Integral field spectroscopy of the ultraluminous X-ray source Holmberg II X-1

Lehmann, I.; Becker, T.; Fabrika, S.; Roth, Martin; Miyaji, Takeshi; Afanasiev, V. L.; Sholukhova, O.; Sánchez, S. F.; Greiner, J.; Hasinger, G.; Costantini, E.; Surkov, A. E.; Буренков, А. Н.

doi:10.1051/0004-6361:20035827

Cited by 66 publications

(91 citation statements)

References 36 publications

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“…Until now, most of the evidence of outflows came from shock-ionized and X-ray ionized nebulae, seen in optical and radio observations and ruling out anisotropic accretion for most ULXs (Pakull and Mirioni 2002;Kaaret et al 2003;Lehmann et al 2005;Kaaret and Corbel 2009, e.g. ).…”

Section: Jets and Outflowsmentioning

confidence: 99%

Ultraluminous X‐ray sources: Three exciting years

Bachetti

2016

Astron Nachr

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The extreme extragalactic sources known as Ultraluminous X-ray Sources (ULX) represent a unique testing environment for compact objects population studies and the accretion process. Their nature has long been disputed. Their luminosity, well above the Eddington luminosity for a stellar-mass black hole, can imply the presence of an intermediate-mass black hole or a stellar black hole accreting above the Eddington limit. Both these interpretations are important to understand better the accretion process and the evolution of massive black holes. The last few years have seen a dramatic improvement of our knowledge of these sources. In particular, the super-Eddington interpretation for the bulk of the ULX population has gained a strong consensus. Nonetheless, exceptions to this general trend do exist, and in particular one ULX was shown to be a neutron star, and another was shown to be a very likely IMBH candidate. In this paper, I will review the progress done in the last few years.

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Section: Jets and Outflowsmentioning

confidence: 99%

Ultraluminous X‐ray sources: Three exciting years

Bachetti

2016

Astron Nachr

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“…In some cases the appearence of a ULXN may be quite different, like the highexcitation photoionized H ii region of HoII X-1 (Lehmann et al, 2005) or a compact very bright shelllike nebula with anomalous excitation conditions (the nebula MF16, (Abolmasov et al2006;Abolmasov et al2007a)). …”

Section: Optical Counterpartsmentioning

confidence: 99%

Spectroscopy of optical counterparts of ultraluminous X-ray sources

et al. 2007

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Abstract. Here we present the results of panoramic and long-slit observations of eight ULX nebular counterparts held with the 6m SAO telescope. In two ULXNe we detected for the first time signatures of high excitation ([O iii]λ5007 / Hβ > 5). Two of the ULXs were identified with young (T ∼ 5 − 10 M yr) massive star clusters. Four of the eight ULX Nebulae (ULXNe) show bright high-excitation lines. This requires existence of luminous (∼ 10 38 ÷ 10 40 ergs s −1 ) UV/EUV sources coinciding with the X-ray sources. Other 4 ULXNe require shock excitation of the gas with shock velocities of 20-100km s −1 . However, all the studied ULXN spectra show signatures of shock excitation, but even those ULXNe where the shocks are prevailing show presence of a hard ionizing source with the luminosity at least ∼ 10 38 ergs s −1 . Most likely shock waves, X-ray and EUV ionization act simultaneously in all the ULXNe, but they may be roughly separated in two groups, shock-dominated and photoionization-dominated ULXNe. The ULXs have to produce strong winds and/or jets powering their nebulae with ∼ 10 39 ergs s −1 . Both the wind/jet activity and the EUV source needed are consistent with the suggestion that ULXs are high-mass X-ray binaries with the supercritical accretion disks of the SS433 type.

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“…Berghea et al (2010aBerghea et al ( , 2010b present mid-IR photometry of the well-studied Holmberg II X-1 (hereafter referred to as X-1; Pakull & Mirioni 2002;Lehmann et al 2005;Tao et al 2012;Walton et al 2015) and analyze its full radio to X-ray spectral energy distribution (SED). Based on the radio and mid-IR fluxes of X-1, Berghea et al (2010aBerghea et al ( , 2010b interpret the emission as arising from a jet; however, their radio and mid-IR data were taken over 10 years apart, which presents difficulties in taking variability into account in their modeling.…”

Section: Introductionmentioning

confidence: 99%

First Detection of Mid-infrared Variability from an Ultraluminous X-Ray Source Holmberg II X-1

Lau

Heida

Kasliwal

et al. 2017

ApJL

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We present mid-infrared (IR) light curves of the Ultraluminous X-ray Source (ULX) Holmberg II X-1 from observations taken between 2014 January 13 and 2017 January 5 with the Spitzer Space Telescope at 3.6 and 4.5 μm in the Spitzer Infrared Intensive Transients Survey. The mid-IR light curves, which reveal the first detection of mid-IR variability from a ULX, is determined to arise primarily from dust emission rather than from a jet or an accretion disk outflow. We derived the evolution of the dust temperature (~-T 600 800, and equilibrium temperature radius (~-R 10 20 au eq ). A comparison of X-1 with a sample of spectroscopically identified massive stars in the Large Magellanic Cloud on a mid-IR color-magnitude diagram suggests that the mass donor in X-1 is a supergiant (sg) B[e]-star. The sgB[e]-interpretation is consistent with the derived dust properties and the presence of the [Fe II] (l m = 1.644 m) emission line revealed from previous near-IR studies of X-1. We attribute the mid-IR variability of X-1 to the increased heating of dust located in a circumbinary torus. It is unclear what physical processes are responsible for the increased dust heating; however, it does not appear to be associated with the X-ray flux from the ULX, given the constant X-ray luminosities provided by serendipitous, near-contemporaneous X-ray observations around the first mid-IR variability event in 2014. Our results highlight the importance of mid-IR observations of luminous X-ray sources traditionally studied at X-ray and radio wavelengths.

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Integral field spectroscopy of the ultraluminous X-ray source Holmberg II X-1

Cited by 66 publications

References 36 publications

Ultraluminous X‐ray sources: Three exciting years

Ultraluminous X‐ray sources: Three exciting years

Spectroscopy of optical counterparts of ultraluminous X-ray sources

First Detection of Mid-infrared Variability from an Ultraluminous X-Ray Source Holmberg II X-1

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