Astro-H data analysis, processing and archive

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Astro-H data analysis, processing and archive

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Angelini, Lorella, et al. "Astro-H Data Analysis, Processing and

Archive." Proceedings Volume 9905, Space Telescopes and

Instrumentation 2016: Ultraviolet to Gamma Ray, 29 June - 1 July,

2016, Edinburgh, Scotland, edited by Jan-Willem A. den Herder et

al., SPIE, 2016, p. 990514. © 2016 SPIE

As Published

http://dx.doi.org/10.1117/12.2234429

Publisher

SPIE

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Final published version

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http://hdl.handle.net/1721.1/114869

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PROCEEDINGS OF SPIE

SPIEDigitalLibrary.org/conference-proceedings-of-spie

Astro-H data analysis, processing

and archive

Lorella Angelini, Yukitatsu Terada, Michael Loewenstein,

Eric D. Miller, Hiroya Yamaguchi, et al.

Lorella Angelini, Yukitatsu Terada, Michael Loewenstein, Eric D. Miller,

Hiroya Yamaguchi, Tahir Yaqoob, Hans Krimm, Ilana Harrus, Hiromitsu

Takahashi, Masayoshi Nobukawa, Makoto Sawada, Michael Witthoeft,

Kristin Rutkowski, Andrew Sargent, Robert S. Hill, Michael Dutka, Joseph

Eggen, "Astro-H data analysis, processing and archive," Proc. SPIE 9905,

Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray,

990514 (15 July 2016); doi: 10.1117/12.2234429

Event: SPIE Astronomical Telescopes + Instrumentation, 2016, Edinburgh,

United Kingdom

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Astro-H data analysis, processing and archive

Lorella Angelini*

a

, Yukikatsu Terada

b

, Michael Loewenstein

a,c

, Eric D. Miller

d

,

Hiroya Yamaguchi

a,c

, Tahir Yaqoob

a,e

, Hans Krimm

a,f

, Ilana Harrus

a,e

,

Hiromitsu Takahashi

g

, Masayoshi Nobukawa

h

, Makoto Sawada

i

, Michael Witthoeft

j

,

Kristin Rutkowski

j

, Andrew Sargent

k

, Robert S. Hill

j

, Michael Dutka

k

, Joseph Eggen

j a

_{Goddard Space Flight Center NASA , 8800 Greenbelt Road, Greenbelt MD 20771;}

b

_Saitama

University, 255 Shimookubo, Sakura, Saitama, Saitama Prefecture, 338-8570, Japan;

c

Department of

Astronomy, University of Maryland, College Park, MD 20742, USA;

d

_{MIT Kavli Institute for}

Astrophysics and Space Research Laboratory

77 Massachusetts Ave, Cambridge, MA 02139

;

e

_{Department of Physics, University of Maryland Baltimore County, Baltimore, MD 21250, USA;}

f

_{Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD 21044,}

USA;

g

Hiroshima University, 1-3-1, Kagamiyama, Higashi-Hiroshima, Hiroshima Prefecture,

739-8526, Japan ;

h

Nara University of Education, Takabatake-cho, Nara, Nara Prefecture, 630-8528,

Japan;

i

Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo-ku, Sagamihara,Kanagawa Prefecture,

252-5258, Japan;

j

ADNET Systems

6720 Rockledge Drive Suite 504 Bethesda, MD 20817, USA;

k

_{Wyle 7315 Mission Drive Lanham, MD 20706, USA.}

ABSTRACT

Astro-H (Hitomi) is an X-ray/Gamma-ray mission led by Japan with international participation, launched on February 17, 2016. The payload consists of four different instruments (SXS, SXI, HXI and SGD) that operate simultaneously to cover the energy range from 0.3 keV up to 600 keV. This paper presents the analysis software and the data processing pipeline created to calibrate and analyze the Hitomi science data along with the plan for the archive and user support. These activities have been a collaborative effort shared between scientists and software engineers working in several institutes in Japan and USA.

Keywords: Astro-H , Software , Calibration , Pipeline, Archive

1. INTRODUCTION

Astro-H 1_{, renamed Hitomi after launch, is a facility-class mission launched on a JAXA H-IIA rocket into low Earth} orbit on Feb 17, 2016 at 5:45 pm JPS from Tanegashima Space Center in Japan. Hitomi is Japan's sixth X-ray astronomy mission primarily developed at the Institute of Space and Astronautical Science of Japan Aerospace Exploration Agency (ISAS/JAXA) in collaboration with U.S. (NASA/GSFC) and Japanese institutions, with contributions from the European Space Agency (ESA), the Netherlands Institute for Space Research (SRON), the Canadian Space Agency (CSA) and US and European institutions. Hitomi is equipped with four different instruments that together cover a wide energy range 0.3-600 keV. The Soft X-ray Spectrometer (SXS 2_{), which pairs a lightweight} Soft X-ray Telescope 3_{with a X-ray Calorimeter Spectrometer, provides non-dispersive spectroscopy with < 7 eV} resolution in the 0.3-10 keV energy range with a field of view of about 3 arcmin. Three additional scientific instruments extend the energy bandpass of the observatory. The Soft X-ray Imager (SXI 4) expands the field of view with a new generation CCD camera in the energy range of 0.5-12 keV at the focus of the second lightweight Soft X-ray Telescope 3_; the Hard X-ray Imager (HXI 5.6_{, two units) performs sensitive imaging spectroscopy in the 5-80 keV band; the} non-imaging Soft Gamma-ray Detector (SGD 7_{, two units) extends Hitomi’s energy band to 600 keV. On March 27, 2016,} JAXA lost contact with the satellite, and on April 28 announced that they would cease the efforts to restore the mission operations. The Hitomi instruments collected about one month worth of data that are processed and archived.

The following sections describe the Hitomi data format, the software developed to calibrate and analyze the science data, how the data are processed on ground, the different levels of data created and how they are archived. The latest updates on software, calibration and archives are posted at http://heasarc.gsfc.nasa.gov/docs/hitomi/ .

*lorella.angelini-1@nasa.gov; phone 1 301 286-3607; fax 1 301 286 -0677

Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, edited by Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Proc. of SPIE Vol. 9905, 990514

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Instrument RAW /PIXEL coords (look -down)

ACT coords (look -down)

DET coords

(look-up)

FOC coords (look

-up) size pixel arc sec size pixel arc sec size pixel arc sec size pixel arc sec SXS 0:35 -- 1:8, 1:8 29.982 1:8, 1:8 29.982 1:2430 1:2430 1.768 SXI segment 0:639 0:319 1.768 -- -- -- -- -- --640 array -- -- -- -- 1:1810, 1.768 1:2430 1.768 1:1810 1:2430 HXI -1 1:128, 4.297 1:256, 4.297 1:256, 4.297 1:2430 1.768 1:128 1:256 1:256 1:2430 HXI -2 1:128, 4.297 1:256, 4.297 1:256, 4.297 1:2430 1.768 1:128 1:256 1:256 1:2430

data and HK with a three steps procedure. The 1st_{step derives the fine time resolution that is assigned internally by the} instruments either using support instrument dependent look-up tables or keywords in the header of the FITS file. The 2nd step derives, for a given L32TI, the corresponding time using the TIM table. The 3rd_{step adds a delay, when appropriate,} between the on-board computer and the instruments. For HK data the steps 1 and 3 are skipped because there is not need of fine time resolution. The times are stored in the column TIME which contains seconds since an epoch set to 2014-01-01 00:00:00 UTC. The epoch is written in the header of all FITS files as an MJD value in the keywords MJDREFI and MJDREFF. The time system is TT (Terrestrial Time) and the MJD value of the epoch in TT corresponds to MJD 56658.0007775925926 (TT).

3.2 Coordinates assignment

Hitomi has three instruments at the focal plane of the telescopes: the SXI, SXS (soft energy telescopes) and the HXI (high energy telescopes). The coordinates for these instruments are described by five different coordinate systems and their values are stored in the FITS columns named PIXEL/RAWn, ACTn, DETn, FOCn, where n is either X or Y, and the columns X/Y that represent the SKY system (see below). Since the SGDs are not imaging detectors, SGD files do not have any of the above columns for coordinates, however the XYZ position in the detector is provided for any reconstructed event. The transformation of coordinates for all instruments are defined in calibration files one for each instrument (teldef). The SXI, SXS and HXI coordinates are calculated by the task ‘coordevt’. The pixel and the FOV sizes in the different coordinate systems are listed in Table 1.

Table 1. List for each coordinate system and detector : the pixel size, the number of pixels and if the coordinate definition is look-up/down with respect to the detector

The RAW coordinates comprise the basic coordinate system. For the SXS, they correspond to the telemetered pixel number where the event landed. This value is stored in the 1-d column PIXEL and ranges from 0-35. For the SXI, the RAW coordinates correspond to the telemetered event location into a segment of the CCD. Each CCD has two segments. The RAWY ranges from 0 to 639 and RAWX from 0 to 319. For the HXI, the RAW coordinates are calculated after the event is reconstructed using the telemetered strip location.

The ACT coordinates are derived from the RAW coordinates. The SXS ACT coordinates represent a 2-d look-down linearized coordinate system starting from the values stored in the PIXEL column. The SXI ACT coordinates correspond to the pixel locations in one SXI CCD. They range from 1 to 640 in the X and Y dimensions. The SXI RAW-to-ACT conversion depends on the window mode and readout node. The HXI ACT coordinates are the RAW coordinate corrected using the CAMS time-dependent misalignments to remove the Extended Optical Bench (EOB) movements, where the HXIs are located, respect to the main satellite body.

The DET coordinates are derived from the ACT coordinates. The SXI DET coordinates combine all four CCDs into a single system, accounting for any misalignments among them. The ACT-to-DET conversion changes the configuration from the look-down to the look-up for all instruments.

The FOC system combines all of the HXI, SXI, and SXS individual DET coordinates into a common system, accounting for misalignments among them. Since the SXI has the largest field of view and smallest detector pixel size, the FOC coordinates for all sensors adopt the pixel scale and range for the SXI.

The X and Y coordinates (or SKY) are derived from the FOC using the satellite attitude and they differ from the FOC for the position angle or roll. The X and Y columns contain pixel number. The pixel number is associated to a position in the sky via the FITS WCS keywords. The SKY system recorded the WCS keywords is a tangent plane projection and oriented such that declination (δ) increases in the +Y direction and Right Ascension (α) increases in the –X direction. Figure 4 shows the in-flight sky images for the G21.5-0.9 source for each individual detector as well as the overlay of the HXIs andd SXS onto thee SXI frame.

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E

s sx Figure 4. image is the area d 3.3 Energy The HXI, SG linearized pu algorithms ap intermediate records the in Table 2. For ea The SXS tel grade. The PHA2 togeth ‘sxsgain’ cal temperature f the PI colum telemetered c video temper corrected 3x3 columns. In t For the HXI photon when may contribu deriving an e tasks determi event by com an event, ‘hx the occurrenc

Left : Each pan the calibration p discriminator on assignment GD, SXI, and ulse height (ch ppropriate for quantities are ntermediate va

ach of the instru

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lculates the SX for that correct mn. The SXI charge around rature part of t 3 array, ‘sxipi the last step, th

and SGD the t n interacting wi

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xievtid’ and ‘sg

ce.

nel shows the im pixel. Right: S . SXS spectra a hannel) where each instrumen e necessary bef alues in addition ument PI_CHAN ergy’ informati econdary medi lemetered PHA XS time-depen tion. Using the

telemetered ‘ the event. ‘sx the CCD elect ’ assigns the g he gain is appli telemetered pul

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are derived usi each channel h nt due to the d fore computing nal columns of N gives the PI ch Instrument SXI SXS HXI SGD ion is in the F ium grade are A for primary e ndent energy e results of ‘sxs energy’ is sto

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dividual detecto contour overlay

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annel range and

PI_CHAN 0-4095 0-32767 0-2047 0-2047 ITS column P first corrected events. The PI correction usi

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ored in the ‘P the PI column e charge trail,

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PHA for each p d by the task ‘ is calculated u ing a calibratio SXS gain file, PHAS’ column n by correcting and for the ch or each event a mputed pulse in signals detecte ignal for one in

a’ gain correct d’ tasks for the

ay with the dete tterns of signal event consideri

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y interaction w s for the SXI,

energy for each P

primary and se sxssecor’ and using ‘sxsgain’ on line and d ‘sxspha2pi’ ca n that contain g the values in harge transfer i and populates nvariant stored ed by the instru nteraction there ts the PHA of e HXI and SGD ector parts are ls. If an occurr ing the energie

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SXS , HXI a

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econdary even written in the and ‘sxspha2p derives the app alculates the va s the 3x3 pix n the 3x3 array inefficiency. U the GRADE a in the PI colum ument. Since a e are many sig

each individua D, respectively consistent with rence is consist es of the signal SXS I has ds to the ated with or. Many and SGD V. nt of any e column pi’ tasks. propriate alues for xel array y for the Using the and PHA mn. an X-ray gnals that al signal, y. These h a valid tent with ls within

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En

10 iergy (key)

Figure 5 show the best fit m RSP file for redistribution energy and c (QE), and a n and RMP bu matrix file ( transmission 4.1 SXI and There is a co to calculate t differs amon focal plane b the outputs o and, for the telescope eff injected into is an event f plane. c) Th calculated gr where no fea distribution o model or a s filtered throu down to the d Figure 5.

4.

ws the SXS, S model. In order r each instrum n matrix (also contains all the number of othe ut because of th RSP). For the . d SXS ARF an ommon frame w the ARF for th ng instruments, by event comin of the exposure SXI and SXS, fective area is the telescope a file containing he ray-tracing e rid with fine e atures are expe of the X-ray so spatial distribu ugh the source detector is acco

G21.5-09 spectr

TELESCO

SXI and HXIs H to model the d ment. The RM known as the e information er detector-rela he different de e SGD the on-nd HXI RSP g work to calcul he SXS and SX

, there are com ng from a fix po e calculation. ‘ , also calculate calculated by t aperture. The r the path of ea energy grid is c nergy samplin ected due to th ource: point so ution from an region selecti ounted at this s ra of the SXI (gr

OPE EFFEC

Hitomi spectra data the spectr MF, ARF and “line-spread fu about the effec ated efficiencie etector characte -axis RSP are

generator

ate the telescop XI, and RSP fo mmonalities ap osition in sky v ‘ahexpmap’ ca es the fractiona the ray-tracing run is made for ach photon thro

coarser than th ng in regions w he telescope or ource, extended image obtaine ion and propag stage. These ar

reen), SXS (blue

CTIVE ARE

a extracted from ral analysis pro d/or RSP are function,” or L ctive area (EA es. For the SXS

eristics for the provided in C

pe effective ar or the HXI. Al pplicable to the

varies with the alculates an his al exposure of g, code which i

r each off-axis ough the telesc he final energy where telescop the detector. d d source flat w ed by different gated down to re the filters for

e) , HXI1 (black)

EA AND RE

m a region cen ogram Xspec re calculated by LSF), while the A) due to the X

S and SXI ther HXI is only p CALDB and th rea.

‘

aharfgen lthough the sch e three instrum attitude movem stogram of tim f each detector is essentially a angle and a pr cope and the f grid of the AR e or detector e d) There are fo within a circle, t mission. Eve the detector. A r SXS and SXI

) and HXI2 (red

ESPONSE

ntered on the G equires an ARF software. Th e ARF is a mu X-ray telescope re are tools to c possible to calc he software co ’ is a script th

heme for creat ments. a) The l ments. This va me spent at diffe

r pixel for each a Monte Carlo re-calculated e final impact co RF, because it edges dominat our options to extended sour ents generated Any object enc I and baffle for

d) with the best fi

G21.5-0.9 toget F and a RMF f he RMF is a ultiplicative fun e, Quantum Ef calculate both t culate the net r orrects for the

hat calls differe ting response f landing positio ariation is accou erent off-axis p h off-axis bin. simulation of energy grid. Th oordinates on t utilizes optimi e and coarse s account for th rce described b by the ray-tra countered by th r the HXI.

fit model overlaid

ther with files or a spectral nction of fficiency the ARF response off-axis ent tasks functions on in the unted by positions b) The f photons he output the focal ized pre-sampling he spatial by a beta acing are he event d.

(10)

For the SXI and SXS the final ARF calculation also includes: the quantum efficiency that is position dependent for the SXI but not for the SXS, the contamination and the exposure information. For the HXI the code outputs an RSP because of the intrinsic detector characteristics that are also time-position dependent. The LSF and QE are different for each of the five layers present in a single HXI unit. The HXI is located in the EOB that moves with respect to the main satellite body where the telescopes are located. The EOB movements are tracked by the CAMS data. Therefore the net response matrix is a weighted combination of the five responses. The weights depends on the relative time-position dependent X-ray source counts, which in turn depends on the movements of the EOB with respect to the telescope and on the telescope effective area.

4.2 SXI and SXS RMF generator

The RMF for the SXS and SXI are calculated by the ‘sxsmkrmf’ and ‘sxirmf’ tasks, respectively. The SXS RMF depends on the grade distribution and the pixels selected to create the spectrum. ‘sxsmkrmf’ first calculates an histograms of grades for the pixels of interest and then calculates the RMF for each pixel and grade and averages the individual RMF according to the histogram. By default, the SXS RMF input and output grids result in an RMF with 32768 channels of width 0.5eV. The RMF for the SXI depends on the extraction region and ‘sxirmf’ uses the WMAP, a coarse-binned image of the extraction region with the spatial counts distribution, to determine the weight distribution for the LSF from different positions on the detector. By default, an RMF is generated with an input energy grid in the range 0.200 to 23.974 keV, and with 5900 output channels of width 2 eV up to ~12 keV and 500 channels up to ~24 keV.

5. SUMMARY

The Hitomi software package and calibration data are in distribution with the HEAsoft package and CALDB both available from HEASARC. The Hitomi data populate the public archive at the HEASARC and DARTS after one year propriety period that starts when the final data processing is completed. Updates on software, calibration and data availability are posted at http://heasarc.gsfc.nasa.gov/docs/hitomi/ .

REFERENCES

[1] Takahashi, T., Mitsuda K., Kelley, R.L., et al., “The Astro-H X-ray astronomy satellite”, Proc SPIE 9144, 994125 (2014)

[2] Mitsuda, K., et al. “Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H", Proc. SPIE 9144, 773211-773211-10 (2014)

[3] Soong, Y., et al. “ASTRO-H Soft X-ray telescope (SXT)", Proc. SPIE 9144 , 994128-914425-14 (2014) [4] Hayashida, K. , et al., “Soft x-ray imager (SXI) onboard ASTRO-H", Proc. SPIE 9144, (2014)

[5] Sato, G., et al., “The hard x-ray imager (HXI) for the ASTRO-H mission", Proc. SPIE 9144 , (2014) [6] Awaki , H., et al., “ASTRO-H Hard X-ray telescope (HXT) ', Proc. SPIE 9144 , (2014)

[7] Fukazawa, Y., et al., “Soft gamma-ray detector for the ASTRO-H Mission", Proc. SPIE 9144 , (2014) [8] Gallo, L., et al., `The Canadian ASTRO-H Metrology System", Proc. SPIE 9144, (2014)

[9] de Vries ,C. P., et al., “Calibration sources for the soft x-ray spectrometer instrument on ASTRO-H", Proc. SPIE 8443, (2012)