Kinematics of Ultra-High-Velocity Gas in the Expanding Molecular Shell Adjacent to the W44 Supernova Remnant

Yamada, Masaya; Oka, Tomoharu; Takekawa, Shunya; Iwata, Yuhei; Tsujimoto, Shiho; Tokuyama, Sekito; Furusawa, Maiko; Tanabe, Keisuke; Nomura, Munehiro

doi:10.3847/2041-8213/834/1/l3

Cited by 12 publications

(9 citation statements)

References 23 publications

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“…PBHs in the mass range of ∼ 10 − 100M ⊙ appear allowed by the available observational data (see discussion in e.g. Carr et al, 2016) and the required abundance would appear in broad agreement with recently claimed abundance of quiescent black hole X-ray binaries in our Galaxy (Tetarenko et al, 2016) and possibly also with the observations of high-velocity clouds near the Galactic Center driven by inactive BHs rapidly plunging into molecular clouds Yamada et al, 2017). The mass range also is within the cosmological horizon at ∼ 0.01 − 0.1 GeV when various mechanisms for generating PBHs in the early Universe operate (e.g.…”

Section: First Black Holessupporting

confidence: 89%

Looking at cosmic near-infrared background radiation anisotropies

et al. 2018

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The cosmic infrared background (CIB) contains emissions accumulated over the entire history of the Universe, including from objects inaccessible to individual telescopic studies. The near-IR (∼ 1 − 10 µm) part of the CIB, and its fluctuations, reflects emissions from nucleosynthetic sources and gravitationally accreting black holes (BHs). If known galaxies are removed to sufficient depths the source-subtracted CIB fluctuations at near-IR can reveal sources present in the first-stars-era and possibly new stellar populations at more recent times. This review discusses the recent progress in this newly emerging field which identified, with new data and methodology, significant source-subtracted CIB fluctuations substantially in excess of what can be produced by remaining known galaxies. The CIB fluctuations further appear coherent with unresolved cosmic X-ray background (CXB) indicating a very high fraction of BHs among the new sources producing the CIB fluctuations. These observations have led to intensive theoretical efforts to explain the measurements and their properties. While current experimental configurations have limitations in decisively probing these theories, their potentially remarkable implications will be tested in the upcoming CIB measurements with the ESA's Euclid dark energy mission. We describe the goals and methodologies of LIBRAE (Looking at Infrared Background Radiation with Euclid), a NASA-selected project for CIB science with Euclid, which has the potential for transforming the field into a new area of precision cosmology. * Alexander. Kashlinsky@nasa.gov; Code 665, Observational Cosmology Lab, E. Probing IGM at pre-reionization: CMB-CIB crosspower 48 F. History of emissions from Lyman tomography 49 G. Probing BAOs and dark energy at 10 < z < 16 50 H. LIBRAE summary 51 VIII. Other forthcoming experimental configurations 52 IX. Outlook for the future 53 X. Appendix: acronyms and abbreviations 54 XI. Acknowledgments 54 References 55 4π c I ν /h Planck = 0.63 Iν MJy/sr cm −3 . For comparison the CMB photons are orders-of-magnitude more abundant with n CMB = 413 cm −3 .CMB observations established the flat geometry of the Universe. We will thus adopt the Friedman-Robertson-Walker flat metric for the Universe with the interval given by dsω are the redshift, comoving coordinate distance, cosmic time, and solid angle. Photons move along null geodesics, ds 2 = 0. The Friedman equations with the matter, dark energy (Λ), radiation/relativistic component and curvature density parameters Ω m , Ω Λ , Ω γ , Ω K lead to c(1 + z)dt/dz = R H /E(z), where E(z) ≡ [Ω γ (1 + z) 4 + Ω m (1 + z) 3 + Ω K (1 + z) 2 + Ω Λ f (z)] 1/2 with f (z) describing the evolution of DE and R H ≡ cH −1 0 . The Hubble constant is H(z) = H 0 E(z) and the distance measures become: the coordinate distance x(z) = c (1 + z)dt = R H z 0 dz/E(z), the comoving angular di-Advanced CCD Imaging Spectrometer -imaging arrays AEGIS XD All-wavelength Extended Groth strip International Survey -X-ray, deep AGB Asymptotic giant branch AKARI A Japane...

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Section: First Black Holessupporting

confidence: 89%

Looking at cosmic near-infrared background radiation anisotropies

et al. 2018

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“…interacting with the W44 SNR (Sashida et al 2013). This high-velocity feature, called the Bullet (Yamada et al 2017), has a compact appearance (0.5 × 0.8 pc 2 ) and its full-width-zero-intensity velocity width exceeds 100 km s −1 . Yamada et al (2017) suggested that the Bullet could be driven by the high-velocity plunge of an invisible massive compact object into the dense GMC.…”

Section: Origin Of the Small Hvccsmentioning

confidence: 99%

“…This high-velocity feature, called the Bullet (Yamada et al 2017), has a compact appearance (0.5 × 0.8 pc 2 ) and its full-width-zero-intensity velocity width exceeds 100 km s −1 . Yamada et al (2017) suggested that the Bullet could be driven by the high-velocity plunge of an invisible massive compact object into the dense GMC. The kinematical structure of the Bullet can be produced by the magneto-hydrodynamical simulation of the plunging scenario (Nomura et al in preparation).…”

Section: Origin Of the Small Hvccsmentioning

confidence: 99%

Discovery of Two Small High-Velocity Compact Clouds in the Central 10 Parsecs of Our Galaxy

Takekawa,

Oka,

Iwata

et al. 2017

Preprint

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We discovered two small high-velocity compact clouds (HVCCs) in HCN J=4-3 and J=3-2 maps of the central 20 pc of our Galaxy. Both HVCCs have broad velocity widths (∆V 40 km s −1 ) and compact sizes (d ∼ 1 pc), and originate from the dense molecular clouds in the position-velocity space. One of them has a faint counterpart in a Paschen-α image. Their spatial structure, kinematics, and absence of luminous stellar object are compatible with the notion that each of the small HVCCs is driven by the plunge of an invisible compact object into a molecular cloud. Such objects are most likely inactive, isolated black holes.

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“…BHs totally (see also, Caputo et al 2017). Recent observations have indicated isolated BHs might be floating in interstellar space (Sashida et al 2013;Oka et al 2016;Oka et al 2017;Takekawa et al 2017;Yamada et al 2017;Takekawa et al 2019). The isolated BHs can attract and swallow the gas while moving in interstellar space.…”

Section: Introductionmentioning

confidence: 99%

Hoyle–Lyttleton accretion on to black hole accretion disks with super-Eddington luminosity for dusty gas

Erika

Ohsuga

Yajima

2021

Publications of the Astronomical Society of Japan

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We investigate the Hoyle–Lyttleton accretion of dusty gas for the case where the central source is the black hole accretion disk. By solving the equation of motion taking into account the radiation force which is attenuated by the dust absorption, we reveal the steady structure of the flow around the central object. We find that the mass accretion rate tends to increase with an increase of the optical thickness of the flow and the gas can accrete even if the disk luminosity exceeds the Eddington luminosity for the dusty gas, since the radiation force is weakened by the attenuation via the dust absorption. When the gas flows in from the direction of the rotation axis for the disk with Γ′ = 3.0, the accretion rate is about $93\%$ of the Hoyle–Lyttleton accretion rate if τHL = 3.3 and zero for τHL = 1.0, where Γ′ is the Eddington ratio for the dusty gas and τHL is the typical optical thickness of the Hoyle–Lyttleton radius. Since the radiation flux in the direction of disk plane is small, the radiation force tends not to prevent gas accretion from the direction near the disk plane. For τHL = 3.3 and Γ′ = 3.4, although the accretion is impossible in the case of Θ = 0°, the accretion rate is $28\%$ of the Hoyle–Lyttleton one in the case of Θ = 90°, where Θ is the angle between the direction the gas is coming from and the rotation axis of the disk. We also obtain relatively high accretion luminosity that is realized when the accretion rate of the disk on to the BH is consistent with that via the Hoyle–Lyttleton mechanism taking into account the effect of radiation. This implies that the intermediate-mass black holes moving in the dense dusty gas are identified as luminous objects in the infrared band.

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Kinematics of Ultra-High-Velocity Gas in the Expanding Molecular Shell Adjacent to the W44 Supernova Remnant

Cited by 12 publications

References 23 publications

Looking at cosmic near-infrared background radiation anisotropies

Looking at cosmic near-infrared background radiation anisotropies

Discovery of Two Small High-Velocity Compact Clouds in the Central 10 Parsecs of Our Galaxy

Hoyle–Lyttleton accretion on to black hole accretion disks with super-Eddington luminosity for dusty gas

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