X-ray CCD calibration for the AXAF CCD Imaging Spectrometer

Bautz, M. W.; Pivovaroff, M. J.; Baganoff, Frederick K.; Isobe, Takashi; Jones, Stephen E.; Kissel, S.; LaMarr, Beverly; Manning, Herbert L.; Prigozhin, G.; Ricker, G.; Nousek, J. A.; Grant, Catherine E.; Nishikida, Koichi; Scholze, Frank; Thornagel, R.; Ulm, G.

doi:10.1117/12.331238

Cited by 104 publications

(39 citation statements)

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“…The Chandra Advanced CCD Imaging Spectrometer Spectroscopic-array (ACIS-S, Garmire et al 1992;Bautz et al 1998 (2000-2006), 1.64 yr (2004-2006) and 7.90 yr (2006-2014). We reprocessed all the level-1 event data, applying all standard data reduction steps with CALDB version 4.7.2, using a custom pipeline based on "chandra_repro" in CIAO version 4.8.…”

Section: Observational Resultsmentioning

confidence: 99%

Freely Expanding Knots of X-Ray-emitting Ejecta in Kepler’s Supernova Remnant

Sato

Hughes

2017

ApJ

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We report measurements of proper motion, radial velocity, and elemental composition for 14 compact X-ray bright knots in Kepler's supernova remnant (SNR) using archival Chandra data. The highest speed knots show both large proper motions (µ ∼ 0.11-0.14 yr −1 ) and high radial velocities (v ∼ 8,700-10,020 km s −1 ). For these knots the estimated space velocities (9,100 km s −1 v 3D 10,400 km s −1 ) are similar to the typical Si velocity seen in SN Ia near maximum light. High speed ejecta knots appear only in specific locations and are morphologically and kinematically distinct from the rest of the ejecta. The proper motions of five knots extrapolate back over the age of Kepler's SNR to a consistent central position. This new kinematic center agrees well with previous determinations, but is less subject to systematic errors and denotes a location about which several prominent structures in the remnant display a high degree of symmetry. These five knots are expanding at close to the free expansion rate (expansion indices of 0.75 m 1.0), which we argue indicates either that they were formed in the explosion with a high density contrast (more than 100 times the ambient density) or that they have propagated through relatively low density (n H < 0.1 cm −3 ) regions in the ambient medium. X-ray spectral analysis shows that the undecelerated knots have high Si and S abundances, a lower Fe abundance and very low O abundance, pointing to an origin in the partial Si-burning zone, which occurs in the outer layer of the exploding white dwarf for SN Ia models. Other knots show slower speeds and expansion indices consistent with decelerated ejecta knots or features in the ambient medium overrun by the forward shock. Our new accurate location for the explosion site has well-defined positional uncertainties allowing for a great reduction in the area to be searched for faint surviving donor stars under non-traditional single-degenerate SN Ia scenarios; because of the lack of bright stars in the search area the traditional scenario remains ruled out.

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Section: Observational Resultsmentioning

confidence: 99%

Freely Expanding Knots of X-Ray-emitting Ejecta in Kepler’s Supernova Remnant

Sato

Hughes

2017

ApJ

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“…XJ1417+52 was in the FOV of seven Chandra observations (C1-C7 hereafter; refer to Table 1), all using the imaging array of the AXAF CCD Imaging Spectrometer (ACIS; Bautz et al 1998). C1-C5 were part of the Chandra survey of the EGS (Laird et al 2009), with C1-C3 taken between 2002 August 11-21 and C4-C5 taken on 2005 October 15.…”

Section: Chandra Observationmentioning

confidence: 99%

Discovery of the Candidate Off-Nuclear Ultrasoft Hyper-Luminous X-Ray Source 3xmm J141711.1+522541

Lin

Carrasco

Webb

et al. 2016

ApJ

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We report the discovery of an off-nuclear ultrasoft hyper-luminous X-ray source candidate 3XMMJ141711.1 +522541 in the inactive S0 galaxy SDSSJ141711.07+522540.8 (z=0.41827, d L =2.3 Gpc) in the Extended Groth Strip. It is located at a projected offset of ∼1 0 (5.2 kpc) from the nucleus of the galaxy and was serendipitously detected in five XMM-Newton observations in 2000 July. Two observations have enough counts and can be fitted with a standard thermal disk with an apparent inner disk temperaturekT 0.13 keV MCD and a 0.28-14.2 keV unabsorbed luminosity L X ∼4 × 10 43 erg s −1 in the source rest frame. The source was still detected in three Chandra observations in 2002 August, with similarly ultrasoft but fainter spectra (kT MCD ∼0.17 keV, L X ∼0.5×1043 erg s −1 ). It was not detected in later observations, including two by Chandra in 2005 October, one by XMM-Newton in 2014 January, and two by Chandra in 2014 September-October, implying a long-term flux variation factor of >14. Therefore the source could be a transient with an outburst in 2000-2002. It has a faint optical counterpart candidate, with apparent magnitudes of m F606W =26.3 AB mag and m F814W =25.5 AB mag in 2004 December (implying an absolute V-band magnitude of ∼−15.9 AB mag). We discuss various explanations for the source and find that it is best explained as a massive black hole (BH) embedded in the nucleus of a possibly stripped satellite galaxy, with the X-ray outburst due to tidal disruption of a surrounding star by the BH. The BH mass is ∼105 M e , assuming the peak X-ray luminosity at around the Eddington limit.

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“…The missions which have been represented in this work are the Chandra X-ray Observatory (Weisskopf et al 2000(Weisskopf et al , 2002, the X-ray Multimirror Mission (XMM-Newton, Jansen et al 2001), the ASTRO-E2 Observatory (Suzaku), and the Swift Gamma-ray Burst Mission (Gehrels et al 2004). Data from the following instruments have been included in this analysis: the High-Energy Transmission Grating (HETG, Canizares et al 2005) and the Advanced CCD Imaging Spectrometer (ACIS, Bautz et al 1998;Garmire et al 2003;Garmire et al 1992) on Chandra, the Reflection Gratings Spectrometers (RGS, den Herder et al 2001), the European Photon Imaging Camera (EPIC) Metal-Oxide Semiconductor (EPIC-MOS, Turner et al 2001) CCDs and the EPIC p-n junction (EPIC-pn, Strüder et al 2001) CCDs on XMM-Newton, the X-ray Imaging Spectrometer (XIS) on Suzaku, and the X-ray Telescope (XRT, Burrows et al 2005;Godet et al 2007) on Swift.…”

Section: Introductionmentioning

confidence: 99%

SNR 1E 0102.2-7219 as an X-ray calibration standard in the 0.5−1.0 keV bandpass and its application to the CCD instruments aboardChandra,Suzaku,SwiftandXMM-Newton

Plucinsky

Beardmore

Foster

et al. 2016

A&A

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Context. The flight calibration of the spectral response of charge-coupled device (CCD) instruments below 1.5 keV is difficult in general because of the lack of strong lines in the on-board calibration sources typically available. This calibration is also a function of time due to the effects of radiation damage on the CCDs and/or the accumulation of a contamination layer on the filters or CCDs. Aims. We desire a simple comparison of the absolute effective areas of the current generation of CCD instruments onboard the following observatories: Chandra ACIS-S3, XMM-Newton (EPIC-MOS and EPIC-pn), Suzaku XIS, and Swift XRT and a straightforward comparison of the time-dependent response of these instruments across their respective mission lifetimes. Methods. We have been using 1E 0102.2-7219, the brightest supernova remnant in the Small Magellanic Cloud, to evaluate and modify the response models of these instruments. 1E 0102.2-7219 has strong lines of O, Ne, and Mg below 1.5 keV and little or no Fe emission to complicate the spectrum. The spectrum of 1E 0102.2-7219 has been well-characterized using the RGS gratings instrument on XMM-Newton and the HETG gratings instrument on Chandra. As part of the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC), we have developed a standard spectral model for 1E 0102.2-7219 and fit this model to the spectra extracted from the CCD instruments. The model is empirical in that it includes Gaussians for the identified lines, an absorption component in the Galaxy, another absorption component in the SMC, and two thermal continuum components with different temperatures. In our fits, the model is highly constrained in that only the normalizations of the four brightest lines/line complexes (the O vii Heα triplet, O viii Lyα line, the Ne ix Heα triplet, and the Ne x Lyα line) and an overall normalization are allowed to vary, while all other components are fixed. We adopted this approach to provide a straightforward comparison of the measured line fluxes at these four energies. We have examined these measured line fluxes as a function of time for each instrument after applying the most recent calibrations that account for the time-dependent response of each instrument. Results. We performed our effective area comparison with representative, early mission data when the radiation damage and contamination layers were at a minimum, except for the XMM-Newton EPIC-pn instrument which is stable in time. We found that the measured fluxes of the O vii Heα r line, the O viii Lyα line, the Ne ix Heα r line, and the Ne x Lyα line generally agree to within ±10% for all instruments, with 38 of our 48 fitted normalizations within ±10% of the IACHEC model value. We then fit all available observations of 1E 0102.2-7219 for the CCD instruments close to the on-axis position to characterize the time dependence in the 0.5−1.0 keV band. We present the measured line normalizations as a function of time for each CCD instrument so that the users may estimate the un...

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X-ray CCD calibration for the AXAF CCD Imaging Spectrometer

Cited by 104 publications

References 1 publication

Freely Expanding Knots of X-Ray-emitting Ejecta in Kepler’s Supernova Remnant

Freely Expanding Knots of X-Ray-emitting Ejecta in Kepler’s Supernova Remnant

Discovery of the Candidate Off-Nuclear Ultrasoft Hyper-Luminous X-Ray Source 3xmm J141711.1+522541

SNR 1E 0102.2-7219 as an X-ray calibration standard in the 0.5−1.0 keV bandpass and its application to the CCD instruments aboardChandra,Suzaku,SwiftandXMM-Newton

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