486 research outputs found
Far-Ultraviolet & X-ray Observations of VV 114: Feedback in a Local Analog to Lyman Break Galaxies
We have analyzed FUSE, XMM, and Chandra observations of VV 114, a local
galaxy merger with strong similarities to typical high-redshift Lyman Break
Galaxies (LBGs). Diffuse thermal X-ray emission encompassing VV114 has been
observed by Chandra and XMM. This region of hot (kT~0.59 keV) gas has an
enhanced alpha to iron element ratio relative to solar abundances and follows
the same relation as typical starbursts between its properties (luminosity,
size, and temperature) and those of the starburst galaxy (star formation rate,
dust temperature, galaxy mass). These results are consistent with the X-ray gas
having been produced by shocks driven by a galactic superwind. The FUSE
observations of VV 114 show strong, broad interstellar absorption lines with a
pronounced blueshifted component(similar to what is seen in LBGs). This implies
an outflow of material moving at 300-400 km/s relative to VV 114. The
properties of the strong OVI absorption line are consistent with radiative
cooling at the interface between the hot outrushing gas seen in X-rays and the
cooler material seen in the other outflowing ions in the FUSE data. We show
that the wind in VV114 has not created a ``tunnel'' that enables more than a
small fraction (< few percent) of the ionizing photons from VV114 to escape
into the IGM. Taken together, these data provide a more complete physical basis
for understanding the outflows that seem to be generic in LBGs. This will lead
to improved insight into the role that such outflows play in the evolution of
galaxies and the inter-galactic medium.Comment: 33 pages, 13 figure
Discovery of a Nearby Low-Surface-Brightness Spiral Galaxy
During the course of a search for compact, isolated gas clouds moving with
anomalous velocities in or near our own Galaxy (Braun and Burton 1998 A&A, in
press), we have discovered, in the data of the Leiden/Dwingeloo survey
(Hartmann and Burton 1997, Atlas of Galactic Neutral Hydrogen, CUP) of Galactic
hydrogen, the HI signature of a large galaxy, moving at a recession velocity of
282 km/s, with respect to our Galaxy. Deep multicolor and spectroscopic optical
observations show the presence of star formation in scattered HII regions;
radio HI synthesis interferometry confirms that the galaxy is rich in HI and
has the rotation signature of a spiral galaxy; a submillimeter observation
failed to detect the CO molecule. The radio and optical evidence combined
suggest its classification as a low-surface-brightness spiral galaxy. It is
located in close spatial and kinematic proximity to the galaxy NGC 6946. The
newly-discovered galaxy, which we call Cepheus 1, is at a distance of about 6
Mpc. It is probably to be numbered amongst the nearest few LSB spirals.Comment: 13 page LaTeX, requires aastex, 4 GIF figures. Accepted for
publication in the AJ, January 199
Far Ultraviolet and H-alpha Imaging of Nearby Spirals: The OB Stellar Population in the Diffuse Ionized Gas
(Abridged) We have compared H-alpha and far ultraviolet (FUV) images of 10
nearby spirals, with the goal of understanding the contribution of field OB
stars to the ionization of the diffuse ionized gas (DIG) in spiral galaxies.
The FUV images were obtained by the Ultraviolet Imaging Telescope (UIT) and the
H-alpha images were obtained using various ground-based telescopes. In all of
the galaxies, the F_H-alpha/F_UIT flux ratio is lower in the DIG than in the
HII regions. This is likely an indication that the mean spectral type for OB
stars in the field is later than that in HII regions. Comparison of the
N_Lyc/L_UIT ratio with models of evolving stellar populations shows that the
stellar population in the DIG is consistent with either an older single burst
population or a steady state model with constant star formation and an initial
mass function (IMF) slope steeper than alpha=2.35. We compared the
F_H\alpha/F_UIT ratio in the DIG of these galaxies with that in M33. If the
mean spectral types of stars in HII regions and in the DIG are the same as in
M33, and the difference in extinction between DIG and HII regions is constant
among galaxies, then the analysis suggests that field stars are important
sources of ionization in most galaxies, and may be the dominant source in some
galaxies.Comment: 29 pages, 8 figures, 6 tables. Accepted for publication in Ap
Escape of Lyman alpha Emission in the Starburst Galaxy Mkn 357 - a Wind's Far Side
HST imaging and slitless spectroscopy are used to examine where the strong
Lyman alpha emission escapes from the interstellar medium in the starburst
galaxy Mkn 357. An H-alpha image shows that the ionized gas is mostly in a
global wind, rather than associated with the individual star-forming regions
seen in the optical and UV continuum. The Lyman alpha emission comes
predominantly from the northwest side of the wind structure spatially, and
shows a significant redshift relative to the optical lines. Both of these
properties are signatures of seeing the line photons backscattered from the far
side of a prolate or bipolar starburst wind, fitting both with escape
calculations and evidence for winds in high-redshift galaxies with net Lyman
alpha emission. Scattering is most important within this wind itself, rather
than involving a surrounding neutral medium, as shown by the decreasing
relative redshift of the line peak from 250 to 30 km/s between the center and
edge of the detected emission. The Lyman alpha emission exhibits strong
asymmetry in comparison with both the starlight and H-alpha structures. These
results add to the evidence that kinematics, rather than gas metallicity or
dust content, are the dominant effect in determining which galaxies have strong
Lyman alpha emission, and that powerful (and perhaps episodic) starbursts are
common among Lyman-break galaxies as well as those discovered from Lyman alpha
line emission.Comment: Accepted for Astron.J., April 200
The Contribution of Field OB Stars to the Ionization of the Diffuse Ionized Gas in M33
(Abridged) We present a study of the ionizing stars associated with the
diffuse ionized gas (DIG) and HII regions in the nearby spiral galaxy M33. We
compare our Schmidt H-alpha image to the far-ultraviolet (FUV, 1520A) image
from the Ultraviolet Imaging Telescope (UIT). The H-alpha/FUV ratio is higher
in HII regions than in the DIG, suggesting an older population of ionizing
stars in the DIG. When compared to models of evolving stellar populations, the
N(Lyc)/FUV ratio in HII regions is consistent with a young burst, while the DIG
ratio resembles an older burst population, or a steady state population built
up by constant star formation. The UIT data is complimented with archival FUV
and optical images of a small portion of the disk of M33 obtained with WFPC2 on
HST. Using the HST FUV and optical photometry, we assign spectral types to the
stars observed in DIG and HII regions. The photometry indicates that ionizing
stars are present in the DIG. We compare the predicted ionizing flux with the
amount required to produce the observed H-alpha emission, and find that field
OB stars in the HST images can account for 40% +/- 12% of the ionization of the
DIG, while the stars in HII regions can provide 107% +/- 26% of the H-alpha
luminosity of the HII regions. We do not find any correlation between leakage
of ionizing photons and H-alpha luminosity for the HII regions in these HST
fields. If stellar photons alone are responsible for ionizing the DIG, the
current results are consistent with no or few ionizing photons escaping from
the galaxy.Comment: 30 pages, 7 figures, accepted for publication in Ap
HST morphologies of local Lyman break galaxy analogs I: Evidence for starbursts triggered by merging
Heckman et al. (2005) used the Galaxy Evolution Explorer (GALEX) UV imaging
survey to show that there exists a rare population of nearby compact
UV-luminous galaxies (UVLGs) that closely resembles high redshift Lyman break
galaxies (LBGs). We present HST images in the UV, optical, and Ha, and
resimulate them at the depth and resolution of the GOODS/UDF fields to show
that the morphologies of UVLGs are also similar to those of LBGs. Our sample of
8 LBG analogs thus provides detailed insight into the connection between star
formation and LBG morphology. Faint tidal features or companions can be seen in
all of the rest-frame optical images, suggesting that the starbursts are the
result of a merger or interaction. The UV/optical light is dominated by
unresolved (~100-300 pc) super starburst regions (SSBs). A detailed comparison
with the galaxies Haro 11 and VV 114 at z=0.02 indicates that the SSBs
themselves consist of diffuse stars and (super) star clusters. The structural
features revealed by the new HST images occur on very small physical scales and
are thus not detectable in images of high redshift LBGs, except in a few cases
where they are magnified by gravitational lensing. We propose, therefore, that
LBGs are mergers of gas-rich, relatively low-mass (~10^10 Msun) systems, and
that the mergers trigger the formation of SSBs. If galaxies at high redshifts
are dominated by SSBs, then the faint end slope of the luminosity function is
predicted to have slope alpha~2. Our results are the most direct confirmation
to date of models that predict that the main mode of star formation in the
early universe was highly collisional.Comment: 32 pages, 15 figures. ApJ In pres
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