An H<i>α</i>survey aiming at the detection of extraplanar diffuse ionized gas in halos of edge-on spiral galaxies

Rossa, J.; Dettmar, R.‐J.

doi:10.1051/0004-6361:20030615

Cited by 121 publications

(168 citation statements)

References 49 publications

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“…Under that assumption, the most important properties of a galaxy for determining whether a halo is formed should be (1) the SF energy injection rate (per unit disk area; see e.g. Dahlem et al 1995;Rossa & Dettmar 2003); and (2) the gravitational potential (traced by v 2 rot ). With NGC 891's larger SFR, smaller disk area (at the distances listed in Table 1), and lower rotational velocity, it would seem that it should indeed be more efficient in maintaining a gaseous halo.…”

Section: Discussionmentioning

confidence: 99%

“…Star formation-driven disk-halo flows, as described by galactic fountain (e.g., Bregman 1980) or chimney (Norman & Ikeuchi 1989) models, are likely part of the explanation. The morphology of the extraplanar gas seems to be related to the properties of the underlying star forming disk (at least in its ionized phase; e.g., Rand 1996), and whether ionized gas is found in the halo or not seems to depend on the energy density provided by star formation (Rossa & Dettmar 2003).…”

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confidence: 99%

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The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey

Heald

Józsa

Serra

et al. 2011

A&A

200

239

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We introduce a new, very deep neutral hydrogen (H i) survey being performed with the Westerbork Synthesis Radio Telescope (WSRT). The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) Survey is producing an archive of some of the most sensitive H i observations available, on the angular scales which are most useful for studying faint, diffuse gas in and around nearby galaxies. The survey data are being used to perform careful modeling of the galaxies, characterizing their gas content, morphology, and kinematics, with the primary goal of revealing the global characteristics of cold gas accretion onto spiral galaxies in the local Universe. In this paper, we describe the survey sample selection, the data acquisition, reduction, and analysis, and present the data products obtained during our pilot program, which consists of UGC 2082, NGC 672, NGC 925, and NGC 4565. The observations reveal a first glimpse of the picture that the full HALOGAS project aims to illuminate: the properties of accreting H i in different types of spirals, and across a range of galactic environments. None of the pilot survey galaxies hosts an H i halo of the scale of NGC 891, but all show varying indications of halo gas features. We compare the properties of detected features in the pilot survey galaxies with their global characteristics, and discuss similarities and differences with NGC 891 and NGC 2403.

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Section: Discussionmentioning

confidence: 99%

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confidence: 99%

The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey

Heald

Józsa

Serra

et al. 2011

A&A

200

239

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“…This extraplanar ionized gas is thought to be due to star formation, and it is present in about 40% of 74 edge-on galaxies (Rossa & Dettmar 2003). It can be widely diffuse or take the shape of filaments, plumes, and bubbles (Rand 1997).…”

Section: Discussionmentioning

confidence: 99%

Dust and gas power spectrum in M 33 (HERM33ES)

Combes

Boquien

Krämer

et al. 2012

A&A

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Power spectra of deprojected images of late-type galaxies in gas or dust emission are very useful diagnostics of the dynamics and stability of their interstellar medium. Previous studies have shown that the power spectra can be approximated as two power laws, a shallow one on large scales (larger than 500 pc) and a steeper one on small scales, with the break between the two corresponding to the line-of-sight thickness of the galaxy disk. The break separates the 3D behavior of the interstellar medium on small scales, controlled by star formation and feedback, from the 2D behavior on large scales, driven by density waves in the disk. The break between these two regimes depends on the thickness of the plane, which is determined by the natural self-gravitating scale of the interstellar medium. We present a thorough analysis of the power spectra of the dust and gas emission at several wavelengths in the nearby galaxy M 33. In particular, we use the recently obtained images at five wavelengths by PACS and SPIRE onboard Herschel. The wide dynamical range (2-3 dex in scale) of most images allows us to clearly determine the change in slopes from −1.5 to −4, with some variations with wavelength. The break scale increases with wavelength from 100 pc at 24 and 100 μm to 350 pc at 500 μm, suggesting that the cool dust lies in a thicker disk than the warm dust, perhaps because of star formation that is more confined to the plane. The slope on small scales tends to be steeper at longer wavelength, meaning that the warmer dust is more concentrated in clumps. Numerical simulations of an isolated late-type galaxy, rich in gas and with no bulge, such as M 33, are carried out to better interpret these observed results. Varying the star formation and feedback parameters, it is possible to obtain a range of power spectra, with two power-law slopes and breaks, that nicely bracket the data. The small-scale power-law does indeed reflect the 3D behavior of the gas layer, steepening strongly while the feedback smoothes the structures by increasing the gas turbulence. M 33 appears to correspond to a fiducial model with an SFR of ∼0.7 M /yr, with 10% supernovae energy coupled to the gas kinematics.

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“…The presence of extraplanar H and/or radio emission, as well as extraplanar dust, is known to qualitatively correlate with this parameter (Rand 1996; see also Dettmar 1998;Howk & Savage 1999;Rossa & Dettmar 2000;Dahlem et al 2001). It underestimates the true SF intensity in starburst galaxies, as the SF is often much more concentrated than the old stellar light measured by D 25 .…”

Section: Star Formation Rates and Intensitiesmentioning

confidence: 99%

“…More progress on investigating the disk/halo interface in normal galaxies has been made at other wavelengths, primarily in the optical, where extraplanar H emission (e.g., Dettmar 1992;Rand 1996;Hoopes, Walterbos, & Rand 1999;Collins et al 2000;Rossa & Dettmar 2003;Miller & Veilleux 2003) and dust (Howk & Savage 1999) has been detected in a variety of nearby, normal spiral galaxies. These studies have shown that the presence of such tracers of disk/halo interaction increases with higher levels of star formation (SF) intensity in the underlying disk, but the mechanisms behind these phenomena, and their energetics, are still unclear.…”

Section: Introductionmentioning

confidence: 99%

A High Spatial Resolution X‐Ray and Hα Study of Hot Gas in the Halos of Star‐forming Disk Galaxies. II. Quantifying Supernova Feedback

Strickland

Heckman

Colbert

et al. 2004

ApJ

250

283

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We investigate how the empirical properties of hot X-ray-emitting gas in a sample of seven starburst and three normal edge-on spiral galaxies (a sample that covers the full range of star formation intensity found in disk galaxies) correlate with the size, mass, star formation rate, and star formation intensity in the host galaxies. From this analysis we investigate various aspects of mechanical energy ''feedback''-the return of energy to the interstellar medium from massive star supernovae and stellar winds-on galactic scales. The X-ray observations make use of the unprecedented spatial resolution of the Chandra X-Ray Observatory to remove X-ray emission from point sources more accurately than in any previous study and hence obtain the X-ray properties of the diffuse thermal emission alone. Intriguingly, the diffuse X-ray properties of the normal spirals (in both their disks and halos) fall where extrapolation of the trends from the starburst galaxies with superwinds would predict. We demonstrate, using a variety of multiwavelength star formation rate and intensity indicators, that the luminosity of diffuse X-ray emission in the disk (and, where detected, in the halo) is directly proportional to the rate of mechanical energy feedback from massive stars in the host galaxies. Accretion of gas from the intergalactic medium (IGM) does not appear to be a significant contributor to the diffuse X-ray emission in this sample. Nevertheless, with only three nonstarburst normal spiral galaxies it is hard to exclude an accretion-based origin for extraplanar diffuse X-ray emission around normal star-forming galaxies. Larger galaxies tend to have more extended X-ray-emitting halos, but galaxy mass appears to play no role in determining the properties of the disk or extraplanar X-ray-emitting plasma. The combination of these luminosity and size correlations leads to a correlation between the surface brightness of the diffuse X-ray emission and the mean star formation rate per unit area in the disk (calculated from the far-infrared luminosity and the optical size of the galaxy, L FIR =D 2 25 ). Further observational work of this form will allow empirical constraints to be made on the critical star formation rate per unit disk area necessary to blow hot gas out of the disk into the halo. We show that a minor generalization of standard superbubble theory directly predicts a critical star formation rate per unit area for superbubble blowout from the disk and by extension for superwinds to blow out of the gaseous halos of their host galaxy. At present there are a variety of poorly known parameters in this theory that complicate comparison between observation and theory, making it impossible to assess the quantitative accuracy of standard superbubble blowout theory. We argue that the crucial spatial region around a galaxy that controls whether gas in starburst-driven superwinds will escape into the IGM is not the outer halo $100 kpc from the host galaxy, but the inner few halo scale heights, within $20 kpc of the galaxy plan...

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An Hαsurvey aiming at the detection of extraplanar diffuse ionized gas in halos of edge-on spiral galaxies

Cited by 121 publications

References 49 publications

The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey

The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey

Dust and gas power spectrum in M 33 (HERM33ES)

A High Spatial Resolution X‐Ray and Hα Study of Hot Gas in the Halos of Star‐forming Disk Galaxies. II. Quantifying Supernova Feedback

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