HISAKI Level2 data basic with IDL. Ver. 1.2 updated HISAKI/EXCEED team

Transcription

1 HISAKI Level2 data basic with IDL Ver. 1.2 updated HISAKI/EXCEED team

2 Before using sample IDL codes 1. Installation of IDL (any version) 2. Sample IDL code and sample data 3. IDL library required in this doc 1. FITS I/O lib 2. SPICE lib (library and space kernel files)

3 1. Instruction of IDL Sample codes used in this doc are supported by any version of IDL IDL version 7.0 and later is recommended to use SPICE.

4 2. Sample IDL codes and sample data IDL sample code to read HISAKI level 2 data and HISAKI s sample data (Jupiter and Venus) are available from following web site IDL sample codes (2MB) Unzip idl_sample.zip and set IDL path to this directory The IDL path should be on upper level than IDL Default path (IDL_DEFAULT) Sample data (35MB) or (42MB) How to extract data_sample_v1_2.tgz $ tar zxvf data_sample_v1_2.tgz SPICE kernel used in this doc (735MB) In this doc, directories of the sample data and SPICE kernels are assumed to be C: HISAKI data euv l2 for sample Level 2 data C: HISAKI data euv cal for EUV Level 2 calibration table C: SPICE kernel for SPICE kernel files. Edit exc_set_env.pro according to directory structure in your computer pro exc_set_env defsysv, '!EXC_EUV_DIR', 'C: HISAKI data euv ' defsysv, '!EXC_SPICE_DIR', 'C: SPICE kernel ' dlm_register, 'C: SPICE icy lib icy.dlm' end

5 3. IDL library required in this doc(1) FITS I/O Download and unzip astron.zip and set IDL path to this directory. The IDL path should be on upper level than IDL Default path (IDL_DEFAULT) Coyote(IDL graphical library) Download and unzip coyote libs and set IDL path to these directories. The IDL path should be on upper level than IDL Default path (IDL_DEFAULT)

6 3. IDL library required in this doc(2) SPICE Download spice toolkit for IDL (icy.zip). Version of the toolkit depends on OS and IDL versions in your computer. For IDL older than 6.X, please refer the following URL. ftp://naif.jpl.nasa.gov/pub/naif/misc/ See toolkit_n00xx/idl/*/packages/readme to find IDL version Unzip icy.zip ex) C: SPICE icy Set IDL_DLM path Set the toolkit directory (C: SPICE icy) as a IDL_DLM path. e.g.) How to set IDL_DLM path from IDL command prompt IDL>dlm_register, ' C: SPICE icy lib icy.dlm'

7 3. IDL library required in this doc(3) How to confirm the SPICE toolkit installation IDL> help, 'icy', /dlm ** ICY IDL/CSPICE interface from JPL/NAIF (not loaded) Version: 1.6.0, Build Date: 03 MAY 2010, Source: Path: C: SPICE icy lib icy.dll How to get SPICE kernels The HISAKI spice kernels (not used in this doc) Generic kernels

8 HISAKI Level 2 data Basic with IDL 1. How to read and display L2 spectrograph image How to apply calibration table (x axis: pixel to Angstrom, y axis: pixel to arc sec) 2. How to accumulate 1 min L2 images during planet and sky observations separately. How to apply calibration table (z axis: counts/min/pixel to Rayleigh/Angstrom) 3. Set a region of interest (ROI) on the image and get average brightness in ROI. 4. Hot to calculate planet ephemeris with SPICE: Io orbital phase and CML

9 Two main targets of EXCEED Simultaneous observation of exosphere, ionosphere, and escaping plasma down the tail (Venus, Mars, and Mercury) charge exchange (solar wind) O + 83nm resonant scattering (ionosphere) slit H 121nm resonant scattering O 130nm resonant scattering (exospheric neutral particle) O + 83nm resonant scattering (escaping plasma) Aurora and gas torus (Jupiter and Saturn) Mass and energy flows in the rotating magnetosphere Allowed transition lines of S,O ions (satellite origin) FUV/EUV aurora H 2 Lyman & Werner bands Io plasma torus : Cassini/UVIS Jupiter s UV aurora : HST/WFPC2 slit

10 Schematics of a spectrograph image Emission lines From Io plasma torus Continuum/band emission Solar reflection on Jupiter & aurora Io plasma torus Slit (140 ) N S Dawn Jupiter Dusk Long Wave length Spectrograph image Short

11 Structure of HISAKI L2 data A_data_format_definition_v1.0.pdf EUV L2 EUV L2 data is 2D (wavelength space) spectral data obtained during a fixed (1 minute) exposure time. The only primary data is the data header, which comprises several basic items such as the presence of any extensions. The Total extension provides QL data, integrating all photons for one day. Each YYYY MM DDThh:mm:ss extension corresponds to a single spectral image obtained during the period from the time given in the extension name and the end of the fixed exposure time(1 min). The image size is 32 bit x 1024 pixels x 1024 pixels. Each data file comprises the set of image data for 1 day of observations, and each item of image data in each extension is 4.2 MB in size. 1 day of observations produces approximately 3 GB of data.

12 1. How to read and display L2 image Set directory (EUV L2 data and spice kernels) IDL> exc_set_env Level 2 fits file during Jupiter observation on Jan IDL> file=!exc_euv_dir + 'l2 exeuv.jupiter.mod lv.02.vr.00.fits' Read primary header (exten_no=0) and find total extension number in the file. IDL> fits_read,file,data,header,exten_no=0 IDL> print, fxpar(header,'nextend') Read a image in the first extension (data: image of 1 day accumulation) IDL>fits_read,file,data,header,exten_no=1 Show the image IDL> xarr=findgen(1024) IDL> yarr=findgen(1024) IDL> exc_img_plot,xarr,yarr,data, xtitle='x [pixel]', ytitle='y [pixel]', ztitle='[count/pixel] ' IDL> exc_img_plot,xarr,yarr,data, xtitle='x [pixel]', ytitle='y [pixel]', ztitle='[count/pixel]',yrange=[500,650],zrange=[0,100] Result1

13 Result1 Geo corona/ Inter stellar OI1304 HI Ly (121.6nm) HI Ly (102.5nm) OII834 HeI 584 Io plasma torus (SII,SIII,SIV,OII,OIII) Aurora X axis: wavelength, Y axis: distance along slit Jupiter/Io plasma torus

14 Continue Read calibration table IDL> cal=!exc_euv_dir +'cal calib_v1.0.fits' IDL> fits_read,cal,cal_x,header,exten_no=1 IDL> fits_read,cal,cal_y,header,exten_no=2 IDL> fits_read,cal,cal_z,header,exten_no=3 Apply the calibration table (x and y axes) IDL> exc_img_plot,cal_x[*,512],cal_y[512,*], data, xtitle='[angstrom]', ytitle='[arcsec]', ztitle='[count/pixel]' IDL> exc_img_plot,cal_x[*,512],cal_y[512,*], data, xtitle='[angstrom]', ytitle='[arcsec]', ztitle='[count/pixel]', yrange=[ 200,200], xrange=[1350,1150], zrange=[0,100] Result2 For Venus observation on Mar IDL> file=!exc_euv_dir + 'l2 exeuv.venus.mod lv.02.vr.00.fits' Result1

15 Result2 Jupiter/Io plasma torus

16 Result1 Geo corona/ Inter stellar OI1304 HI Ly (121.6nm) HI Ly (102.5nm) OII834 HeI 584 Venus Venus

17 2. exc_sample1 How to accumulate 1 min L2 images during planet and sky observations separately IDL> file=!exc_euv_dir +'l2 exeuv.jupiter.mod lv.02.vr.00.fits' IDL> exc_sample1,file=file,im_pla=im_pla,im_sky=im_sky IDL> cal=!exc_euv_dir + 'cal calib_v1.0.fits' IDL> fits_read,cal,cal_x,header,exten_no=1 IDL> fits_read,cal,cal_y,header,exten_no=2 IDL> fits_read,cal,cal_z,header,exten_no=3 IDL> zarr=im_pla*cal_z IDL> zarr_sky=im_sky*cal_z IDL> exc_img_plot,cal_x[*,512],cal_y[512,*],zarr, Applying the calibration table im_pla: Averaged spectrograph image during Jupiter observation on Jan. 1, 2014 (unit: counts/min) im_sky: Averaged spectrograph image during sky observation on Jan. 1, 2014 (unit: counts/min) (5 arcmin northward of Jupiter) xtitle='[angstrom]', ytitle='[arcsec]', ztitle='[rayleigh/angstrom]', xrange=[1450,550], yrange=[ 200,200], zrange=[0,100] IDL> exc_img_plot,cal_x[*,512],cal_y[512,*],zarr_sky, xtitle='[angstrom]', ytitle='[arcsec]', ztitle='[rayleigh/angstrom]', xrange=[1450,550], yrange=[ 200,200], zrange=[0,100] Result3 Result4

18 Jupiter (+Sky) Result3 Spectrum profile (next slide) Result4 Off Jupiter (Sky)? Sky = foreground geocoronal emission (H, O, O+) and interstellar emission (H, He)

19 Continue Spectrum of Io plasma torus (at y=140[arcsec]) IDL> ret = min(abs(cal_y[512,*] 140.0), i_trg) IDL> plot,cal_x[*,i_trg],zarr[*,i_trg] IDL> plot,cal_x[*,i_trg],zarr[*,i_trg], yrange=[ 5,100], xtitle='wavelength[a]', ytitle='[rayleigh/angstrom]', xstyle=1, ystyle=1, /nodata IDL> oplot,cal_x[*,i_trg],zarr[*,i_trg], color=cgcolor('red') IDL> oplot,cal_x[*,i_trg],zarr_sky[*,i_trg], color=cgcolor('blue') Result5 Result5 Red: Io plasma torus Blue: SKY Sample code to show Result 3 5: x_exc_sample1.pro

20 Continue Spectrum from Venus on Mar. 10, 2014 at y= 100[arcsec] Result5 Red: Venus Blue: SKY Sample code to show Result 3 5 : x_exc_sample1_v.pro

21 Result3 Venus (+Sky) Averaged spectrum (previous slide) Result4 Off Venus (Sky)

22 3. exc_sample2 Set a region of interest (ROI) on the image and get time variation in average brightness in ROI. IDL> file=!exc_euv_dir +'l2 exeuv.jupiter.mod lv.02.vr.00.fits' IDL> cal=!exc_euv_dir +'cal calib_v1.0.fits' Set ROI for OI1304(emission of oxygen atoms at 130.4nm, primary geo corona) and ROI for HI1216 (emission of hydrogen atoms, geo corona) ex) ROI for OI1304: from to 129.9nm, from 100 to 150arcsec IDL> roi= [[1309.,1299., 100., 150.], [1221.,1211., 100., 150.]] Get time series of total counts in ROIs IDL> exc_sample2, l2_file=file, cal_file=cal, roi=roi, count=count, jd=jd, ltesc=ltesc Plot the time series IDL> plot, jd,count[*,0],xtitle='julius day', ytitle='oi1304', psym=1 IDL> plot, ltesc, count[*,0],xtitle='lt', ytitle='oi1304', psym=1 IDL> plot, ltesc, count[*,1],xtitle='lt', ytitle= HI1216', psym=1 count: total count in ROIs jd: Julius day ltesc: local time of HISAKI Result6 Result7

23 Result6 Geo corona OI1304 vs. Julius day(24 hours) Result7 Geo corona OI1304 vs. HISAKI local time

24 exc_sample2(continue) Example to get time variation in several emissions with exc_sample2 (dt=1min) (See next page to find position of ROIs on a spectrograph image) Three geo corona lines (OI,HI,HeI) Jupiter s aurora (integrated intensity from 105nm to 145nm) Io plasma torus (integrated intensities; 65 78nm and nm) Contamination from radiation belt (60 110nm, arcsec=outside of FOV) Flags from attitude control system (calibration flag, sub mode, and sub mode status) IDL> x_exc_sample2 Result8 CALFLG=ena(1) and SUBMST=2 mean the sky mode. Very low counts from Io plasma torus and Jupiter s aurora during this mode (Counts during this mode come from high energy charged particle contamination and MCP noise). (See 1 st and 2 nd panels) Near the South Atlantic Anomaly(SAA), contamination from high energy charged particle is not negligible. One should not use L2 data here (4 th panel). The aurora could be contaminated by geo corona emission. Be careful if you set the aurora ROI near the HI Ly alpha (2 nd panel, after UT20). Data Just after MCP s high voltage (HV) on and just before the HV off has low count rate. These should be removed (2 nd panel).

25 ROIs used in x_exc_sample2.pro (9) (3) (0) (1) (8) (4) (6) (2) (7) (5) roi=[ [1309.,1299., 100., 150.], $ ; (0) OI1304 [1221.,1211., 100., 150.], $ ; (1) HI1216 [ 589., 579., 100., 150.], $ ; (2) HeI584 [1450.,1250., 10., 40.], $ ; (3) Aurora1 [1200.,1050., 10., 40.], $ ; (4) Aurora2 [ 780., 650., 180., 50.], $ ; (5) Io plasma torus dawn (65 to 78nm) [ 780., 650., 50., 180.], $ ; (6) Io plasma torus dusk (65 to 78nm) [1150.,1050., 180., 50.], $ ; (7) Io plasma torus dawn (105 to 115nm) [1150.,1050., 50., 180.], $ ; (8) Io plasma torus dusk (105 to 115nm) [1100., 600., 300., 500.] ] ; (9) Radiation belt contamination

26 Result8 Blue : IPT short wavelength Red: IPT long wavelength Jupiter UV aurora Geocorona Red: HI1216 Yellow:HeI584 Blue:OI1304 Radiation belt contamination Attitude flags Red: Sub mode Yellow: Sub mode status Blue:Cal flag HISAKI Local time

27 4. exc_sample3 Find CML and Io phase angle with SPICE Reference frame:iau_jupiter Origin: Earth Target: Jupiter and Io Io Phase angle Y IAU_JUP CML Find a Earth to Jupiter vector (IAU_JUPITER) CML= tan 1 ( y/ x) Io phase angle Find a Earth to Jupiter vector Find a Jupiter to Io vector Project both vector on Jupiter s equatorial plane. Io phase angle = angular distance between two vectors projected Jupiter CML X IAU_JUP Earth

28 (Continue) Find CML and Io phase angle with SPICE load LSK file IDL> cspice_furnsh,!exc_spice_dir +'lsk naif0010.tls' load SPK files IDL> cspice_furnsh,!exc_spice_dir + 'spk de430.bsp' IDL> cspice_furnsh,!exc_spice_dir + 'spk jup309.bsp' Load text PCK file IDL> cspice_furnsh,!exc_spice_dir + 'pck pck00010.txt' Get CML and Io phase angle on T00:00:00 IDL> exc_get_io_param, utc_str=' T00:00:00', pa=pa, lon=lon, dist=dist, ar=ar IDL> print, pa, lon, dist, ar e pa=io phase angle[deg] lon:cml[deg] dist: distance from Earth and Jupiter[km] ar:angular radius of Jupiter seen from Earth[argsec]

29 (Continue) Sample code to show time variation in the plasma torus (dawn and dusk sides separately) Read L2 data from Jan. 1 to Jan. 3 in 2015, and get time variations in Io plasma torus at dawn and dusk sides separately (dt=1min). Data during the sky mode and high radiation contamination (contamination is greater than 0.003count/pixel/min) are removed. Data Just after HV on and just before HV off are removed. IDL> x_exc_sample3 Result9 Result10 Result9 Dependences of Io plasma torus brightness in dawn(blue) and dusk(red) sides on Io phase angle.

30 Result10 Brightness (total count in ROIs for 1 min) of Io plasma torus (blue : dawn, red: dusk)(65 78nm). Io phase angle (Io s orbital period = 42h) Radiation belt contamination CAL flag

31 Some notes 1. Observation mode and slit selection 2. Satellite y axis reversal 3. Cal flag, submode, and submode status

32 1. Observation mode and slit selection (Jupiter) ~360 Mode 1 (10 slit) Plasma torus Highest spectral resolution exeuv.jupiter.mod.01.yyyymmdd.lv.02.vr.00.fits Mode 3 (140 slit) Nominal observation mode for Jupiter Plasma torus & northern aurora exeuv.jupiter.mod.03.yyyymmdd.lv.02.vr.00.fits ~ Mode 4 (140 slit) Plasma torus & southern aurora exeuv.jupiter.mod.04.yyyymmdd.lv.02.vr.00.fits ~360

33 2. Satellite y axis reversal Dawn Before opposition +X=dawn +Y=north X Dusk Jupiter Z Y Earth After opposition +X=dusk +Y=south Y Dawn Z X Dusk The satellite operation team rotates the satellite attitude 180deg about z axis around opposition of planet. This causes reversal of dawn dusk and north south direction of spectrograph image. This also cases wavelength of emission lines from Io plasma torus (in the case of Jupiter s 140 slit observation). Sun From To Y axis Obs mode Y dusk Y North 1& South 3 X north X north North South North 1& South 1&3 dusk North 1,3& South 3

34 3. Cal flag(calflg), submode status(submst) Observation of Jupiter Io plasma torus Slit (140 ) Observation of background and foreground emissions (geocorona and interstellar matter) Slit (140 ) Jupiter 5 Jupiter CALFLG SUBMST CALFLG SUBMST CALFLG and SUBMST are found in a header of each fits extension.