Survey
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Very Large Telescope wikipedia , lookup
James Webb Space Telescope wikipedia , lookup
Allen Telescope Array wikipedia , lookup
Wilkinson Microwave Anisotropy Probe wikipedia , lookup
Arecibo Observatory wikipedia , lookup
International Ultraviolet Explorer wikipedia , lookup
Leibniz Institute for Astrophysics Potsdam wikipedia , lookup
X-ray astronomy satellite wikipedia , lookup
High energy Astrophysics Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 15. Cosmology and High Energy Astrophysics in the future Slide 2 15. High energy astrophysics in the future • This lecture: • Future missions and observatories: – What they are XEUS+Con-X -> IXO ->ATHENA->ATHENA(+) SKA EUSO Euclid – What they do – What they will tell us XEUS Slide 3 • X-ray Evolving Universe Spectroscopy mission • Dreamed up in 1995 • “The future of European high energy astrophysics” • Most sensitive X-ray observatory ever • 2 spacecraft: mirror module separate from detector spacecraft Slide 4 Initial concept: • 6 m2 collecting area at 1 keV – (c.f. XMM 0.25 m2) • Spatial resolution of < 2 arcseconds • Spectral resolution of 1-10 eV between 50eV and 30 keV (better than XMM RGS, and imaging rather than gratings!) Slide 5 Growth on ISS • After initial 4-6 years, the mirror spacecraft docks with the international space station. • New mirror segments added to give 30 m2 collecting area at 1 keV • New detector spacecraft launched with the next generation of detectors Slide 6 Slide 7 Slide 9 New concept • With space shuttle grounded, space station was no longer an advantage. – XEUS looked like a dead turkey :( • Rapidly rethought! • New technology mirrors use ‘micropore optics’, glass with tiny (mirror) holes like a microchannel plate. • Much larger mirror now possible for same weight. • No ISS assembly required. Slide 8 Revised concept 2005 Slide 10 Objectives: • Detecting the first massive black holes • Finding the first galaxy groups and tracing their evolution to today’s clusters • Evolution of the heavy element abundances • Absorption line spectroscopy of the intergalactic medium What did I think it would do? Slide 11 • Crucial aspect in my mind is the spectroscopy. • Better spectral resolution than XMM with imaging rather than grating instruments – can go much fainter • 100 times the XMM collecting area with grown mirrors • Spectroscopy of not just the brightest X-ray sources. • We may have been thinking a bit too big – the observatory is supposed to do everything! – Americans could have beaten us to some important parts of the science with Con-X Slide 12 Constellation-X Slide 13 Slide 14 Constellation X • Launch 4 identical spacecraft to build up the collecting area rather than launching 1 big spacecraft • If one goes wrong, the whole mission is only set back a bit (i.e. it has a high level of redundancy). • About 6 times the collecting area of XMM – more at harder energies • Similar spatial resolution to XMM – bit like launching a fleet of XMMs • < 10 eV resolution from 6-10 keV Slide 15 What would it do? • High resolution spectroscopy of Fe lines, particularly relativistic lines in AGN. • Absorption lines from the interstellar medium • X-ray astronomy in general. Bigger and better than XMM • Not as big, poorer spatial resolution than XEUS Slide 16 XEUS + Con-X merged to become International X-ray Observatory in 2009 • Large X-ray observatory, launch date ~2025(+). • Will pick up highly obscured AGN directly from their X-ray emission. • Single spacecraft, extendable optical bench, 25m long • Like a giant XMM-Newton with a cryogenic spectrometer. • 2011: US decadal survey didn’t rank IXO high enough that they are likely to have money for it: IXO was dead. • ESA hastily went back to studying a European only mission. Slide 17 March 2011: Athena • Large X-ray observatory, launch date ~2025(+). • Single spacecraft 12m long – very similar spacecraft dimensions and layout as XMM-Newton • Key science objectives: strong gravity (relativistic iron lines) and detecting distant AGN. • Like XMM-Newton with a larger collecting area split between 2 telescopes and a cryogenic spectrometer. • ESA down-selection for L1 mission April 2012. • Lost out to JUICE. Slide 18 March 2013 on: Athena+ • The call for science themes for the next 2 large ESA missions is out: launches in 2028, 2034. • X-ray community proposed a new large X-ray observatory, codenamed Athena+. • 2 m2 collecting area, cryo spectrometer, wide-field imager. • Spatial resolution will be between 2 and 5 arcseconds. • Key science will be intergalactic warm gas, outflows from AGN. “Most of the baryons and the hot Universe” was what I advocated as the emphasis of the case. • Announcement November 2013. “Hot and energetic Universe” theme accepted as ESA’s L2 mission. • Athena (“+” dropped now) anticipated for launch in 2028 (now only 14 years away, and with 18 years now passed since original XEUS concept in 1996). Slide 19 Slide 20 Square Kilometer Array • Huge array of radio telescopes. • Earlier design of 30, 200m diameter radio telescopes now exchanged for design with hundreds of dishes. • Will stretch over 8 African countries and into Australia • Synthesized aperture of 1000 km • Collecting area of 106 m2 • Should be able to see 1 deg2 at 0.1 arcsecond resolution. Slide 21 Square Kilometre Array Slide 22 Square Kilometre Array Slide 23 SKA science • The dawn of galaxies and the reionization of the Universe, seen in 21cm absorption and emission. • Measurements of gazillions of redshifts using 21cm line to make incredibly detailed cosmological surveys. • milliarcsecond imaging of radio galaxy cores with orders of magnitude better sensitivity • Supernova remnants in starburst galaxies out to 100 Mpc • Will generate (and have to process) more data per year than the entire Earth does at present. Slide 24 LOFAR right now. • While SKA is being planned, there is already a small prototype called the LOw Frequency ARray (LOFAR). • Main centre is in Holland, but antennas are located in other countries as well, including the UK, to extend baselines and improve resolution. • UCL has bought into the observatory, collaboratively between MSSL and Physics and Astronomy. Slide 25 LOFAR central array. Extreme Universe Space Observatory (EUSO) Slide 26 • Experiment to observe ultra-high energy cosmic rays • Rather than looking up at the atmosphere from the Earth’s surface, EUSO looks down from above the dark Earth • huge sky area ~ 160 000 km2. • Images ultraviolet fluorescence from atmospheric nitrogen in extensive air showers • Sited on ISS (in original proposal at least). • Should detect ~1000 events with > 1020 eV energy per year Slide 27 Slide 28 What will it tell us? • Where do ultrahigh energy cosmic rays come from? • Are there celestial UHECR ‘sources’? • Is there a maximum cosmic ray energy? • Are there high energy cosmic neutrinos? Slide 29 Just like the fluorescence imagers of Auger observatory HIRES, AGASA, etc but from above rather than from below Slide 30 Euclid • The acceleration of the Universe is a very puzzling thing. • What is this ‘dark energy’ associated with the vacuum? • Is it Einstein’s cosmological constant? • A “new” and very big question for astronomers and physicists. Slide 33 Euclid • • • • • ESA “Medium” mission selected in October 2011. Will study dark energy using Weak lensing Baryon acoustic oscillations Carries optical and infrared imaging, infrared spectroscopy. Slide 34 Euclid • Its near-IR imaging will go far deeper than VISTA or any other ground-based imaging survey because of the reduced background and lack of atmospheric absorption. The IR imaging isn’t at HST resolution – it isn’t for weak lensing, but for photometric redshifts. • It will also take near-IR spectra of > 107 galaxies to measure baryon acoustic oscillations. • Extremely precise tests of dark energy compared to anything that has come before. Slide 35 Euclid • Weak lensing is at the core of Euclid. In essence, Euclid will have a wide field optical imager with spatial resolution similar to the HST, but with an exceptionally carefully controlled point spread function. • Only a 1.2m telescope, but it will take HST-like images of at least half of the extragalactic sky. • Visible imager consortium led by Mark Cropper of MSSL. • Extremely ambitious. Slide 36 Euclid • US participation in Euclid has been on and off several times. Overall, (arguably) not a positive interaction. • US decadal plan indicated number 1 priority would be a dark energy mission more ambitious than Euclid to come soon after – WFIRST. • But NASA was (is?) in big trouble with the cost overrun of JWST. It doesn’t look likely that WFIRST will be launched less than 5 years after Euclid. • Europe has a really superb opportunity to lead the way in addressing astronomy’s biggest mystery . Some key points: Slide 37 • Athena could identify the first quasars and measure the warm intergalactic medium (i.e. most of baryons). • The Square kilometer array could enable super-high resolution imaging of radio galaxies and measure galaxy redshifts through 21cm line back into the epoch of reionization. • EUSO (or something similar) could identify what and where the highest energy cosmic rays come from better than any of its predecessors. • Euclid will probe dark energy to a precision much better than achieved today, to address questions like: is there a cosmological constant, or is dark energy different?