1,671 research outputs found
The Physical Parameters of the Micro-quasar S26 in the Sculptor Group Galaxy NGC 7793
NGC 7793 - S26 is an extended source (350 pc 185 pc) previously
studied in the radio, optical and x-ray domains. It has been identified as a
micro-quasar which has inflated a super bubble. We used Integral Field Spectra
from the Wide Field Spectrograph on the ANU 2.3 m telescope to analyse spectra
between 3600--7000 \AA. This allowed us to derive fluxes and line ratios for
selected nebular lines. Applying radiative shock model diagnostics, we estimate
shock velocities, densities, radiative ages and pressures across the object. We
show that S26 is just entering its radiative phase, and that the northern and
western regions are dominated by partially-radiative shocks due to a lower
density ISM in these directions. We determine a velocity of expansion along the
jet of 330 km s, and a velocity of expansion of the bubble in the minor
axis direction of 132 km s. We determine the age of the structure to be
yr, and the jet energy flux to be erg
s The jet appears to be collimated within deg, and to undergo
very little precession. If the relativistic , then some 4
M of relativistic matter has already been processed through the jet.
We conclude that the central object in S26 is probably a Black Hole with a mass
typical of the ultra-luminous X-ray source population which is currently
consuming a fairly massive companion through Roche Lobe accretion.Comment: Accepted for publication in MNRAS; 12 pages, 7 figures and 3 table
Galaxy-Wide Shocks in Late-Merger Stage Luminous Infrared Galaxies
We present an integral field spectroscopic study of two nearby Luminous
Infrared Galaxies (LIRGs) that exhibit evidence of widespread shock excitation
induced by ongoing merger activity, IC 1623 and NGC 3256. We show the
importance of carefully separating excitation due to shocks vs. excitation by
HII regions and the usefulness of IFU data in interpreting the complex
processes in LIRGs. Our analysis focuses primarily on the emission line gas
which is extensive in both systems and is a result of the abundant ongoing star
formation as well as widespread LINER-like excitation from shocks. We use
emission-line ratio maps, line kinematics, line-ratio diagnostics and new
models as methods for distinguishing and analyzing shocked gas in these
systems. We discuss how our results inform the merger sequence associated with
local U/LIRGs and the impact that widespread shock excitation has on the
interpretation of emission-line spectra and derived quantities of both local
and high-redshift galaxies.Comment: 14 pages, 11 figures, Accepted to Ap
The Infrared Emission from the Narrow Line Region
We present models for the mid- and far- infrared emission from the Narrow
Line Region (NLR) of Active Galactic Nuclei (AGN). Using the MAPPINGS III code
we explore the effect of typical NLR parameters on the spectral characteristics
of the IR emission. These include useful IR emission line ratio diagnostic
diagrams for the determination of these parameters, as well as Star
formation--AGN mixing diagnostics. We also examine emission line to continuum
correlations which would assist in separating the IR emission arising from the
NLR from that coming from the inner torus. We find for AGN like NGC 1068 and
NGC 4151 that the NLR only contributes ~10% to the total IRAS 25 mum flux, and
that other components such as a dusty torus are necessary to explain the total
AGN IR emission.Comment: 15 pages, 12 figures, accepted for publication in A&A. Paper with
full resolution figures available at
http://www.mpa-garching.mpg.de/~brent/publications/bgrovesnlrIRpaper.pd
The Physical Conditions in Starbursts Derived from Bayesian Fitting of Mid-IR SEDS: 30 Doradus as a Template
To understand and interpret the observed Spectral Energy Distributions (SEDs)
of starbursts, theoretical or semi-empirical SED models are necessary. Yet,
while they are well-founded in theory, independent verification and calibration
of these models, including the exploration of possible degeneracies between
their parameters, are rarely made. As a consequence, a robust fitting method
that leads to unique and reproducible results has been lacking. Here we
introduce a novel approach based on Bayesian analysis to fit the Spitzer-IRS
spectra of starbursts using the SED models proposed by Groves et al. (2008). We
demonstrate its capabilities and verify the agreement between the derived best
fit parameters and actual physical conditions by modelling the nearby,
well-studied, giant HII region 30 Dor in the LMC. The derived physical
parameters, such as cluster mass, cluster age, ISM pressure and covering
fraction of photodissociation regions, are representative of the 30 Dor region.
The inclusion of the emission lines in the modelling is crucial to break
degeneracies. We investigate the limitations and uncertainties by modelling
sub-regions, which are dominated by single components, within 30 Dor. A
remarkable result for 30 Doradus in particular is a considerable contribution
to its mid-infrared spectrum from hot ({\simeq} 300K) dust. The demonstrated
success of our approach will allow us to derive the physical conditions in more
distant, spatially unresolved starbursts.Comment: 17 pages, 10 figures. Accepted por publication in the Astrophysical
Journa
Local Analogs for High-redshift Galaxies: Resembling the Physical Conditions of the Interstellar Medium in High-redshift Galaxies
We present a sample of local analogs for high-redshift galaxies selected in
the Sloan Digital Sky Survey (SDSS). The physical conditions of the
interstellar medium (ISM) in these local analogs resemble those in
high-redshift galaxies. These galaxies are selected based on their positions in
the [OIII]/H versus [NII]/H nebular emission-line diagnostic
diagram. We show that these local analogs share similar physical properties
with high-redshift galaxies, including high specific star formation rates
(sSFRs), flat UV continuums and compact galaxy sizes. In particular, the
ionization parameters and electron densities in these analogs are comparable to
those in galaxies, but higher than those in normal SDSS galaxies
by 0.6~dex and 0.9~dex, respectively. The mass-metallicity
relation (MZR) in these local analogs shows ~dex offset from that in SDSS
star-forming galaxies at the low mass end, which is consistent with the MZR of
the galaxies. We compare the local analogs in this study with those
in other studies, including Lyman break analogs (LBA) and green pea (GP)
galaxies. The analogs in this study share a similar star formation surface
density with LBAs, but the ionization parameters and electron densities in our
analogs are higher than those in LBAs by factors of 1.5 and 3, respectively.
The analogs in this study have comparable ionization parameter and electron
density to the GP galaxies, but our method can select galaxies in a wider
redshift range. We find the high sSFR and SFR surface density can increase the
electron density and ionization parameters, but still cannot fully explain the
difference in ISM condition between nearby galaxies and the local
analogs/high-redshift galaxies.Comment: 13 pages, 11 figures, accepted by Ap
On Radiation Pressure in Static, Dusty HII Regions
Radiation pressure acting on gas and dust causes HII regions to have central
densities that are lower than the density near the ionized boundary. HII
regions in static equilibrium comprise a family of similarity solutions,
parametrized by 3 parameters: beta, gamma, and the product (Q_0 n_rms); beta
characterizes the stellar spectrum, gamma characterizes the dust/gas ratio, Q_0
is the ionizing output from the star (photons/s), and n_rms is the rms density
within the ionized region. Adopting standard values for beta and gamma, varying
(Q_0 n_rms) generates a one-parameter family of density profiles, ranging from
nearly uniform density (small Q_0 n_rms), to hollow-sphere HII regions (large
Q_0 n_rms). When (Q_0 n_rms) exceeds 10^{52} cm^{-3} s^{-1}, dusty HII regions
have conspicuous central cavities, even if no stellar wind is present. For
given beta, gamma and (Q_0 n_rms), a fourth quantity, which can be Q_0,
determines the overall size and density of the HII region. Examples of density
and emissivity profiles are given. We show how quantities of interest -- such
as the peak-to-center emissivity ratio, the rms-to-mean density ratio, the
edge-to-rms density ratio, and the fraction of the ionizing photons absorbed by
the gas -- depend on the 3 parameters beta, gamma, and (Q_0 n_rms). For dusty
HII regions, compression of the gas and dust into an ionized shell results in a
substantial increase in the fraction of the >13.6 eV photons that actually
ionize H (relative to a uniform density HII region with the same dust/gas ratio
and density n=n_rms). We discuss the extent to which radial drift of dust
grains in HII regions can alter the dust-to-gas ratio. The applicability of
these solutions to real HII regions is discussed.Comment: New material and figures that were not in version 1. To appear in Ap
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