Solar wind Magnetosphere Ionosphere Link Explorer: SoH X-ray Imager (SMILE-SXI)

Transcription

1 Solar wind Magnetosphere Ionosphere Link Explorer: SoH X-ray Imager (SMILE-SXI) Steve Sembay SMILE-SXI PI Department of Physics and Astronomy University of Leicester, UK On behalf of the SMILE-SXI collaborabon 29th February, 216 IACHEC, ICUAA Pune, India 1

2 now planned Q3 221 SMILE Mission Joint Co-PIs: Graziella Branduardi-Raymont, MSSL, UK Chi Wang, NSSC, China 29th February, 216 IACHEC, ICUAA Pune, India 2

3 29th February, 216 IACHEC, ICUAA Pune, India 3

4 Magnetosheath 29th February, 216 IACHEC, ICUAA Pune, India 4

5 Magnetospheric Solar Wind Charge exchange (SWCX) SWCX: Heavy solar wind ions, A, in collision with neutral target atoms, B A q+ + B A (q-1)+* + B + A (q-1)+* A (q-1)+ + hν X-ray power depends on SW density and velocity and exosphere density Efficiency factor α depends on CX X-sections and SW heavy ion and target neutral composition α ~ 9.4 x 1-16 ev cm 2 (slow wind) α ~ 3.3 x 1-16 ev cm 2 (fast wind) SW heavy ion content is ~1% n sw v av n H MHD model Robertson & Cravens (23, 26) Exosphere model (Hodges 1994) 29th February, 216 IACHEC, ICUAA Pune, India 5

6 MHD Model CX Emissivity: POV at 2 R E T. Sun, NSSC N SW = 4.5 cm -3 V SW = 42 km s -1 N SW = 22.7 cm -3 V SW = 623 km s -1 Bowshock Earth Cusp Cusp Magnetopause 29th February, 216 IACHEC, ICUAA Pune, India 6

7 MHD Model CX Emissivity: POV at 2 R E T. Sun, NSSC N SW = 4.5 cm -3 V SW = 42 km s -1 N SW = 22.7 cm -3 V SW = 623 km s -1 Bowshock Earth Cusp Cusp Magnetopause 29th February, 216 IACHEC, ICUAA Pune, India 7

8 History: ROSAT PSPC LEO All-Sky Survey, 199 ROSAT ¼ kev Survey Pre-cleaning ROSAT ¼ kev Survey Post-cleaning ¼ kev band 29th February, 216 IACHEC, ICUAA Pune, India 8

9 C ts s- 1 ke V Residuals.5. Example XMM Spectra: Narrow FOV LOS through magnetosheath (similar spectra from Suzaku in LEO) Snowden, Collier & Kuntz 24 Carter, Sembay & Read OVIII Ne X MOS1 CME Flare Cts s -1 kev -1.1 Si XIII.1 1. CX Signal ~ 3 x Background.3 2. kev Residuals Energy (kev) 29th February, 216 IACHEC, ICUAA Pune, India 9

10 SMILE-SXI simulated observabons: SMILE orbit ~ 5 hours, 19 R E Apogee, 1R E Perigee Ian Whigaker,UoL Coronal Mass EjecBon interacbon: 31 March 21 1

11 SoH X-ray Imager Basic configurabon 1 UVI FOV SXI FOV T. Sun (NSSC) Relative Intensity Cts s -1 kev Input CX spectrum SWCX Spectrum Observed BGD subtracted spectrum C VI O VII O VIII Fe Ne X 54.8 Kcts Mg XI Mg XI Si XIII Si XIV Energy (kev) CCD Detector Plane Photon counbng High QE in soh X-rays ~8% at 25 ev Medium energy resolubon ~5 ev FWHM at 5 ev Lobster-eye Micropore Op7c Ultra-wide field of view ~22 x mm focal length Low Mass ~ 1kg opbc array (only) 29th February, 216 IACHEC, ICUAA Pune, India 11

12 OpBcs Lobster-eye Micropore OpBcs (MPO) Square-packed 2 μm pores, 6 μm walls Manufactured (Photonis) as glass plates, typically 4x4 cm, 1mm thick, heat-slumped to required radius of curvature Plates glued onto frame to build FOV. 1mm overlap. Low mass: Flight opbc ~ 1kg SVOM breadboard, UoL 29th February, 216 IACHEC, ICUAA Pune, India 12

13 OpBcs Space InstrumentaBon Heritage MIXS (MIXS-T and MIXS-C) instruments on ESA/JAXA BepiColombo mission to Mercury, Launch 217, arrival 224. MIXS PI insbtute UoL MIXS-T: Radially-packed MPOs in Wolter Geometry MIXS-C: Square-packed MPOs employed as collimators. MPOs slumped to 55 cm ROC, detector at distance equal to slump radius DXL/STORM Module. PI Michael Collier, NASA/GSFC Flew on DXL sounding rocket flight, December 212 First Lobster-eye MPO telescope to be launched into space. Detected X-rays from soh X-ray background. Successfully recovered despite abnormal vibrabon during launch. SVOM breadboard, UoL 29th February, 216 IACHEC, ICUAA Pune, India 13

14 Detector plane CCD Baseline 2x2 array e2v CCD27 PLATO: ESA M3 exoplanet mission 36 cameras, each with 2x2 array of CCDs SMILE leverages work done for PLATO on CCDs and readout electronics e2v CCD27 PLATO (ESA M3) derivabve NaBve 451 x μm pixels NaBve Image area 8.12 x 8.12 cm Back-illuminated 2-node readout available Operated with asymmetric frame store 6 x binning giving 18 μm pixels Baseline ~1s frame Bme SMILE-SXI CCDs opbmised for X-ray detecbon e.g. no AR coabng 29th February, 216 IACHEC, ICUAA Pune, India 14

15 Detector plane ComparaBve sizes (to scale) SMILE-SXI: 4 x PLATO derivabve CCDs ~226 cm 2 AcBve Area XMM-EPIC: Athena WFI: 14 x MOS 12 x pn CCDs M1 M2 4 x DEPFETS ~177 cm 2 ~12 cm 2 pn 29th February, 216 IACHEC, ICUAA Pune, India 15

16 1 Instrument Response.1 3 Eff. Area (cm 2 ) 2 1 SXI Response Peak Eff. Area ~ 1 cm 2 Optic Optic * QE Total 1.2 Energy (kev) Simulated SXI PSF PSF at 5 ev OpBc only, Iridium CoaBng with 85% baffle vignesng OpBc x CCD-QE OpBc x CCD-QE x Filter 6 Å MgF 2, 6Å Al 5-5 Measured PSF Core ~6 arcminutes FWHM ~32% of flux within 15 arcminutes radius ~48% of flux within 6 arcminutes radius at 5 ev 29th February, IACHEC, ICUAA Pune, India 16

17 Predicted SXI performance N SW : 4.54 cm -3 V SW : km s -1 By: 8.56 nt Bz: -.7 nt MHD Simulation Position: GSE Aim Point: GSE CX Intensity (kev cm -2 s -1 sr -1 ) Counts (Bgd.Subtr.): 3 s Cts per 1.x1. deg pixel SWCX at magnetosheath peak Energy range.1 to 2. kev Pixel = 1. degrees Component Rate (cts s -1 pixel -1 ) SWCX.3 Sky Background.12 ParBcle Background.2 Average point sources Time for pixel > 3σ s N SW : cm -3 V SW : km s -1 By: 5.48 nt Bz: nt MHD Simulation Position: GSE Aim Point: GSE CX Intensity (kev cm -2 s -1 sr -1 ) Counts (Bgd.Subtr.): 3 s Cts per 1.x1. deg pixel Component Rate (cts s -1 pixel -1 ) SWCX.7 Sky Background.12 ParBcle Background.2 Average point sources.15 29th February, 216 IACHEC, ICUAA Pune, India Time for pixel > 3σ 15 s 17

18 Predicted SXI performance Note on rela7ve par7cle background: EsBmated SXI parbcle background (conbnuum) is ~.24 cts cm -2 s -1 kev -1 Observed quiescent XMM EPIC-MOS parbcle bgd ~.28 cts cm -2 s -1 kev -1 i.e. SXI factor ~ 1 higher than EPIC-MOS 1 cm 2 on SXI detector has grasp (FOV x Eff. Area) of ~ 2.3 sq. degrees x 1 cm 2 = cm 2 on MOS detector has grasp (FOV x Eff. Area) of SWCX at magnetosheath peak Energy range.1 to 2. kev Pixel = 1. degrees Component Rate (cts s -1 pixel -1 ) SWCX.3 Sky Background.12 ParBcle Background.2 Average point sources Time for pixel > 3σ s Component Rate (cts s -1 pixel -1 ) SWCX.7 ~.48 sq. degrees x 45 cm 2 = 2.2 i.e. X-ray diffuse flux to parbcle background rabo per detector pixel is similar in both instruments. Sky Background.12 ParBcle Background.2 Average point sources.15 29th February, 216 IACHEC, ICUAA Pune, India Time for pixel > 3σ 15 s 18

19 SIMS N SW : 4.54 cm -3 V SW : km s -1 By: 8.56 nt Bz: -.7 nt Position: GSE Aim Point: GSE N SW : cm -3 V SW : 65. km s -1 By: nt Bz: nt Position: GSE Aim Point: GSE MHD Simulation CX Intensity (kev cm -2 s -1 sr -1 ) Counts (Bgd.Subtr.): 3 s Cts per 1.x1. deg pixel Processed: 3 s Cts per 1.x1. deg pixel MHD Simulation CX Intensity (kev cm -2 s -1 sr -1 ) Counts (Bgd.Subtr.): 3 s Cts per 1.x1. deg pixel Processed: 3 s Cts per 1.x1. deg pixel Image Scan, Solar Wind: N=4.54, V=42.41 Image Scan, Solar Wind: N=12.35, V= Normalised profile.4.3 MHD Simulation CTS Image PSF Deconvolved Shift from magnetopause location (degrees) Normalised profile.5.4 PSF deconvolubon using LIRA package hgps://github.com/astrostat/lira.3 MHD Simulation CTS Image PSF Deconvolved Shift from magnetopause location (degrees) 29th February, 216 IACHEC, ICUAA Pune, India 19

20 SMILE Orbit Simulator -> Deep coverage towards South EclipBc Pole Andy Read, University of Leicester 29th February, 216 IACHEC, ICUAA Pune, India 2

21 Bright X-ray sources SXI counts v on-bme, example orbit 1, 1, 29th February, 216 IACHEC, ICUAA Pune, India 21

22 Bright X-ray sources SXI counts v SXI on-bme 1, AB Dor ~3, cts 1E12 ~7,5 cts N132D ~6, cts 1, 29th February, 216 IACHEC, ICUAA Pune, India 22

23 Thankyou 29th February, 216 IACHEC, ICUAA Pune, India 23