A highly accreting low-mass black hole hidden in the dust: <i>Suzaku</i> and <i>NuSTAR</i> observations of the NLS1 Mrk 1239

Jiang, Jiachen; Baloković, Mislav; Brightman, Murray; Harrison, Fiona A.; Lansbury, G. B.

doi:10.1093/mnras/stab1306

Cited by 5 publications

(7 citation statements)

References 68 publications

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“…We used the spectra from all three XIS detectors for the simultaneous fitting in the energy range 0.5-10 keV of all four observations. We removed the energy bins between 1.7 and 2.3 keV to avoid the calibration uncertainties due to the artificial structures around Si and Au edges (Jiang et al 2021).…”

Section: Xis Spectramentioning

confidence: 99%

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Sharma

Jain

Dutta

2022

Monthly Notices of the Royal Astronomical Society

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We present the broad-band spectral analysis of the low-mass X-ray binary 2S 0921-63 by using the Suzaku archival data covering the orbital phase between 0.31 and 1.16 during four close observations. It is the first time that a broad-band spectral analysis of 2S 0921-63 has been done up to 25 keV. The 0.5–10 keV XIS count rate varied between ∼ 1 and ∼ 5 counts s−1 during the observations. A partial X-ray eclipse and broad post-eclipse intensity dip were observed during the observations. The X-ray emission hardened marginally during the intensity dip. We have modelled the source spectra by simultaneously fitting the XIS and HXD-PIN spectra for each of the four observations. The broad-band spectra of the source can be described by a model comprising a very hot blackbody having temperature, kTBB ≈ 1.66 − 2.13 keV, a high-energy cutoff power law, and an Fe emission line at Eline ∼ 6.7 keV. A second model, accounting for the Comptonization of the thermal emission from accretion disc along with an Fe emission line, describes the broad-band spectra of 2S 0921-63 equally well.

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Section: Xis Spectramentioning

confidence: 99%

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Sharma

Jain

Dutta

2022

Monthly Notices of the Royal Astronomical Society

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“…Typically, the photon index is linked to the photon index of the primary continuum (power law). There is no evidence of a power law below 2 keV; thus, Γ was fixed to Γ = 2.5, a typical value of the photon index found in Mrk 1239 (Buhariwalla et al 2020;Jiang et al 2021). The iron abundance was fixed to solar abundance.…”

Section: The Low-energy Spectrum Below 2 Kevmentioning

confidence: 99%

A Hot Mess: The Rich and Complex Soft Emitting Regions Surrounding the Reflection Dominated Flaring Central Engine of Mrk 1239

Buhariwalla,

Gallo,

Mao

et al. 2024

ApJ

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Previous X-ray works on Mrk 1239 have revealed a complex narrow-line Seyfert 1 that exhibits substantial absorption and strong emission from both collisionally ionized and photoionized plasmas. Here, we report on deep-pointed observations with XMM-Newton and NuSTAR, along with Swift monitoring, to understand the 0.3–30 keV continuum emission and the central engine geometry. A strong X-ray flare, where the AGN brightens by a factor of 5 in ∼30 ks, is captured between 4 and 30 keV and can be attributed to a brightening of the primary continuum. However, the lack of any variability below ∼3 keV on long or short timescales requires complete absorption of the AGN continuum with a neutral medium of column density ∼1023.5 cm−2. The timing and spectral properties are consistent with a blurred reflection interpretation for the primary emission. The variability and presence of a Compton hump disfavors ionized partial covering. The neutral absorber, if outflowing, could be crashing into the surrounding medium and interstellar medium to produce the low-energy continuum and collisionally ionized emission. Scattered emission off the inner torus could produce the photoionized emission. The intricate scenario is demanded by the data and highlights the complexity of the environment that is normally invisible when overwhelmed by the AGN continuum. Objects like Mrk 1239 serve as important sources for unveiling the interface between the AGN and host galaxy environments.

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“…They did not detect the O triplet located at ∼ 0.56 keV leading them to conclude that there was an overabundance of Ne in Mrk 1239. Subsequent works have used this overabundance while fitting the X-ray spectra (see Jiang et al 2021). The analysis of Buhariwalla et al (2020) suggested the excess emission at 0.91 keV was in fact due to a blend of emission lines including the Ne triplet and Fe-L emission lines.…”

Section: Neon Abundancementioning

confidence: 99%

“…As for Mrk 1239 this does not seem to be the case as no matter the number of photoionized components applied (in addition to powerlaw components) the spectra is still under fit between 13 − 17 Å without the addition of . Mrk 1239 is a polar scattered Seyfert 1 galaxy, meaning our line of sight (LOS) passes through the upper layers of the torus polarizing the optical emission (Smith et al 2004;Jiang et al 2021). ESO 323-G77, another polar scattered Seyfert1, presents an X-ray spectra similar to Mrk 1239.…”

Section: Mrk 1239 Compared To Seyfert Galaxiesmentioning

confidence: 99%

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The Collisional and Photoionized Plasma in the Polarized NLS1 galaxy Mrk 1239

Buhariwalla¹,

Gallo²,

Mao³

et al. 2023

Preprint

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Mrk 1239 is a highly polarized NLS1 in the optical band, whose 0.3 − 3 keV spectrum has remained remarkably consistent over more than two decades of observation. Previous analysis of this object suggested that the soft X-ray band was dominated by emission lines (collisionally and/or photoionized) from the distant host galaxy as the X-ray emission from the central engine was highly obscured. New XMM-Newton data of Mrk 1239 are presented here to investigate the soft X-ray band of this galaxy with high resolution. The first RGS spectra of this source reveal a plethora of ionized emission lines originating from two distinct plasmas, one collisionally ionized and the other photoionized at approximately equal brightness. The best fit model uses and grids to account for the collisionally ionized and photoionized components, respectively. The fit improves significantly if the photoionized material is allowed to outflow at ≈ 500 km s −1 , matching the outflow velocity of the forbidden O emission line. From constraints on the ionization and density of the photoionized material we can estimate the location of it to be no further than a few pc from the central source, around the outer radius of the torus, which is consistent with the O ( 𝑓 ) emission line. Properties of the collisionally ionized plasma are consistent with star formation rate (SFR) of ≈ 3 M yr −1 , which is comparable with several previous measurements of the SFR in this galaxy.

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A highly accreting low-mass black hole hidden in the dust: Suzaku and NuSTAR observations of the NLS1 Mrk 1239

Cited by 5 publications

References 68 publications

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

Broad-band spectral analysis of LMXB 2S 0921-63 with Suzaku

A Hot Mess: The Rich and Complex Soft Emitting Regions Surrounding the Reflection Dominated Flaring Central Engine of Mrk 1239

The Collisional and Photoionized Plasma in the Polarized NLS1 galaxy Mrk 1239

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