Discovery of pulsations from NGC 300 ULX1 and its fast period evolution

Carpano, S.; Haberl, F.; Maitra, Chandreyee; Vasilopoulos, Georgios

doi:10.1093/mnrasl/sly030

Cited by 288 publications

(334 citation statements)

References 25 publications

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“…These authors point out that the detection of a strong outflow from a PULX is evidence for a relatively weak dipole neutron-star magnetic field. They also note that an outflow was recently discovered from ULX-1 in NGC 300 (Kosec, et al 2018), for which Carpano et al (2018) deduced a magnetic field of B ∼ 10 12 G. Our model (see below) predicts B = 1.2 × 10 12 G for this source (see King & Lasota 2019, and Table 1).…”

Section: Introductionsupporting

confidence: 61%

Pulsing and non-pulsing ULXs: the iceberg emerges

King

Lasota

2020

Monthly Notices of the Royal Astronomical Society

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We show that ultraluminous X-ray sources (ULXs) with coherent X-ray pulsing (PULXs) probably have neutron-star spin axes significantly misaligned from their central accretion discs. Scattering in the funnels collimating their emission and producing their apparent super-Eddington luminosities is the most likely origin of the observed correlation between pulse fraction and X-ray photon energy. Pulsing is suppressed in systems with the neutron-star spin closely aligned to the inner disc, explaining why some ULXs show cyclotron features indicating strong magnetic fields, but do not pulse. We suggest that alignment (or conceivably, field suppression through accretion) generally occurs within a fairly short fraction of the ULX lifetime, so that most neutron-star ULXs become unpulsed. As a result we further suggest that almost all ULXs actually have neutron-star accretors, rather than black holes or white dwarfs, reflecting their progenitor high-mass X-ray binary and supersoft X-ray source populations.

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Section: Introductionsupporting

confidence: 61%

Pulsing and non-pulsing ULXs: the iceberg emerges

King

Lasota

2020

Monthly Notices of the Royal Astronomical Society

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“…A Gaussian absorption line at E ∼ 12.8 keV improved the fit significantly with respect to a simple single-component model, and implies the existence of a magnetic field with B ∼ 10 12 G close to the surface of the NS. This value is very close to what was measured in Carpano et al [28] from the spin-up rate, and similar to the magnetic field strengths of Galactic X-ray pulsars [45].…”

Section: The X-ray Spectrumsupporting

confidence: 91%

“…Using archival data, it was shown by Vasilopoulos et al [37] and Vasilopoulos et al [33] that the spin period of NGC 300 ULX-1 was as large as 126.3 s in a Chandra observation from 2014 November. Assuming almost steady accretion rateṀ after the initial outburst, the spin-period evolution could only be explained by an accretion disk formed rotating retrograde with respect to the spin of the NS, with the NS spinning down until its rotation was stopped and then starting in the opposite direction Figure 1 from Carpano et al [28], showing the period evolution during the deep XMM-Newton/NuSTAR observations. [37].…”

Section: Period Evolutionmentioning

confidence: 99%

“…In Carpano et al [28], the authors successfully fit a model composed of two absorption components (one for the interstellar absorption in the light of sight, and one partial-covering absorber in the vicinity Kosec et al [40] used a similar model for the X-ray continuum using both the soft X-ray spectra from the XMM-Newton RGS instrument and in the harder band from the XMM-Newton EPIC (pn, MOS1 and MOS2) instruments, as well as NuSTAR, combining a hard power law component with a multicolor blackbody; their detailed analysis of fit residuals shows evidence of a UFO at >3σ significance from the NS. If confirmed, this would be the first direct evidence of a UFO (with a projected velocity ∼ 0.22c, similar to other ULXs) from a pulsar-ULX, consistent with the theoretical predictions of Mushtukov et al [41].…”

Section: The X-ray Spectrummentioning

confidence: 99%

“…The XMM-Newton and NuSTAR spectra of NGC 300 ULX-1 (top panel ofFigure 3in Carpano et al[28]). XMM-Newton/EPIC pn spectra are shown in black and blue, while the MOS spectra are shown in red, green, magenta and cyan.…”

mentioning

confidence: 99%

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From SN 2010da to NGC 300 ULX-1: Ten Years of Observations of an Unusual High Mass X-Ray Binary in NGC 300

et al. 2020

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In 2010 May, an intermediate luminosity optical transient was discovered in the nearby galaxy NGC 300 by a South African amateur astronomer. In the decade since its discovery, multi-wavelength observations of the misnamed "SN 2010da" have continually re-shaped our understanding of this high mass X-ray binary system. In this review, we present an overview of the multi-wavelength observations and attempts to understand the 2010 transient event and, later, the re-classification of this system as NGC 300 ULX-1: a red supergiant + neutron star ultraluminous X-ray source.On 2010 May 24, the amateur astronomer L. A. G. Monard of Pretoria, South Africa, reported the discovery of an optical transient in the nearby spiral galaxy NGC 300, shown in Figure 1 [1]. The event was given the supernova (SN) designation SN 2010da. The apparent V-band magnitude from the discovery images (16.0±0.2 mag), however, immediately presented a contradiction: at the distance of the host galaxy (2 Mpc [2]), the implied absolute magnitude (M V ∼ −10.5 at maximum; [3]) was too low to be consistent with a true SN explosion. Follow-up spectroscopy confirmed that the transient event was not a genuine SN, and instead resembled a luminous blue variable (LBV)-like outburst from a dust-enshrouded massive star [4,5]. Multi-color imaging of the outburst was obtained with the SMARTS 1.3m telescope at Cerro Tololo ∼2 days after the initial discovery [6] and ∼3 weeks post-outburst [7]. SN 2010da thus joined the heterogeneous group of objects known as "supernova impostors," which are frequently interpreted as massive stars experiencing non-terminal eruptions or outbursts [5,6]. Additional spectroscopy from the SOAR 4.1m telescope spanned 400-860 nm [5] showed similarity to the SN impostor SN 1997bs [10]. The blue continuum emission of SN 2010da shortly after outburst was dominated by strong Hα emission, with a full width at half maximum (FWHM) of ∼1000 km s −1 and no evidence of a P Cygni profile, along with other narrow Balmer lines and a possible detection of weak He II λ4686 [5]. These results stood in contrast to those obtained with near-simultaneous GMOS on Gemini-South by Chornock and Berger [4], which observed an Hα FWHM of ∼660 km s −1 and higher-order Balmer lines with clear P-Cygni profiles. These spectral properties led Chornock and Berger [4] to speculate that the SN 2010da event originated in "an LBV-like outburst of a massive star." arXiv:2002.04113v1 [astro-ph.HE]

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Constraints on the number of X‐ray pulsars in IC 10 from a deep XMM‐Newton observation

2019

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We report the most sensitive search yet for X-ray pulsars in the dwarf starburst galaxy IC 10, which is known to contain a population of young, high-mass X-ray binaries. We searched for pulsations in 207 point-like X-ray sources in the direction of IC 10 by a 2012 XMM-Newton observation with a total exposure time of 134.5 ks. Pulsation searches in faint objects can be sensitive to the energy bands of the light curves, as well as the source and background extraction areas. We analyzed separately the PN and metal-oxide-semiconductor barycenter corrected 0.2-12 keV data, with good time interval filtering. Different schemes for source and background extraction were compared, and the search was repeated in the narrower 0.5-8 keV energy band to increase the signal-to-noise ratio. For the most conservative parameters, five point sources produced significant peaks in the Lomb-Scargle periodogram (99% significance, single trial, assuming white noise). A similar number of different candidates result from alternative analyses. A ∼4,100 s period seen in all three instruments for the black hole (BH) + Wolf-Rayet binary IC 10 X-1 is probably due to red noise of astrophysical origin. Considering the periods, luminosities, and spatial distribution of the pulsar candidates in the direction of IC 10, they do not belong to the same distribution as the ones in the Magellanic Clouds and Milky Way. This result holds even if the candidates are spurious, since if the Small Magellanic Cloud were placed at the distance of IC 10, we would expect to see nearly five pulsars at L x > 10 36 erg s -1 inside the D 25 contour, and their periods would be of order 100 s, rather than the mostly ∼1 s periods for the candidates reported here, which lie outside the main body of the galaxy. KEYWORD galaxies: individual (IC 10) -stars: neutron -X-rays: binaries 1

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Discovery of pulsations from NGC 300 ULX1 and its fast period evolution

Cited by 288 publications

References 25 publications

Pulsing and non-pulsing ULXs: the iceberg emerges

Pulsing and non-pulsing ULXs: the iceberg emerges

From SN 2010da to NGC 300 ULX-1: Ten Years of Observations of an Unusual High Mass X-Ray Binary in NGC 300

Constraints on the number of X‐ray pulsars in IC 10 from a deep XMM‐Newton observation

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