139 research outputs found
Perspectives on Interstellar Dust Inside and Outside of the Heliosphere
Measurements by dust detectors on interplanetary spacecraft appear to
indicate a substantial flux of interstellar particles with masses exceeding
10^{-12}gram. The reported abundance of these massive grains cannot be typical
of interstellar gas: it is incompatible with both interstellar elemental
abundances and the observed extinction properties of the interstellar dust
population. We discuss the likelihood that the Solar System is by chance
located near an unusual concentration of massive grains and conclude that this
is unlikely, unless dynamical processes in the ISM are responsible for such
concentrations. Radiation pressure might conceivably drive large grains into
"magnetic valleys". If the influx direction of interstellar gas and dust is
varying on a ~10 yr timescale, as suggested by some observations, this would
have dramatic implications for the small-scale structure of the interstellar
medium.Comment: 13 pages. To appear in Space Science Review
Spitzer Observations of Cold Dust Galaxies
We combine new Spitzer Space Telescope observations in the mid- and
far-infrared with SCUBA 850 micron observations to improve the measurement of
dust temperatures, masses and luminosities for 11 galaxies of the SCUBA Local
Universe Galaxy Survey (SLUGS). By fitting dust models we measure typical dust
masses of 10E7.9 M_sol and dust luminosities of ~ 10E10 L_sol, for galaxies
with modest star formation rates. The data presented in this paper combined
with previous observations show that cold dust is present in all types of
spiral galaxies and is a major contributor to their total luminosity. Because
of the lower dust temperature of the SCUBA sources measured in this paper, they
have flatter Far-IR nu F_nu(160um)/nu F_nu(850um) slopes than the larger
Spitzer Nearby Galaxies Survey (SINGS), the sample that provides the best
measurements of the dust properties of galaxies in the nearby universe. The new
data presented here added to SINGS extend the parameter space that is well
covered by local galaxies, providing a comprehensive set of templates that can
be used to interpret the observations of nearby and distant galaxies.Comment: Accepted by A.J. 16 pages, 10 figures, 7 tables. High resolution
version at http://mips.as.arizona.edu/~cnaw/slugs_hires.pd
Interstellar extinction and polarization -- A spheroidal dust grain approach perspective
We extend and investigate the spheroidal model of interstellar dust grains
used to simultaneously interpret the observed interstellar extinction and
polarization curves. We compare our model with similar models recently
suggested by other authors, study its properties and apply it to fit the
normalized extinction and the polarizing efficiency
measured in the near IR to far UV region for several
stars seen through one large cloud. We conclude that the model parameter
being the angle between the line of sight and the magnetic field
direction can be more or less reliably determined from comparison of the theory
and observations. This opens a way to study the spatial structure of
interstellar magnetic fields by using multi-wavelength photometric and
polarimetric observations.Comment: 11 pages, 4 figures and 4 tables, To appear in MNRAS (added
Interstellar polarization and grain alignment: the role of iron and silicon
We compiled the polarimetric data for a sample of lines of sight with known
abundances of Mg, Si, and Fe. We correlated the degree of interstellar
polarization and polarization efficiency (the ratio of to the colour
excess or extinction ) with dust phase abundances. We detect an
anticorrelation between and the dust phase abundance of iron in non
silicate - containing grains ]_\rm d, a correlation
between and the abundance of Si, and no correlation between or
and dust phase abundances. These findings can be explained if mainly
the silicate grains aligned by the radiative mechanism are responsible for the
observed interstellar linear polarization.Comment: Accepted for publication in Astronomy and Astrophysic
Photoelectric Emission from Interstellar Dust: Grain Charging and Gas Heating
We model the photoelectric emission from and charging of interstellar dust
and obtain photoelectric gas heating efficiencies as a function of grain size
and the relevant ambient conditions. Using realistic grain size distributions,
we evaluate the net gas heating rate for various interstellar environments, and
find less heating for dense regions characterized by R_V=5.5 than for diffuse
regions with R_V=3.1. We provide fitting functions which reproduce our
numerical results for photoelectric heating and recombination cooling for a
wide range of interstellar conditions. In a separate paper we will examine the
implications of these results for the thermal structure of the interstellar
medium. Finally, we investigate the potential importance of photoelectric
heating in H II regions, including the warm ionized medium. We find that
photoelectric heating could be comparable to or exceed heating due to
photoionization of H for high ratios of the radiation intensity to the gas
density. We also find that photoelectric heating by dust can account for the
observed variation of temperature with distance from the galactic midplane in
the warm ionized medium.Comment: 50 pages, including 18 figures; corrected title and abstract field
AKARI's infrared view on nearby stars : Using AKARI Infrared Camera All-Sky Survey, 2MASS, and Hipparcos catalog
--Results-- We found that the (B-V) v.s. (V-S9W) color-color diagram is
useful to identify the stars with infrared excess emerged from circumstellar
envelopes/disks. Be stars with infrared excess are well separated from other
types of stars in this diagram. Whereas (J-L18W) v.s. (S9W-L18W) diagram is a
powerful tool to classify several object-types. Carbon-rich asymptotic giant
branch (AGB) stars and OH/IR stars form distinct sequences in this color-color
diagram. Young stellar objects (YSOs), pre-main sequence (PMS) stars, post-AGB
stars and planetary nebulae (PNe) have largest mid-infrared color-excess, and
can be identified in infrared catalog. Finally, we plot L18W v.s. (S9W-L18W)
color-magnitude diagram, using the AKARI data together with Hipparcos
parallaxes. This diagram can be used to identify low-mass YSOs, as well as AGB
stars. We found that this diagram is comparable to the [24] vs ([8.0]-[24])
diagram of Large Magellanic Cloud sources using the Spitzer Space Telescope
data. Our understanding of Galactic objects will be used to interpret
color-magnitude diagram of stellar populations in nearby galaxies which Spitzer
Space Telescope has observed. --Conclusions-- Our study of the AKARI
color-color and color-magnitude will be used to explore properties of unknown
objects in future. In addition, our analysis highlights a future key project to
understand stellar evolution with circumstellar envelope, once the forthcoming
astronometrical data with GAIA are available.Comment: 14 pages, 11 figures, accepted for publication in A&A. High
resolution version is available at:
http://www.ir.isas.jaxa.jp/%7Eyita/allsky20100302.pdf (26Mb
Mid-infrared spectral evidence for a luminous dust enshrouded source in Arp220
We have re-analyzed the 6-12 micron ISO spectrum of the ultra-luminous
infrared galaxy Arp220 with the conclusion that it is not consistent with that
of a scaled up version of a typical starburst. Instead, both template fitting
with spectra of the galaxies NGC4418 and M83 and with dust models suggest that
it is best represented by combinations of a typical starburst component,
exhibiting PAH emission features, and a heavily absorbed dust continuum which
contributes ~40% of the 6-12 micron flux and likely dominates the luminosity.
Of particular significance relative to previous studies of Arp220 is the fact
that the emission feature at 7.7 micron comprises both PAH emission and a
broader component resulting from ice and silicate absorption against a heavily
absorbed continuum. Extinction to the PAH emitting source, however, appears to
be relatively low. We tentatively associate the PAH emitting and heavily
dust/ice absorbed components with the diffuse emission region and the two
compact nuclei respectively identified by Soifer et al. (2002) in their higher
spatial resolution 10 micron study. Both the similarity of the absorbed
continuum with that of the embedded Galactic protostars and results of the dust
models imply that the embedded source(s) in Arp220 could be powered by, albeit
extremely dense, starburst activity. Due to the high extinction, it is not
possible with the available data to exclude that AGN(s) also contribute some or
all of the observed luminosity. In this case, however, the upper limit measured
for its hard X-ray emission would require Arp220 to be the most highly obscured
AGN known.Comment: 11 pages, 9 figures. Accepted for publication in A&A. Also available
at http://www.astro.rug.nl/~spoon/publications.htm
Gas morphology and energetics at the surface of PDRs: new insights with Herschel observations of NGC 7023
We investigate the physics and chemistry of the gas and dust in dense
photon-dominated regions (PDRs), along with their dependence on the
illuminating UV field. Using Herschel-HIFI observations, we study the gas
energetics in NGC 7023 in relation to the morphology of this nebula. NGC 7023
is the prototype of a PDR illuminated by a B2V star and is one of the key
targets of Herschel. Our approach consists in determining the energetics of the
region by combining the information carried by the mid-IR spectrum (extinction
by classical grains, emission from very small dust particles) with that of the
main gas coolant lines. In this letter, we discuss more specifically the
intensity and line profile of the 158 micron (1901 GHz) [CII] line measured by
HIFI and provide information on the emitting gas. We show that both the [CII]
emission and the mid-IR emission from polycyclic aromatic hydrocarbons (PAHs)
arise from the regions located in the transition zone between atomic and
molecular gas. Using the Meudon PDR code and a simple transfer model, we find
good agreement between the calculated and observed [CII] intensities. HIFI
observations of NGC 7023 provide the opportunity to constrain the energetics at
the surface of PDRs. Future work will include analysis of the main coolant line
[OI] and use of a new PDR model that includes PAH-related species.Comment: Accepted for publication in Astronomy and Astrophysics Letters
(Herschel HIFI special issue), 5 pages, 5 figure
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