The Large-scale Interstellar Medium of SS 433/W50 Revisited

Su, Yang; Zhou, Xin; Yang, Ji; Chen, Yang; Chen, Xuepeng; Zhang, Shaobo

doi:10.3847/1538-4357/aad04e

Cited by 25 publications

(26 citation statements)

References 93 publications

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“…When atomic gas is assembled by large-scale converging flows, collision between these filamentary flows becomes inevitable and will lead to gas compression. Furthermore, in the environment of pressure enhancement by colliding flows, MC formation is probably rapid due to dynamical processes (e.g., Koyama & Inutsuka 2000;Bergin et al 2004;Glover & Mac Low 2007;Glover et al 2010;Su et al 2018) and various instabilities (e.g., Hennebelle & Falgarone 2012;Dobbs et al 2014;Klessen & Glover 2016). This scenario indicates that MCs are likely evolving transient objects from filamentary HI gas to H 2 gas, and then MCs traced by observed CO emission (e.g., Blitz et al 2007;Hennebelle et al 2008).…”

Section: Formation By Large-scale Converging Flows?mentioning

confidence: 99%

Local Molecular Gas toward the Aquila Rift Region

Su¹,

Yang

Yan³

et al. 2020

ApJ

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We present the results of a ∼250 square degrees CO mapping (+26 • < ∼ l < ∼ + 50 • and −5 • < ∼ b < ∼ + 5 • ) toward the Aquila Rift region at a spatial resolution of ∼ 50 and a grid spacing of 30 . The high dynamic range CO maps with a spectral resolution of ∼ 0.2 km s −1 display highly structured molecular cloud (MC) morphologies with valuable velocity information, revealing complex spatial and dynamical features of the local molecular gas. In combination with the MWISP CO data and the Gaia DR2, distances of the main MC structures in the local ISM are well determined toward the Aquila Rift region. We find that the total MC mass within 1 kpc is about > ∼ 4.1×10 5 M in the whole region. In fact, the mass of the molecular gas is dominated by the W40 giant molecular cloud (GMC) at ∼ 474 pc (∼ 1.4×10 5 M ) and the GMC complex G036.0+01.0 at ∼ 560-670 pc (∼ 2.0 × 10 5 M ), while the MCs at ∼ 220-260 pc have gas mass of ∼ 10 2 −10 3 M . Interestingly, a ∼ 80 pc long filamentary MC G044.0−02.5 at a distance of ∼ 404 pc shows a systematic velocity gradient along and perpendicular to the major axis of the filament. The HI gas with the enhanced emission has the similar spatial morphologies and velocity features compared to the corresponding CO structure, indicating that the large-scale converging HI flows is probably responsible for the formation of the MC. Meanwhile, the long filamentary MC consists of many sub-filaments with the lengths ranging from ∼ 0.5 pc to several pc, as well as prevalent networks of filaments in other large-scale local MCs.

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Section: Formation By Large-scale Converging Flows?mentioning

confidence: 99%

Local Molecular Gas toward the Aquila Rift Region

Su¹,

Yang

Yan³

et al. 2020

ApJ

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“…Liu et al (2020) observed a few clouds detected by Yamamoto et al (2008) and suggested that one of them was within the western wing of W50. Su et al (2018) found other clouds near the western wing and a straight extension of the eastern wing in the velocity range 73 -84 km s −1 . Thus, the intrinsic velocity range of the ISM interacting with W50 has not been identified yet.…”

Section: Introductionmentioning

confidence: 87%

Energy estimation of high energy particles associated with the SS433/W50 system through radio observation at 1.4 GHz

Sakemi,

Omae,

Ohmura

et al. 2021

Preprint

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The radio nebula W50 is a unique object interacting with the jets of the microquasar SS433.The SS433/W50 system is a good target for investigating the energy of cosmic-ray particles accelerated by galactic jets. We report observations of radio nebula W50 conducted with the NSF's Karl G. Jansky Very Large Array (VLA) in the L band (1.0 -2.0 GHz). We investigate the secular change of W50 on the basis of the observations in 1984, 1996, and 2017, and find that most of its structures were stable for 33 years. We revise the upper limit velocity of the eastern terminal filament by half to 0.023c assuming a distance of 5.5 kpc. We also analyze the observational data of the Arecibo Observatory 305-m telescope and identify the HI cavity around W50 in the velocity range 33.77 km s −1 -55.85 km s −1 . From this result, we estimate the maximum energy of the cosmic-ray protons accelerated by the jet terminal region to be above 10 15.5 eV. We also use the luminosity of the gamma-rays in the range 0.5 -10 GeV to estimate the total energy of accelerated protons below 5.2 × 10 48 erg.

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“…Hence, Galactic X-ray binaries may provide some contribution to the PeV CRs (cf., Cooper et al 2020). The lifetime of SS 433 may be longer, t age ∼ 10 5 − 10 6 yr (Yamamoto et al 2008;Su et al 2018), and the escaping CRs can arrive at Earth if we use t age = 10 6 yr. In this case, SS 433 can contribute to the observed PeV CRs up to 6 %.…”

Section: Effects Of Escaping Crsmentioning

confidence: 99%

Deciphering the Origin of the GeV--TeV Gamma-ray Emission from SS 433

Kimura,

Murase,

Mészáros

2020

Preprint

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We investigate hadronic and leptonic models for the GeV-TeV gamma-ray emission from jets of the microquasar SS 433. The emission region of the TeV photons coincides with the X-ray knots, where electrons are efficiently accelerated. On the other hand, the optical high-density filaments are also located close to the X-ray knots, which may support a hadronic scenario. We calculate multi-wavelength photon spectra of the extended jet region by solving the transport equations for the electrons and protons. We find that both hadronic and leptonic models can account for the observational data, including the latest Fermi LAT result. The hadronic scenario predicts higher-energy photons than the leptonic models, and future observations such as the Cherenkov Telescope Array (CTA), the Large High-Altitude Air Shower Observatory (LHAASO), and the Southern Wide-field Gamma-ray Observatory (SWGO) may distinguish between these models and unravel the emission mechanism of GeV-TeV gamma-rays. Based on our hadronic secenario, the analogy between microquasars and radio galaxies implies that the X-ray knot region of the jets in radio galaxies may accelerate heavy nuclei up to ultrahigh energies.

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The Large-scale Interstellar Medium of SS 433/W50 Revisited

Cited by 25 publications

References 93 publications

Local Molecular Gas toward the Aquila Rift Region

Local Molecular Gas toward the Aquila Rift Region

Energy estimation of high energy particles associated with the SS433/W50 system through radio observation at 1.4 GHz

Deciphering the Origin of the GeV--TeV Gamma-ray Emission from SS 433

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