A New Concept of Transonic Galactic Outflows in a Cold Dark Matter Halo with a Central Super-Massive Black Hole

Igarashi, Asuka; Mori, Masao; Nitta, S.

doi:10.48550/arxiv.1405.3978

Cited by 1 publication

(3 citation statements)

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“…Igarashi et al (2014) apply their model to the Sombrero galaxy, and the model agrees with the radial density profile measured by observations. If the outflow is accelerated in OiiB 10 as claimed by Igarashi et al (2014), more fraction of the gas would escape from OiiB 10. The escape of the outflowing gas indicates that the star formation activity may be suppressed in OiiB 10, and that the IGM would be chemically enriched by this outflow process 11 .…”

Section: Difference Of the Velocities Of Mgii And Feiisupporting

confidence: 63%

“…This escape velocity is comparable to the outflow velocity, v = 80 − 260 km s −1 , implying that some fraction of the outflowing gas can escape from OiiB 10. Recently, the analytic models of Igarashi et al (2014) predict the slowly accelerated outflows with increasing radius in the gravitational potential of a cold dark matter halo and a central super-massive black hole. Igarashi et al (2014) apply their model to the Sombrero galaxy, and the model agrees with the radial density profile measured by observations.…”

Section: Difference Of the Velocities Of Mgii And Feiimentioning

confidence: 99%

“…Recently, the analytic models of Igarashi et al (2014) predict the slowly accelerated outflows with increasing radius in the gravitational potential of a cold dark matter halo and a central super-massive black hole. Igarashi et al (2014) apply their model to the Sombrero galaxy, and the model agrees with the radial density profile measured by observations. If the outflow is accelerated in OiiB 10 as claimed by Igarashi et al (2014), more fraction of the gas would escape from OiiB 10.…”

Section: Difference Of the Velocities Of Mgii And Feiimentioning

confidence: 99%

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MOSFIRE AND LDSS3 SPECTROSCOPY FOR AN [O II] BLOB ATz= 1.18: GAS OUTFLOW AND ENERGY SOURCE

Harikane

Ouchi

Yuma

et al. 2014

ApJ

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We report our Keck/MOSFIRE and Magellan/LDSS3 spectroscopy for an [Oii] Blob, OiiB 10, that is a high-z galaxy with spatially extended [Oii]λλ3726, 3729 emission over 30 kpc recently identified by a Subaru large-area narrowband survey. The systemic redshift of OiiB 10 is z = 1.18 securely determined with [Oiii]λλ4959, 5007 and Hβ emission lines. We identify Feiiλ2587 and Mgiiλλ2796,2804 absorption lines blueshifted from the systemic redshift by 80 ± 50 and 260 ± 40 km s −1 , respectively, which indicate gas outflow from OiiB 10 with the velocity of ∼ 80 − 260 km s −1 . This outflow velocity is comparable with the escape velocity, 250±140 km s −1 , estimated under the assumption of a singular isothermal halo potential profile. Some fraction of the outflowing gas could escape from the halo of OiiB 10, suppressing OiiB 10's star-formation activity. We estimate a mass loading factor, η, that is a ratio of mass outflow rate to star-formation rate, and obtain η > 0.8 ± 0.1 which is relatively high compared with low-z starbursts including U/LIRGs and AGNs. The major energy source of the outflow is unclear with the available data. Although no signature of AGN is found in the X-ray data, OiiB 10 falls in the AGN/star-forming composite region in the line diagnostic diagrams. It is possible that the outflow is powered by star formation and a type-2 AGN with narrow FWHM emission line widths of 70 − 130 km s −1 . This is the first detailed spectroscopic study of oxygen-line blobs, which includes the analyses of the escape velocity, the mass loading factor, and the presence of an AGN, and a significant step to understanding the nature of oxygen-line blobs and the relation with gas outflow and star-formation quenching at high redshift.

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Section: Difference Of the Velocities Of Mgii And Feiisupporting

confidence: 63%

Section: Difference Of the Velocities Of Mgii And Feiimentioning

confidence: 99%