Colliding winds in and around the stellar group IRS 13E at the galactic centre

Wang, Q. Daniel; Li, J.; Russell, Christopher M. P.; Cuadra, Jorge

doi:10.1093/mnras/stz3624

Cited by 20 publications

(20 citation statements)

References 61 publications

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“…Based on this scenario, we compare the results of the numerical simulation with the observed eccentricity distribution of the CWSs to constrain the IMC's orbital semi-major axis to be in the range of 0.3 − 0.4 pc which is somewhat larger than IRS 13E's projected separation from Sgr A as suggested by the X-ray morphology of its surrounding region (Wang et al 2020). We also find that for a co-orbiting IMC, the effectiveness of this process requires the depletion timescale (τ dep ) to be comparable to or larger than a fraction of the liberation timescale.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…Recent ALMA observations also unveiled ionized gas which appears flowing along eccentric Keplerian streams around a point-mass potential at the location of IRS 13E (Tsuboi et al 2017). However, this interpretation would break down if the gas properties of IRS 13E is due to a colliding winds (Wang et al 2020;Zhu et al 2020). Although the suggestion that it may be an intermediatemass black hole (IMBH) remains a controversial issue (Maillard et al 2004;Hansen & Milosavljević 2003;Kim et al 2004), its total inferred mass (∼ 10 4 M ) would be reasonable if the young stars in the IRS 13E complex are gravitationally bound (Schödel et al 2005;Tsuboi et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center

Zheng,

Lin,

Mao

2020

Preprint

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There is a dense group of OB and Wolf-Rayet stars within a fraction of a parsec from the supermassive black hole (SMBH) at the Galactic Center. These stars appear to be coeval and relatively massive. A subgroup of these stars orbits on the same plane. If they emerged with low to modest eccentricity orbits from a common gaseous disk around the central super-massive black hole, their inferred lifespan would not be sufficiently long to account for the excitation of their high orbital eccentricity through dynamical relaxation. Here we analyze the secular perturbation on Galactic Center stars by an intermediate-mass companion (IMC) as a potential mechanism to account for these young disk stars' high eccentricity. This IMC may be either an intermediate-mass black hole (IMBH) or a compact cluster such as IRS-13E. If its orbital angular momentum vector is anti-parallel to that of the disk stars, this perturbation would be effective in exciting the eccentricity of stars with orbital precession rates which resonate with IMC's precession rate. If it orbits around the SMBH in the same direction as the disk stars, the eccentricity of the young stars can still be highly excited by the IMC during the depletion of their natal disk, possible associated with the launch of the Fermi bubble. In this scenario, IMC's precession rate decreases and its secular resonance sweeps through the proximity of the young stars. We carry out numerical simulations with various inclination angles between the orbits of IMC and the disk stars and show this secular interaction is a robust mechanism to excite the eccentricity and inclination of some disk stars.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center

Zheng,

Lin,

Mao

2020

Preprint

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“…The relation of E60 to IRS13E is unclear, but its proper motion along R.A. has a value of -210 km s −1 , quite comparable to the mean value of E1, E2 and E4. Wang et al (2020) suggested that E60 is an interacting binary emitting X-rays and may alone be responsible for the flux associated with what we refer to as the "tail". The X-ray intensity profile examined in Figure 3 instead suggests a continuous distribution rather than a sum of two overlapping point sources.…”

Section: Discussionmentioning

confidence: 99%

“…During the final preparation stage of our manuscript,Wang et al (2020) published a study of IRS13E, which also identifies its extended X-ray morphology based on a similar set of Chandra data. Our interpretation for this morphology is different from theirs, as will be explained in later Sections.3 http://cxc.harvard.edu/ciao…”

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confidence: 99%

Galactic Center IRS13E: Colliding Stellar Winds or an Intermediate Mass Black Hole?

Zhu,

Li,

Ciurlo

et al. 2020

Preprint

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A small cluster of massive stars residing in the Galactic center, collectively known as IRS13E, is of special interest due to its close proximity to Sgr A* and the possibility that an embedded intermediate-mass black hole (IMBH) binds its member stars. It has been suggested that colliding winds from two member stars, both classified as Wolf-Rayet type, are responsible for the observed X-ray, infrared and radio emission from IRS13E. We have conducted an in-depth study of the X-ray spatial, temporal and spectral properties of IRS13E, based on 5.6 Ms of ultra-deep Chandra observations obtained over 20 years. These X-ray observations show no significant evidence for source variability. We have also explored the kinematics of the cluster members, using Keck near-infrared imaging and spectroscopic data on a 14-yr baseline that considerably improve the accuracy of stars' proper motions. The observations are interpreted using 3-dimensional hydrodynamical simulations of colliding winds tailored to match the physical conditions of IRS13E, leading us to conclude that the observed X-ray spectrum and morphology can be well explained by the colliding wind scenario, in the meantime offering no support for the presence of a putative IMBH. An IMBH more massive than a few 10 3 M ⊙ is also strongly disfavored by the stellar kinematics.

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“…Other observations that can be explained by the impact of the jet with the mini-cavity is an X-ray source with a luminosity of 2×10 33 erg s −1 coincides with the cluster of stars, IRS 13E, (Wang et al 2020;Zhu et al 2020) embedded within the western edge of the minicavity. Recent analysis of X-ray data concludes that colliding winds of masslosing stars in the cluster are responsible for production of X-rays (Wang et al 2020;Zhu et al 2020). Alternatively, we note that X-ray emission from the minicavity can also be explained by the violent collision with the jet shocking the gas to high temperatures.…”

Section: Collimated Outflow and Interaction Sitesmentioning

confidence: 95%

Evidence for a jet and outflow from Sgr A*: a continuum and spectral line study

Yusef-Zadeh,

Royster,

Wardle

et al. 2020

Preprint

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We study the environment of Sgr A* using spectral and continuum observations with the ALMA and VLA. Our analysis of sub-arcsecond H30α, H39α, H52α and H56α line emission towards Sgr A* confirm the recently published broad peak ∼ 500 km s −1 spectrum toward Sgr A*. We also detect emission at more extreme radial velocities peaking near −2500 and 4000 km s −1 within 0.2 . We then present broad band radio continuum images at multiple frequencies on scales from arcseconds to arcminutes. A number of elongated continuum structures lie parallel to the Galactic plane, extending from ∼ 0.4 to ∼ 10 . We note a nonthermal elongated structure on an arcminute scale emanating from Sgr A* at low frequencies between 1 and 1.4 GHz where thermal emission from the mini-spiral is depressed by optical depth effects. The position angle of this elongated structure and the sense of motion of ionized features with respect to Sgr A* suggest a symmetric, collimated jet emerging from Sgr A* with an opening angle of ∼ 30 • and a position angle of ∼60 • punching through the medium before accelerating a significant fraction of the orbiting ionized gas to high velocities. The jet with estimated mass flow rate ∼ 1.4 × 10 −5 M yr −1 emerges perpendicular to the equatorial plane of the accretion flow near the event horizon of Sgr A* and runs along the Galactic plane. To explain a number of east-west features near Sgr A*, we also consider the possibility of an outflow component with a wider-angle launched from the accretion flow at larger radii.

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Colliding winds in and around the stellar group IRS 13E at the galactic centre

Cited by 20 publications

References 61 publications

The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center

The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center

Galactic Center IRS13E: Colliding Stellar Winds or an Intermediate Mass Black Hole?

Evidence for a jet and outflow from Sgr A*: a continuum and spectral line study

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