High-Velocity Clouds in the Nearby Spiral Galaxy M 83

Miller, Eric D.; Bregman, J. N.; Wakker, Bart P.

doi:10.1088/0004-637x/692/1/470

Cited by 70 publications

(104 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We do not follow the subsequent interaction between the cloud and the disc gas (see Bregman 2004 and references therein for a review on this subject). We consider a cloud entering the grid with a velocity v z =−150 km s −1 from the top boundary, with mass M = 3.5 × 10 6 M ⊙ , which is consistent with the estimate for Complex C (Miller, Bregman & Wakker 2009). We also assume T = 10 4 K and density n = 0.2 cm −3 .…”

Section: Interaction With Accreting Gassupporting

confidence: 64%

Hydrodynamical simulations of Galactic fountains - II. Evolution of multiple fountains

Melioli¹,

Brighenti²,

D’Ercole³

et al. 2009

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The ejection of gas out of the disc in late‐type galaxies is related to star formation and is mainly due to the explosion of Type II supernovae (SN II). In a previous paper, we considered the evolution of a single Galactic fountain, that is, a fountain powered by a single SN cluster. Using three‐dimensional hydrodynamical simulations, we studied in detail the fountain flow and its dependence with several factors, such as the Galactic rotation, the distance to the Galactic centre and the presence of a hot gaseous halo. As a natural followup, this paper investigates the dynamical evolution of multiple generations of fountains generated by ∼100 OB associations. We have considered the observed size–frequency distribution of young stellar clusters within the Galaxy in order to appropriately fuel the multiple fountains in our simulations. Most of the results of the previous paper have been confirmed, like for example the formation of intermediate velocity clouds above the disc by the multiple fountains. Also, this work confirms the localized nature of the fountain flows: the freshly ejected metals tend to fall back close to the same Galactocentric region where they are delivered. Therefore, the fountains do not change significantly the radial profile of the disc chemical abundance. The multiple fountain simulations also allowed us to consistently calculate the feedback of the star formation on the halo gas. We found that the hot gas gains about 10 per cent of all the SN II energy produced in the disc. Thus, the SN feedback more than compensate for the halo radiative losses and allow for a quasi steady‐state disc–halo circulation to exist. Finally, we have also considered the possibility of mass infall from the intergalactic medium and its interaction with the clouds that are formed by the fountains. Though our simulations are not suitable to reproduce the slow rotational pattern that is typically observed in the haloes around the disc galaxies, they indicate that the presence of an external gas infall may help to slow down the rotation of the gas in the clouds and thus the amount of angular momentum that they transfer to the coronal gas, as previously suggested in the literature.

show abstract

Section: Interaction With Accreting Gassupporting

confidence: 64%

Hydrodynamical simulations of Galactic fountains - II. Evolution of multiple fountains

Melioli¹,

Brighenti²,

D’Ercole³

et al. 2009

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Similar processes should operate in the nuclei of other galaxies, and may actually be more efficient in low-mass galaxies with no or low-mass central BHs (e.g. Miller & Lauburg 2009). Because of its proximity, the centre of the Milky Way is however the most interesting, observationally, at present.…”

Section: Introductionmentioning

confidence: 84%

Pulsar-black hole binaries in the Galactic Centre

Faucher-Giguère

Loeb

2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Binaries consisting of a pulsar and a black hole (BH) are a holy grail of astrophysics, both for their significance for stellar evolution and for their potential application as probes of strong gravity. In spite of extensive surveys of our Galaxy and its system of globular clusters, no pulsar–black hole (PSR–BH) binary has been found to date. Clues as to where such systems might exist are therefore important. We show that if the central parsec around Sgr A★ harbours a cluster of ∼25 000 stellar BHs (as predicted by mass‐segregation arguments) and if it is also rich in recycled pulsar binaries (by analogy with globular clusters), then three‐body exchange interactions should produce PSR–BHs in the Galactic Centre. Simple estimates of the formation rate and survival time of these binaries suggest that a few PSR–BHs should be present in the central parsec today. The proposed formation mechanism makes unique predictions for the PSR–BH properties: (1) the binary would reside within ∼1 pc of Sgr A★; (2) the pulsar would be recycled, with a period of ∼1 to a few tens of milliseconds, and a low magnetic field B≲ 1010 G; (3) the binary would have high eccentricity, e∼ 0.8, but with a large scatter and (4) the binary would be relatively wide, with semimajor axis ab∼ 0.1 −≳3 au. The potential discovery of a PSR–BH binary therefore provides a strong motivation for deep, high‐frequency radio searches for recycled pulsars towards the Galactic Centre.

show abstract

“…Two Suprime-Cam fields cover the entire XUV disk of M83, i.e., the whole area with an H i surface density above 1.5 × 10 20 cm −2 (roughly the detection limit in Miller et al 2009) and a large surrounding area. Figure 1 shows the area coverage and the H i contour (red) on a GALEX FUV image.…”

Section: Subarumentioning

confidence: 99%

The Universal Initial Mass Function in the Extended Ultraviolet Disk of M83

Koda

Yagi

Boissier

et al. 2012

ApJ

View full text Add to dashboard Cite

We report deep Subaru Hα observations of the extended ultraviolet (XUV) disk of M83. These new observations enable the first complete census of very young stellar clusters over the entire XUV disk. Combining Subaru and Galaxy Evolution Explorer data with a stellar population synthesis model, we find that (1) the standard, but stochastically sampled, initial mass function (IMF) is preferred over the truncated IMF because there are low-mass stellar clusters (10 2-3 M ) that host massive O-type stars; (2) the standard Salpeter IMF and a simple aging effect explain the counts of far-UV (FUV)-bright and Hα-bright clusters with masses >10 3 M ; and (3) the Hα-to-FUV flux ratio over the XUV disk supports the standard IMF. To reach conclusion (2), we assumed instantaneous cluster formation and a constant cluster formation rate over the XUV disk. The Subaru Prime Focus Camera covers a large area even outside the XUV disk-far beyond the detection limit of the H i gas. This enables us to statistically separate the stellar clusters in the disk from background contamination. The new data, model, and previous spectroscopic studies provide overall consistent results with respect to the internal dust extinction (A V ∼ 0.1 mag) and low metallicity (∼0.2 Z ) using the dust extinction curve of the Small Magellanic Cloud. The minimum cluster mass for avoiding the upper IMF incompleteness due to stochastic sampling and the spectral energy distributions of O, B, and A stars are discussed in the Appendices.

show abstract

High-Velocity Clouds in the Nearby Spiral Galaxy M 83

Cited by 70 publications

References 66 publications

Hydrodynamical simulations of Galactic fountains - II. Evolution of multiple fountains

Hydrodynamical simulations of Galactic fountains - II. Evolution of multiple fountains

Pulsar-black hole binaries in the Galactic Centre

The Universal Initial Mass Function in the Extended Ultraviolet Disk of M83

Contact Info

Product

Resources

About