<i>Chandra</i>X-ray spectroscopy of focused wind in the Cygnus X-1 system

Miškovičová, Ivica; Hell, N.; Hanke, Manfred; Nowak, Bernadeta; Pottschmidt, K.; Schulz, Norbert S.; Grinberg, V.; Duro, Refiz; Madej, Oliwia; Lohfink, A.; Rodríguez, J.; Bel, M. Cadolle; Bodaghee, A.; Tomsick, John A.; Lee, J.C.; Brown, G. V.; Wilms, J.

doi:10.1051/0004-6361/201322490

Cited by 43 publications

(49 citation statements)

References 78 publications

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“…The variation among the inner-shell transition energies calculated with various codes is ∼2-5 eV, i.e., on the order of several 100 -km s 1 for the diagnostically important L-shell silicon Kα lines. This variation is comparable to the expected Doppler shift of the L-shell silicon Kα lines (Miller et al 2005(Miller et al , 2012Watanabe et al 2006;Liedahl & Brown 2008;Miškovičová et al 2016), and significantly larger than the systematic wavelength error of Chandraʼs High Energy Transition Grating spectrometer (HETG), which is on the order of -100 km s 1 (Marshall et al 2004;Canizares et al 2005;Chandra X-ray Center 2015). Hence, the main systematic uncertainty in the determination of Doppler shifts from X-ray lines is our knowledge of atomic physics.…”

Section: Introductionmentioning

confidence: 65%

“…The results have been compared to our own FAC calculations and earlier calculations of Palmeri et al (2008), Behar & Netzer (2002), and House (1969). The newly available data (Table 3) can directly be applied to resolve astrophysical problems such as, e.g., wind diagnostics in high-mass X-ray binary systems like Vela X-1 (Liedahl & Brown 2008) and Cyg X-1 (Miškovičová et al 2016). The 90% confidence limits of 0.5 eV on the measured line centers presented here correspond to Doppler shifts of less than 90 -km s 1 .…”

Section: Discussionmentioning

confidence: 99%

“…Prominent absorption and emission X-ray features from highly charged silicon and sulfur ions have been detected and measured in a medley of celestial sources, including solar flares (Neupert 1971), other stellar coronae (e.g., Kastner et al 2002;Huenemoerder et al 2013), various types of active galactic nuclei (e.g., Lee et al 2001;Kaspi et al 2002;Kinkhabwala et al 2002;Holczer et al 2007;Holczer & Behar 2012;Reeves et al 2013), and high-mass X-ray binaries (HMXBs; e.g., Sako et al 2002;Boroson et al 2003;Watanabe et al 2006;Chang & Cui 2007;Hanke et al 2008;Miškovičová et al 2016). HMXBs, although well studied and cataloged, are not yet fully understood.…”

Section: Introductionmentioning

confidence: 99%

“…Watanabe et al (2006) build a three-dimensional Monte-Carlo radiative transfer model and report a mass loss rate for the companion star and the structure of the wind, although they do not analyze the line emission from the L-shell silicon ions, but only from H-like Si. In the case of Cygnus X-1, the Kα absorption features in L-and K-shell ions of silicon and sulfur have been measured and used to diagnose the nature of the stellar wind (Hanke et al 2008;Hell et al 2013;Miškovičová et al 2016). Specifically, these features have been shown to be produced by "clumps" of onion-structured material, where the inner layers are colder, denser, and less ionized, moving in and out of the observational line of sight.…”

Section: Introductionmentioning

confidence: 99%

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Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

Hell

Brown

Wilms

et al. 2016

ApJ

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We have measured the energies of the strongest 1s-2 ( ) = ℓ ℓ s, p transitions in He-through Ne-like silicon and sulfur ions to an accuracy of <1 eV using the Lawrence Livermore National Laboratory's electron beam ion traps, EBIT-I and SuperEBIT, and the NASA/GSFC EBIT Calorimeter Spectrometer (ECS). We identify and measure the energies of 18 and 21 X-ray features from silicon and sulfur, respectively. The results are compared to new Flexible Atomic Code calculations and to semi-relativistic Hartree-Fock calculations by Palmeri et al. (2008). These results will be especially useful for wind diagnostics in high-mass X-ray binaries, such as Vela X-1 and Cygnus X-1, where high-resolution spectral measurements using Chandraʼs high-energy transmission grating has made it possible to measure Doppler shifts of -100 km s 1 . The accuracy of our measurements is consistent with that needed to analyze Chandra observations, exceeding Chandraʼs -100 km s 1 limit. Hence, the results presented here not only provide benchmarks for theory, but also accurate rest energies that can be used to determine the bulk motion of material in astrophysical sources. We show the usefulness of our results by applying them to redetermine Doppler shifts from Chandra observations of Vela X-1.

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Section: Introductionmentioning

confidence: 65%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

Hell

Brown

Wilms

et al. 2016

ApJ

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“…L-shell ions of S have been observed in the spectra of astrophysical objects such as the stellar coronae of Capella (Audard et al 2001) and Procyon (Raassen et al 2002; Li et al 2013), AGNs MCG-6–30–15 (Lee et al 2001), IRAS 13349+2438 (Holczer et al 2007) and NGC 3783 (Kaspi et al 2007), the high-mass X-ray binaries 4U1700–37 (Boroson et al 2003), Vela X-1 (Watanabe et al 2006), and Cygnus X-1 (Chang & Cui 2007). L- and K-shell ions of S and Si have been used to establish the nature of stellar wind in Cygnus X-1 (Hell et al 2013; Miškoviˇová et al 2016). The lines of S ions are also valuable tools for analysis of observational data (Keenan et al 2000, 2002, 2004; Lepson et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Relativistic MR-MP Energy Levels for L-shell Ions of Sulfur and Argon

Santana

Lopez-Dauphin

Butler

et al. 2018

ApJS

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Calculated level energies for valence and K-vacancy states are provided for the ion series S VII - S XIV and Ar IX - Ar XVI. The calculations were performed with the relativistic Multi-Reference Mxller-Plesset Perturbation Theory method (MR-MP). The data set includes all the level energies with configurations 1s22(s, p)q, 1s22(s, p)q−1nl, 1s12(s, p)q+1, 1s12(s, p)qnl, 2(s, p)q+2 and 2(s, p)q+1nl, where 1 ≤ q ≤ 8, n ≤ 5 and l ≤ 3. We have compared our results with data from the National Institute of Standards and Technology (NIST) on-line database and with previous calculations. The average deviation of valence level energies ranges from 0.16 eV in Ne-like ions to 0.01 eV in Li-like ions, showing that the present MR-MP valence level energies are highly accurate. In the case of K-vacancy states, the deviation is generally below 0.3 eV for Li-like S XIV and Ar XVI. The deviation for K-vacancy energies in other L-shell ions (Be-, B-, C-, N- and O-like Ar ions) is higher but likely because the NIST-recommended values have a higher uncertainty. The data set includes many n = 4 and n = 5 valence and K-vacancy levels in L-shell ions of S and Ar not previously reported. The data can be used for line identification and modeling of L-shell ions of S and Ar in astrophysical and laboratory-generated plasmas, and as energy references in the absence of more accurate laboratory measurements.

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Leveraging high‐resolution spectra to understand black hole spectra

Nowak

2017

Astron Nachr

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For the past 17 years, both XMM-Newton and Chandra have brought the powerful combination of high spatial and spectral resolution to the study of black hole systems. Each of these attributes requires special consideration-in comparison to lower spatial resolution charge-coupled device (CCD)-quality spectra-when modeling observations obtained by these spacecraft. A good understanding of the high-resolution spectra is in fact required to model properly lower resolution CCD spectra, with the reflection grating spectrometer (RGS) instrument on XMM-Newton maintaining the highest "figure of merit" at soft X-ray energies for all missions flying or currently planned for the next decade. Thanks to its even higher spectral resolution, the use of Chandra high-energy transmission gratings (HETGs), albeit with longer integration times, allows for one to bring further clarity to RGS studies. A further promising route for continued studies is the combination of high spectral resolution at soft X-rays, via RGS and/or HETG, with contemporaneous broadband coverage extending to hard X-rays (e.g., NuSTAR or INTEGRAL spectra). Such studies offer special promise for answering fundamental questions about accretion in black hole systems; however, they have received only moderate consideration to date. This may be due in part to the difficulty of analyzing high-resolution spectra. In response, we must continue to develop software tools that make the analysis of high-resolution X-ray spectra more accessible to the wider astrophysics community.

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ChandraX-ray spectroscopy of focused wind in the Cygnus X-1 system

Cited by 43 publications

References 78 publications

Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

Laboratory Measurements of the K-Shell Transition Energies in L-Shell Ions of Si and S

Relativistic MR-MP Energy Levels for L-shell Ions of Sulfur and Argon

Leveraging high‐resolution spectra to understand black hole spectra

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