<i>XMM-Newton</i> campaign on the ultraluminous X-ray source NGC 247 ULX-1: outflows

Pinto, C.; Soria, Roberto; Walton, D. J.; D’Aí, A.; Pintore, Fabio; Kosec, P.; Alston, W. N.; Middleton, Matthew; Roberts, T. P.; Santo, M. Del; Barret, D.; Ambrosi, E.; Robba, A.; Earnshaw, Hannah P.; Fabian, A. C.

doi:10.1093/mnras/stab1648

Cited by 50 publications

(58 citation statements)

References 58 publications

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“…This is a very high value, exceeding the UFO column densities measured in both ULXs and AGNs (e.g. Tombesi et al 2011;Pinto et al 2016Pinto et al , 2021). An outflow of such high column density would plausibly produce a strong associated emission signature such as a P-Cygni feature with a strong emission component, but this is not observed in the current spectra.…”

Section: Potential Identification As Absorption By a Highly Ionized O...mentioning

confidence: 54%

An 8.56 keV absorption line in the hyperluminous X-ray source in NGC 4045: ultra-fast outflow or cyclotron line?

Brightman,

Kosec,

Fürst

et al. 2022

Preprint

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We report on the discovery of an absorption line at E = 8.56 +0.05 −0.11 keV detected with a significance of > 3.3σ in the NuSTAR and XMM-Newton spectra of a newly discovered hyperluminous X-ray source (HLX, L X > 10 41 erg s −1 ) in the galaxy NGC 4045 at a distance of 32 Mpc. The source was first discovered serendipitously in a Swift/XRT observation of the galaxy, and Swift monitoring reveals a highly variable source changing by over an order of magnitude from maximum to minimum. The origin of the absorption line appears likely to be by highly ionized iron with a blue shift of 0.19c, indicating an ultrafast outflow (UFO). However, the large equivalent width of the line (EW= −0.22 +0.08 −0.09 keV) paired with the lack of other absorption lines detected are difficult to reconcile with models. An alternative explanation is that the line is due to a cyclotron resonance scattering feature (CRSF), produced by the interaction of X-ray photons with the powerful magnetic field of a neutron star.

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Section: Potential Identification As Absorption By a Highly Ionized O...mentioning

confidence: 54%

An 8.56 keV absorption line in the hyperluminous X-ray source in NGC 4045: ultra-fast outflow or cyclotron line?

Brightman,

Kosec,

Fürst

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Unfortunately, the column density of the PION model is pegged to our upper limit of 2 × 10 24 cm −2 . This is a very high value, exceeding the ultrafast outflow (UFO) column densities measured in both ULXs and AGNs (e.g., Tombesi et al 2011;Pinto et al 2016Pinto et al , 2021). An outflow of such high column density would plausibly produce a strong associated emission signature such as a P Cygni feature with a strong emission component, but this is not observed in the current spectra.…”

Section: Potential Identification As Absorption By a Highly Ionized O...mentioning

confidence: 62%

An 8.56 keV Absorption Line in the Hyperluminous X-Ray Source in NGC 4045: Ultrafast Outflow or Cyclotron Line?

Brightman

Kosec

Earnshaw

et al. 2022

ApJ

Self Cite

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We report on the discovery of an absorption line at E = 8.56 − 0.11 + 0.05 keV detected with a significance of >3.3σ in the NuSTAR and XMM-Newton spectra of a newly discovered hyperluminous X-ray source (L X > 1041 erg s−1) in the galaxy NGC 4045 at a distance of 32 Mpc. The source was first discovered serendipitously in a Swift/XRT observation of the galaxy, and Swift monitoring reveals a highly variable source changing by over an order of magnitude from maximum to minimum. The origin of the absorption line appears likely to be from highly ionized iron with a blueshift of 0.19c, indicating an ultrafast outflow. However, the large equivalent width of the line ( EW = − 0.22 − 0.09 + 0.08 keV) paired with the lack of other absorption lines detected is difficult to reconcile with models. An alternative explanation is that the line is due to a cyclotron resonance scattering feature produced by the interaction of X-ray photons with the powerful magnetic field of a neutron star.

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“…These features are believed to be the signatures of outflowing wind from the system (Sutton et al 2015;Feng et al 2016;Soria & Kong 2016;Urquhart & Soria 2016;Pinto et al 2020). Recently, the direct detection of outflowing wind has been reported in a handful of ULXs (Pinto et al 2016(Pinto et al , 2017(Pinto et al , 2021, which confirm the existence of the outflow from super-Eddington accretion systems.…”

Section: Introductionmentioning

confidence: 78%

“…The X-ray flux dipping episodes have been observed in many ULXs, for example NGC 55 ULX1 (Stobbart et al 2004;Pintore et al 2015), NGC 628 (Liu et al 2005), M94 (Lin et al 2013, NGC 5408 (Pasham & Strohmayer 2013;Grisé et al 2013), NGC 247 (Feng et al 2016;D'Aì et al 2021;Alston et al 2021;Pinto et al 2021), M 51 ULX-7 (Vasilopoulos et al 2021;Hu et al 2021), M51 and M81 (Urquhart & Soria 2016). Significant X-ray dipping behaviour has been reported in NGC 55 ULX1 using the XMM-Newton observations conducted in 2001 (Stobbart et al 2004).…”

Section: Discussionmentioning

confidence: 94%

Spectral and Temporal Properties of Ultra-luminous X-ray Source NGC 55 ULX1

Jithesh

2021

Preprint

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We investigate the spectral and temporal properties of ultra-luminous X-ray source (ULX) NGC 55 ULX1 using Swift, XMM-Newton and NuSTAR observations conducted during 2013-2021. In these observations, the source flux varies by a factor of ∼ 5 − 6, and we identify the source mainly in the sof t ultraluminous (SUL) state of ULXs. We fit the X-ray spectra with a two thermal component model consisting of a blackbody (for the soft component) and a disc (for the hard component), and the soft component dominates in these observations. The soft component in the SUL state shows properties similar to that of ultraluminous supersoft sources, for example, an anti-correlation between the characteristic radius and temperature of the blackbody component. In addition, we observe a positive correlation between the blackbody and inner disc temperatures when the X-ray spectra are fitted with the two-thermal component model. The source exhibits marginal evidence of X-ray flux dips in the Swift and XMM-Newton observations at different intensity levels. We explain the observed spectral and temporal properties of the source by invoking the supercritical radiatively driven outflow mechanism.

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XMM-Newton campaign on the ultraluminous X-ray source NGC 247 ULX-1: outflows

Cited by 50 publications

References 58 publications

An 8.56 keV absorption line in the hyperluminous X-ray source in NGC 4045: ultra-fast outflow or cyclotron line?

An 8.56 keV absorption line in the hyperluminous X-ray source in NGC 4045: ultra-fast outflow or cyclotron line?

An 8.56 keV Absorption Line in the Hyperluminous X-Ray Source in NGC 4045: Ultrafast Outflow or Cyclotron Line?

Spectral and Temporal Properties of Ultra-luminous X-ray Source NGC 55 ULX1

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