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Transcript of High energy Astrophysics Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab,...
![Page 1: High energy Astrophysics Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 15. Cosmology and High Energy Astrophysics in the.](https://reader035.fdocuments.net/reader035/viewer/2022062314/56649edb5503460f94bea611/html5/thumbnails/1.jpg)
High energy AstrophysicsCosmology and extragalactic
astronomyMat Page
Mullard Space Science Lab, UCL
15. Cosmology and High Energy Astrophysics in the
future
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15. High energy astrophysics in the future
• This lecture:• Future missions and observatories:
– What they areXEUS+Con-X -> IXO ->ATHENA->ATHENA(+)SKAEUSOEuclid
– What they do – What they will tell us
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XEUS
• 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
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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 4
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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 5
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Slide 7
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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 9
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Revised concept 2005
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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
Slide 10
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What did I think it would do?• 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 11
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Constellation-X
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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
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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
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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.
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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.
Slide 17
• 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.
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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).
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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 20
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Square Kilometre Array
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Square Kilometre Array
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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.
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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.
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LOFAR central array.Slide 25
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Extreme Universe Space Observatory (EUSO)
• 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
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Slide 27
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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?
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Just like the fluorescence imagers of Auger observatory HIRES, AGASA, etc but from above rather than from below
Slide 29
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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 30
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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 33
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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 34
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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 35
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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 .
Slide 36
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• 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?
Some key points: Slide 37