X-ray Astronomy School 2002 The Future of X-ray Astronomy Keith Arnaud NASA/GSFC and UMCP

X-ray Astronomy School 2002 High sensitivity, high resolution spectroscopy. Polarimetry Interferometry Theme In the first 40 years of X-ray astronomy we increased sensitivity by a factor of 10 9, image resolution by 2.5x10 5, spectral resolution by How do we keep this progress up for the next 40 years ?

X-ray Astronomy School 2002 About 150 years ago, James Joule and Julius von Mayer independently determined that HEAT = ENERGY, and calorimetry was born. But, only about 20 years ago, the power of performing calorimetric measurements at very low temperatures (< 0.1 K) was realized, independently, by Harvey Moseley and by Etorre Fiorini and Tapio Niinikoski. This is called MICROCALORIMETRY, or occasionally QUANTUM CALORIMETRY, because of its ability to measure the energy of individual photons or particles with high sensitivity. Calorimetry Stahle

X-ray Astronomy School 2002 X-ray calorimetry Stahle

X-ray Astronomy School 2002 Microcalorimeters vs. Gratings Resolutions comparable with gratings. Microcalorimeters win at high energies, gratings at low energies. Non-dispersive so : o high efficiency o low background o no problems for extended sources o wide bandpass However, microcalorimeters are cryogenic experiments requiring cooling to ~60 mK.

X-ray Astronomy School 2002 A Multiwavelength Note Microcalorimeters were first developed for IR and are being used on IR astronomy space missions. They are also being used on optical telescopes - where they provide filter type spectral resolution without using filters. They are also used in laboratory dark matter searches.

X-ray Astronomy School 2002 X-rays on Ice The XRS X-ray microcalorimeter built for Astro-E (the fifth Japanese X-ray astronomy satellite) Resolution : eV FWHM ( keV)

X-ray Astronomy School 2002 Inserting the He dewar in the Ne dewar A solid Ne dewar outside a liquid He dewar outside an adiabatic demagnetization refrigerator.

Ready for Launch from Kagoshima Space Center (KSC) February 2000

X-ray Astronomy School 2002 You need all the help you can get

X-ray Astronomy School 2002 Astro-E Launch

X-ray Astronomy School seconds and going well

X-ray Astronomy School 2002 Uh - oh

You really don’t want to see this Astro-E is being rebuilt as Astro-E2 and will be launched in Jan/Feb 2005.

X-ray Astronomy School 2002 XRS on EBIT at LLNL

X-ray Astronomy School 2002 Laboratory Astrophysics with a Microcalorimeter

X-ray Astronomy School 2002 Constellation-X

X-ray Astronomy School 2002

oUse X-ray spectroscopy to observe  Black holes: strong gravity & evolution  Large scale structure in the Universe & trace the underlying dark matter  Production and recycling of the elements oMission parameters  Telescope area: 3 m 2 at 1 keV 100 times XMM/Chandra for high res. spectra  Spectral resolving power: 300-3,000 5 times improvement at 6 keV  Band pass: 0.25 to 40 keV 100 times more sensitive at 40 keV Constellation-X Overview

X-ray Astronomy School Energy (eV) Counts per 0.25 eV bin Instrument Resolution: 2.0  0.1 eV FWHM Al K  1,2 Al K  3,4 Bismuth absorber TES Al/Ag bilayer 450 counts/sec K. Irwin Calorimeter developement

X-ray Astronomy School 2002 Goddard Mo/Au TES: 2.4 +/- 0.2 eV at 1.5 keV and 3.7 +/- 0.2 eV at 3.3 keV. Al K  into 300 x 300 micron TES K K  into 500 x 500 micron TES

X-ray Astronomy School 2002 McKee-Taylor Decadal Survey “Constellation-x observatory is the premier instrument to probe the formation and evolution of black holes... The first clusters of galaxies... Quasars at high redshift... And the formation of the chemical elements…” “Constellation-x will complement Chandra, much as Keck and Gemini complement HST…”

X-ray Astronomy School 2002 ESA proposed mission for low Earth orbit. 6 m 2 of collecting area at 1 keV. Imaging resolution goal of 2" HEW (Half Energy Width) at 1 keV. Limiting sensitivity 100 times deeper than XMM-NEWTON. XEUS Spectral resolution of 1 to 10 eV between 0.05 and 30 keV.

X-ray Astronomy School 2002 After completion of the initial 4-6 year mission phase, XEUS will rendezvous with the ISS for refurbishment and adding extra mirror area. New detector spacecraft with next generation of focal plane technologies. Grown mirror will have 30 m 2 collecting area at 1 keV; 3 m 2 at 8 keV. Sensitivity 250 times better than XMM-NEWTON. XEUS II

X-ray Astronomy School 2002 Con-x

X-ray Astronomy School 2002 Generation X o Scientific goal: to probe the X-ray emission from the universe at z = o An effective area of 150 m 2 at 1 keV with an angular resolution of ~ 0.1 arc second. o Detect sources 1000 times fainter than Chandra (flux limit of 2 x ergs/cm 2 /s). o Obtain high resolution spectra from sources x fainter than observable by Constellation-X. o Six identical satellites with 40 to 150 m focal length to L2.

Telescope Evolution No. of mo d s Angu lar HPD Eff. 1 keV (cm 2 ) per mod. Mass (kg) per mod. Notes Chandra 10.5"1,000 Ground and polished glass shells XMM-Newton 315"1,500420Replicated Ni shells Astro-E 590"40012 Replicated Al segments Constellation-X 415"7,500420Material and technology under study/development Generation-X 60.1"250,0003,000 Materials and fabrication technology to be determined

X-ray Astronomy School 2002 Why X-ray Polarimetry ? Because it’s there ! Whenever we look at the Universe in a new way we make unexpected discoveries. We expect polarization from X-ray synchrotron sources such as SNR and jets. Also from X-ray reflection in binaries and AGN. There is one detection of X-ray polarization - that of the Crab Nebula SNR. No X-ray polarimeter has flown on a satellite since the 1970s. There is a new idea for a more efficient polarimeter…

Polarization

X-ray Astronomy School 2002 Electron Tracks Bellazzini et al.

X-ray Astronomy School 2002 Microwell detector Bellazzini et al.

X-ray Astronomy School 2002 Bellazzini et al.

X-ray Astronomy School 2002 Accumulation of many events 5.9 KeV unpolarized 5.4 KeV polarized Bellazzini et al.

X-ray Astronomy School 2002 X-ray Interferometry While astronomical sensitivity has increased by a vast factor imaging resolution has not. HST is only 100 times better than Galileo’s telescope. To do better requires interferometry. Radio interferometry is well developed but baselines are very long and few sources have high enough surface brightness in the radio band. Optical interferometry is in the experimental stage and milliarcsec resolutions should be achievable.

X-ray Astronomy School 2002 X-ray Interferometry II The X-ray band is the natural place for interferometry ! Microarcsecond resolutions are possible with a baseline of ~10 meters. X-ray sources have very high surface brightness on microarcsecond scales. X-ray interferometry allows virtual interstellar travel…

100 milliarcseconds

10 milliarcseconds

1 milliarcsecond

100 microarcseconds

10 microarcseconds

1 microarcsecond

X-ray Astronomy School 2002

MAXIM Pathfinder Milliarcsecond resolution

X-ray Astronomy School 2002 Timeline 2002 (Integral) 2004 Swift 2005 Astro-E (GLAST) 2009? NeXT 2012? Constellation-X 2015?? XEUS, Maxim Pathfinder 2025??? Generation X, Maxim