An X-Ray and Optical Study of the Dwarf Galaxy NGC 1569: Evidence for a Starburst-driven Outflow

Heckman, Timothy M.; Dahlem, M.; Lehnert, M. D.; Fabbiano, G.; Gilmore, Diane; Waller, William H.

doi:10.1086/175944

Cited by 156 publications

(219 citation statements)

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“…More information on other dwarf and irregular galaxies, including, e.g., NGC 1569, NGC 1705, NGC 4449, and NGC 5253, can be found for example in Heckman et al (1995); Bomans et al (1997); Meurer et al (1992); Marlowe et al (1995); Hunter and Gallagher (1997), and references therein.…”

Section: Irregular Galaxiesmentioning

confidence: 99%

Gaseous Halos of Late-Type Spiral Galaxies

Dahlem¹

1997

PASP

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ABSTRACT. This article reviews the most recent observational results on disk-halo interactions in nearby galaxies. The implications of these results on our understanding of the structure of the interstellar medium (ISM) in our Galaxy and external spiral galaxies, with particular emphasis on the halo ISM, are discussed. Disk-halo interactions occur only above the brightest HII regions, which are found almost exclusively in late-type spirals and dwarf and irregular galaxies. Circumnuclear starbursts are the most energetic flavor of this phenomenon. The existence, the shapes, and the properties of gaseous halos depend on the level of energy input into the disk ISM per unit surface area, i.e., on the feedback of mass, momentum, and energy produced by vigorous star formation. Thus, current theoretical models of the ISM take into account that gaseous halos are natural extensions of disk ISMs and are heated by the winds and ionizing radiation of massive stars, and by the shock waves of Supernovae and their remnants. Observationally, this is reflected by the fact that all phases of the ISM known to exist in galaxy disks have also been detected in halos. Disk-halo interactions are a very effective way of redistributing energy, metals, and magnetic fields in galaxies and of expelling them into intergalactic space when outflows reach escape velocity. MOTIVATION AND OUTLINESpiral galaxies consist of three spatially and dynamically dinstinct components, namely bulge, disk, and halo. Of these, the central bulge consists primarily of old stars and has a low gas fraction. The disk and halo consist of stars plus gas, dust, and in many cases "dark matter." Here I want to concentrate on the interstellar medium (ISM) in the disks and halos of galaxies, with emphasis on late-type spirals. Massive dark halos will not be described (see, e.g., Ashman 1992; Holt and Bennett 1995). In the current context "latetype" stands for disk-dominated spirals with rather inconspicuous bulges (Hubble types Sb -Sdm). The ISM of elliptical galaxies and early-type spirals (S0-Sab) will also not be presented here (cf. Walsh et al. 1989;and Fabbiano 1989).Studies of the ISM contribute significantly to our understanding of the structure, kinematics, and evolution of galaxies. The level of star formation (SF), its spatial distribution, and its temporal changes depend strongly on the properties of the interstellar gas from which stars can form. Stars feed energy and metal-enriched matter back into the ambient medium via stellar winds and supernovae (SNe), thereby distributing processed material throughout the ISM. Hence, through this gas-star-gas cycle, the ISM becomes a mediator of SF.In Sec. 2, the different phases of the ISM in galaxies will be introduced, and Sec. 3 presents observations of the ISM in the Milky Way. Section 4 will show that the Galactic ISM is l A\\ correspondence should be directed to this address. not confined to the thin disk, but extends to high distances (z) above the plane, forming a gaseous halo. However, being located within the...

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Section: Irregular Galaxiesmentioning

confidence: 99%

Gaseous Halos of Late-Type Spiral Galaxies

Dahlem¹

1997

PASP

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“…Their winds and supernova (SN) ejecta stir and inject energy into the surrounding ISM. In the most extreme starbursts, the combined effects of a starburst drive large-scale galactic winds (e.g., in M82; Shopbell & Bland-Hawthorn 1998) that can eject matter into the intergalactic medium (especially in dwarf galaxies, e.g., NGC 1569; Heckman et al 1995). SSCs are concentrated power sources for feedback on both star cluster and galactic scales.…”

Section: Introductionmentioning

confidence: 99%

Feedback in the Antennae Galaxies (NGC 4038/9). I. High‐Resolution Infrared Spectroscopy of Winds from Super Star Clusters

Gilbert

Graham

2007

ApJ

103

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We present high-resolution (R $ 24;600) near-IR spectroscopy of the youngest super star clusters (SSCs) in the prototypical starburst merger, the Antennae galaxies. These SSCs are young (3Y7 Myr old) and massive (10 5 Y10 7 M for a Kroupa initial mass function), and their spectra are characterized by broad, extended Brackett (Br ) emission, so we refer to them as emission-line clusters (ELCs) to distinguish them from older SSCs. The Br lines of most ELCs have supersonic widths (60Y110 km s À1 FWHM) and non-Gaussian wings whose velocities exceed the clusters' escape velocities. This high-velocity unbound gas is flowing out in winds that are powered by the clusters' massive O and Wolf-Rayet stars over the course of at least several crossing times. The large sizes of some ELCs relative to those of older SSCs may be due to expansion caused by these outflows; many of the ELCs may not survive as bound stellar systems, but rather dissipate rapidly into the field population. The observed tendency of older ELCs to be more compact than young ones is consistent with the preferential survival of the most concentrated clusters at a given age.

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“…More specifically, we required that F(Hβ) > 10 −14 erg s −1 cm −2 and F( [OIII]) > 10 −13 erg s −1 cm −2 in order to provide high signal-to-noise (S/N) NIR spectra, see also Heckman et al (1995) and González Delgado et al (2001).…”

Section: Sample Selectionmentioning

confidence: 99%

Near-infrared long-slit spectra of Seyfert galaxies: gas excitation across the central kiloparsec

Laan

Schinnerer

Armus

2013

A&A

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Context. The excitation of the gas phase of the interstellar medium can be driven by various mechanisms. In galaxies with an active nucleus, such as Seyfert galaxies, both radiative and mechanical energy from the central black hole, or the stars in the disk surrounding it may play a role. Aims. We investigate the relative importance and range of influence of the active galactic nucleus for the excitation of ionized and molecular gas in the central kiloparsec of its host galaxy. Methods. We present H-and K-band long-slit spectra for a sample of 21 nearby (D < 70 Mpc) Seyfert galaxies obtained with the NIRSPEC instrument on the Keck telescope. For each galaxy, we fit the nebular line emission, stellar continua, and warm molecular gas as a function of distance from the nucleus. Results. Our analysis does not reveal a clear difference between the nucleus proper and off-nuclear environment in terms of excitation mechanisms, suggesting that the influence of an AGN reaches far into the disk of the host galaxy. The radial variations in emission line ratios indicate that, while local mechanisms do affect the gas excitation, they are often averaged out when measuring over extended regions.

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An X-Ray and Optical Study of the Dwarf Galaxy NGC 1569: Evidence for a Starburst-driven Outflow

Cited by 156 publications

References 0 publications

Gaseous Halos of Late-Type Spiral Galaxies

Gaseous Halos of Late-Type Spiral Galaxies

Feedback in the Antennae Galaxies (NGC 4038/9). I. High‐Resolution Infrared Spectroscopy of Winds from Super Star Clusters

Near-infrared long-slit spectra of Seyfert galaxies: gas excitation across the central kiloparsec

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