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

Binder, B.; Carpano, S.; Heida, Marianne; Lau, Ryan M.

doi:10.3390/galaxies8010017

Cited by 6 publications

(6 citation statements)

References 51 publications

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“…The picture that has been emerging for the evolution of ULX-1 is of a pulsar that is being obscured as a result of outflows and/or Lense-Thirring precession causing the plane of the accretion disk to precess along the line of sight (Carpano et al 2018;Kosec et al 2018;Middleton et al 2018;Vasilopoulos et al 2019;Binder et al 2020). The Lense-Thirring precession is thought to arise from super-Eddington accretion (  > M 20 Edd ) building up a large scale-height wind cone outside of the magnetosphere (Middleton et al 2018;Vasilopoulos et al 2019;King & Lasota 2020).…”

Section: Discussionmentioning

confidence: 99%

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Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1

Remillard

Steiner

et al. 2022

ApJ

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We report on results from a 1 yr soft X-ray observing campaign of the ultraluminous X-ray pulsar NGC 300 ULX-1 by the Neutron star Interior Composition Explorer (NICER) during 2018–2019. Our analysis also made use of data from Swift/XRT and XMM-Newton in order to model and remove contamination from the nearby eclipsing X-ray binary NGC 300 X-1. We constructed and fitted a series of 5 day averaged NICER spectra of NGC 300 ULX-1 in the 0.4–4.0 keV range to evaluate the long-term spectral evolution of the source, and we found that an absorbed power-law model provided the best fit overall. Over the course of our observations, the source flux (0.4–4.0 keV; absorbed) dimmed from 2 × 10−12 to below 10−13 erg s−1 cm−2 and the spectrum softened, with the photon index going from Γ ≈ 1.6 to Γ ≈ 2.6. We interpret the spectral softening as reprocessed emission from the accretion disk edge coming into view while the pulsar was obscured by the possibly precessing disk. Some spectral fits were significantly improved by the inclusion of a disk blackbody component, and we surmise that this could be due to the pulsar emerging in between obscuration episodes by partial covering absorbers. We posit that we observed a low-flux state of the system (due to line-of-sight absorption) punctuated by the occasional appearance of the pulsar, indicating short-term source variability nested in longer-term accretion disk precession timescales.

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Section: Discussionmentioning

confidence: 99%

“…NGC 300 ULX-1 (hereafter called ULX-1) hosts a ULX pulsar originally associated with supernova impostor SN 2010 da (Binder et al 2011b(Binder et al , 2020. Pulsations with an average value of 31.6 s were discovered during simultaneous XMM-Newton and NuSTAR observations in December 2016 (Carpano et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1

Remillard

Steiner

et al. 2022

ApJ

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“…The picture that has been emerging for the evolution of ULX-1 is of a pulsar that is being obscured as a result of outflows and/or Lense-Thirring precession causing the plane of the accretion disk to precess along the line-of-sight (Carpano et al 2018;Middleton et al 2018;Kosec et al 2018;Vasilopoulos et al 2019;Binder et al 2020). The Lense-Thirring precession is thought to arise from super-Eddington accretion (> 20 ṀEdd ) building up a large scale-height wind cone outside of the magnetosphere (Middleton et al 2018;Vasilopoulos et al 2019;King & Lasota 2020).…”

Section: Discussionmentioning

confidence: 99%

“…NGC 300 ULX-1 (hereafter called ULX-1) hosts a ULX pulsar originally associated with supernova impostor SN 2010da (Binder et al 2011b(Binder et al , 2020. Pulsations with an average value of 31.6 s were discovered during simultaneous XMM-Newton and NuSTAR observations in December 2016 (Carpano et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Spectral Evolution of Ultraluminous X-ray Pulsar NGC 300 ULX-1

Ng,

Remillard,

Steiner

et al. 2022

Preprint

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We report on results from a one-year soft X-ray observing campaign of the ultraluminous X-ray pulsar NGC 300 ULX-1 by the Neutron star Interior Composition Explorer (NICER) during 2018-2019. Our analysis also made use of data from Swift/XRT and XMM-Newton in order to model and remove contamination from the nearby eclipsing X-ray binary NGC 300 X-1. We constructed and fitted a series of 5-day averaged NICER spectra of NGC 300 ULX-1 in the 0.4-4.0 keV range to evaluate the long-term spectral evolution of the source, and found that an absorbed power-law model provided the best fit overall. Over the course of our observations, the source flux (0.4-4.0 keV; absorbed) dimmed from 2 × 10 −12 to below 10 −13 erg s −1 cm −2 and the spectrum softened, with the photon index going from Γ ≈ 1.6 to Γ ≈ 2.6. We interpret the spectral softening as reprocessed emission from the accretion disk edge coming into view while the pulsar was obscured by the possibly precessing disk. Some spectral fits were significantly improved by the inclusion of a disk blackbody component, and we surmise that this could be due to the pulsar emerging in between obscuration episodes by partial covering absorbers. We posit that we observed a low-flux state of the system (due to line-of-sight absorption) punctuated by the occasional appearance of the pulsar, indicating short-term source variability nested in longer-term accretion disk precession timescales.

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“…All quasars have broad emission features and are at redshifts between 1-2. Another noteworthy target (P1) is the "emission object" NGC 300-309, which turns out to be the supernova imposter SN 2010da or NGC 300 ULX-1 (Binder et al 2020). It has been explained as an ultraluminous X-ray source with a RSG donor and a neutron star (Heida et al 2019).…”

Section: Other Objects Of Interestmentioning

confidence: 99%

Investigating episodic mass loss in evolved massive stars

Bonanos,

Tramper,

de Wit

et al. 2024

A&A

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Episodic mass-loss events such as giant eruptions in luminous blue variables or pre-supernova eruptions in red supergiants drastically alter the evolutionary path of a massive star, resulting in a rich and complex circumstellar environment and IR excess. However, the incidence of these events, and hence their importance in massive star evolution, remains unknown. The ASSESS project (Episodic Mass Loss in Evolved Massive Stars: Key to Understanding the Explosive early Universe) aims to determine the role of episodic mass loss in the evolution of massive stars. As a first step, we constructed a catalog of spectroscopically identified dusty, evolved massive stars in ten southern galaxies for which Spitzer point-source catalogs are available. The resulting catalog may be used to identify stars that have undergone an episodic mass-loss event. The target galaxies span a range of metallicities, Z = 0.06--1.6 allowing for the investigation of a potential metallicity dependence. We conducted multi-object spectroscopy of dusty massive star candidates in ten target galaxies using the Very Large Telescope. We obtained 763 spectra from WLM, NGC 55, NGC 247, NGC 253, NGC 300, NGC 1313, NGC 3109, Sextans A, M83, and NGC 7793. The targets were selected using their Spitzer photometry, by prioritizing targets with a strong IR excess, which indicates the presence of hot dust. We determined a spectral classification for each target. Additionally, we used archival images from the Hubble Space Telescope (HST), available for 150 of our targets, to provide a visual classification for 80 targets, as a star, cluster, or galaxy. We provide a catalog of 541 spectroscopically classified sources that includes 185 massive stars, of which 154 are newly classified massive stars. The catalog contains 129 red supergiants, 27 blue supergiants, 10 yellow supergiants, 4 luminous blue variable candidates, 7 supergiant B e stars, and 8 emission-line objects. Evidence for circumstellar dust is found in 24<!PCT!> of these massive stars, based on their IR colors. We report a success rate of $28<!PCT!>$ for identifying massive stars from our observed spectra, while the average success rate of our priority system for selecting evolved massive stars is 36<!PCT!>. Additionally, the catalog contains 21 background galaxies (including active galactic nuclei and quasars), 10 carbon stars, and 99 regions. We measured the line ratios N ii /Halpha and S ii /Halpha for 76 regions and 36 other spectra with nebular emission lines, thereby identifying eight sources with shocked emission. We present the largest catalog of evolved massive stars and in particular of red supergiants in nearby galaxies at low Z beyond the Local Group. The brightest and reddest of these are candidates for episodic mass loss. The fraction of dusty massive stars observed with respect to the initial selection is $ We expect this catalog to trigger follow-up studies and pave the way for a comprehensive study of the eruptive late stages of massive star evolution in the era of the James Webb Space Telescope and the new survey telescopes (e.g., the Euclid mission Nancy Grace Roman Space Telescope, and Vera C. Rubin Observatory).

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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

Cited by 6 publications

References 51 publications

Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1

Spectral Evolution of Ultraluminous X-Ray Pulsar NGC 300 ULX-1

Spectral Evolution of Ultraluminous X-ray Pulsar NGC 300 ULX-1

Investigating episodic mass loss in evolved massive stars

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