Welcome to the 4th Chandra – CIAO Workshop 20 – 22 May 2002 Martin Elvis Smithsonian Astrophysical Observatory Chandra X-ray Chandra X-ray Observatory Overview Martin Elvis Smithsonian Astrophysical Observatory CIAO Workshop 20 May 2001 Chandra X-ray NASA Great Observatories CHANDRA Chandra X-ray Focusing X-rays Chandra X-ray Chandra Mission Summary Launch: July 23, 1999 – STS-93/ Inertial Upper Stage / Integral Propulsion System – 10,000 km x 140,000 km, 28.4o Inclined Orbit Design Lifetime > 5 Years (in NASA plan for 10 year life) 10-m Focal Length Wolter -1 Mirror: 4 nested Mirror Pairs Energy Range: 0.1-10 keV ¼ arcsecond resolution. Sub-0.5arcsec in practice 2 Imaging Focal Plane Science Instruments – ACIS (Advanced CCD Imaging Spectrometer) – HRC (High Resolution Camera) 2 Objective Transmission Gratings for Dispersive Spectroscopy – LETG (Low-Energy Transmission Grating) – HETG (High-Energy Transmission Grating) Chandra X-ray Mission and Observatory Description Chandra X-ray High Resolution Mirror Assembly 4 pairs of concentric thin-walled zerodur, grazing incidence Wolter Type-I mirrors >large area. ->800cm2 E<2keV Antennae galaxies figured to 0.5” FWHM -> sensitivity, -> megapixel images Focal length 10 m. -> response to 10keV Many independent pixels High sensitivity Iridium edge polished to 3A -> low scattering high dynamic range PSR nebula PKS1127-145 95% High energy sources 1.6” Chandra X-ray 100:1 AGN/jet contrast Aspect Camera and Fiducial Transfer System Aspect Camera 4.25inch dia. 15”pixels <0.25” r ms (typical) Chandra X-ray Chandra Science Instruments Z+ ACIS-I Advanced CCD Imaging Spectrometer (ACIS) – CCD array with 16’x16’ field of view (ACIS-I) – grating readout array (ACIS-S) BI High Resolution Camera (HRC) – microchannel plate imager with 31’x31’ field of view (HRC-I) – low energy grating readout array (HRC-S) – High time resolution High Energy Transmission Grating Spectrometer (HETG) BI Y+ ACIS-S HRC-I – transmission grating pairs for medium and high energy Low Energy Transmission Grating Spectrometer (LETG) – transmission grating for low energy Chandra X-ray HRC-S Advanced CCD Imaging Spectrometer (ACIS) Ten 1024x1024 pixel CCDs (any 6 simultaneously) – Intrinsic energy resolution ~100eV -> imaging spectroscopy – ACIS-I: 2x2 array for imaging (16x16 arcmin) – ACIS-S: 1x6 array for imaging (8x8arcmin) or spectroscopy – 2 `back illuminated’ (BI) chips: good low E QE, higher throughput Chandra X-ray ACIS Issues CTI Front Iluminated (FI) chips suffered proton damage just after launch. -> charge transfer inefficiency (CTI) -> much degraded energy resolution CTI correction (Townsley, PSU) restores linearity, most dE/E Pileup 3.2 s full frame readout time -> for sources >0.1ct/s suffer “pileup” I.e. 2 photons in same pixel/frame -> loss of energy information, and -> loss of PSF peak Pileup correction (J.Davis, MIT) available in CIAO, Sherpa Chandra X-ray Low Energy Calibration Non-linear gain Changing QE See H. Donnely talk Chandra Grating Spectrometers m=2 Incoming Radiation d m=1 m=0 m=-1 m = d sin Chandra X-ray m=-2 Grating Spectrometers:HETG HETG: High Energy Transmission Gratings – Designed for use with ACIS-S providing E/delta(E) to 1000 between 0.4 and 10.0 keV – Two sets of gratings – Medium Energy Gratings (MEG) use outer 2 mirrors – High Energy Gratings (HEG) use inner 2 mirrors – Mounted at different angles to form an “X” dispersed pattern Capella HETG spectrum Chandra X-ray Grating Spectrometers: LETG LETG High Energy Transmission Gratings – – – – Provides highest resolving power at low energies Designed for use with HRC-S with 0.07 – 7.29 keV E/delta(E) > 1000 for 0.07 < E < 0.15 keV E/delta(E) < 1000 for E > 0.15 keV Chandra X-ray Chandra Operations Mission science plan converted to command loads and uplinked to Chandra X-ray events collected and stored on Solid-State Recorders (SSR) Ground contact established every ~8 hours through Deep Space Network – SSR data downlinked – new command load uplinked (up to 72 hours of stored commands) Data transferred to OCC through JPL for science processing Chandra X-ray sssssssssssssssssssssss CXO CXC OCC 6. Chandra X-ray Center Architecture uplink downlink Chandra Observing Cycle High (66%) observing efficiency TOOs, solar flares ->big hit on mission planning team Annual Proposal Cycle: Next Deadline: 15 March 2003 (anticipated) + Archive, Theory grants Funding expected to 2009 Chandra X-ray enjoy the workshop! Chandra X-ray