The X-Ray Luminosity Function of Ultraluminous X-Ray Sources in Collisional Ring Galaxies

Wolter, A.; Fruscione, A.; Mapelli, Michela

doi:10.3847/1538-4357/aacb34

Cited by 23 publications

(23 citation statements)

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“…The differential forms of observed XLFs (𝑑𝑁/𝑑𝐿) are often fitted with power-laws, or variants such as broken or exponential cutoff power-laws (see Grimm et al 2003;Swartz et al 2011;Mineo et al 2012;Wang et al 2016;Wolter et al 2018;Kovlakas et al 2020). In Figure 3 we plot a subset of the differential forms of our synthetic XLFs versus the best fit models from Wang et al (2016) who used Chandra observations of 343 galaxies (totalling 4970 sources, 218 of which are ULXs) to create differential XLFs.…”

Section: Modelling the Xlfmentioning

confidence: 99%

The impact of precession on the observed population of ULXs

Khan

Middleton

Wiktorowicz

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The discovery of neutron stars powering several ultraluminous X-ray sources (ULXs) raises important questions about the nature of the underlying population. In this paper we build on previous work studying simulated populations by incorporating a model where the emission originates from a precessing, geometrically beamed wind-cone, created by a super-critical inflow. We obtain estimates – independent of the prescription for the precession period of the wind – for the relative number of ULXs that are potentially visible (persistent or transient) for a range of underlying factors such as the relative abundance of black holes or neutron stars within the population, maximum precessional angle, and LMXB duty cycle. We make initial comparisons to existing data using a catalogue compiled from XMM-Newton. Finally, based on estimates for the precession period, we determine how the eROSITA all-sky survey (eRASS) will be able to constrain the underlying demographic.

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Section: Modelling the Xlfmentioning

confidence: 99%

The impact of precession on the observed population of ULXs

Khan

Middleton

Wiktorowicz

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…In few cases they are associated with older stellar populations in elliptical galaxies (Feng & Kaaret 2008, Roberts et al 2008. A large number of ULXs has been found also in the young and star forming rings of ring galaxies (Wolter et al 2018). Many of them are located in or close to young O-B associations (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

Ambrosi

Zampieri

2018

Monthly Notices of the Royal Astronomical Society

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We study the evolution of binary systems of Ultra-luminous X-ray sources and compute their optical emission assuming accretion onto a black hole via a non standard, advection-dominated slim disc with an outflow. We consider systems with black holes of 20M and 100M , and donor masses between 8M and 25M . Super-critical accretion has considerable effects on the optical emission. The irradiating flux in presence of an outflow remains considerably stronger than that produced by a standard disc. However, at very high accretion rates the contribution of X-ray irradiation becomes progressively less important in comparison with the intrinsic flux emitted from the disc. After Main Sequence the evolutionary tracks of the optical counterpart on the colourmagnitude diagram are markely different from those computed for Eddington-limited accretion. Systems with stellar-mass black holes and 12 − 20M donors accreting supercritically are characterized by blue colors (F450W -F555W −0.2 : +0.1) and high luminosity (M V −4 : −6.5). Systems with more massive black holes accreting supercritically from evolved donors of similar mass have comparable colours but can reach M V −8. We apply our model to NGC 1313 X-2 and NGC 4559 X-7. Both sources are well represented by a system accreting above Eddington from a massive evolved donor. For NGC 1313 X-2 the agreement is for a ∼ 20M black hole, while NGC4559 X-7 requires a significantly more massive black hole.

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“…The smooth connection with the lower luminosity sources and the slope of the XLF are consistent with our hypothesis. This is also shown by the XLF of both a large number of ULXs collected in the rings of seven collisional RiGs (Wolter et al 2018) and those in the collection of nearby galaxies (Swartz et al 2011) observed by Chandra, which yield a similar number of ULXs and consistent results between each other, even if the RiGs have a possible excess at high luminosity. The combination of many galaxies relies on the assumption that we are witnessing a single burst of star formation in each galaxy, with a reasonable short age (possibly less than 100 Myr as per the simulations of Renaud et al 2018), close to the formation time of HMXB, and that the spread in metallicity is not large.…”

Section: The X-ray Luminosity Function Of Ulxsmentioning

confidence: 58%

The Cartwheel galaxy as a stepping stone for binaries formation

et al. 2018

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Ultraluminous X-ray sources (ULXs) are end points of stellar evolution. They are mostly interpreted as binary systems with a massive donor. They are also the most probable progenitors for BH-BH, and even more, for BH-NS coalescence. Parameters of ULXs are not know and need to be better determined, in particular the link with the metallicity of the environment which has been invoked frequently but not proven strongly. We have tackled this problem by using a MUSE DEEP mosaic of the Cartwheel galaxy and applying a Monte Carlo code that jointly fits spectroscopy and photometry. We measure the metallicity of the emitting gas in the ring and at the positions of X-ray sources by constructing spatially resolved emission line ratio maps and BPT diagnostic maps. The Carthweel is the archetypal ring galaxy and the location and formation time of new stellar populations is easier to reconstruct than in more normal galaxies. It has the largest population of ULXs ever observed in a single galaxy (16 sources have been classified as ULXs in Chandra and XMM-Newton data). The Cartwheel galaxy is therefore the ideal laboratory to study the relation between Star Formation (SF Rates and SF History) and number of ULXs and also their final fate. We find that the age of the stellar population in the outer ring is consistent with being produced in the impact (≤300Myr) and that the metallicity is mostly sub-solar, even if solutions can be found with a solar metallicity that account for most observed properties. The findings for the Cartwheel will be a testbed for further modelisation of binary formation and evolution paths.

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The X-Ray Luminosity Function of Ultraluminous X-Ray Sources in Collisional Ring Galaxies

Cited by 23 publications

References 100 publications

The impact of precession on the observed population of ULXs

The impact of precession on the observed population of ULXs

Modelling optical emission of Ultra-luminous X-ray Sources accreting above the Eddington limit

The Cartwheel galaxy as a stepping stone for binaries formation

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