Future Japanese X-ray TES calorimeter satellite: DIOS (Diffuse Intergalactic Oxygen Surveyor)

Transcription

1 LTD16, 2015, Future Japanese X-ray TES calorimeter satellite: DIOS (Diffuse Intergalactic Oxygen Surveyor) Shinya Yamada Tokyo Metropolitan University T. Ohashi 1, Y. Ishisaki 1, Y. Ezoe 1, N. Miyazaki 1, K. Kuwabara 1, G. Kuromaru 1, S. Suzuki 1, K. Mitsuda 2, N. Y. Yamasaki 2, Y. Takei 2, K. Sakai 2, K. Nagayoshi 2, R. Yamamoto 2, T. Hayashi 2, H. Muramatsu 2, Y. Tawara 3, I. Mitsuishi 3, Y. Babazaki 3, Ren Nakamichi 3, Ayako Bandai 3, Y. Yuasa 4, N. Ota 5, and the DIOS team 1 : Tokyo Metropolitan University, 2 : JAXA/ISAS, 3 : Nagoya University 4: RIKEN 5: Nara Women s U. Dark baryon surveyor X-ray TES calorimeter (~400 pixel) Japanese small satellite mission A pathfinder to ATHENA DIOS

2 DIOS collaboration Tokyo Metropolitan University (TMU) T. Ohashi, Y. Ishisaki, Y. Ezoe, S. Yamada, S. Sasaki Nagoya University Y. Tawara, A. Furuzawa, I. Sakurai, S. Sugita, I. Mitsuishi Univeristy of Tokyo Y. Suto, H. Kawahara Tsukuba University K. Yoshikawa Tokyo Tech. University N. Kawai Kanazawa University Support from overseas colleagues R. Fujimoto SRON (NL) Toho University T. Kitayama J.-W. den Herder, H. Akamatsu ISAS/JAXA IASF (Italy) K. Mitsuda, N. Yamasaki, Y. Takei, M. Ishida L. Piro Tokyo University of Science NASA/GSFC (US) K. Matsushita, K. Sato RIKEN R. Kelley, S. Bandler H. Noda, T. Yuasa MIT (US) Saitama University E. Figueroa-Feliciano M. Tashiro NASA/MSFC (US) Aoyama Gakuin University A. Bamba, M. Sawada C. Kouveliotou Nara Wemen's University N. Ota + many graduate students

3 LTD16, 2015, Japanese X-ray missions ~ Suzaku(1700kg) ASTRO-H (2500kg) 2022(?) ~ DIOS (700kg) X-ray CCD Si & GSO detectors X-ray Si micro-calorimeter Si-CdTe Compton camera X-ray TES calorimeter Astrophysics galaxies, clusters, SNR Suzaku stars, blackholes, etc. micro-calorimeter science for the first time detail gas motions in cluster, AGN feedback Epsilon rocket, DIOS ASTRO-H Dark Baryon Cosmic large structure DIOS HII rocket, suzaku, Astro-H 3

4 Inter Galactic Medium Temperature (K) Big Bang Light elements Synthesis Recombination First star Reionization Galaxy formation Cluster formation Structural formation Present Thermal history of the Universe 10 6 K 10 4 K 10 2 K Reionization by UV and X-ray Cooling by expansion Metal synthesis & circulation Shock heating 3min 0.38M 0.2G 0.8G 5G 13.7Gyr Age of the Universe WHIM (warm-hot intergalactic medium) will tell us the evolution of the hot-phase material in the universe

5 Large-scale structure Galaxy!Cluster! Virgo!ConsorWum,!Springel!et!al.!05!

6 dark matter, hot gas and galaxies SPH simulation: ΛCDM, (75h -1 Mpc) 3 box (Yoshikawa, Taruya, Jing & Suto 2001)

7 Intergalactic medium to map cosmic structure WHIM ( K) traces the cosmic large-scale structure = Missing baryon 30-50% baryon are still not observationally confirmed, which are believed to be WHIM. The goal of the DIOS is clarify WHIM existence and its large-scale structures. Dark matter IGM ( K) Galaxies (~10 4 K) Cluster gas (10 7 K) Typical matter density: d (=n/ n B ) = size = 30 h -1 Mpc box 5 deg at z=0 Yoshikawa et al. 2001, ApJ, 558, Mpc

8 DIOS: Expected spectra Takei et al Detectable fraction Galactic + BGD WHIM (z = 0.033) 5 Ms with DIOS (200cm Line-free energy ranges of MW emission give us windows in redshift space for WHIM detection 5 deg 5 deg survey (1 Ms 30) plus one deep (5 Ms) pointing can be likely to be planed.

9 4-reflection telescope and TES calorimeter array de < 5 ev, Energy range < 2 kev, F.O.V. = arcmin 2 Mechanical coolers are same as ASTRO-H DIOS and its grasp (SΩ) 1 m Orbit: 550 km altitude, Inclination 30, period 95 min

10 DIOS spacecraft & instruments (Baseline design) Mass total ~ 700 kg payload ~ 320 kg Size launch m in orbit m Attitude control 3-axis accuracy 30 arcsec Power total 700 W Effective Area 200 cm2 (> 100 cm 2 ) F. o. v 50' diameter SW Angular resol. Energy resol. Energy range > 100 cm 2 deg 2 (0.6 kev) 3' (16 x 16 pix or more) < 5 ev (FWHM) kev (or more) payload 380 W Mission life > 1 yr (goal 5 yr)

11 Payload configuration 4-reflection telescope Focal length = 70 cm: wide field with small instrument TES calorimeter Stable against noise, arrays are possible ADR Mechanical coolers 図 2: DIOS 観測装置 (FXT+ XSA) のシステム構成 Cryogen-free cooling system (cf. LHe-tank installed in ASTRO-H Dewar) light Dewar system, leading to IR and X-ray future missions

12 Payload mechanical design fitted into payload fairing Vacuum tight Dewar will be supported by torus structure Vibration characteristics satisfies spacecraft requirements Payload mass is about 320 kg, 692.2kg in total (<720 kg limit) X-ray telescope Spacecraft bus TES calorimeter Dewar 1m Radiator Solar array panel 1m

13 Payload thermal design Cooling system Almost same as ASTRO-H but without liquid He Thermal design Cooler power ~ 290 W Dewar surface -10 to -40 degc JT cooler is operable. Spacecraft Power: about 700 W Solar paddle will be type Thermal input to S/C bus radiator panels, location of the Dewar are optimized. Cooling chain Thermal analysis model

14 ADU ADU Baseline Design Top View Side View We designed Four-stage X-ray Telescope for this requirement which has extended Wolter-I optics (Tawara et al. SPIE 2005, fig. 5). FXT mirror design and fabrication Mirrors methods are based on a conical Fig 5 Schematic optics view applied of for Suzaku and ASTRO-H. X-ray mirrors & detectors 4-reflection telescope Table 2 Design parameters of DI OS/FXT 4. Developed X-ray M easurement by Nagoya at I SAS U (Y. Tawara et al.) We performed X-ray measurement of the demonstration model at ISAS beam line (fig. 8) Nov Energy of X-ray beam was 1.5 kev (Al) and focal plain detector was CCD. We obtained on-axis image and off-axis image (vignetting) in pitch and yaw angle between 40 arcmin which are vignetting data of four reflection image. In On-axis image, focal length was consistent with ~700 mm and angular resolution HPD of 10 sets of 4 stage mirrors was 8.8 arcmin (fig ). arcmin The best HPD at of present these sets was (< 6.5 arcmin 5 arcmin as shown in required) fig. 10. The angular resolution is approximately twice as good as that of our previous study. Although angular resolution is slightly worse than the requirement 5 arcmin, the field of view and the effective area (EA) are consistent with those expected from the ray-tracing simulations (fig. 9 and fig. 11). Mirrors will be made in-house. 193 layers. Angular resolution TES calorimeter Angular resolution and Effective area 10 3 extended Wolter-I optics (four-stage) Japan - US 5 (NASA/GSFC) arcmin collaboration after Suzaku Half Power Diameter; and HPDASTRO-H US plans Micro-X rocket HPD: experiment 6.5 arcmin soon 10 Pixel size is um 2 HPD: 8.8 arcmin Previous study (HPD of 4 sets of 4 stage mirrors): 15 arcmin 16x16 EA: 0.28 ± 0.01 ± (or 0.05 cm20x20) pixels will cover 50 x50 2 (The value expected by ray-tracing simulations: 0.30 cm Mass, power, 2 ) thermal load to JT is under Fig. 9: X-ray image of 10 sets of 4 stage mirrors consideration 5. Enhanced FXT T3.4 Hayashi T4.3 Yamamoto X-ray M easurement at 4 5 arcmin I SAS Babazaki M-thesis 2015, etc. 4-reflection telescope Fig 5 Schematic view of Field of View extended Wolter-I optics data, - gaussian function fitted to the data (four-stage) 口径 60 cm クオドラントハウジング θz1 cm We performed X-ray measurement of the 10 demonstration model at ISAS beam line (fig. 3 Nov Energy of X-ray beam was 1.5 kev (Al) and focal plain detector was CCD. We obtained on-axis image and off-axis image (vignetting) in pitch off-axis θz and [arcmin] yaw angle between offarcmin which are vignetting data of four reflection FoV image. = 32.0 ± In 0.2 On-axis arcmin (35.0 image, arcmin) focal FoV length = 76.8 ± 0.2 w 20x20 *The pixel value TES in parentheses calorimeter is one expected Fig. 10: X-ray image of 1 sets of 4 consistent with ~700 LTD16. mm stage and T1.1 mirrors Muramatsu angular resolution T1.1 Kuromaru HPD of 10 Fig. developed sets 11: Vignetting of 4 stage curve in mirrors of θz axis Japan was (left) and 8.8θ T1.4 Kikuchi. T3.1 Sakai T3.3 Nagayoshi arcmin (fig. 9). The best HPD of these sets was 6.5 arcmin as shown in fig. 10. The angula Norm alizede ffe ctive Are a 290 mm Effective area Fig. 6: FXT demonstration model (quarter size) X-ray CCD Ezoe+2012, Field of View Yamada+13 (FWHM) 170 mm 700 Fig. 8: Setup of X-ray measurement in the Vacuu θy

15 Larger mirror and fast re-pointing Two features added on DIOS (within the spacecraft constraint) Focal length = 1.2 m Larger X-ray telescope focal length 0.7 (default) to 1.2 m 3 times larger effective area with high energy coverage Focal Length = 0.7 m (default) (from U. Nagoya group) Fast re-pointing to observe gamma-ray bursts or transients within tens of minutes UHF/VHF? iridium satellite? Absorption by ISM in high-z host galaxies through gamma-ray bursts Emission & absorption of the same WHIM clouds lead to gas geometry emission ~ n 2 L absorption ~ nl absorption emission (EDGE proposal)

16 Wide range of targets for DIOS 3-dim structure of dark baryons charge exchange lines from low density fields hot interstellar gas (Galactic fountain and winds) Large-scale shocks and particle acceleration Beyond the edge of clusters of galaxies Structure of dark baryons Super Nova Remnant RX J Milky-way hot gas Earth's magnetosphere Cluster: A3667

17 (tentative) Schedule of DIOS Pre Phase-A Phase-A Phase-B Phase-C Phase-D Phase-E call for next missio n Spacecraft Basic design detailed design (MTM, TTM) FM production Integration Final integration test cryocoolers Basic design detailed design (MTM, TTM) FM production TES calorimeters Basic design Fabrication & performance Integration of detector stage & performance tests Electronics Basic design detailed design (MTM, TTM) FM production Environmental test Telescope Basic design detailed design (MTM, TTM) FM production Performance test

18 High evaluation from the community In Autumn 2012 DIOS was nominated by HEAPA (High-Energy AstroPhysics Association) as the top rating mission of 6 other missions, and formally recommended to Science Council of Japan In Spring 2013 Science Council of Japanese Astrophysics subcommittee recommended 8 future projects to SCJ, nominating DIOS as the only X-ray program (cf. other 7 missions are SPICA, Solar-C, LiteBIRD, SKA, JEM-EUSO, South pole, CTA) In March 2014 Science Council of Japan Master plan of future large projects, nominated DIOS as the only X-ray program.

19 Message from Takaya Ohashi (PI) Ohashi (PI) ~ Bitter history ~ 2003 DIOS group started. First proposal with simulation by Yoshikawa+2003 Detectability of WHIM 2006 DIOS Working Group under space science committee 2007 EDGE proposed to ESA Cosmic Vision, 1 st M class mission rejected 2009 XENIA proposed to NASA Decadal Survey rejected 2010 ORIGIN proposed to ESA Cosmic Vision, 2 nd M class mission rejected DIOS is a long collaboration with US and European partners over 10 years. Even if Japanese community supports DIOS as the next small satellite, it is not clear if DIOS really come true, but your strong support will give us the power.

20 Summary Science:perform dark baryon survey and expand the X-ray spectroscopy science opened with ASTRO-H. The large f.o.v. (30-50 arcmin) and low BGD will enable us to detect faint extended emission from wide range of objects. New technologies of TES microcalorimeters and cooling system will be further improved through DIOS mission; a useful pathfinder to a future mission like ATHENA. International partners in U.S. and Europe have been critically important to realize a space mission with TES calorimeters. Recognition and support for DIOS in Japanese science community are becoming very strong. LTD16, 2015,

21 Temperature Search for Dark Baryons Numerical simulations indicate local baryons are mostly in the form of Warm-Hot Intergalactic Medium (WHIM: ~10 6 K). simulated baryon phases DIOS observable Emission lines like H-like and He-like triplets are simple, and spatial structure can be measured. Absorption lines through bright quasars and gamma-ray burst can break degeneracy bet. density n and the line of sight L, because emission ~ n 2 L absorption ~ nl High-resolution spectroscopy is necessary to separate out redshifted WHIM features from galactic foreground emission. Starforming Ly a Density (overdensity) Branchini et al