1,780 research outputs found
Probing Cool and Warm Infrared Galaxies using Photometric and Structural Measures
We have analyzed a sample of nearby cool and warm infrared (IR) galaxies
using photometric and structural parameters. The set of measures include
far-infrared color (), total IR
luminosity (), radio surface brightness as well as radio,
near-infrared, and optical sizes. In a given luminosity range cool and warm
galaxies are considered as those sources that are found approximately below and above the mean color in the far-infrared
diagram. We find that galaxy radio surface brightness is well correlated with
color whereas size is less well correlated with color. Our analysis indicates
that IR galaxies that are dominated by cool dust are large, massive spirals
that are not strongly interacting or merging and presumably the ones with the
least active star formation. Dust in these cool objects is less centrally
concentrated than in the more typical luminous and ultra-luminous IR galaxies
that are dominated by warm dust. Our study also shows that low luminosity early
type unbarred and transitional spirals are responsible for the large scatter in
the diagram. Among highly luminous galaxies, late type unbarred
spirals are predominately warm, and early type unbarred and barred are
systematically cooler. We highlight the significance of diagram
in terms of local and high redshifts sub-millimeter galaxies.Comment: Accepted for publication in ApJ, 2006, 23 pages, 3 postscript
figures, 1 table. The table can be obtained on request from the author
The Influence of Bars on Nuclear Activity
We test ideas on fueling of galactic nuclei by bar-driven inflow by comparing
the detection rate and intensity of nuclear H II regions and AGNs among barred
and unbarred galaxies in a sample of over 300 spirals selected from our recent
optical spectroscopic survey of nearby galaxies. Among late-type spirals
(Sc-Sm), but not early-type (S0/a-Sbc), we observe in the barred group a very
marginal increase in the detection rate of H II nuclei and a corresponding
decrease in the incidence of AGNs. The minor differences in the detection
rates, however, are statistically insignificant, most likely stemming from
selection effects and not from a genuine influence from the bar. The presence
of a bar seems to have no noticeable impact on the likelihood of a galaxy to
host either nuclear star formation or an AGN. The nuclei of early-type barred
spirals do exhibit measurably higher star-formation rates than their unbarred
counterparts, as indicated by either the luminosity or the equivalent width of
H-alpha emission. By contrast, late-type spirals do not show such an effect.
Bars have a negligible effect on the strength of the AGNs in our sample,
regardless of the Hubble type of the host galaxy. This result confirms similar
conclusions reached by other studies based on much smaller samples.Comment: To appear in the Astrophysical Journal. LaTex, 31 pages including 6
postscript figures and 3 tables. AAStex macros include
A census of X-ray nuclear activity in nearby galaxies
We have studied the X-ray nuclear activity of 187 nearby (distance < 15 Mpc)
galaxies observed with Chandra/ACIS. We found that 86 of them have a point-like
X-ray core, consistent with an accreting black hole (BH). We argue that the
majority of them are nuclear BHs, rather than X-ray binaries. The fraction of
galaxies with an X-ray detected nuclear BH is higher (~60 per cent) for
ellipticals and early-type spirals (E to Sb), and lower (~30 per cent) for
late-type spirals (Sc to Sm). There is no preferential association of X-ray
cores with a large-scale bar; in fact, strongly barred galaxies appear to have
slightly lower detection fraction and luminosity for their nuclear X-ray
sources, compared with non-barred or weakly barred galaxies of similar Hubble
types. The cumulative luminosity distribution of the nuclear sources in the
0.3-8 keV band is a power-law with slope ~-0.5, from ~2 x 10^{38} erg/s to
~10^{42} erg/s. The Eddington ratio is lower for ellipticals (L_{X}/L_{Edd} ~
10^{-8}) and higher for late-type spirals (up to L_{X}/L_{Edd} ~ 10^{-4}), but
in all cases, the accretion rate is low enough to be in the
radiatively-inefficient regime. The intrinsic NH is generally low, especially
for the less luminous sources: there appear to be no Type-2 nuclear BHs at
luminosities <~ 10^{39} erg/s. The lack of a dusty torus or of other sources of
intrinsic absorption (e.g., an optically-thick disk wind) may be directly
related to the lack of a standard accretion disk around those faint nuclear
BHs. The fraction of obscured sources increases with the nuclear BH luminosity:
2/3 of the sources with L_{X} > 10^{40} erg/s have a fitted NH > 10^{22}
cm^{-2}. This is contrary to the declining trend of the obscured fraction with
increasing luminosities, observed in more luminous AGN and quasars.Comment: 27 pages, 353 kB, accepted by Ap
The Integrated Polarization of Spiral Galaxy Disks
We present integrated polarization properties of nearby spiral galaxies at
4.8 GHz, and models for the integrated polarization of spiral galaxy disks as a
function of inclination. Spiral galaxies in our sample have observed integrated
fractional polarization in the range < 1% to 17.6%. At inclinations less than
50 degrees, the fractional polarization depends mostly on the ratio of random
to regular magnetic field strength. At higher inclinations, Faraday
depolarization associated with the regular magnetic field becomes more
important. The observed degree of polarization is lower (<4%) for more luminous
galaxies, in particular those with L_{4.8} > 2 x 10^{21} W/Hz. The polarization
angle of the integrated emission is aligned with the apparent minor axis of the
disk for galaxies without a bar. In our axially symmetric models, the
polarization angle of the integrated emission is independent of wavelength.
Simulated distributions of fractional polarization for randomly oriented spiral
galaxies at 4.8 GHz and 1.4 GHz are presented. We conclude that polarization
measurements, e.g. with the SKA, of unresolved spiral galaxies allow
statistical studies of the magnetic field in disk galaxies using large samples
in the local universe and at high redshift. As these galaxies behave as
idealized background sources without internal Faraday rotation, they can be
used to detect large-scale magnetic fields in the intergalactic medium.Comment: 13 pages, 6 figures; Accepted for publication in The Astrophysical
Journa
Rotation Curves of Spiral Galaxies
Rotation curves of spiral galaxies are the major tool for determining the
distribution of mass in spiral galaxies. They provide fundamental information
for understanding the dynamics, evolution and formation of spiral galaxies. We
describe various methods to derive rotation curves, and review the results
obtained. We discuss the basic characteristics of observed rotation curves in
relation to various galaxy properties, such as Hubble type, structure,
activity, and environment.Comment: 40 pages, 6 gif figures; Ann. Rev. Astron. Astrophys. Vol. 39, p.137,
200
Non-linear Dependence of L(B) on L(FIR) and M(H2) among Spiral Galaxies and Effects of Tidal Interaction
Through the study of a carefully selected sample of isolated spiral galaxies,
we have established that two important global physical quantities for tracing
star forming activities, L(FIR) and M(H2), have non-linear dependence on
another commonly cited global quantity L(B). Furthermore we show that simple
power law relations can effectively describe these non-linear relations for
spiral galaxies spanning four orders of magnitude in FIR and M(H2) and nearly
three orders of magnitude in L(B). While the existence of non-linear dependence
of M(H2) (assuming a constant CO-to-H2 conversion) and L(FIR) on optical
luminosity L(B) has been previously noted in the literature, an improper
normalization of simple scaling by L(B) has been commonly used in many previous
studies to claim enhanced molecular gas content and induced activities among
tidally interacting and other types of galaxies. We remove these non-linear
effects using the template relations derived from the isolated galaxy sample
and conclude that strongly interacting galaxies do not have enhanced molecular
gas content, contrary to previous claims. With these non-linear relations among
L(B), L(FIR) and M(H2) properly taken into account, we confirm again that the
FIR emission and the star formation efficiency L(FIR)/M(H2) are indeed enhanced
by tidal interactions. Virgo galaxies show the same level of M(H2) and L(FIR)
as isolated galaxies. We do not find any evidence for enhanced star forming
activity among barred galaxies.Comment: 19 pages and 5 figures, requires AAS style files, ApJ, accepte
Molecular Gas, Dust and Star Formation in the Barred Spiral NGC 5383
We present multi-wavelength (interferometer and single-dish CO J=1-0, Halpha,
broadband optical and near-infrared) observations of the classic barred spiral
NGC 5383. We compare the observed central gas and dust morphology to the
predictions of recent hydrodynamic simulations. In the nuclear region, our
observations reveal three peaks lying along a S-shaped gas and dust
distribution. In contrast, the model predicts a circumnuclear ring, not the
observed S-shaped distribution; moreover, the predicted surface density
contrast between the central gas accumulation and the bar dust lanes is an
order of magnitude larger than observed. The discrepancies are not due to
unexplored model parameter space or a nuclear bar but are probably due to the
vigorous (7 solar masses per year) star formation activity in the center.
As is common in similar bars, the star formation rate in the bar between the
bar ends and the central region is low (~0.5 solar masses per yr), despite the
high gas column density in the bar dust lanes; this is generally attributed to
shear and shocks. We note a tendency for the HII regions to be associated with
the spurs feeding the main bar dust lanes, but these are located on the leading
side of the bar. We propose that stars form in the spurs, which provide a high
column density but low shear environment. HII regions can therefore be found
even on the leading side of the bar because the ionizing stars pass
ballistically through the dust laneComment: Accepted for publication in The Astrophysical Journal, 33 pages
(includes 10 figures
- âŠ