A new ultraluminous X-ray source in the galaxy NGC 5907

Pintore, Fabio; Belfiore, A.; Novara, G.; Salvaterra, R.; Marelli, M.; Luca, A. De; Rigoselli, Michela; Israel, G. L.; Rodríguez, Guillermo; Mereghetti, S.; Wolter, A.; Walton, D. J.; Ambrosi, E.; Zampieri, L.; Tiengo, A.; Salvaggio, Chiara

doi:10.1093/mnrasl/sly048

Cited by 26 publications

(28 citation statements)

References 52 publications

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“…NGC 5907 ULX-2 is located further away from the central dust lane; Pintore et al (2018) found no local extinction on top of the foreground Galactic absorption from their analysis of the X-ray spectrum of this source.…”

Section: Reddeningmentioning

confidence: 94%

“…We detect four sources brighter than the limiting magnitude in the 2-σ error circle of NGC 5907 ULX-2 in our F160W image (see right-hand panel in Figure 1 and Ta- Figure 1), but its position is inconsistent (at > 3-σ) with our localization of the ULX. This is due to our smaller localization uncertainty: our 1 − σ uncertainty is 0.3 versus 0.42 for Pintore et al (2018), as they used a different method to register the Chandra and HST images.…”

Section: Ngc 5907mentioning

confidence: 97%

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Searching for the Donor Stars of ULX Pulsars

Heida

Harrison

Brightman

et al. 2019

ApJ

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We report on our search for the optical counterparts of two ultraluminous X-ray pulsars with known orbital periods, M82 X-2 and NGC 5907 X-1, in new and archival HST observations, in an effort to characterize the donor stars in these systems. We detect five near-infrared sources consistent with the position of M82 X-2 that are too bright to be single stars. We also detect seven sources in the WFC3/UVIS F336W image whose photometry matches that of 10 -15 M stars turning off the main sequence. Such stars have densities consistent with the properties of the donor star of M82 X-2 as inferred from X-ray timing analysis, although it is also possible that the donor is a lower mass star below our detection limit or that there is a significant contribution from the accretion disc to the optical emission. We detect three candidate counterparts to NGC 5907 X-1 in the near-infrared. All of these are too bright to be the donor star of the ULX, which based on its orbital period is a red giant. The high background at the location of NGC 5907 X-1 precludes us from detecting this expected donor star. The recently discovered NGC 5907 ULX-2 also falls within the field of view of the near-infrared imaging; we detect four sources in the error circle, with photometry that matches AGB stars. The star suggested to be the counterpart of NGC 5907 ULX-2 by Pintore et al. (2018) falls outside our 2-σ error circle.

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Section: Reddeningmentioning

confidence: 94%

Section: Ngc 5907mentioning

confidence: 97%

Searching for the Donor Stars of ULX Pulsars

Heida

Harrison

Brightman

et al. 2019

ApJ

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“…We excluded from our analysis the XMM-Newton observation 0795712601 as source contamination, mainly from NGC 5907 ULX-2 but also from other sources in NGC 5907, undermines a clear characterization of ULX1. 39 We simultaneously analysed all XMM-Newton spectra in the energy range 0.3-10 keV and we fitted them with an absorbed broken power law model (bknpow in XSPEC 40 ). The Tuebingen-Boulder ISM absorption model (tbabs) was adopted and the abundances were set to those of ref.…”

Section: Xmm-newtonmentioning

confidence: 99%

Diffuse X-ray emission around an ultraluminous X-ray pulsar

et al. 2019

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Ultraluminous X-ray sources (ULXs) are extragalactic X-ray emitters located off-center of their host galaxy and with a luminosity in excess of a few 10 39 erg s −1 , if emitted isotropically. 1,2 The discovery of periodic modulation revealed that in some ULXs the accreting compact object is a neutron star, 3,4,6,7,55 indicating luminosities substantially above their Eddington limit. The most extreme object in this respect is NGC 5907 ULX-1 (ULX1), with a peak luminosity that is 500 times its Eddington limit. During a Chandra observation to probe a low state of ULX1, we detected diffuse X-ray emission at the position of ULX1. Its diameter is 2.7 ± 1.0 arcsec and contains 25 photons, none below 0.8 keV. We interpret this extended structure as an expanding nebula powered by the wind of ULX1. Its diameter of about 200 pc, characteristic energy of ∼ 1.9 keV, and luminosity of ∼ 2 × 10 38 erg s −1 imply a mechanical power of 1.3 × 10 41 erg s −1 and an age ∼ 7 × 10 4 yr. This interpretation suggests that a genuinely super-Eddington regime can be sustained for time scales much longer than the spin-up time of the neutron star powering the system. As the mechanical power from a single ULX nebula can rival the injection rate of cosmic rays of an entire galaxy, 8 ULX nebulae could be important cosmic ray accelerators. 9 NGC 5907 is a nearly edge-on (inclination of 87 • [ref. 56 ]) spiral galaxy at a distance D = 17.1 Mpc [ref. 11 ]. Its source NGC 5907 ULX-1 (henceforth ULX1), with a peak X-ray luminosity 10 41 erg s −1 , is driven by an accreting neutron star with a spin period of ∼ 1 s [ref. 55 ]. During an X-ray multi-1 arXiv:1910.11876v1 [astro-ph.HE]

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“…Of the many sources confirmed as ULXs, a number of those associated with star forming galaxies have been found to have pulsations, implying that the compact object is a neutron star (e.g., Bachetti et al 2014 to Pintore et al 2018). Although ULXs in star forming galaxies have been studied extensively, ULXs also exist in a completely different environment: globular clusters (GCs).…”

Section: Introductionmentioning

confidence: 99%

X-ray spectral variability of ultraluminous X-ray sources in extragalactic globular clusters

Dage

Zepf

Peacock

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A number of ultraluminous X-ray sources (ULXs) are physically associated with extragalactic globular clusters (GCs). We undertake a systematic X-ray analysis of eight of the brightest of these sources. We fit the spectra of the GC ULXs to single power law and single disk models. We find that the data never require that any of the sources change between a disk and a power law across successive observations. The GC ULXs best fit by a single disk show a bimodal distribution: they either have temperatures well below 0.5 keV, or variable temperatures ranging above 0.5 keV up to 2 keV. The GC ULXs with low kT have significant changes in luminosity but show little or no change in kT. By contrast, the sources with higher kT either change in both kT and L X together, or show no significant change in either parameter. Notably, the X-ray characteristics may be related to the optical properties of these ULXs, with the two lowest kT sources showing optical emission lines.

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A new ultraluminous X-ray source in the galaxy NGC 5907

Cited by 26 publications

References 52 publications

Searching for the Donor Stars of ULX Pulsars

Searching for the Donor Stars of ULX Pulsars

Diffuse X-ray emission around an ultraluminous X-ray pulsar

X-ray spectral variability of ultraluminous X-ray sources in extragalactic globular clusters

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