X-ray and radio studies of SNR CTB 37B hosting the magnetar CXOU J171405.7−381031

ABSTRACT We present a Chandra and XMM–Newton study of the supernova remnant (SNR) CTB 37B, along with archival radio observations. In radio wavelengths, the SNR CTB 37B is an incomplete shell showing bright emission from the eastern side, while the X-ray morphology shows diffuse emission from regions surrounding the magnetar CXOU J171405.7–381031. We used archival H i absorption measurements to constrain the distance to the remnant and obtain D = 9.8 ± 1.5 kpc. The X-ray spectrum of the remnant is described by a thermal model in the 1–5 keV energy range, with a temperature of kT = 1.3 ± 0.1 keV. The abundances from the spectral fits are consistent with being solar or sub-solar. A small region of diffuse emission is seen to the southern side of the remnant, best fitted by a non-thermal spectrum with an unusually hard photon index of Γ = 1.3 ± 0.3. Assuming a distance of 9.8 kpc to the SNR, we infer a shock velocity of Vs = 915 ± 70 km s−1 and an explosion energy of E = (1.8 ± 0.6) × 1050 erg. The overall imaging and spectral properties of CTB 37B favour the interpretation of a young SNR (≲6200 yr old), propagating in a low-density medium under the assumption of a Sedov evolutionary phase.

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XMM-Newton Observation of SNR RX J1713.7–3946

Symposium - International Astronomical Union ◽

10.1017/s0074180900180623 ◽

2004 ◽

Vol 218 ◽

pp. 73-76 ◽

Cited By ~ 3

Author(s):

G. Cassam-Chenaï ◽

A. Decourchelle ◽

J. Ballet ◽

J.-L. Sauvageot ◽

G. Dubner

Keyword(s):

Column Density ◽

Supernova Remnant ◽

Synchrotron Emission ◽

Spectral Parameters ◽

X Ray ◽

First Results ◽

Photon Index

We present the first results of the observations of the supernova remnant RX J1713.7–3946 (also known as G347.3–0.5) obtained with the EPIC instrument on board the XMM-Newton satellite. We show a 5-pointings mosaiced image of the X-ray synchrotron emission. We characterize this emission by mapping its spectral parameters (absorbing column density NH and photon index γ). The synchrotron spectrum is flat at the shock and steep in the interior of the remnant. NH is well correlated with the X-ray brightness. A strong NH is found in the southwest rim of RX J1713.7–3946. We suggest that the SNR is interacting with a HI region there.

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XMM-Newton spectrum of the magnetar CXOU J171405.7–381031

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/psz066 ◽

2019 ◽

Vol 71 (4) ◽

Cited By ~ 1

Author(s):

Haruka Watanabe ◽

Aya Bamba ◽

Shinpei Shibata ◽

Eri Watanabe

Keyword(s):

Power Law ◽

Time Variation ◽

Supernova Remnant ◽

Component Model ◽

Time Variability ◽

Spectral Parameters ◽

X Ray ◽

Two Component ◽

Photon Index ◽

Higher Temperature

Abstract We observe the magnetar CXOU J171405.7−381031 with XMM-Newton and obtain the most reliable X-ray spectral parameters for this magnetar. After removing the flux from the surrounding supernova remnant CTB 37B, the radiation of CXOU J171405.7−381031 is best described by a two-component model, consisting of a blackbody and power law. We obtain a blackbody temperature of $0.58^{+0.03}_{-0.03}$ keV, a photon index of $2.15^{+0.62}_{-0.68}$, and an unabsorbed 2–10 keV band flux of $2.33^{+0.02}_{-0.02} \times 10^{-12}$ erg cm−2 s−1. These new parameters enable us to compare CXOU J171405.7−381031 with other magnetars, and it is found that the luminosity, temperature, and photon index of CXOU J171405.7−381031 are aligned with the known trend among the magnetar population with a slightly higher temperature, which could be caused by its young age. All magnetars with a spin-down age of less than 1000 yr show time variation or bursts except for CXOU J171405.7−381031. We explore the time variability for six observations between 2006 and 2015, but there is no variation larger than ∼10%.

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X-ray Emission from G359.1-0.5

International Astronomical Union Colloquium ◽

10.1017/s0252921100071359 ◽

1997 ◽

Vol 166 ◽

pp. 417-420

Author(s):

Roland Egger ◽

Xuejun Sun

Keyword(s):

Thermal Plasma ◽

Large Distance ◽

Supernova Remnant ◽

Radio Observation ◽

Plasma Model ◽

Diffuse Emission ◽

X Ray ◽

Pointed Observation

AbstractWe report on the detection of X-ray emission from the supernova remnant (SNR) G359.1-0.5 in a deep ROSAT PSPC pointed observation. The diffuse emission is well confined within the radio shell of the SNR. Its spectrum can be represented by a thermal plasma model at T ~ 1 keV and Fx ~ 2×10−11 erg cm−2 s−1 (0.1–2.0 keV) modified by the column absorption of NH ~ 3 × 1022 cm−2. This result supports the view that the source is at a large distance consistent with that from radio observation, and helps to resolve a puzzle about the SNR in previous observations.

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Progressive steepening of the SNR RX J1713.7–3946 X-ray spectrum from XMM–Newton to INTEGRAL

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2261 ◽

2019 ◽

Vol 489 (2) ◽

pp. 1828-1836 ◽

Cited By ~ 1

Author(s):

Ekaterina Kuznetsova ◽

Roman Krivonos ◽

Eugene Churazov ◽

Natalia Lyskova ◽

Alexander Lutovinov

Keyword(s):

Energy Range ◽

Supernova Remnant ◽

X Rays ◽

X Ray ◽

North West ◽

South West ◽

Photon Index ◽

Coded Mask ◽

First Time ◽

Single Emission

ABSTRACT In this work, we present the first detailed analysis of the supernova remnant RX J1713.7–3946 in the hard X-ray energy range with the Imager on Board the INTEGRAL Satellite (IBIS) coded-mask telescope onboard the INTEGRAL observatory. The shell-type morphology of the entire remnant is mapped in hard X-rays for the first time and significantly detected up to 50 keV. The IBIS sky image of RX J1713.7–3946, accumulated over 14 yr of operations, demonstrates two extended hard X-ray sources. These sources are spatially consistent with north-west and south-west rims of RX J1713.7–3946 and are also clearly visible at energies below 10 keV with XMM–Newton. This points to a single emission mechanism operating in soft and hard X-rays. The INTEGRAL 17–120 keV spectrum of RX J1713.7–3946 is characterized by a power-law continuum with the photon index of Γ ≈ 3 that is significantly softer than Γ ≈ 2 determined by XMM–Newton in the 1–10 keV energy range, suggesting a progressive steepening of the spectrum with the energy.

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An XMM-Newton study of the mixed-morphology supernova remnant W28

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009824 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 360-361

Author(s):

Ping Zhou ◽

Samar Safi-Harb ◽

Yang Chen ◽

Xiao Zhang

Keyword(s):

Thermal Model ◽

Column Density ◽

Supernova Remnant ◽

Thermal Power ◽

Hard Photon ◽

Thermal Component ◽

Absorption Column ◽

X Ray ◽

Photon Index ◽

Two Temperature

AbstractWe perform an XMM-Newton study of the mixed-morphology supernova remnant (MMSNR) W28. The X-ray spectrum arising from the northeastern shell consists of a thermal component plus a non-thermal power-law component with a hard photon index (~1.5). Non-thermal bremsstrahlung is the most favourible origin of the hard X-ray emission. The gas in the SNR interior is centrally peaked and best described by a two-temperature thermal model. We found a non-uniform absorption column density and temperature profile for the central gas, indicating that the remnant is evolving in a non-uniform environment with denser material in the east. We argue that the cloudlet evaporation is an indispensable process to explain both the spectral properties and the clumpiness in the X-ray emission.

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X-ray properties of reverberation-mapped AGNs with super-Eddington accreting massive black holes

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320002756 ◽

2019 ◽

Vol 15 (S356) ◽

pp. 143-143

Author(s):

Jaya Maithil ◽

Michael S. Brotherton ◽

Bin Luo ◽

Ohad Shemmer ◽

Sarah C. Gallagher ◽

...

Keyword(s):

Black Holes ◽

Black Hole ◽

Accretion Rate ◽

Time Lags ◽

Black Hole Mass ◽

Host Galaxies ◽

Massive Black Holes ◽

X Ray ◽

Photon Index ◽

The Impact

AbstractActive Galactic Nuclei (AGN) exhibit multi-wavelength properties that are representative of the underlying physical processes taking place in the vicinity of the accreting supermassive black hole. The black hole mass and the accretion rate are fundamental for understanding the growth of black holes, their evolution, and the impact on the host galaxies. Recent results on reverberation-mapped AGNs show that the highest accretion rate objects have systematic shorter time-lags. These super-Eddington accreting massive black holes (SEAMBHs) show BLR size 3-8 times smaller than predicted by the Radius-Luminosity (R-L) relationship. Hence, the single-epoch virial black hole mass estimates of highly accreting AGNs have an overestimation of a factor of 3-8 times. SEAMBHs likely have a slim accretion disk rather than a thin disk that is diagnostic in X-ray. I will present the extreme X-ray properties of a sample of dozen of SEAMBHs. They indeed have a steep hard X-ray photon index, Γ, and demonstrate a steeper power-law slope, ασx.

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Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2461 ◽

2019 ◽

Vol 489 (3) ◽

pp. 4300-4310 ◽

Cited By ~ 5

Author(s):

A Sezer ◽

T Ergin ◽

R Yamazaki ◽

H Sano ◽

Y Fukui

Keyword(s):

Supernova Remnant ◽

Gamma Ray ◽

Radio Continuum ◽

Continuum Emission ◽

Large Area ◽

Imaging Spectrometer ◽

X Ray ◽

East Region ◽

X Ray Imaging ◽

Collisional Ionization

ABSTRACT We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible scenarios to explain the origin of the RP emission based on the observational properties and concluded that the rarefaction scenario is a possible explanation for the existence of RP. In addition, the gamma-ray emission morphology and spectrum within the energy range of 0.2–300 GeV are investigated using 10 yr of data from the Fermi Large Area Telescope (LAT). The gamma-ray morphology of HB9 is best described by the spatial template of radio continuum emission. The spectrum is well fit to a log-parabola function and its detection significance was found to be 25σ. Moreover, a new gamma-ray point source located just outside the south-east region of the SNR’s shell was detected with a significance of 6σ. We also investigated the archival H i and CO data and detected an expanding shell structure in the velocity range of $-10.5$ and $+1.8$ km s−1 that is coinciding with a region of gamma-ray enhancement at the southern rim of the HB9 shell.

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An X-ray characterization of the central region of the supernova remnant G332.5-5.6

Astronomy and Astrophysics ◽

10.1051/0004-6361/201526699 ◽

2015 ◽

Vol 583 ◽

pp. A84 ◽

Cited By ~ 1

Author(s):

A. E. Suárez ◽

J. A. Combi ◽

J. F. Albacete-Colombo ◽

S. Paron ◽

F. García ◽

...

Keyword(s):

Central Region ◽

Supernova Remnant ◽

X Ray

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X-ray Properties of 3C 111: Separation of Primary Nuclear Emission and Jet Continuum

Universe ◽

10.3390/universe6110219 ◽

2020 ◽

Vol 6 (11) ◽

pp. 219

Author(s):

Elena Fedorova ◽

B.I. Hnatyk ◽

V.I. Zhdanov ◽

A. Del Popolo

Keyword(s):

Accretion Disk ◽

Power Law ◽

Line Emission ◽

High Energy ◽

Power Law Model ◽

X Ray ◽

Additional Information ◽

Observational Dataset ◽

Simple Power ◽

Photon Index

3C111 is BLRG with signatures of both FSRQ and Sy1 in X-ray spectrum. The significant X-ray observational dataset was collected for it by INTEGRAL, XMM-Newton, SWIFT, Suzaku and others. The overall X-ray spectrum of 3C 111 shows signs of a peculiarity with the large value of the high-energy cut-off typical rather for RQ AGN, probably due to the jet contamination. Separating the jet counterpart in the X-ray spectrum of 3C 111 from the primary nuclear counterpart can answer the question is this nucleus truly peculiar or this is a fake “peculiarity” due to a significant jet contribution. In view of this question, our aim is to estimate separately the accretion disk/corona and non-thermal jet emission in the 3C 111 X-ray spectra within different observational periods. To separate the disk/corona and jet contributions in total continuum, we use the idea that radio and X-ray spectra of jet emission can be described by a simple power-law model with the same photon index. This additional information allows us to derive rather accurate values of these contributions. In order to test these results, we also consider relations between the nuclear continuum and the line emission.

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