于枚举和表型。
第二部分危险性概述一般危险品信息:皮肤接触可能引发过敏.危险性标记:Xi - 有刺激性.最主要的危险性R - 类警示句R43 - 接触皮肤可引起过敏。
.致癌性等级:Johnson & Johnson:无.欧盟:无.第三部分成分/组成信息成分化学文摘编号重量百分含量别名EINECS编号.(欧洲存货目录中已有的编号).分类咪唑烷基脲39236-46-9<502543726 Listed.Xi;R43氢氧化钠1310-73-2<0.5215-185-5C; R35第四部分急救措施眼睛接触:立即用大量水冲洗,眼睑下部也要洗,至少15分钟. 睁大眼睛,同时淋洗. 如果症状持续,请就医。
皮肤接触:立即用肥皂和大量的水冲洗. 如有皮肤刺激或过敏反应的情况,看医生.食入:不要引发呕吐. 用水嗽口然后喝大量水. 切勿给失去知觉者从嘴里喂食任何东西。
. 立即呼叫医生.吸入 :给医治人员的提示.5. 第五部分消防措施灭火方法及灭火剂:使用任何适用于环境火灾的灭火器.出于安全原因而不能使用的灭火材料:无.特殊的暴露危害来自于物质和制剂本身,它们的燃烧产物或释放出来的气体:无任何合理预见。
If the coolant level in the reserve tank is at or below the MIN line,add coolant to bring it up to between the MIN and MAX lines.Inspect the cooling system for leaks.If the reserve tank is completely empty,you should also check the coolant level in the radiator.Always use Honda Long-life Anti-freeze/Coolant Type 2.This coolant is pre-mixed with 50percent antifreeze and 50percent water.Never add straight antifreeze or plain water.If Honda antifreeze/coolant is not available,you may use anothermajor-brand non-silicate coolant as a temporary replacement.Make sure it is a high-quality coolantrecommended for aluminum engines.Continued use of any non-Honda coolant can result in corrosion,causing the cooling system tomalfunction or fail.Have the cooling system flushed and refilled with Honda antifreeze/coolant as soon as possible.Engine CoolantAdding Engine CoolantMaintenance221When the radiator and engine are cool,relieve any pressure in the cooling system by turning the radiator cap counterclockwise,without pressing down.Remove the radiator cap by pushing down and turning counterclockwise.The coolant level should be up to the base of the filler neck.Addcoolant if it is low.Pour the coolant slowly and carefully so you do not spill any.Clean up any spill immediately;it could damage components in the engine compartment.Put the radiator cap back on and tighten it.Pour coolant into the reserve tank.Fill it to halfway between the MAX and MIN marks.Put the cap back on the reserve tank.Do not add any rust inhibitors or other additives to your vehicle’s cooling system.They may not be compatible with the coolant or engine components.Check the fluid level in thewindshield washer reservoir at least monthly during normal use.If the fluid levelis low,a message will be shown on the multi-information display.Fill the reservoir with a good-quality windshield washer fluid.Thisincreases the cleaning capability and prevents freezing in cold weather.When you refill the reservoir,clean the edges of the windshield wiper blades with windshield washer fluid on a clean cloth.This will help to condition them.3.1.2.4.5.On Canadian models:Engine Coolant,Windshield WashersWindshield Washers 222Do not use engine antif reeze or a vinegar/water solution in thewindshield washer reservoir.Antif reeze can damage your vehicle’s paint,while a vinegar/water solution can damage the windshield washer e only commercially-available windshield washer fluid.Check the fluid level with the engine at normal operating temperature.Park the vehicle on level ground.Shut off the engine.Within 60to 90seconds,remove the dipstick (yellow loop)from the transmission,and wipe it with a clean cloth.Insert the dipstick all the way into the transmission securely.The transmission should be drained and refilled with new fluid when this service is shown on a maintenance message in the multi-information display.Always use Honda ATF-Z1(automatic transmission fluid).If it’s not available,you may use a DEXRON III automatictransmission fluid as a temporary replacement.However,continued use can affect the shift quality.Have the transmission flushed and refilled with Honda ATF-Z1as soon as it is convenient.To thoroughly flush the transmission,the technician should drain and refill it with Honda ATF-Z1,then drive the vehicle for a short distance.Do this three times.Then drain and refill the transmission a final time.Insert the dipstick all the way back in the transmission.1.2.3. 6.AutomaticTransmission FluidMaintenance223Check the fluid level with the transmission at normal operating temperature and the vehicle sitting on level ground.Remove the check bolt,and look for transmission fluid coming out of the bolt hole.If a small amount of fluid drips out of the bolt hole,reinstall the check bolt.If no fluid comes out,remove the filler bolt.Slowly add Honda Manual Transmission Fluid (MTF)until it starts to run out of the check bolt hole.Let the fluid run out until it stops,then reinstall the check bolt and the filler bolt.If Honda MTF is not available,you may use an SAE 10W-30or 10W-40viscosity motor oil with the API Certification seal that says ‘‘FOR GASOLINE ENGINES’’as atemporary replacement.However,motor oil does not contain the proper additives,and continued use can cause stiffer shifting.Replace as soon as it is convenient.The transmission should be drained and refilled with new fluid when this service is shown on a maintenance message in the multi-information display.Manual Transmission FluidManual Transmission Fluid224Check the brake fluid level in the reservoirs monthly after removing the engine compartment rear cover (see page ).The fluid level should be between the MIN and MAX marks on the side of the reservoir.If it is not,addbrake fluid to bring it up to that e the same fluid specified for the brake system.A low fluid level can indicate a leak in the clutch system.Have thissystem inspected as soon as possible.Brake fluid marked DOT 5is not compatible with your vehicle’s braking system and can cause extensive damage.Replace the brake fluid every 3years,independent of mileage.Always use Honda Heavy Duty Brake Fluid DOT 3.If it is notavailable,you should use only DOT 3or DOT 4fluid,from a sealed container,as a temporary replacement.Using any non-Honda brake fluid can cause corrosion and decrease the life of the system.Have the brake system flushed and refilled with Honda Heavy Duty Brake Fluid DOT 3as soon as possible.217Manual Transmission onlyBrake and Clutch FluidClutch FluidMaintenance225Check the level on the side of the reservoir when the engine is cold,and the engine compartment right-side cover is off (see page ).The fluid should be between the UPPER LEVEL and LOWER LEVEL.If not,add power steering fluid to the UPPER LEVEL mark.217Power Steering Fluid226。
BackgroundTemperature Screening for Entrances and ArrivalsVast numbers of people are constantly moving through airports and railway stations every day.Hikvision Temperature Screening Solutions are designed for the rapid and efficient detection of skin-surface temperatures,meeting safety needs for three typical scenarios:01EntrancesDepartures & TransfersArrivalsEntrances &Arrivals are alwaysbusy with heavy foot traffic.So a quick and convenient setup is recommended for preliminary temperature screening.For people with abnormal temperatures,secondary,precision measurement will be available.Temperature Screening for Departures and Transfers02Temperature Screening with Route Guide –Real-Time Audio and Visual AlarmTypical ScenarioMetal Detector Door•18 independent detection zones, LCD screen•Thermal camera resolution: 160 x 120•Temperature range: 30~45℃•Temperature accuracy: ±0.5℃ISD-SMG318LT-FMetal detector doors with thermal cameras provide quick deployment at building entrances,lobbies,and more.Real-time onboard light and audio alarm warnings are supported.Departures &TransfersEvery passengershould undergo temperature screening before boarding a flight.The procedure should be quick and convenient to prevent crowding and missed connections.Normal TemperatureAbnormal TemperatureOptical ImagingThermal Imaging Typical ScenarioBlackbody Calibrator (Optional)•Temperature resolution: 0.1℃•Accuracy: ±0.1℃•Temperature stability: ±0.1℃/h •Effective emissivity: 0.97±0.021-1 Temperature Screening & Security Surveillance –Visualized, Bi-spectrum Live ViewThermographic Bullet Camera•Thermal: 384 ×288, lens: 10, 13, 15 mm •Optical: 2688 ×1520, lens: 4, 6, 6 mm•Accuracy: ±0.5℃(±0.3℃with blackbody calibrator )•Measurement range: 30-45℃•AI human detection, false alarms reduction•Simultaneous temperature screening for multiple people (Up to 30 people at once)DS-2TD2636B-15/P DS-2TD2636B-13/P DS-2TD2637B-10/P DS-2TE127-G4AThe visualized bi-spectrum (thermal &optical)live view provides both temperature measurement and basic surveillance at the same time.Tripod mounting and simple wiring make for easy installation and use.Thermographic Handheld Camera•Thermal resolution: 160 ×120 •Optical resolution: 640 ×480 •Measurement range: 30-45℃•Accuracy: ±0.5℃•Bi-spectrum image fusion •Supports Wi-Fi DS-2TP21B-6AVF/WTypical Scenario Real Image1-2 Easy Supplemental Temperature Screening –Simple Wireless ConnectionHandheld thermographic cameras can be added at entrances for temporary temperature screening with secondary queues during busy periods.DeepinMind NVRiDS-9616(/32)NXI-I8/X(B)(T)•16 channels of face image comparison•32-library capacity with up to 100,000 face imagesMask-Detection & Intuitive DemonstrationWith DeepinMind NVRs and thermal cameras,users will enjoy additional functions:1)Mask Detection2)Intuitive Demonstration 3)Search by ImageLocal Storage and Information RecordingWith HikCentral Professional,users will enjoy additional functions:1)Local storage with pStor2)Identity information can be registered upon detection of abnormal temperatures 3)The data can be intuitively displayed and easily exportedValue-Added ChoicesHikCentral Professional•Flexible, scalable, reliable, and powerful central surveillance system.•Supports live view, play back, access control, alarm management, personnel identification, temperature data storage, abnormal temperature trend analysis etc.Personnel Access Management& Skin-TemperatureMeasurementReal-Time Pop-Up AlarmDashboardHikvision Temperature Screening Solutionfor Airports & RailwayStationsSafer, Faster, Smarter。
Agilent 81980A, 81960A, 81940A,81989A, 81949A, and 81950ACompact Tunable Laser SourcesData SheetIntroductionThe Agilent 819xxA Series of compacttunable lasers enables optical devicecharacterization at high power levelsand measurement of nonlinear effects.Each of the 819xxA lasers enhancesthe testing of systems, all types ofoptical amplifiers and other activecomponents, as well as passive opticalcomponents.As single-slot plug-in modules forthe Agilent Technologies 8163A/B,8164A/B, and 8166A/B mainframes,Agilent’s compact tunable lasersources are a flexible and cost effec-tive stimulus for single channel andDWDM test applications.New: Fast Swept SpectralLoss MeasurementThe Agilent 81960A sets a new markin tunable laser performance withfaster sweep speeds and repetitionrates combined with the dynamicaccuracy specifications needed forDWDM component measurements.Dynamically specified sweeps in bothdirections enhance the repetitionrate even further for real-time usein adjustment and calibration proce-dures. Rocket-fast and accurate, the81960A helps you hit your develop-ment and production targets.Accurate DWDM Component Measurements at Full Scan RateThe 81960A module adds the new and unique capability to sweep in both direc-tions, and sports increased sweep speeds and acceleration. Its dramatically improved and fully specified dynamic accuracy enables DWDM component measurements and adjustments at high repetition rate, and boosts the char-acterization of single and multichannel components. The laser is especially well supported by the swept-wavelength measurement engines in the N7700A software suite and can be programmed directly.The most specially adapted application for this laser is high repetition-rate scanning for real-time updates, enabled by the Agilent N7700A-102 fast-sweep insertion loss engine. It synchronizes the laser with the N7744A or N7745A power meters to produce power and loss spectra in a convenient GUI display, and accelerates the uploading of the logged wavelength monitor data.The wavelength resolution and 50-60 dB dynamic range achieved surpass com-parable measurements by an Optical Spectrum Analyzer (OSA), with repetition rates better than 2 Hz for add-drop filter adjustment and calibration.The high performance in continuous sweeps also matches this laser well to the single-sweep PDL and IL N7700A-101 measurement engine. The enhanced dynamic wavelength accuracy will satisfy the test needs for many DWDM com-ponents at an optimized performance/price balance. The source to spontaneous noise ratio, SSE, while not as high as the 81600B series, is also sufficient to qualify the isolation of many filter devices. The higher sweep speeds save time measuring broadband devices not needing such high wavelength resolution.These same advantages apply to use with the N7788B component analyzer for measuring PMD and DGD in addition to PDL and IL. The relative wavelength accuracy during the sweeps is especially important for accurate DGD measure-ments using the JME method, since the result depends on the derivatives with respect to wavelength. The high speed is great for measuring isolators, PMF and other broadband components.The powerful lambda scan functions of the 816x Plug&Play driver for customized programs, and the N7700A IL engine which provides a GUI interface to these functions also support power and IL measurements together with any of the Agilent power meters. And the performance of swept-wavelength measure-ments in the N4150A PFL, including fast repetitive sweeps are also supported with this newest member of the Agilent swept tunable lasers.High Power Compact Tunable Lasers for S-, C-, and L-BandAgilent’s 8198xA, 81960A and 8194xA compact tunable laser sources pro-vide high output power up to +13 dBm.The 81980A and 81989A modules cover a 110 nm wavelength range in the S- and C-band, the 81940A and 81949A modules operate over110 nm in the C- and L-band, and the 81960A scans even 125 nm including the C- and L-band.The Agilent Technologies 81950A system-loading source is step-tunable for setting channel frequencies within the C- or L-band. With high output power up to +15 dBm, narrow linewidth of 100 kHz, gridless and grid-defined wavelength setting, and offset fine-tuning capability, the 81950A is a universal source for realistic loading of the latest trans-mission systems.Modular Design for Multichannel PlatformThe 819xxA tunable lasers are a family of plug-in modules for the Agilent Technologies 8163A/B,8164A/B, and 8166A/B mainframes. Their compact single-slot format makes them a flexible and cost-effective stimulus for single channel and multichannel dense wavelength division multiplexing (DWDM) appli-cations.Internal ModulationThe internal modulation feature of 81940A, 81960A, 81980A, 81949A and 81989A enables an efficient and simple time-domain extinction (TDE) method for Erbium-based optical amplifier test. It also supports the transient testing of optical amplifiers by simulating channel add and drop events.Continuous Sweep Mode with Wavelength LoggingAll 819xxA modules can be operated in the stepped mode usually used where measurements are done at particular wavelength.The 81940A, 81960A and 81980A can also be operated in the continuous sweep mode with dynamic wavelength logging to make measurements during the wavelength sweep.Built-In Wavelength Meter for Active Wavelength ControlThe 81940A, 81960A and 81980A feature a built-in wavelength meter with a closed feedback loop for enhanced wavelength accuracy. In continuous sweep mode, the meter allows dynamic wavelength logging to make accurate measure-ments during the sweep.Dynamic Power Control for Excellent ReproducibilityThe integrated dynamic power control loop ensures a high reproducibility in power level. Highly repeatable measurements reduce errors when comparing the results of several wavelength sweeps. As the 81940A, 81960A and 81980A feature mode-hop-free tunability over their entire tuning range with continuous output power, they achieve highly accurate measurements over wavelength.Coherence Control Avoids Interference-Induced Power FluctuationsIn 8194xA, 81960A and 8198xA modules, a high-frequency modulation function is used to increase the effective linewidth to avoid power fluctuations due to coherent interference effects. The modulation pattern is optimized for stable power measurements, even in the presence of reflections.Device Characterization at High Power LevelsThe high optical output power of the 819xxA tunable lasers makes them ideal sources for the test of active and passive optical components. Each laser helps overcome losses in test setups or in the device under test itself. Thus, engineers can test optical amplifiers such as EDFAs, Raman amplifiers, SOAs, and EDWAs to the amplifier’s limits. The tunable laser provides the high power levels required to help speed the development of innovative devices by enabling the test and measurement of nonlinear effects.SBS Suppression Feature Enables High Launch PowerThe stimulated Brillouin scattering (SBS) suppression feature avoids the reflec-tion of light induced by SBS. The feature enables the launch of the high optical output power into long fibers without intensity modulation, avoiding impairment in time-domain measurements.Certified QualityThe 81940A, 81950A, 81960A,81980A, 81949A, and 81989A are pro-duced to the ISO 9001 international quality system standard as part of Agilent’s commitment to continually increasing customer satisfaction through improved quality control. Specifications describe the instru-ment’s warranted performance. They are verified at the end of a 2-meter-long patchcord and are valid after warm-up, and for the stated output power and wavelength ranges.Each specification is assured bythoroughly analyzing all measurement uncertainties. Supplementary perfor-mance characteristics describe the instrument’s non-warranted typical performance.Every instrument is delivered with a commercial certificate of calibration and a detailed test report.For further details on specifications, refer to Chapter 3 in Agilent 81940A, 44A, 49A, 80A, and 89A Compact Tunable Laser Source Modules User’s Guide (publication number 81980-90A11), or respectively, to Chapter 5 in the Agilent 81950ATunable System Source User’s Guide (publication number 81950-90B01) or, respectively, to Chapter 5 in the Agilent 81960A Compact Tunable Laser User’s Guide (publication number 81960-90B01).81960A Fast-Swept Compact Tunable Laser Source, 1505 nm to 1630 nm Unless otherwise noted, specifications apply to sweeps in both directions.Wavelength range, Option 1621505 nm to 1630 nmWavelength (frequency) resolution0.1 pm, 12.5 MHz at 1550 nmMode-hop free tunability Full wavelength rangeAbsolute wavelength accuracy 1± 10 pm; typical ± 5 pmRelative wavelength accuracy± 7 pm; typical ± 3 pmWavelength repeatability± 2.5 pm; typical ± 1.5 pmWavelength stability (typical) 3≤ ±0.5 pm, 1 minute≤ ±2.5 pm, 15 minutesMaximum output power (continuous power during sweep)≥ +14 dBm peak, typical≥ +13 dBm (1570 nm to 1620 nm)≥ +10 dBm (1505 nm to 1630 nm)Power range (nominal)+6 dBm to maximum output powerPower repeatability (typical)± 0.01 dBPower stability 3± 0.01 dB, 1 hour± 0.03 dB, typical, 24 hoursPower linearity± 0.15 dB (1505 nm, 1575 nm, 1630 nm)Power flatness versus wavelength± 0.2 dB (1570 nm to 1620 nm, +13 dBm)± 0.3 dB (full wavelength range)Continuous sweep mode, both directions 7 5 nm/s10 nm/s20, 40 nm/s50 nm/s80, 100 nm/s200 nm/s Absolute wavelength accuracy (typical)± 5 pm± 10 pm± 15 pm± 8 pm± 8 pm± 15 pm Relative wavelength accuracy (typical)± 4 pm± 9 pm± 14 pm± 7 pm± 7 pm± 14 pm Wavelength repeatability (typical) 6± 0.8 pm± 4 pm± 4 pm± 2 pm± 3 pm± 3 pm Dynamic power reproducibility (typical) 6± 0.01 dB± 0.01 dB± 0.02 dB± 0.02 dB± 0.04 dB± 0.04 dB Dynamic relative power flatness (typical)± 0.01 dB± 0.01 dB± 0.03 dB± 0.03 dB± 0.07 dB± 0.10 dB Linewidth, coherence control off (typical)100 kHzEffective linewidth, coherence control on (typical) 2> 50 MHz (at max. constant output power)Side-mode suppression ratio (typical) 2≥ 50 dBSignal to source spontaneous emission ratio 2≥ 45 dB/nm (full wavelength range, +10 dBm) 4≥ 50 dB/nm (1525 nm to 1620 nm, +12 dBm) 4≥ 60 dB/0.1 nm (typical, 1525 nm to 1620 nm, +12 dBm) 5Signal to total source spontaneous emission ratio (typical) 2≥ 25 dB (full wavelength range, +10 dBm)≥ 30 dB (1525 nm to 1620 nm, +12 dBm)Relative intensity noise (RIN) (typical) 2-145 dB/Hz (0.1 GHz to 6 GHz)Dimensions (H x W x D)75 mm x 32 mm x 335 mmWeight0.95 kg1. At day of calibration.2. At maximum output power as specified per wavelength range.3. At constant temperature ± 0.5 K.4. Value for 1 nm resolution bandwidth.5. Value for 0.1 nm resolution bandwidth.6. Repeatability within the same sweep direction. At 200 nm/s, the specification value is double for sweeps from long to shortwavelength.7. For sweep range 1510 nm to 1625 nm. For 200 nm/s, sweep range is 1528 nm to 1608 nm.Wavelength range1465 nm to 1575 nmWavelength (frequency) resolution 1 pm, 125 MHz at 1550 nmMode-hop free tunability Full wavelength rangeMaximum sweep speed50 nm/sAbsolute wavelength accuracy± 20 pm, typical ± 5 pm 1Relative wavelength accuracy± 10 pm, typical ± 5 pmWavelength repeatability± 2.5 pm, typical ± 1 pmWavelength stability (typical, over 24 hours) 4± 2.5 pmLinewidth (typical), coherence control off100 kHzEffective linewidth (typical), coherence control on 2> 50 MHz (1525 nm to 1575 nm) Maximum output power (continuous power during tuning)≥ +14.5 dBm peak (typical)≥ +13 dBm (1525 nm to 1575 nm)≥ +10 dBm (1465 nm to 1575 nm)Power linearity± 0.1 dBPower stability 4± 0.01 dB over 1 hourTypical ± 0.0075 dB over 1 hourTypical ± 0.03 dB over 24 hoursPower flatness versus wavelength± 0.2 dB, typical ± 0.1 dB (1525 nm to 1575 nm)± 0.3 dB, typical ± 0.15 dB (full range) Power repeatability (typical)± 0.01 dBSide-mode suppression ratio (typical) 2≥ 50 dBSignal to source spontaneous emission ratio 2≥ 45 dB/nm 3≥ 48 dB/nm (1525 nm to 1575 nm) 3Typical 58 dB/0.1 nm (1525 nm to 1575 nm) 5 Signal to total source spontaneous emission ratio (typical) 2≥ 25 dB≥ 30 dB (1525 nm to 1575 nm)Relative intensity noise (RIN) (typical) 2-145 dB/Hz (0.1 GHz to 6 GHz) Dimensions (H x W x D)75 mm x 32 mm x 335 mmWeight0.95 kg1. At day of calibration.2. At maximum output power as specified per wavelength range.3. Value for 1 nm resolution bandwidth.4. At constant temperature ± 0.5 K.5. Value for 0.1 nm resolution bandwidth.Wavelength range1520 nm to 1630 nmWavelength (frequency) resolution 1 pm, 125 MHz at 1550 nmMode-hop free tunability Full wavelength rangeMaximum sweep speed50 nm/sAbsolute wavelength accuracy± 20 pm, typical ± 5 pm 1Relative wavelength accuracy± 10 pm, typical ± 5 pmWavelength repeatability± 2.5 pm, typical ± 1 pmWavelength stability (typical, over 24 hours) 4± 2.5 pmLinewidth (typical), coherence control off100 kHzEffective linewidth (typical), coherence control on 2> 50 MHz (1570 nm to 1620 nm) Maximum output power (continuous power during tuning)≥ +14.5 dBm peak (typical)≥ +13 dBm (1570 nm to 1620 nm)≥ +10 dBm (1520 nm to 1630 nm)Power linearity± 0.1 dBPower stability 4± 0.01 dB over 1 hourTypical ± 0.0075 dB over 1 hourTypical ± 0.03 dB over 24 hoursPower flatness versus wavelength± 0.2 dB, typical ± 0.1 dB (1570 nm to 1620 nm)± 0.3 dB, typical ± 0.15 dB (full range) Power repeatability (typical)± 0.01 dBSide-mode suppression ratio (typical) 2≥ 50 dBSignal to source spontaneous emission ratio 2≥ 45 dB/nm 3≥ 48 dB/nm (1570 nm to 1620 nm) 3Typical 58 dB/0.1 nm (1570 nm to 1620 nm) 5 Signal to total source spontaneous emission ratio (typical) 2≥ 25 dB≥ 30 dB (1570 nm to 1620 nm)Relative intensity noise (RIN) (typical) 2-145 dB/Hz (0.1 GHz to 6 GHz) Dimensions (H x W x D)75 mm x 32 mm x 335 mmWeight0.95 kg1. At day of calibration.2. At maximum output power as specified per wavelength range.3. Value for 1 nm resolution bandwidth.4. At constant temperature ± 0.5 K.5. Value for 0.1 nm resolution bandwidth.Wavelength range1465 nm to 1575 nmWavelength (frequency) resolution 5 pm, 625 MHz at 1550 nmMode-hop free tunability Full wavelength rangeTuning time (typical) 3 sec for 100 nmAbsolute wavelength accuracy ± 100 pmRelative wavelength accuracy ± 50 pmWavelength repeatability ± 5 pmWavelength stability (typical, over 24 hours) 3± 5 pmLinewidth (typical), coherence control off100 kHzEffective linewidth (typical), coherence control on 1> 50 MHz (1525 nm to 1575 nm) Maximum output power (continuous power during tuning)≥ +14.5 dBm peak (typical)≥ +13 dBm (1525 nm to 1575 nm)≥ +10 dBm (1465 nm to 1575 nm)Power linearity± 0.1 dBPower stability 3± 0.01 dB over 1 hourTypical ± 0.0075 dB over 1 hourTypical ± 0.03 dB over 24 hoursPower flatness versus wavelength± 0.2 dB, typical ± 0.1 dB (1525 nm to 1575 nm)± 0.3 dB, typical ± 0.15 dB (full range) Power repeatability (typical)± 0.01 dBSide-mode suppression ratio (typical) 1≥ 50 dBSignal to source spontaneous emission ratio 1≥ 45 dB/nm 2≥ 48 dB/nm (1525 nm to 1575 nm) 2Typical 58 dB/0.1 nm (1525 nm to 1575 nm) 4 Signal to total source spontaneous emission ratio (typical) 1≥ 25 dB≥ 30 dB (1525 nm to 1575 nm)Relative intensity noise (RIN) (typical) 1-145 dB/Hz (0.1 GHz to 6 GHz) Dimensions (H x W x D)75 mm x 32 mm x 335 mmWeight0.95 kg1. At maximum output power as specified per wavelength range.2. Value for 1 nm resolution bandwidth.3. At constant temperature ± 0.5 K.4. Value for 0.1 nm resolution bandwidth.Wavelength range1520 nm to 1630 nmWavelength (frequency) resolution 5 pm, 625 MHz at 1550 nmMode-hop free tunability Full wavelength rangeTuning time (typical) 3 sec for 100 nmAbsolute wavelength accuracy ± 100 pmRelative wavelength accuracy ± 50 pmWavelength repeatability ± 5 pmWavelength stability (typical, over 24 hours) 3± 5 pmLinewidth (typical), coherence control off100 kHzEffective linewidth (typical), coherence control on 1> 50 MHz (1570 nm to 1620 nm) Maximum output power (continuous power during tuning)≥ +14.5 dBm peak (typical)≥ +13 dBm (1570 nm to 1620 nm)≥ +10 dBm (1520 nm to 1630 nm)Power linearity± 0.1 dBPower stability 3± 0.01 dB over 1 hourTypical ± 0.0075 dB over 1 hourTypical ± 0.03 dB over 24 hoursPower flatness versus wavelength± 0.2 dB, typical ± 0.1 dB (1570 nm to 1620 nm)± 0.3 dB, typical ± 0.15 dB (full range) Power repeatability (typical)± 0.01 dBSide-mode suppression ratio (typical) 1≥ 50 dBSignal to source spontaneous emission ratio 1≥ 45 dB/nm 2≥ 48 dB/nm (1570 nm to 1620 nm) 2Typical 58 dB/0.1 nm (1570 nm to 1620 nm) 4 Signal to total source spontaneous emission ratio (typical) 1≥ 25 dB≥ 30 dB (1570 nm to 1620 nm)Relative intensity noise (RIN) (typical) 1-145 dB/Hz (0.1 GHz to 6 GHz) Dimensions (H x W x D)75 mm x 32 mm x 335 mmWeight0.95 kg1. At maximum output power as specified per wavelength range.2. Value for 1 nm resolution bandwidth.3. At constant temperature ± 0.5 K.4. Value for 0.1 nm resolution bandwidth.This laser source is available in a C-band and L-band version. Specifications apply to wavelengths on the 50 GHz ITU-T grid, after warm up.Wavelength (frequency) range • Option 210• Option 201• 1527.6 nm to 1565.50 nm (196.25 THz to 191.50 THz)• 1570.01 nm to 1608.76 nm (190.95 THz to 186.35 THz)Frequency resolution 100 MHz, 0.8 pm at 1550 nm Tuning time Typical < 30 sec 3Fine tuning range Typical ± 6 GHzFine tuning resolution Typical 1 MHzAbsolute wavelength (frequency) accuracy ± 22 pm (± 2.5 GHz)Relative wavelength (frequency) accuracy ± 12 pm (± 1.5 GHz) Wavelength (frequency) repeatability 2Typical ± 2.5 pm (± 0.3 GHz) Wavelength (frequency) stability (typical, over 24 hours) 2Typical ± 2.5 pm (± 0.3 GHz), 24 hours Linewidth (typical), SBS suppression off< 100 kHzMaximum output power ≥ +13.5 dBm (typical ≥ +15 dBm) Power stability Typical ± 0.03 dB over 1 hour 2Typical ± 0.03 dB over 24 hours 2 Power flatness Typical ± 0.2 dB (full wavelength range) Power repeatability Typical ± 0.08 dB 2Side-mode suppression ratio Typical 50 dBSignal to source spontaneous emission ratio Typical 50 dB/1 nm 1Typical 60 dB/0.1 nm 1Relative intensity noise (RIN) Typical -145 dB/Hz 1 (10 MHz to 40 GHz) Dimensions (H x W x D) 75 mm x 32 mm x 335 mmWeight 0.45 kg1. At maximum output power, as specified, per wavelength range.2. At constant temperature ± 0.5 K.3. Including power stabilization.81950A Tunable System Source• Full wavelength range at output power ≥ +10 dBm • Ambient temperature within +20 °C and +30 °C1. Displayed wavelength represents average wavelength while digital modulation is active.2. External analog modulation is not available for 81960A.Specifications11Agilent 81950AExternal analog modulation 5% pp at 2.5 Vp-p input voltage swing (max)10 kHz to 1000 kHzModulation input: max 5 Vp-pInput impedance: 50 ΩSBS suppressionFM p-p modulation range: 0 GHz to 1 GHz (typical)Dither frequency: 20.8 kHz Power setting Power attenuation range: 8 dBPower setting resolution: 0.1 dBResidual output power (shutter closed): ≤ -45 dBmFine tuning speed15 sec from -6 GHz to +6 GHz Grid spacing 100 GHz, 50 GHz, 25 GHz, or arbitrary grid• 8194xA, 81960A and 8198xA • 81950A• 50 dB • 30 dB Return loss (typical)60 dB (Option 072, 8194xA, 81960A and 8198xA)40 dB (Option 071, 8194xA and 8198xA)Wavelength stability (typical, over 1 min)± 0.5 pm Fiber typePanda OrientationTE mode in slow axis, in line with connector key Polarization extinction ratio16 dB typical Recommended re-calibration period2 years Connector option (required)Tunable laser must be ordered with one connector option Option 071PMF, straight contact output connector (not available for 81960A) Option 072PMF, angled contact output connector Connector interface One Agilent 81000xI-Series connector interface is requiredSpecifications (continued)For more information on Agilent Technologies’ products, applications or services, please contact your local Agilent office. The complete list is available at:/find/contactus Americas Canada (877) 894 4414 Brazil (11) 4197 3600Mexico 01800 5064 800 United States (800) 829 4444 Asia Pacific Australia 1 800 629 485China 800 810 0189Hong Kong 800 938 693India 1 800 112 929Japan 0120 (421) 345Korea 080 769 0800Malaysia 1 800 888 848Singapore 180****8100Taiwan 0800 047 866Other AP Countries (65) 375 8100Europe & Middle East Belgium 32 (0) 2 404 93 40 Denmark 45 45 80 12 15Finland 358 (0) 10 855 2100France 0825 010 700* *0.125 €/minuteGermany 49 (0) 7031 464 6333 Ireland 1890 924 204Israel 972-3-9288-504/544Italy 39 02 92 60 8484Netherlands 31 (0) 20 547 2111Spain 34 (91) 631 3300Sweden 0200-88 22 55United Kingdom 44 (0) 118 927 6201For other unlisted countries: /find/contactus Revised: January 6, 2012Product specifications and descriptions in this document subject to change without notice.© Agilent Technologies, Inc. 2012Published in USA, April 2, 20125988-8518EN /find/tls Agilent Advantage Services is committed to your success throughout your equip-ment’s lifetime. To keep you competitive, we continually invest in tools and processes that speed up calibration and repair and reduce your cost of ownership. You can also use Infoline Web Services to manage equipment and services more effectively. By sharing our measurement and service expertise, we help you create the products that change our /quality /find/advantageservices Quality Management System Quality Management Sys ISO 9001:2008DEKRA Certified Agilent Email Updates /find/emailupdates Get the latest information on the products and applications you select. LAN eXtensions for Instruments puts the power of Ethernet and the Web inside your test systems. Agilent is a founding member of the LXI consortium.Agilent Channel Partners w w w /find/channelpartners Get the best of both worlds: Agilent’s measurement expertise and product breadth, combined with channel partner convenience.。
专利名称:CATHODE-RAY TUBE发明人:MATSUDA SHUZO,ITO TAKEO,KOIKE NORIO 申请号:JP21216985申请日:19850927公开号:JPS6273535A公开日:19870404专利内容由知识产权出版社提供摘要:PURPOSE:To reduce a deterioration of emission property of a cathode-ray tube owing to a long service, by furnishing a substance of a specific ratio of surface area inside the cathode-ray tube, and specifying the surface area of the substance per a unit volume in the tube. CONSTITUTION:By feeding a substance with a surface area ratio more than 10m<2>/g and less than 1,100m<2>/g inside a cathode-ray tube, to make the surface area of the substance more than 2.2X10<-3>m<2>/cm<3> and less than 2.8X10<-1>m<2>/cm<3> per a unit volume of the tube, hydrocarbon and the other gas in the cathode-ray tube can be absorbed to the surface of the substance, and the emission surviving rate is improved broadly. Therefore, the service life of the CRT is extensively improved, operating correctly for a longer period, and an excellent picture can be reproduced.申请人:TOSHIBA CORP更多信息请下载全文后查看。
a r X i v :a s t r o -p h /9802341v 1 26 F eb 1998A&A manuscript no.(will be inserted by hand later)1.Introduction.Since their discovery in 1969(Klebesadel et al.1973)the gamma-ray bursts (GRBs)phenomenon is the subject of2V.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant. GRBRs have been obtained at SAO with the1-m and6-m telescopes.The second GRB with an optical after-glow was in a very favorable place in the northern sky(in the Camelopardalis constellation).The high declination of∼+79◦allows us to observe this object at SAO at all dates being at a zenith distance of less than57◦.Preliminary results of multi-color photometry of the GRB970508optical remnant were reported elsewhere (Sokolov et al.1997).In this paper we report the results of BV R c I c photometry from May to August1997discussing the correlation between the features of the optical light curves and those observed at other wavelengths.The sec-ond section deals with the search and detection of this optical source with the SAO telescopes and describes the BV R c I c photometry with the1-m and6-m telescopes. The third section is dedicated to the results of CCD pho-tometry in the phase of the source brightness maximum and to the following brightness fading in differentfilters up to the87th day after the burst.The fourth section is dedicated to the discussion of the results and to the com-parison of the optical light curves with those in X-ray and radio.2.GRB970508optical counterpart search.The alert of a new GRB detection by BeppoSAX reached SAO only3.5hours after the high energy event(May 8.904UT).Due to morning twilight,follow-up observa-tions could start at the1-m telescope on May9.74UT. The5′WFC error box was completely covered with the CCD mosaic of29images in R c band with300and600 sec exposure times.The1-m(Zeiss-1000)telescope is equipped with a CCD photometer ISD015A,520×580 pixels corresponding to thefield of view2.′0×3.′6.The images from the1-m telescope were compared to the cor-respondingfields of the Digitized Sky Survey(DSS).No new bright object was found up to the DSS limit for this field.On the next night,May10/11,a refined WFC error circle position was available:α2000=06h53m28s;δ2000= +79o17′.4with a3′error radius(99%confidence level). Photometric observations of GRB970508field were then continued with the6-m telescope.The1040×1160pixel CCD chip“Electron ISD017A”installed at the Primary Focus has afield of view of2.′38×2.′66.A2×2binning mode was employed,so that each of the520×580zoomed pixels has angular size of0.′′274×0.′′274.The gain is2.3e−per DN(Data Number).The readout noise is about10e−.Thefirst image at the6-m telescope was obtained on May10.76UT and a variable object was discovered by comparison with the image taken the night before. Its brightness,from May9.85UT to May10.76UT,in-creased of about1.5magnitudes.This object wasfirst re-ported by Bond(1997)as a possible optical counterpart of GRB970508and was independently found in our data only about0.5day later.The summary of the observations Table1.First week observations of GRB970508optical rem-nant.09/1009.751-m300-”-09.85-”-60010/1110.776-m300200100300-”-10.93-”-30020010030011/1211.76-”-45030015045012/1312.87-”-45060015090013/1413.88-”-1200600450450#α2000δ2000B V R c I c Observations were carried out withfilters closely matching the BV R c I c Johnson-Kron-Cousins system.The data were processed using the ESO-MIDAS software. Standard data reduction includes bias subtraction,flat-fielding and cosmic particle traces removal.Photomet-ric conditions remained stable during two nights of May13/14and May21/22.Four bright stars(Fig.1)in the GRB970508field were used as secondary photometric standards.Magnitudes of these stars were determined on the night of May13/14 with good photometric conditions using four standard stars in thefield of PG1657+078(Landolt,1992).Zero-point errors are better than0.05m.Coordinates and mag-nitudes of secondary photometric standards are given in Table2.Our R c magnitudes of stars2,3,4are0.20±0.01 higher than the magnitudes measured by Schaefer et al. (1997).The application of the analogous photometric pro-cedure in BV R c I c Johnson-Kron-Cousins system,used at SAO RAS,is given in details in the paper by Kurt et al. (1998).V.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant.3 Fig.1.Thefield near the optical source of GRB970508imaged with the1-m telescope(before the maximum of the transient brightness)and with the6-m telescope(the4th night after the maximum)in R c band.The object brightness in both images corresponds to R c≈21.1.The stars–secondary photometric standards–are indicated.3.The brightness maximum phase and followingsource fadingWe define as source brightness maximum phase the period when the optical object brightness increased to the maxi-mum(or close to the maximum)and then began to drop down to V≈21.5and R c≈21.1.It corresponds approx-imately to thefirst week of observations after the GRB when the optical source could still be observed with many telescopes-big and medium ones.The results of the ob-servations performed during these nights at SAO together with those from Palomar and Loiano are shown in Fig.2. Many more observations other than those from Palomar and Loiano were performed,but the different photomet-ric systems used and relatively smaller accuracy of the measurements do not allow a better evaluation of the OT behavior.Johnson-Kron-Cousins magnitudes in the BV R c I c bands with the associated errors for GRB970508opti-cal counterpart are given in Table 3.Given the Bep-poSAX/GRBM trigger time t0=May8.904UT,we note (see Fig.2):1)from t−t0=0.226to t−t0=0.944the R c brightness of the object seems to remain constant(Castro-Tirado et al.1997;Djorgovski et al.1997);2)from t−t0=0.944to t−t0=1.866the R c brightness increased of1.5mag.The magnitude increase rate using our1-m data and the data from Palomar(Djorgovski et al.1997)was about0.12mag per hour;3)at t−t0=1.866the R c magnitude reached the bright-ness maximum of19.70and from that date a decline of brightness began;4)the magnitude decrease during the beginning(2–5days) of the fading phase follows an exponential law in all four bands:B=19.689(±0.036)+0.452(±0.014)(t−t0)V=19.264(±0.053)+0.449(±0.020)(t−t0)(1) R c=18.874(±0.029)+0.443(±0.011)(t−t0)I c=18.355(±0.050)+0.450(±0.019)(t−t0)A power law did notfit the data for the brightness fading after the maximum.For example for the R c data it isχ2n=0.97for the exponentialfit while it isχ2n=4.5 for the power law.All the R c data from t−t0=1.8664V.Sokolov,et al.:BV R c I c photometry of GRB970508opticalremnant.Fig.2.The light curves of GRB970508optical counterpart during5days after the burst.SAO RAS(filled symbols),Loiano (Mignoli M.et al.1997,t−t0=1.95)and Palomar(Djorgovski et al.1997,transformed to R c=r−0.34+A r)(open triangles) magnitudes with their errors are shown.Lines correspond to equations(1)of exponential decline of brightness reported in the text.For R c also the bestfit power law is shown(dotted line).to t−t0=4.976(10.77UT–13.88UT)are used:SAO,Loiano and Palomar.The spectrum of the object was close to a power lawand its slope Fν∝ν−1.2did not change in time,with(B−V)=0.43,(V−R c)=0.39,(R c−I c)=0.52Taking into account galactic absorption E(B−V)=0.03givesFν∝ν−1.1and the following color indeces:(B−V)0=0.40,(V−R c)0=0.37,(R c−I c)0=0.50After the5th day the decline of brightness is sloweddown.In the BV R c bands during about85th day and I cband until the≈36th day,the light curve can be describedby a power-law relation,B=19.713(±0.139)+3.000(±0.048)×log(t−t0)V=19.323(±0.135)+2.860(±0.046)×log(t−t0)(2)R c=18.865(±0.092)+2.927(±0.031)×log(t−t0)I c=18.313(±0.151)+2.961(±0.066)×log(t−t0)withαB=−1.200(±0.019)αV=−1.144(±0.018)αRc=−1.171(±0.012)αIc=−1.184(±0.026),neglecting the fact that for thefirst5days the light curvedecay is better described by the exponential law in allthe4bands.Figure3shows this averaged power-law lightcurve for the R c band up to about84days(t−t0=83.940)after the burst.Starting from the≈36th day after the burst,the ob-ject did not show the further fall of the brightness in theI cfilter up to t−t0=87.085.The magnitude of the objectin the I cfilter in that period was stable around I c=23.07.Figure4a shows the light curves in the BV R c I c bands upto day87.085.parison of optical,X-ray andradio brightness curvesThe data obtained with the SAO RAS1-m and6-m tele-scopes allow us to divide the GRBR970508brightnesschange curve into three stages(Fig.2,4and Table3):1)the increase of brightness on time scale of about oneday;2)the exponential brightness fall during about4days withV.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant.5Fig.3.R c light curve of the optical counterpart of GRB970508during ≈86days after the burst.SAO RAS (filled marks)and Palomar (Djorgovski et al.1997),Loiano (Mignoli et al.1997),HST (Fruchter et al.1997),Keck II (Metzger et al.1997)(open squares,transformed from Schaefer’s photometric system to ours)magnitudes are shown.Lines correspond to power (up to t −t 0=83.940)and exponential law (dashed)for fading brightness.a stable broadband power-law spectrum;3)the further brightness fading according to a power law.Nevertheless,from the 36th day after the burst the object did not show the further fall of the brightness in the I c filter.After 87days,the deviation from the average power law (2)achieved already ≈1mag.As Figure 3shows,our observations with the 6-m tele-scope alone can be approximately described by a single law in the R c filter,but in the phase of brightness maximum (Fig.2),when all fluxes were measured with the small-est errors,we see the same deviations from the “average”power law in all 4bands.Garsia et al.(1997)also mention that the brightness fading after the maximum cannot be well described by a single power law.As discussed by Piro et al.(1998),after about 30sec-onds from the high energy event,the GRB970508X-ray flux began to fall according to a power law with a slope of −1.1±0.1.Nevertheless,in about 16.6hours after the GRB the flux decay showed a temporal behavior analo-gous to the optical one during the first hours after the GRB (Pedersen et al.1998).(We did not observe at that time,but in the R band the optical flux was either stable or showed a slow decrease in the first 8hours after the GRB.)The features of the optical curves immediately af-ter the maximum (May 10.77UT)correlate with those of the X-ray transient light curve (Piro et al.1998).In Figure 4the SAO RAS BV R c I c brightness curves are presented together with the radio at 8.46GHz (Frail et al.1997)and the X-ray (BeppoSAX NFIs,Piro et al.1998).Apparently,the most interesting moment in this phase was the sharp fall of the X-ray flux and its subse-quent fast increase which was observed in details in the BeppoSAX MECS range 2–10keV,but unfortunately no simultaneous optical observations were performed.The subsequent optical brightness increase which was observed also at SAO (Fig.2)began with a small (≈5.5hours)delay.(Though now it can be supposed that before that moment there was a genuine optical brightness minimum missed by the observers.)Piro et al.(1998)notice that the following behavior of X-ray flux deviates from the power law.In the X-ray range this deviation,lasting about 4days,took about 30%of the energy released in the “af-terglow”part of the power-law drop.It is about 10%of the gamma-ray energy itself.During the same period the optical decay does not follow a power-law too,but the ex-ponential one (Fig.2and 3).This is in favor of a common origin of the X-ray and optical events.Taking into account the ratio of X-ray to optical flux during the 4days after the optical maximum,more than 16%of the energy of the GRB event itself was released in optical together with X-rays.Thus,it is believable indeed that the energy of the GRB remnant is not only determined by the afterglow,but there is also an intrinsic burst activity of the source which has an energy comparable to that of the burst in a time scale 10.000times longer than the duration of the GRB itself.When comparing the radio and optical behavior of the source (Frail et al.1997;Taylor et al.1997)after the brightness maximum phase ,the attention is immediately drawn to the fact that the decrease of the “twinkling”am-6V.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant. Table3.GRB970508OT photometry results9.75May0.84121.19±0.259.850.94421.13±0.1810.77 1.86620.50±0.0320.06±0.0319.70±0.0319.19±0.0410.93 2.02620.60±0.0320.22±0.0319.80±0.0319.30±0.0311.76 2.85621.03±0.0420.52±0.0320.10±0.0319.58±0.0412.87 3.96621.48±0.0621.10±0.0420.63±0.0520.19±0.0613.88 4.97621.92±0.0721.47±0.0521.09±0.0720.58±0.0920.79511.89122.10±0.1820.87511.97121.81±0.1020.97012.06621.27±0.1321.89212.98823.12±0.3522.09±0.0721.90813.00422.18±0.1421.94213.03821.96±0.1307.917Jun.30.08523.66±0.1008.96431.06024.65±0.2508.98031.07523.84±0.2408.99131.08723.54±0.2010.92833.02423.34±0.2210.94033.03624.08±0.2510.94533.04123.09±0.3513.95436.05024.62±0.1413.96636.06123.42±0.1413.99236.08823.30±0.3527.86549.96124.50±0.2227.87349.96924.17±0.1627.89349.98923.88±0.1627.91050.00623.05±0.1407.946Jul.60.04225.07±0.2124.62±0.2524.08±0.2007.96160.05723.10±0.1531.84383.94024.54±0.2531.85783.95224.60±0.2431.86283.95823.08±0.2302.807Aug.85.90224.28±0.3502.82585.92024.59±0.2502.85585.95025.32±0.2503.98987.08523.04±0.14V.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant.7Fig.4.GRB970508light curves:(a)BV R c I c SAO RAS data;(b)VLA/VLBA 8.46GHz data (Frail et al.1997);(c)2–10keV BeppoSAX MECS X-ray data with the t −1.1decay law (Piro et al.1998).The power law with the slope of −1.1is shown (dashed line).with FWHM =0′′.15and with R ≥25.4.The possible deceleration of brightness fading rate in HST/NIMCOS H band and the observed flattening of the light curve in the I c filter 36days after the GRB might be interpreted as a sign of the detection of such a galaxy.(This would imply a quite red object for z =0.835,but we do not discuss this implication in this work.)On the other hand,the multi-wavelenght (optical,X-ray,radio)behavior we observe can also be explained by some intrinsic features of GRB970508OT,rather than by the manifestation of an host galaxy.For example,it is possible to suppose that we observe the formation of a jet-like structure related to the activity of a stellar mass compact object,i.e.a gamma-ray burster .The possibility of explanation of all the observational data by the intrinsic8V.Sokolov,et al.:BV R c I c photometry of GRB970508optical remnant.features of the source in the model of asymmetrical rela-tivistic jets is now actively discussed(Dar1997;Paczyn’ski 1997).5.SummaryThe variable optical source associated to GRB970508was observed with the1-m and6-m telescopes of SAO RAS from May9to August4,1997.The details of temporal changes of brightness in the BV R c I c bands were compared with observations in X-ray and radio bands.We confirm the burst activity of the object detected by Piro et al. (1998)in X-rays in thefirst week after the high energy event.We notice also that the further brightness fading of the point-like object deviates from the average power law.This behavior was clearly seen at≈8000˚A when, approximately36days after the GRB,a period of constant brightness starts.Taking into account the global multi-wavelength be-havior of GRBR970508,it is presumable that the burst activity and subsequent deceleration of the brightness fad-ing of the optical stellar-like source is caused by some in-trinsic features of the object itself.Alternatively we prob-ably observe the displaying of a dwarf underlying host galaxy with I c≈23.1.To be certain of the absence of ap-preciable variability of a conjectural constant source fur-ther observational monitoring of a“quiet state”of the GRBR970508could give crucial inputs to the solution of this mystery.Acknowledgements:We thank:the BeppoSAX team for the quick alert of the GRB970508event;the6-m Telescope Program Committee for allocating the observational time for the program of gamma-ray bursters identification;the Director of SAO Yu.Yu.Balega for his support to our pro-gram;the observers Yu.N.Parijskij,V.H.Chavushyan, N.A.Tikhonov,L.I.Snezhko and T.N.Sokolova for her help during the preparation of this text.The work was carried out with the support of the RF Astronomy foundation(grant97/1.2.6.4)and also INTAS N96-0315.ReferencesBoella G.,et al.,1997,A&AS122,299Bond H.E.,1997,IAU Circ No.6654Castro-Tirado A.J.,et al.,1997,IAU Circ No.6657Costa E.,et al.,1997a,IAU Circ No.6649Costa E.,et al.,1997b,Nat,387,783Dar A.,1997(astro-ph/9709231)Galama T.,et al.,1997,Nat,387,479Garcia M.R.,et al.,1997,ApJL(submitted;astro-ph/9710346) Djorgovski S.,et al.,1997,Nat387,876Klebesadel R.W.,et al.,1973,ApJ182,L85Kurt V.G.,et al.,1998,A&A(in press.,astro-ph/9706076) Landolt A.U.,1992,AJ104,340Metzger M.R.,et al.,1997,IAU Circ No.6676Metzger M.R.,et al.,1997a,Nat387,879Mignoli M.,et al.,1997,IAU Circ No.6661Frail D.A.,et al.,1997,Nat389,261Fruchter A.,et al.,1997,IAU Circ No.6674Paczyn’ski B.,1997(astro-ph/9710086)Pedersen H.,et al.,1998,ApJ496(in press,March20)Pian E.,et al.,1998,ApJ492,L103(astro-ph/9710334)Piro L.,et al.,1998,A&A331,L41(astro-ph/9710355) Sahu K.C.,et al.,1997,Nat387,476Schaefer B.,et al.,1997,IAU Circ No.6658Sokolov V.,et al.,4-th Huntsville’s Symp.1997(astro-ph/9709093)van Paradijs J.,et al.,1997,Nat386,686Taylor G.B.,et al.,1997,Nat389,263。