Introduction The Chandra X-Ray Observatory (originally called the Advanced X-Ray Astrophysics Facility - AXAF) is the X-Ray component of NASA's "Great Observatory" Program. Chandra is a NASA facility that provides scientific data to the international astronomical community in response to scientific proposals for its use. The Observatory is the product of the efforts of many organizations in the United States and Europe. The Great Observatories also include the Hubbte Space Telescope for space-based observations of astronomical objects primarily in the visible portion of the electromagnetic spectrum, the now defunct Compton Gamma- Ray Observatory that was designed to observe gamma-ray emission from astronomical objects, and the soon-to-be-launched Space Infrared Telescope Facility (SIRTF). The Chandra X-Ray Observatory (hereafter CXO) is sensitive to X-rays inthe energy range from below 0.1 to above 10.0 keV corresponding to wavelengths from 12 to 0.12 nanometers. The relationship among the various parts of the electromagnetic spectrum, sorted by characteristic temperature and the corresponding wavelength, is illustrated in Figure 1. The German physicist Wilhelm Roentgen discovered what he thought was a new form of radiation in 1895. He called it X-radiation to summarize its properties. The radiation had the ability to pass through many materials that easily absorb visible light and to free electrons from atoms. We now know that X-rays are nothing more than light (electromagnetic radiation) but at high energies. Light has been given many names: radio waves, microwaves, infrared, visible, ultraviolet, X-ray and gamma radiation are all different forms. Radio waves are composed of low energy particles of light (photons). Optical photons - the only photons perceived by the human eye - are a million times more energetic than the typical radio photon, whereas the energies of X-ray photons range from hundreds to thousands of times higher than that of optical photons. Very low temperature systems (hundreds of degrees below zero Celsius) produce low energy radio and microwave photons, whereas cool bodies like our own (about 30 degrees Celsius) produce infrared radiation. Very high temperatures (millions of degrees Celsius) are one way of producing X-rays. Gamma X-rays Ultra- Infrared Radio Rays violet ...... t0 billion K 0.0005 0.1 0.5 50 0.5 Wavelength nlno_t_r eta_lee miCromehlrl talc romet4rs ¢Onl_m41er$ Figure 1.The electromagnetic spectrum as a function of temperature and wavelength. X-Ray astronomy is an extremely important field as all categories of astronomical objects (or a subset thereof), from comets to quasars, have been found to emit x-rays. Thus learning how and why these objects produce X-Rays is fundamental to our understanding of how astronomical systems work. This, together with the large amounts of energy required to produce X-rays in the first place, makes their study interesting and exciting. A second reason that the field is so important is that the vast bulk of the matter in the Universe that we can directly observe through the electromagnetic radiation that it emits is in the very hot (temperatures of millions of degrees) x-ray emitting gas that fills the space between galaxies in clusters of galaxies (Figure 2), the largest collections of matter in the Universe The CXO is the prime method of gaining new information about the X-ray emission seen inthe universe. Figure2.TheChandrXa-rayimagoefHydraA,agalaxycluste8r40millionlightyearsfromEarths,hows strand(sblue/pinko)f35-40milliondegreCeelsiugsasembeddeindalargecloudofequallhyotgas(blue) thatisseveramlillionlightyearsacrossA.brightwhitewedgeofhotmultimilliondegreeCelsiugsasis seenpushinigntothehearotfthecluste(rC. reditN:ASA/CXC/SAO) TheObservatowryasnamedin honorof thelateIndian-AmericNanobellaureateS,ubrahmanyan Chandrasek(hFaigrure3),nickname"Cdhandraw"hichmean"smoon"or"luminousin" SanskriHt.ewas oneoftheforemosatstrophysiciosftsthetwentietchenturayndi,n1983w,asawardetdheNobePl rizefor hisstudieosfthephysicaplrocessiemsportatnotthestructuraendevolutioonfstars. Figure3.SubrahmanCyahnandrasekhar Figure4.ArtistsrenderinogftheCXO TheObservatoarnyditsInstrumentation AnartistdsrawingoftheCXOisshowninFigure4.TheCXOhasthreemajoprartsasshowninFigure5: (1)theX-raytelescopoerHighResolutioMnirrorAssemb(lyHRMA)w, hosemirrorsfocusX-raysfrom celestiaolbjects(2; )thesciencienstrumen-tstheAdvanceCdCDImagingCamer(aACIS)andtheHigh ResolutioCnamera(HRC)whichrecordtheX-raysandtwosetsofObjectiveTransmissioGnratings (OTG)discussebdelowa;nd(3)thespacecrawft,hichprovidefsunctionssuchaspowerandtelemetry necessaforyrthetelescopaendtheinstrumentotswork. / _ign _una,_on -- .... :: .... , '"_ ""N. (HRMA} " / : _. _ .jJ carr_ra {HRC) / Ofat,ngs(2) I (IS#,t) Lowga_ antenna(2) CCD W'_ag_9 Spoct_e,me4ef(ACI$) Figure 5.Line drawing illustrating the major components of the CXO. The building and operation of this 1.5-billion-dollar facility has been a marvel of modern technology and ingenuity. Overall program management and technical and scientific oversight is provided by NASA's Marshall Space Flight Center. The Marshall Center was ably assisted by The Smithsonian Astrophysical Observatory (SAO). The Prime Contractor was the company TRW, which was responsible for the spacecraft construction and integration of all subsystems into the Observatory. Major subcontractors and their principal functions were: Raytheon Optical Systems - telescope grinding and polishing; Optical Coating Laboratories, Inc. - telescope coating; Eastman Kodak Corporation - telescope assembly and alignment; Ball Aerospace and Technology Corp.- science instrument accommodation module & aspect system. Because the Earth's atmosphere absorbs X-rays, the CXO was placed high above this atmosphere. This meant that the ultra-precise mirrors and detectors, together with the sophisticated electronics that conveys the information back to Earth, had to be able to withstand the rigors of a rocket launch, and operate in the hostile environment of space. Chandra's unusual orbit, shown in Figure 6, was achieved after initial deployment by the Space Shuttle Columbia, Eileen Collins (Figure 7) commanding. This particular Shuttle launch was especially noteworthy as Commander Collins was the first female commander. Initial deployment was followed by a boost into a high earth orbit by an Inertial Upper Stage built by the Boeing Corporation. Final placement into the orbit used a built-in propulsion system. The orbit, which has the shape of an ellipse, takes the spacecraft more than a third of the way to the moon before returning to its closest approach to the earth of 10,000 kilometers (9,942 miles). The time to complete an orbit about 65 hours. The spacecraft spends about 75% of its orbit above the belts of charged particles that surround the Earth. Uninterrupted observations as long as 55 hours are possible. ' i ver_iew AXA// lhunml Omm_M v_" ..__,___ , _,' :_I*rluilIra_ ', ,'\ I_' "(qA- -- / ]", Figure 6. CXO launch sequence and orbit. Figure 7. Commander Eileen Collins X-rays do not easily reflect off mirrors because of their high energy. However, reflection can take place when the angle of incidence is shallow. This property can be exploited to build optical systems that can bring x-rays to a common focus. A particular design, and the one utilized for the CXO, is illustrated in Figure. 8. The design, referred to as a Wolter type I, uses a paraboloid of revolution followed by a hyperboloid of revolution - two reflections being necessary to bring objects away from the axis of symmetry into focus. Nesting several of these pairs of paraboloids and hyperboloids increases efficiency for collecting the x-rays. The CXO has four such systems with diameters ranging from 0.65 m (2.13 fl) to 1.2 m (3.94 fl). Each optical element is 0.84 m (2.75 ft) long. The elements are constructed of Zerodur, a glassy ceramic, and together weigh over 2000 pounds. I)_rahM°id 1typcrh_A.id Surface .', Sur|'act's ....:...-.:.s.:.:.:...... I:oc,d P_)illt ..... >, Figure 8. Illustration of a cross-section of two, nested, Wolter I, X-Ray optics. The most unique attributes of the CXO X-ray optics, and the ones that makes this observatory so powerful, are the angular resolution (the ability to distinguish two separate objects very close to each other), and the high efficiency with which photons are collected within the narrow spot that defines its ability to resolve different objects. This high efficiency is a result of the smoothness of the x-ray reflecting surfaces so that the x-rays are not scattered away from the intended path. The angular resolution is better than 0.5 seconds of arc, i.e. the ability to distinguish the letters of an x-ray-emitting STOP sign at a distance of 12miles! The surface roughness is measured in angstroms• If the state of Colorado were as smooth as Chandra's mirrors, Pike's Peak would be less than one inch tall. The angular resolution of Chandra is significantly better than any previous, current, or even currently planned X-ray observatory. Figures 9 and 10 and illustrate the utility of the superb angular resolution and low scattering. Figure 9. Chandra's image of what had been a puzzling X-ray source in the globular star cluster M15shows that it is not a single system, but two sources that are so close together (2.7 seconds of arc) that they were indistinguishable with previous X-ray telescopes. (Credit: NASA/White and Angelini, 2001 .) FigureI0.ChandrimaageofthesupernorveamnanCtassiopeiab-aAseodnabou3tAofanhourofdataT.he pointsourceat the center,previouslyundetecteds,implyleapsout of the Chandraimage. Credit:NASA/CXC. The science instruments aboard the Observatory and the organizations that led their development are: the Advanced CCD Imaging Spectrometer (ACIS) - Penn State University and the Massachusetts Institute of Technology (MIT); the High Resolution Camera (HRC) - Smithsonian Astrophysical Observatory (SAO); the High Energy Transmission Grating (HETG) - MIT; and, the Low Energy Transmission Grating (LETG) - Space Research Institute of the Netherlands and the Max Planck Institute for Extraterrestial Physics in Garching, Germany. Either (but not both simultaneously) of the two transmission gratings can be commanded in place directly behind the telescope. When in position, X-rays are diverted (dispersed) according to their energy, along one dimension, from their normal path. The X-ray image now represents, to a high degree of accuracy, the energy of the incident photons. Determining the energy iscalled spectroscopy. The ACIS detectors record X-ray images and can, to a certain degree, also determine the energy of the incident X-ray but not as well as the gratings. Their spectroscopic advantage is that they are far more efficient for detecting x-rays when the gratings are not in place. There are two ACIS detectors, either of which can be placed at the focus of the telescope by command. ACIS-I is made of a 2-by-2 array of front- illuminated, 2.5-cm-square, X-ray sensitive charge coupled devices (CCDs) analogous to those found in visible-light-sensitive digital cameras. ACIS-I provides high-resolution spectrometric imaging over a 17- arcmin-square field of view. ACIS-S, a 6-by-1 array of 4 FI CCDs and two back-illuminated CCDs, is mounted along the dispersion direction of the transmission gratings, and serves both as the primary read- out detector for the HETG, and, using a one of the back-illuminated CCDs, that which can be placed at the aim point of the telescope, also provides high-resolution spectrometric imaging extending to lower energies, but over a smaller (8-arcmin-square) field than ACIS-I. As with ACIS, there are two HRC detectors, which may be moved into place to record X-Ray images. Both are microchannel-plate detectors, consisting of millions of tiny tubes of cesium-iodide coated glass. These detectors record the position of the x-rays, but unlike ACIS can barely distinguish energies. The HRC-I array isa 10-cm square plate with of field of view of 31-arcmin-square. Comprising 3rectangular segments (3-by 10-cm each) and mounted end-to-end along the dispersion direction, the HRC-S serves as the primary read-out detector for the LETG. A important advantage of the HRC for certain scientific experiments is the ability to determine the time that the x-ray event was detected to high a much higher precision (microseconds) than achievable with ACIS (milliseconds). Scientific Results X-rays are produced by highly energetic processes - thermal processes in plasmas with temperatures of millions of degrees or non-thermal processes, such as synchrotron emission (realized when charge particles are accelerated by magnetic fields) or scattering of visible light or radio waves from very hot electrons. Consequently, X-ray sources are frequently exotic: supernova explosions and remnants, where the explosion shocks the ambient interstellar medium or a pulsar, a rotating neutron star, powers the emission; disks of accreting nearby material or jets around stellar-mass neutron stars or black holes; accretion disks or jets around massive black holes in the nucleus of galaxies; hot gas in galaxies and in clusters of galaxies which traces the gravitational field and can be used for determining the mass. These are all examples of sites of, and methods for, producing x-rays. Here we give several examples of observations performed with the CXO that illustrate the capability for investigating these processes and objects. Chandra's capability for high-resolution imaging enables studies of the structure of extended x-ray sources, including supernova remnants (See Figure 10), astrophysical jets (Figure 11), and hot gas in galaxies and clusters of galaxies (Figure 2). The capability for spectrometric imaging allows studies of structure, not only in x-ray intensity, but also in temperature and in chemical composition. Through observations with Chandrsac,ientishtsavebeguntoaddressseveraolfthemosetxcitintgopicsincontemporaarsytrophysics. Figure11.ThisChandriamage2,4arcsecondosnasides,howdsetailsinthepowerfujeltshootinfgrom thequasa3rC273p,rovidinagnX-rayviewintotheareabetwee3nC27Ycsoreandthebeginninogfthejet. (CourtesNyASA/CXC/SAO/Mareshtaal.l2l 001) CometasndPlanets Besidetshesunw, hichistoobrighttobesafelyobservebdytheObservatooryth,erknownX-raysources inoursolasrystemincludteheEartht,hemoonV,enusJ,upitearndsomeofitsmoonsa,ndcometsT.heX- raysfromthemoonV, enuasndt,oacertainextentt,heEartha,reduetothefluorescenocfesolarX-rays strikingtheatmospherTeh.ediscoveriymageofX-rayemissiofnromVenus(Figure12)withChandra showashalfcrescednutetotherelativoerientatioonftheSunE, arthandVenusS.olaXr -raysareabsorbed intheVenusiaantmosphearbeovethesurfacoeftheplanetk,nockineglectronosutoftheinnerpartsof atomsa,ndexcitingtheatomstoahigheernerglyevelT. heatomaslmositmmediaterleyturntotheirlower energsytatewiththeemissioonfacharacterisotirc"fluorescenXt"-rayI.nasimilarway,ultraviolelitght producethsevisiblelightoffluorescelnatmpsI.nthecaseofJupite(rFigure13),theoriginoftheX-ray emissioinsmorecomplexandnotcompleteluynderstooIdm.portanintgredienatsrethepresencoefa magneticfield,androtationof theplanet.StudieswithChandrashouldhelpto providea better understandoinfgthephysicaplrocessiensvolved. Figure12.Chandriamaget,he first X-ray image ever, of Venus, shows a half crescent due to the relative orientation of the sun, Earth and the planet - the Sun is to the right. X-rays from Venus are produced by fluorescent radiation from oxygen and other atoms in the atmosphere about 130 kilometers above the surface. Credit: NASA/MPE/Dennerl et al. Figure 13. Chandra image of the x-ray emission from Jupiter. The red colors indicate the highest intensity. The bulk of the emission takes place near the magnetic poles. Credit: NASA/MSFC/Gladstone et al. 2002. Normal Stars The CXO has optical instrumentation aboard that provides an "aspect solution", which shows where the observatory was pointing during an observation to an accuracy that is about 1second of arc. However, it is usual for Chandra observations to detect the X-ray emission from several stars that have much more accurate cataloged positions based on their optical emission. Using the stellar positions as a local reference, the remaining X-ray sources in the field can be positioned far more precisely, to about 0.2 to 0.4 seconds of arc. One example of using such positions is the determination of the positions of the more than 1000 x-ray sources in the Orion Nebula star cluster (Figure 14). It is interesting that this single Chandra image contains more X-ray sources than had been detected in the first fifteen years of X-ray astronomy. The Orion Trapezium, a region only 3 light years across at the core of the Orion Nebula star cluster, contains very young stars and therefore offers astronomers a view into a region where stars are born. The cluster is composed of stars with a median age of only around 300,000 years, and, at a distance of 1400 light years, is one of the nearest star-forming regions. The CXO was used to identify X-ray emission from individual stars and found that almost all these young stars were much hotter than expected. Figure14.TheCXOimageoftheOrionstacrlusterT.heregionshowninthisimageisabou1t0lightyears acrossT•hebrighsttarsinthecentearrepartoftheTrapeziuman,associatioonfveryyoungstarswithages lessthanamillionyearsC.reditN: ASA/PSU TheCenteorfourGalaxy PrecispeositioninwgascriticaflortheuniqueidentificatioonftheX-rayemissiofnromtheobjecktnown asSagitariuAs*,thesourcaettheextremeclyrowdecdenteorfourownMilkyWaygalaxy(Figure15). Thissourciesamoderateslymalla,bou3t millionsolarmassb,lackholeandisveryfaintcomparetod othegralactincucleiX.-raysareemittejdustbeyontdhehorizonwithinwhichnolightcanescapaen, dthus theblackholemaybe"seen"A. brightflarewasdetectebdytheCXOon27Octobe2r000w, herethex-ray intensitiyncreasebdymorethanafactoorf10forabou3thoursandthenrapidlydippedonatimescaleof 10minuteTs.herapidvariatioinnX-rayintensitiyndicatethsattheflarewasduetomateriaalsclosetothe blackholeastheEarthistotheSun.Thisiscompellinegvidenctehatmattefrallingtowardthecentral blackholeisfuelingenergetaicctivityinthecenteorrourgalaxy. Figure15.TheACIS-iImageoftheGalactiCcenteTr.hisfalse-coloimrageshowtshecentrarlegionofour MilkyWayGalaxyasseenwiththeCXO.Thebrightp, oint-likesourceatthecenteorftheimagewas producebdyahugeX-rayflarethatoccurreidnthevicinityoftheblackholeatthecenteorfourgalaxy. CreditN: ASAfMIT/Baganeotaffl.2001. SupemovRaemnants AnotheerxamploefChandraa'sbilitytoprovidehigh-contraimstageissexemplifiebdythenowclassic imagoeftheremainosftheremnanfotrmedbytheimplosioonfastara,supernovcaa,lledtheCrabNebula anditscompacctorea,rotatinngeutrosntarthatpulsesT.heimages,howninFigure16,showtsheintricate structurperoducebdythepulsarinteractinwgiththelocalenvironmenTth.isimageisnotstatica, nd observatiownisththeCXO,spaceodutovertime,haveshowthedynamicamlotiontshattakeplaceasa resulotftheinteractioonfthepulsaartthecenteorftheremnanatndthelocael nvironment O ) O I -50 0 50 aFCSeC Figure 16.Chandra image of the Crab pulsar and nebula made with the LETGS and the HRC-S. The nearly horizontal line in the figure is a cross-dispersed spectrum of the pulsar produced by the LETG fine support bars. The nearly vertical line is the LETG-dispersed spectrum from the pulsar. Credit: NASA/MSFC/ Weisskopf et al. 2000. Globular Clusters One of the most striking examples of the power of Chandra X-ray imaging, is in the spectacular Chandra images of globular clusters. Figure 17 is an ACIS-I image of the Globular cluster 47 Tucanae. The left panel is composed of red/green/blue images derived from x-rays recorded in different energy bands and shows the central portion of the cluster. The enlargement at the right is the central core. Some 108 sources, excluding the central core, are detected. This number is more than ten times that found by previous X-ray satellites. These Chandra images of 47 Tucanae provided the first complete census of the brighter x-ray producing stars in the core of the globular cluster. As the oldest stellar systems in galaxies, globular clusters are laboratories for how stars evolve. Nearly all objects inthe Chandra images are "binary systems", in which a normal, Sun-like star orbits a collapsed star, either a white dwarf or neutron star from which the X-rays are emitted. The data also reveal the presence of many "millisecond pulsars", neutron stars that rotate extremely rapidly, between 100 to nearly 1000 times a second.