Optical instrument design of the high-energy x-ray probe (HEX-P)

Madsen, K. K.; Christensen, Finn Erland; Grefenstette, Brian W.; Harrison, Fiona A.; Hornschemeier, A. E.; Miyasaka, Hiromasa; Okajima, Takashi; Pike, Sean N.; Saha, Timo T.; Zhang, William W.; Pivovaroff, M. J.; Vogel, Julia K.; Descalle, Marie-Anne; Broadway, David M.; Gurgew, Danielle; Stern, Daniel; Ferreira, Desiree Della Monica; Windt, David L.

doi:10.1117/12.2314117

Cited by 33 publications

(29 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Although unlikely to be detectable with current X-ray telescopes (e.g. XMM, NuSTAR, or NICER), our preliminary estimation indicates that they may possibly be within the reach of future high-sensitivity missions such as eXTP (Zhang et al 2016), STROBE-X (Ray et al 2018), and Athena (Nandra et al 2013) for the ∼ 4 keV line and HEX-P (Madsen et al 2018) for the ∼ 28 keV line.…”

Section: X-ray Confirmation Of Candidatesmentioning

confidence: 74%

“…However, proposed next generation balloon or satellite missions could achieve line sensitivities of ∼ 10 −8 -10 −6 γ cm −2 s −1 (see a summary in e.g., Fryer et al 2019). These include balloon missions such as COSI (Kierans et al 2016) and GRAMS (Aramaki et al 2019), as well as several satellite missions, e.g., AMEGO (Moiseev & Team 2018), e-ASTROGAM (Tavani et al 2018), ETCC (Tanimori et al 2017), HEX-P (Madsen et al 2018), and LOX (Miller et al 2018).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Finding the Remnants of the Milky Way's Last Neutron Star Mergers

Banerjee

Metzger

et al. 2019

ApJ

View full text Add to dashboard Cite

The discovery of a binary neutron star merger (NSM) through both its gravitational wave and electromagnetic emission has revealed these events to be key sites of r-process nucleosynthesis. Here, we evaluate the prospects of finding the remnants of Galactic NSMs by detecting the gamma-ray decay lines from their radioactive r-process ejecta. We find that 126 Sn, which has several lines in the energy range 415-695 keV and resides close to the second r-process peak, is the most promising isotope, because of its half-life t 1/2 = 2.30(14) × 10 5 yr being comparable to the ages of recent NSMs. Using a Monte Carlo procedure, we predict that multiple remnants are detectable as individual sources by next-generation γ-ray telescopes which achieve sub-MeV line sensitivities of ∼ 10 −8 -10 −6 γ cm −2 s −1 . However, given the unknown locations of the remnants, the most promising search strategy is a systematic survey of the Galactic plane and bulge extending to high Galactic latitudes. Individual known supernova remnants which may be mis-classified NSM remnants could also be targeted, especially those located outside the Galactic plane. Detection of a moderate sample of Galactic NSM remnants would provide important clues to unresolved issues such as the production of actinides in NSMs, properties of merging NS binaries, and even help distinguish them from rare supernovae as current Galactic rprocess sources. We also investigate the diffuse flux from longer-lived nuclei (e.g. 182 Hf) that could in principle trace the Galactic spatial distribution of NSMs over longer timescales, but find that the detection of the diffuse flux appears challenging even with next-generation telescopes.

show abstract

Section: X-ray Confirmation Of Candidatesmentioning

confidence: 74%

Section: Introductionmentioning

confidence: 99%

Finding the Remnants of the Milky Way's Last Neutron Star Mergers

Banerjee

Metzger

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…To estimate the extent to which future missions can distinguish between the two main models proposed to explain the soft excess (i.e., warm corona or relativistic reflection), we utilize the fakeit task in XSPEC to generate simulated data of future missions by using Model B with the exact best-fit values, and use Model A to fit the fake data. We choose the Advanced Telescope for High-energy Astrophysics (Athena, Nandra et al 2013), the enhanced X-ray Timing and Polarimetry mission (eXTP, Zhang et al 2017), and the High-Energy X-ray Probe (HEX-P, Madsen et al 2018). The X-ray Integral Field Unit (X-IFU, Barret et al 2016) instrument on Athena has an effective energy range of 0.2-12 keV with 2.5 eV spectral resolution, satisfying our requirement to make a distinction.…”

Section: Simulations Of the Future Missionsmentioning

confidence: 99%

The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy

García

Walton

et al. 2021

ApJ

Self Cite

View full text Add to dashboard Cite

We present a detailed spectral analysis of the joint XMM-Newton and NuSTAR observations of the active galactic nuclei (AGNs) in the Seyfert 1.5 Galaxy ESO 362-G18. The broadband (0.3-79 keV) spectrum shows the presence of a power-law continuum with a soft excess below 2 keV, iron Kα emission (∼6.4 keV), and a Compton hump (peaking at ∼20 keV). We find that the soft excess can be modeled by two different possible scenarios: a warm (kT e ∼ 0.2 keV) and optically thick (τ ∼ 34) Comptonizing corona, or with a relativistically blurred reflection off a high-density ( [ ]>n log cm 18.3 e 3) inner disk. These two models cannot be easily distinguished solely from their fit statistics. However, the low temperature (kT e ∼ 20 keV) and the thick optical depth (τ ∼ 5) of the hot corona required by the warm corona scenario are uncommon for AGNs. We also fit a "hybrid" model, which includes both disk reflection and a warm corona. Unsurprisingly, as this is the most complex of the models considered, this provides the best fit, and more reasonable coronal parameters. In this case, the majority of the soft excess flux arises in the warm corona component. However, based on recent simulations of warm coronae, it is not clear whether such a structure can really exist at the low accretion rates relevant for ESO 362-G18 ( m 0.015). This may therefore argue in favor of a scenario in which the soft excess is instead dominated by the relativistic reflection. Based on this model, we find that the data would require a compact hot corona (h ∼ 3 R Horizon ) around a rapidly spinning (a å > 0.927) black hole.Unified Astronomy Thesaurus concepts: Supermassive black holes (1663); X-ray astronomy (1810); Seyfert galaxies (1447); High energy astrophysics (739); Active galactic nuclei (16); Astrophysical black holes (98); Spectroscopy (1558); X-ray active galactic nuclei (2035)

show abstract

“…This will enable more straightforward comparison between coronae of obscured and unobscured AGNs, their physical properties, and possibly scaling relations and evolution (e.g., Kammoun et al 2017;Lanzuisi et al 2019). More similar studies are expected in the future based on NuSTAR data, though higher-sensitivity and higher-energy coverage of the proposed missions HEX-P (Madsen et al 2018(Madsen et al , 2019 or FORCE (Nakazawa et al 2018) will be needed in order to reach large AGN samples and detailed coronal physics (Kamraj et al 2019 We have made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations.…”

mentioning

confidence: 92%

NuSTAR Survey of Obscured Swift/BAT-selected Active Galactic Nuclei. II. Median High-energy Cutoff in Seyfert II Hard X-Ray Spectra

Baloković

Harrison

Madejski

et al. 2020

ApJ

View full text Add to dashboard Cite

Broadband X-ray spectroscopy of the X-ray emission produced in the coronae of active galactic nuclei (AGNs) can provide important insights into the physical conditions very close to their central supermassive black holes. The temperature of the Comptonizing plasma that forms the corona is manifested through a high-energy cutoff that has been difficult to directly constrain even in the brightest AGN because it requires high-quality data at energies above 10 keV. In this paper we present a large collection of coronal cutoff constraints for obscured AGNs based on a sample of 130AGNs selected in the hard X-ray band with Swift/BAT and observed nearly simultaneously with NuSTAR and Swift/XRT. We find that under a reasonable set of assumptions regarding partial constraints the median cutoff is well constrained to 290±20 keV, where the uncertainty is statistical and given at the 68% confidence level. We investigate the sensitivity of this result to our assumptions and find that consideration of various known systematic uncertainties robustly places the median cutoff between 240 and 340 keV. The central 68% of the intrinsic cutoff distribution is found to be between about 140 and 500 keV, with estimated uncertainties of 20 and 100 keV, respectively. In comparison with the literature, we find no clear evidence that the cutoffs in obscured and unobscured AGNs are substantially different. Our analysis highlights the importance of carefully considering partial and potentially degenerate constraints on the coronal high-energy cutoff in AGNs.Unified Astronomy Thesaurus concepts: Active galactic nuclei (16); X-ray active galactic nuclei (2035); Seyfert galaxies (1447); High energy astrophysics (739); X-ray surveys (1824)

show abstract

Optical instrument design of the high-energy x-ray probe (HEX-P)

Cited by 33 publications

References 23 publications

Finding the Remnants of the Milky Way's Last Neutron Star Mergers

Finding the Remnants of the Milky Way's Last Neutron Star Mergers

The Nature of Soft Excess in ESO 362-G18 Revealed by XMM-Newton and NuSTAR Spectroscopy

NuSTAR Survey of Obscured Swift/BAT-selected Active Galactic Nuclei. II. Median High-energy Cutoff in Seyfert II Hard X-Ray Spectra

Contact Info

Product

Resources

About