Large-Scale Effects of Supernova Remnants on the Galaxy: Generation and Maintenance of a Hot Network of Tunnels

Cox, D. P.; Smith, Barham W.

doi:10.1086/181476

Cited by 422 publications

(235 citation statements)

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“…Although our simplified model provides a very good result, a homogeneous distribution of gas and dust seems clearly inconsistent with observations of real ISMs. There is indeed ample evidence for a multiphase ISM in star-forming galaxies, galactic fountains, and outflowing halos (Geach et al 2014;Veilleux et al 2009;Cox & Smith 1974;McKee & Ostriker 1977;McKee 1995;Spitzer 1990;Mac Low & Klessen 2004). In the most frequently employed picture of McKee & Ostriker (1977), most of the volume of the ISM is occupied by hot (HIM, T ≈ 10 6 K), warm (WNM, T ≈ 10 4 K), and cold (molecular phase, T ≈ 10 2 K) media in thermal equilibrium.…”

Section: Hi and Dust Clumpiness Inside The Disk And The Outflowing Halosmentioning

confidence: 99%

The Lyman alpha reference sample

Duval

Östlin

Hayes

et al. 2016

A&A

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Context. Recent numerical simulations suggest that the strength of the Lyman alpha (Lyα) line of star-forming disk galaxies strongly depends on the inclination at which they are observed: from edge-on to face-on, we expect to see a change from a strongly attenuated Lyα line to a strong Lyα emission line. Aims. We aim to understand how a strong Lyα emission line is able to escape from the low-redshift highly inclined (edge-on) disk galaxy Mrk 1486 (z ∼ 0.0338). To our knowledge, this work is the first observational study of Lyα transport inside an edge-on disk galaxy. Methods. Using a large set of HST imaging and spectroscopic data, we investigated the interstellar medium (ISM) structure and the dominant source of Lyα radiation inside Mrk 1486. Moreover, using a 3D Monte Carlo Lyα radiation transfer code, we studied the radiative transfer of Lyα and UV continuum photons inside a 3D geometry of neutral hydrogen (HI) and dust that models the ISM structure at the galaxy center. Our numerical simulations predicted the Lyα line profile that we then compared to the one observed in the HST/COS spectrum of Mrk 1486. Results. While a pronounced Lyα absorption line emerges from the disk of Mrk 1486, very extended Lyα structures are observed at large radii from the galaxy center: a large Lyα-halo and two very bright Lyα regions located slightly above and below the disk plane. The analysis of IFU Hα spectroscopic data of Mrk 1486 indicates the presence of two bipolar outflowing halos of HI gas at the same location as these two bright Lyα regions. Comparing different diagnostic diagrams (such as [OIII] 5007 /Hβ versus [OI] 6300 /Hα) to photo-and shock-ionization models, we find that the Lyα production of Mrk 1486 is dominated by photoionization inside the galaxy disk. From this perspective, our numerical simulations succeed in reproducing the strength and shape of the observed Lyα emission line of Mrk 1486 by assuming a scenario in which the Lyα photons are produced inside the galaxy disk, travel along the outflowing halos, and scatter on cool HI materials toward the observer. Conclusions. Extended bipolar galactic winds are frequently observed from star-forming disk galaxies. Given the advantage Lyα photons take of such outflowing HI materials to easily escape from Mrk 1486, this mechanism may explain the origin of strong Lyα emission lines frequently observed from highly inclined galaxies at high-redshift. This therefore challenges the robustness of the expected viewing-angle effect on the Lyα properties of star-forming disk galaxies.

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Section: Hi and Dust Clumpiness Inside The Disk And The Outflowing Halosmentioning

confidence: 99%

The Lyman alpha reference sample

Duval

Östlin

Hayes

et al. 2016

A&A

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“…Several decades ago, the ISM was thought of as a fairly quiescent place, with interstellar clouds wafting along and gradually forming stars. However, after the discovery of a voluminous, hot (T ϳ10 6 K) intercloud medium, caused by enormous shock waves from supernovae (exploding stars) propagating through the ISM (Cox and Smith, 1974;Jenkins and Meloy, 1974;York, 1974;Burstein et al, 1977), it was clear the ISM was not as quiescent as previously believed. McKee and Ostriker (1977) formulated a theory of the ISM in which supernova shocks played the dominant role in determining the overall morphology of the medium.…”

Section: Introductionmentioning

confidence: 99%

Photodissociation regions in the interstellar medium of galaxies

Hollenbach

Tielens²

1999

Rev. Mod. Phys.

751

712

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The interstellar medium of galaxies is the reservoir out of which stars are born and into which stars inject newly created elements as they age. The physical properties of the interstellar medium are governed in part by the radiation emitted by these stars. Far-ultraviolet (6 eVϽh Ͻ13.6 eV) photons from massive stars dominate the heating and influence the chemistry of the neutral atomic gas and much of the molecular gas in galaxies. Predominantly neutral regions of the interstellar medium in which the heating and chemistry are regulated by far ultraviolet photons are termed PhotoDissociation Regions (PDRs). These regions are the origin of most of the non-stellar infrared (IR) and the millimeter and submillimeter CO emission from galaxies. The importance of PDRs has become increasingly apparent with advances in IR and submillimeter astronomy. The IR emission from PDRs includes fine structure lines of C, C ϩ , and O; rovibrational lines of H 2 ; rotational lines of CO; broad mid-IR features of polycyclic aromatic hydrocarbons; and a luminous underlying IR continuum from interstellar dust. The transition of H to H 2 and C ϩ to CO occurs within PDRs. Comparison of observations with theoretical models of PDRs enables one to determine the density and temperature structure, the elemental abundances, the level of ionization, and the radiation field. PDR models have been applied to interstellar clouds near massive stars, planetary nebulae, red giant outflows, photoevaporating planetary disks around newly formed stars, diffuse clouds, the neutral intercloud medium, and molecular clouds in the interstellar radiation field-in summary, much of the interstellar medium in galaxies. Theoretical PDR models explain the observed correlations of the [CII] 158 m with the CO Jϭ1 -0 emission, the CO Jϭ1 -0 luminosity with the interstellar molecular mass, and the [CII] 158 m plus [OI] 63 m luminosity with the IR continuum luminosity. On a more global scale, PDR models predict the existence of two stable neutral phases of the interstellar medium, elucidate the formation and destruction of star-forming molecular clouds, and suggest radiation-induced feedback mechanisms that may regulate star formation rates and the column density of gas through giant molecular clouds. [S0034-6861(99)01001-6] CONTENTS

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“…We have been able to demonstrate for the first time that a SNR has re-energized an old interstellar cavity as envisaged by Cox and Smith (1974). S.P., D.R., and J.F.V.…”

Section: " 30'mentioning

confidence: 60%

The Interaction of the Supernova Remnant VRO 42.05.01 with its HI Environment

Landecker¹,

Pineault²,

Routledge³

et al. 1988

International Astronomical Union Colloquium

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VRO 42.05.01 (G166.0+4.3) is a SNR which has broken into and re-energized an old i n t e r s t e l l a r c a v i t y . Observations of HI in a f i e l d containing the SNR show features associated with i t . An expanding shell of mass ~40 VQ is associated with the semi-circular shell of the SNR. The cavity, which the SNR has re-energized, is seen in the H I . A cloud of HI of mass ~25 M© has apparently been h i t by the shock and has been accelerated by the post-shock flow.

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Large-Scale Effects of Supernova Remnants on the Galaxy: Generation and Maintenance of a Hot Network of Tunnels

Cited by 422 publications

References 0 publications

The Lyman alpha reference sample

The Lyman alpha reference sample

Photodissociation regions in the interstellar medium of galaxies

The Interaction of the Supernova Remnant VRO 42.05.01 with its HI Environment

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