8 research outputs found
CO(4-3) and dust emission in two powerful high-z radio galaxies, and CO lines at high redshifts
We report the detection of sub-mm emission from dust at 850 microns and of
the 12CO J=4-3 line in the two distant powerful radio galaxies 4C 60.07
(z=3.79) and 6C 1909+722 (z=3.53). In the case of 4C 60.07 the dust emission is
also detected at 1.25 mm. The estimated molecular gas masses are large, of the
order of ~(0.5-1)x10^{11} Solar. The large FIR luminosities (L_fir ~ 10^{13}
Solar) suggest that we are witnessing two major starburst phenomena, while the
observed large velocity widths (FWHM > 500 km/sec) are characteristic of
mergers. In the case of 4C 60.07 the CO emission extends over ~30 kpc and spans
a velocity range of >1000 km/sec. It consists of two distinct features with
FWHM of >= 550 km/sec and ~150 km/sec and line centers separated by >=700
km/sec The least massive of these components is probably very gas-rich with
potentially >=60% of its dynamical mass in the form of molecular gas. The
extraordinary morphology of the CO emission in this object suggests that it is
not just a scaled-up version of a local Ultra Luminous Infrared Galaxy, and it
may be a formative stage of the elliptical host of the residing radio-loud AGN.
Finally we briefly explore the effects of the wide range of gas excitation
conditions expected for starburst environments on the luminosity of high-J CO
lines. We conclude that in unlensed objects, CO (J+1-->J), J+1>3 lines can be
significantly weak with respect to CO J=1-0 and this can hinder their detection
even in the presence of substantial molecular gas masses.Comment: 34 pages, 5 figures, accepted for publication in The Astrophysical
Journa
Molecular gas in the Andromeda galaxy
We present a new 12CO(J=1-0)-line survey of the Andromeda galaxy, M31,
covering the bright disk with the highest resolution to date (85 pc along the
major axis), observed On-the-Fly (in italics) with the IRAM 30-m telescope. We
discuss the distribution of the CO emission and compare it with the
distributions of HI and emission from cold dust traced at 175mum. Our main
results are: 1. Most of the CO emission comes from the radial range R=3-16 kpc,
but peaks near R=10 kpc. The emission is con- centrated in narrow, arm-like
filaments defining two spiral arms with pitch angles of 7d-8d. The average
arm-interarm brightness ratio along the western arms reaches 20 compared to 4
for HI. 2. For a constant conversion factor Xco, the molecular fraction of the
neutral gas is enhanced in the arms and decreases radially. The apparent
gas-to-dust ratios N(HI)/I175 and (N(HI)+2N(H2))/I175 increase by a factor of
20 between the centre and R=14 kpc, whereas the ratio 2N(H2)/I175 only
increases by a factor of 4. Implications of these gradients are discussed. In
the range R=8-14 kpc total gas and cold dust are well correlated; molecular gas
is better correlated with cold dust than atomic gas.Comment: 21 pages, 16 figures. Accepted for publication in A&
The Pressure of an Equilibrium Interstellar Medium in Galactic Disks
Based on an axisymmetric galactic disk model, we estimate the equilibrium gas
pressure P/k in the disk plane as a function of the galactocentric distance R
for several galaxies (MW, M33, M51, M81, M100, M101, M106, and the SMC). For
this purpose, we solve a self-consistent system of equations by taking into
account the gas self-gravity and the presence of a dark pseudo-isothermal halo.
We assume that the turbulent velocity dispersions of the atomic and molecular
gases are fixed and that the velocity dispersion of the old stellar disk
corresponds to its marginal stability (except for the Galaxy and the SMC). We
also consider a model with a constant disk thickness. Of the listed galaxies,
the SMC and M51 have the highest pressure at a given relative radius R/R_25,
while M81 has the lowest pressure. The pressure dependence of the relative
molecular gas fraction confirms the existence of a positive correlation between
these quantities, but it is not so distinct as that obtained previously when
the pressure was estimated very roughly. This dependence breaks down for the
inner regions of M81 and M106, probably because the gas pressure has been
underestimated in the bulge region. We discuss the possible effects of factors
other than the pressure affecting the relative content of molecular gas in the
galaxies under consideration.Comment: 10 pages, 5 figure
Dynamics of Disks and Warps
This chapter reviews theoretical work on the stellar dynamics of galaxy
disks. All the known collective global instabilities are identified, and their
mechanisms described in terms of local wave mechanics. A detailed discussion of
warps and other bending waves is also given. The structure of bars in galaxies,
and their effect on galaxy evolution, is now reasonably well understood, but
there is still no convincing explanation for their origin and frequency. Spiral
patterns have long presented a special challenge, and ideas and recent
developments are reviewed. Other topics include scattering of disk stars and
the survival of thin disks.Comment: Chapter accepted to appear in Planets, Stars and Stellar Systems, vol
5, ed G. Gilmore. 32 pages, 17 figures. Includes minor corrections made in
proofs. Uses emulateapj.st